FN Thomson Reuters Web of Science™ VR 1.0 PT J AU Salvador-Reyes, LA Engene, N Paul, VJ Luesch, H AF Salvador-Reyes, Lilibeth A. Engene, Niclas Paul, Valerie J. Luesch, Hendrik TI Targeted Natural Products Discovery from Marine Cyanobacteria Using Combined Phylogenetic and Mass Spectrometric Evaluation SO JOURNAL OF NATURAL PRODUCTS LA English DT Article ID HISTONE DEACETYLASE INHIBITOR; SECONDARY METABOLITES; DOLASTATIN-10 ANALOG; MAXIMUM-LIKELIHOOD; SYMPLOCA-HYDNOIDES; DRUG DISCOVERY; SYMPLOSTATIN 1; LARGAZOLE; DEREPLICATION; BIODIVERSITY AB Combined phylogenetic and HPLC-MS-based natural products dereplication methods aimed at identifying cyanobacterial collections containing the potent cytotoxins largazole, dolastatin 10, and symplostatin 1 were developed. The profiling of the phylogeny, chemical space, and antiproliferative activity of cyanobacterial collections served to streamline the prioritization of samples for the discovery of new secondary metabolites. The dereplication methods highlighted the biosynthetic potential and combinatorial pharmacology employed by marine cyanobacteria. We found that largazole was always coproduced with dolastatin 10 or with symplostatin 1 and consequently tested combinations of these agents against colon cancer cells. Combinatorial regimens of largazole and dolastatin 10 aimed at curbing the growth of HCT116 cancer cells showed cooperative activity. C1 [Salvador-Reyes, Lilibeth A.; Luesch, Hendrik] Univ Florida, Dept Med Chem, Gainesville, FL 32610 USA. [Salvador-Reyes, Lilibeth A.] Univ Philippines, Coll Sci, Inst Marine Sci, Quezon City 1101, Philippines. [Engene, Niclas; Paul, Valerie J.] Smithsonian Marine Stn, Ft Pierce, FL 34949 USA. [Engene, Niclas] Florida Int Univ, Dept Biol Sci, Miami, FL 33199 USA. [Luesch, Hendrik] Univ Florida, CNPD3, Gainesville, FL 32610 USA. RP Luesch, H (reprint author), Univ Florida, Dept Med Chem, 1345 Ctr Dr, Gainesville, FL 32610 USA. EM luesch@cop.ufl.edu FU National Institutes of Health [R01CA172310]; University of the Philippines Research Dissemination Grant; Smithsonian Marine Science Network Postdoctoral Fellowships FX This research was supported by the National Institutes of Health grant R01CA172310. We thank the Florida Institute of Oceanography for providing the R/V Bellows and the National Park Service for granting the collection permits for Dry Tortugas National Park. We acknowledge the governments of Curacao and Bonaire, National Park Service, for permission to collect cyanobacterial specimens. We are grateful to E. Bartels at the Mote Tropical Marine Laboratory for assistance collecting specimens in the FL Keys. L.A.S.R was supported by a University of the Philippines Research Dissemination Grant. N.E. was supported by the Smithsonian Marine Science Network Postdoctoral Fellowships. This is SMSFP contribution no. 978. NR 44 TC 9 Z9 9 U1 2 U2 39 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0163-3864 EI 1520-6025 J9 J NAT PROD JI J. Nat. Prod. PD MAR PY 2015 VL 78 IS 3 BP 486 EP 492 DI 10.1021/np500931q PG 7 WC Plant Sciences; Chemistry, Medicinal; Pharmacology & Pharmacy SC Plant Sciences; Pharmacology & Pharmacy GA CE7PN UT WOS:000352033900019 PM 25635943 ER PT J AU Soares, AR Engene, N Gunasekera, SP Sneed, JM Paul, VJ AF Soares, Angelica R. Engene, Niclas Gunasekera, Sarath P. Sneed, Jennifer M. Paul, Valerie J. TI Carriebowlinol, an Antimicrobial Tetrahydroquinolinol from an Assemblage of Marine Cyanobacteria Containing a Novel Taxon SO JOURNAL OF NATURAL PRODUCTS LA English DT Article ID LYNGBYA-MAJUSCULA; PRODUCTS AB A combined biodiversity- and bioassay-guided natural products discovery approach was used to explore new groups of marine cyanobacteria for novel secondary metabolites with ecologically relevant bioactivities. Phylogenetic analysis of cyanobacterial collections from Belize revealed a new taxon not previously well explored for natural products. The new alkaloid 5-hydroxy-4-(chloromethyl)-5,6,7,8-tetrahydroquinoline (1), named carriebowlinol, and the known compound lyngbic acid (2) were isolated from a nonpolar extract and identified by NMR and MS techniques. Compounds 1 and 2 inhibited the growth of pathogenic and saprophytic marine fungi, and 1 inhibited the growth of marine bacteria, suggesting an antimicrobial ecological function. C1 [Soares, Angelica R.; Engene, Niclas; Gunasekera, Sarath P.; Sneed, Jennifer M.; Paul, Valerie J.] Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL 34949 USA. [Soares, Angelica R.] Univ Fed Rio de Janeiro, Nucleo Ecol & Desenvolvimento Socioambiental Maca, GPNOA, BR-27910970 Macae, RJ, Brazil. [Engene, Niclas] Florida Int Univ, Dept Biol Sci, Miami, FL 33199 USA. RP Soares, AR (reprint author), Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL 34949 USA. EM angelica@iq.ufrj.br FU Smithsonian Institution Competitive Grants Program for Science; Marine Science Network Postdoctoral Fellowship; Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPq) FX This research was supported by the Smithsonian Institution Competitive Grants Program for Science to V.J.P. and J.M.S. and a Marine Science Network Postdoctoral Fellowship to N.E. We are also grateful to the Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPq) for a postdoctoral fellowship to A.R.S. We thank S. Harrison and L. J. Houk for assistance with the marine antibacterial assays, the Harbor Branch Oceanographic Institute at Florida Atlantic University spectroscopy facility for 600 MHz NMR spectrometer time and use of their polarimeter, and the Florida Atlantic University, Boca Raton Campus, for use of their polarimeter and infrared spectrometer. We also thank J. Piraino and H. Reichardt for general lab assistance, and H. M. Duarte for his comments. The HRMS analysis was performed at the UCR mass spectrometry facility, Department of Chemistry, University of California at Riverside. This is contribution no. 967 from the Smithsonian Marine Station at Fort Pierce and no. 969 from the CCRE program. NR 20 TC 4 Z9 4 U1 4 U2 17 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0163-3864 EI 1520-6025 J9 J NAT PROD JI J. Nat. Prod. PD MAR PY 2015 VL 78 IS 3 BP 534 EP 538 DI 10.1021/np500598x PG 5 WC Plant Sciences; Chemistry, Medicinal; Pharmacology & Pharmacy SC Plant Sciences; Pharmacology & Pharmacy GA CE7PN UT WOS:000352033900025 PM 25536090 ER PT J AU Soreng, RJ Peterson, PM Romaschenko, K Davidse, G Zuloaga, FO Judziewicz, EJ Filgueiras, TS Davis, JI Morrone, O AF Soreng, Robert J. Peterson, Paul M. Romaschenko, Konstantin Davidse, Gerrit Zuloaga, Fernando O. Judziewicz, Emmet J. Filgueiras, Tarciso S. Davis, Jerrold I. Morrone, Osvaldo TI A worldwide phylogenetic classification of the Poaceae (Gramineae) SO JOURNAL OF SYSTEMATICS AND EVOLUTION LA English DT Review DE classification; DNA; Gramineae; grasses; morphology; phylogeny; Poaceae; subfamily; subtribe; tribe ID GRASS FAMILY POACEAE; RESTRICTION SITE VARIATION; BRIZA COMPLEX POACEAE; CHLOROPLAST TRNL-F; MOLECULAR PHYLOGENY; SEQUENCE DATA; CHLORIDOIDEAE POACEAE; PANICEAE POACEAE; DNA-SEQUENCES; EVOLUTIONARY RELATIONSHIPS AB Based on recent molecular and morphological studies we present a modern worldwide phylogenetic classification of the +/- 12074 grasses and place the 771 grass genera into 12 subfamilies (Anomochlooideae, Aristidoideae, Arundinoideae, Bambusoideae, Chloridoideae, Danthonioideae, Micraioideae, Oryzoideae, Panicoideae, Pharoideae, Puelioideae, and Pooideae), 6 supertribes (Andropogonodae, Arundinarodae, Bambusodae, Panicodae, Poodae, Triticodae), 51 tribes (Ampelodesmeae, Andropogoneae, Anomochloeae, Aristideae, Arundinarieae, Arundineae, Arundinelleae, Atractocarpeae, Bambuseae, Brachyelytreae, Brachypodieae, Bromeae, Brylkinieae, Centotheceae, Centropodieae, Chasmanthieae, Cynodonteae, Cyperochloeae, Danthonieae, Diarrheneae, Ehrharteae, Eragrostideae, Eriachneae, Guaduellieae, Gynerieae, Hubbardieae, Isachneae, Littledaleeae, Lygeeae, Meliceae, Micraireae, Molinieae, Nardeae, Olyreae, Oryzeae, Paniceae, Paspaleae, Phaenospermateae, Phareae, Phyllorachideae, Poeae, Steyermarkochloeae, Stipeae, Streptochaeteae, Streptogyneae, Thysanolaeneae, Triraphideae, Tristachyideae, Triticeae, Zeugiteae, and Zoysieae), and 80 subtribes (Aeluropodinae, Agrostidinae, Airinae, Ammochloinae, Andropogoninae, Anthephorinae, Anthistiriinae, Anthoxanthinae, Arthraxoninae, Arthropogoninae, Arthrostylidiinae, Arundinariinae, Aveninae, Bambusinae, Boivinellinae, Boutelouinae, Brizinae, Buergersiochloinae, Calothecinae, Cenchrinae, Chionachninae, Chusqueinae, Coicinae, Coleanthinae, Cotteinae, Cteniinae, Cynosurinae, Dactylidinae, Dichantheliinae, Dimeriinae, Duthieinae, Eleusininae, Eragrostidinae, Farragininae, Germainiinae, Gouiniinae, Guaduinae, Gymnopogoninae, Hickeliinae, Hilariinae, Holcinae, Hordeinae, Ischaeminae, Loliinae, Melinidinae, Melocanninae, Miliinae, Monanthochloinae, Muhlenbergiinae, Neurachninae, Olyrinae, Orcuttiinae, Oryzinae, Otachyriinae, Panicinae, Pappophorinae, Parapholiinae, Parianinae, Paspalinae, Perotidinae, Phalaridinae, Poinae, Racemobambosinae, Rottboelliinae, Saccharinae, Scleropogoninae, Scolochloinae, Sesleriinae, Sorghinae, Sporobolinae, Torreyochloinae, Traginae, Trichoneurinae, Triodiinae, Tripogoninae, Tripsacinae, Triticinae, Unioliinae, Zizaniinae, and Zoysiinae). In addition, we include a radial tree illustrating the hierarchical relationships among the subtribes, tribes, and subfamilies. We use the subfamilial name, Oryzoideae, over Ehrhartoideae because the latter was initially published as a misplaced rank, and we circumscribe Molinieae to include 13 Arundinoideae genera. The subtribe Calothecinae is newly described and the tribe Littledaleeae is new at that rank. C1 [Soreng, Robert J.; Peterson, Paul M.; Romaschenko, Konstantin] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA. [Davidse, Gerrit] Missouri Bot Garden, St Louis, MO 63166 USA. [Zuloaga, Fernando O.; Morrone, Osvaldo] Inst Bot Darwin, Buenos Aires, DF, Argentina. [Judziewicz, Emmet J.] Univ Wisconsin, Dept Biol, Stevens Point, WI 54481 USA. [Judziewicz, Emmet J.] Univ Wisconsin, Museum Nat Hist, Stevens Point, WI 54481 USA. [Filgueiras, Tarciso S.] Secretaria Meio Ambiente, Inst Bot, BR-04301902 Sao Paulo, Brazil. [Davis, Jerrold I.] Cornell Univ, Dept Plant Biol, Ithaca, NY 14853 USA. RP Peterson, PM (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA. EM peterson@si.edu RI Romaschenko, Konstantin/K-3096-2014 OI Romaschenko, Konstantin/0000-0002-7248-4193 FU National Geographic Society Committee for Research and Exploration [8848-10, 8087-06]; Smithsonian Institution's Restricted Endowments Fund; Scholarly Studies Program; Atherton Seidell Foundation; Biodiversity Surveys and Inventories Program; Laboratory of Analytical Biology; Missouri Botanical Garden for supporting Tropicos; United States Department of Agriculture FX We thank the National Geographic Society Committee for Research and Exploration (Grant Nos. 8848-10, 8087-06) for field and laboratory support, the Smithsonian Institution's Restricted Endowments Fund, the Scholarly Studies Program, Research Opportunities, Atherton Seidell Foundation, Biodiversity Surveys and Inventories Program, Small Grants Program, the Laboratory of Analytical Biology, the Missouri Botanical Garden for supporting Tropicos, and the United States Department of Agriculture, all for financial support. We would also like to acknowledge Lynn J. Gillespie and Jeffery M. Saarela for discussions pertinent to the manuscript, and Sun Hang and Jimmy K. Triplett for providing helpful comments on the manuscript. NR 114 TC 68 Z9 72 U1 16 U2 67 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1674-4918 EI 1759-6831 J9 J SYST EVOL JI J. Syst. Evol. PD MAR PY 2015 VL 53 IS 2 BP 117 EP 137 DI 10.1111/jse.12150 PG 21 WC Plant Sciences SC Plant Sciences GA CE2XT UT WOS:000351686000001 ER PT J AU Soreng, RJ Gillespie, LJ Koba, H Boudko, E Bull, RD AF Soreng, Robert J. Gillespie, Lynn J. Koba, Hidehisa Boudko, Ekaterina Bull, Roger D. TI Molecular and morphological evidence for a new grass genus, Dupontiopsis (Poaceae tribe Poeae subtribe Poinae s.l.), endemic to alpine Japan, and implications for the reticulate origin of Dupontia and Arctophila within Poinae s.l. SO JOURNAL OF SYSTEMATICS AND EVOLUTION LA English DT Review DE Arctophila; DNA; Dupontia; Japan; leaf anatomy; phylogeny; Poa; polyploidy; reticulate evolution; taxonomy ID CHLOROPLAST DNA-SEQUENCES; CHROMOSOME-NUMBERS; POA POACEAE; PHYLOGENETIC-RELATIONSHIPS; NORTH-AMERICA; TAXONOMIC IMPLICATIONS; DISSANTHELIUM POACEAE; CLASSIFICATION; POOIDEAE; NUCLEAR AB Phylogenetic analyses within Poaceae tribe Poeae subtribes Puccinellinae (=Coleanthinae), Phleinae, Poinae s.l. (including Alopecurinae), and Miliinae (PPAM clade), revealed that one species formerly placed in Poa represents a new monotypic genus belonging to subtribe Poinae s.l., Dupontiopsis gen. nov., D. hayachinensis comb. nov. (based on Poa hayachinensis), endemic to wet, gravelly, serpentine, alpine habitats in northern Japan. This genus forms a strongly supported clade (DAD) with two circumarctic Poinae genera, Arctophila and Dupontia, in phylogenetic analyses of plastid and nuclear ribosomal DNA sequence data. Both morphology and DNA sequence analyses provide support for D. hayachinensis as a lineage distinct from either Arctophila or Dupontia, with moderate DNA support for a position as sister to these two genera. Dupontiopsis resembles these other monotypic genera in its several-flowered spikelets, lemmas usually 3-nerved, with frequently awned attenuate scarious apices (as in Dupontia) and calluses with a crown of hairs around the base of the lemma, but differs in its keeled lemmas, scabrous palea keels, glumes shorter than the first lemma. Our investigation suggests that the most recent shared ancestor of the DAD clade evolved from a single hybridization event, as a hexaploid, probably in western Beringia. The probable parentage of the ancestor is considered to be within the Poinae-Alopecurinae clade excluding Poa. We provide evidence for possible secondary hybridization and introgression of duodecaploid Dupontia fisheri with Puccinellia. A key to perennial genera of PPAM with hairy calluses, and a supplemental table of morphological characters in the genera accepted in PPAM are provided. C1 [Soreng, Robert J.] Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, Washington, DC 20013 USA. [Gillespie, Lynn J.; Boudko, Ekaterina; Bull, Roger D.] Canadian Museum Nat, Res & Collect, Ottawa, ON 3443, Canada. [Koba, Hidehisa] JF Oberlin Univ, Div Nat Sci, Machida, Tokyo 1940294, Japan. RP Soreng, RJ (reprint author), Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, Washington, DC 20013 USA. EM sorengr@si.edu FU Smithsonian Institution; Canadian Museum of Nature FX Our thanks are extended to Marina Olonova, Evren Cabi, Musa Dogan, Laurie Consaul, Doug Johnson, Paul Peterson, Surrey Jacobs, Michel Paradis, Alicia Alonso, the curators of CAN, K, TI, US, for their various contributions of specimens, assistance with field or laboratory work, or loans; Stephen Darbyshire for permission to use Agriculture and Agri-Food Canada photos; Anne Brysting for sharing unpublished Dupontia fisheri cloned ITS sequences; Konstantin Romaschenko for assistance with and discussion of MrBayes; Jerrold Davis for discussions of analytical issues related to Parsimony and BI analyses; Alice Tangerini for assistance with images; Stephen Darbyshire, Lynn Clark, and anonymous reviewers and editors for helpful comments on the manuscript; the Smithsonian Institution for support of RJS's research activities; and the Canadian Museum of Nature for financial assistance with the molecular research. With regard to this publication we have no conflicts of interest. NR 100 TC 2 Z9 2 U1 1 U2 8 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1674-4918 EI 1759-6831 J9 J SYST EVOL JI J. Syst. Evol. PD MAR PY 2015 VL 53 IS 2 BP 138 EP 162 DI 10.1111/jse.12146 PG 25 WC Plant Sciences SC Plant Sciences GA CE2XT UT WOS:000351686000002 ER PT J AU Bozarth, CA Gardner, B Rockwood, LL Maldonado, JE AF Bozarth, Christine A. Gardner, Beth Rockwood, Larry L. Maldonado, Jesus E. TI Using Fecal DNA and Spatial Capture-Recapture to Characterize a Recent Coyote Colonization SO NORTHEASTERN NATURALIST LA English DT Article ID ESTIMATING POPULATION-SIZE; VULPES-MACROTIS-MUTICA; WOLF CANIS-LUPUS; HOME-RANGE; HABITAT USE; URBAN-ENVIRONMENT; ELUSIVE ANIMALS; WOLVERINE POPULATION; SOUTHERN CALIFORNIA; MAXIMUM-LIKELIHOOD AB The arrival of a novel predator in an ecosystem necessitates many wildlife-management decisions that should be based on sound demographic data. Canis latrans (Coyote) has experienced a dramatic range expansion across North America since the early 19th century, completing its colonization of the continental US in the mid-Atlantic region over the past 20 years. Their arrival in the suburbs of Washington, DC, has generated much public attention, and demonstrated a need for demographic information about this species. To address the challenges of surveying an elusive animal, we used fecal DNA to describe the population genetics and demographics of a newly colonized Coyote population at Marine Corps Base Quantico (MCBQ) in northern Virginia. We collected 331 scats over a period of 2 years at MCBQ, resulting in identification of 23 unique individual Coyotes and 41 total Coyote captures that were analyzed using spatial capture-recapture models. We found evidence of colonization by multiple genetic lineages and a low population density of 0.047 individuals/km(2). Importantly, this study incorporates a new class of models on individual animals identified by genotype data derived from fecal DNA and demonstrates the utility of these models in surveying elusive animals. C1 [Bozarth, Christine A.; Rockwood, Larry L.; Maldonado, Jesus E.] Smithsonian Conservat Biol Inst, Ctr Conservat & Evolutionary Genet, Washington, DC 20008 USA. [Bozarth, Christine A.; Rockwood, Larry L.; Maldonado, Jesus E.] George Mason Univ, Dept Environm Sci & Policy, Fairfax, VA 22030 USA. [Gardner, Beth] N Carolina State Univ, Dept Forestry & Environm Resources, Fisheries Wildlife & Conservat Biol Program, Raleigh, NC 27695 USA. [Maldonado, Jesus E.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20013 USA. RP Bozarth, CA (reprint author), Smithsonian Conservat Biol Inst, Ctr Conservat & Evolutionary Genet, Washington, DC 20008 USA. EM cbozarth@nvcc.edu FU Naval Facilities Engineering Command Washington [N40080-08-LTC-0001]; Smithsonian Conservation Biology Institute's Center for Conservation and Evolutionary Genetics FX Funding was provided by Naval Facilities Engineering Command Washington Cooperative Agreement N40080-08-LTC-0001 for Coyote Population Study at MCB Quantico and the Smithsonian Conservation Biology Institute's Center for Conservation and Evolutionary Genetics. We thank T. Stamps, C. Himmelberger, N. McInerney, T. Wilbert, K. Robinson, C. Garcia, L. Lakeman, M. Tsuchiya, and C. Edwards for samples, assistance, and guidance. NR 97 TC 2 Z9 2 U1 8 U2 47 PU HUMBOLDT FIELD RESEARCH INST PI STEUBEN PA PO BOX 9, STEUBEN, ME 04680-0009 USA SN 1092-6194 EI 1938-5307 J9 NORTHEAST NAT JI Northeast. Nat PD MAR PY 2015 VL 22 IS 1 BP 144 EP 162 DI 10.1656/045.022.0124 PG 19 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA CE1CZ UT WOS:000351550900013 ER PT J AU Cowan, NB Greene, T Angerhausen, D Batalha, NE Clampin, M Colon, K Crossfield, IJM Fortney, JJ Gaudi, BS Harrington, J Iro, N Lillie, CF Linsky, JL Lopez-Morales, M Mandell, AM Stevenson, KB AF Cowan, N. B. Greene, T. Angerhausen, D. Batalha, N. E. Clampin, M. Colon, K. Crossfield, I. J. M. Fortney, J. J. Gaudi, B. S. Harrington, J. Iro, N. Lillie, C. F. Linsky, J. L. Lopez-Morales, M. Mandell, A. M. Stevenson, K. B. CA ExoPAG SAG-10 TI Characterizing Transiting Planet Atmospheres through 2025 SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID SUPER-EARTH EXOPLANET; INFRARED TRANSMISSION SPECTROSCOPY; SYSTEMATIC RETRIEVAL ANALYSIS; HUBBLE-SPACE-TELESCOPE; HD 189733B; EXTRASOLAR PLANET; SECONDARY-ECLIPSE; GJ 1214B; MU-M; HOT JUPITERS AB The discovery of planets around other stars is revolutionizing our notions of planet formation and is poised to do the same for planetary climate. Studying transiting planets is complementary to eventual studies of directly imaged planets: (1)we can readily measure the mass and radius of transiting planets, linking atmospheric properties to bulk composition and formation, (2)many transiting planets are strongly irradiated and exhibit novel atmospheric physics, and (3)the most common temperate terrestrial planets orbit close to red dwarf stars and are difficult to image directly. We have only been able to comprehensively characterize the atmospheres of a handful of transiting planets, because most orbit faint stars. The Transiting Exoplanet Survey Satellite (TESS) will discover transiting planets orbiting the brightest stars, enabling, in principle, an atmospheric survey of 10(2)-10(3) bright hot Jupiters and warm sub-Neptunes. Uniform observations of such a statistically significant sample would provide leverage to understandand learn fromthe diversity of short-period planets, and would identify the minority of truly special planets worthy of more intensive follow-up. We argue that the best way to maximize the scientific returns of TESS is to adopt a triage approach. A space mission consisting of a approximate to 1m telescope with an optical-NIR spectrograph could measure molecular absorption for nonterrestrial planets discovered by TESS, as well as eclipses and phase variations for the hottest jovians. Such a mission could observe up to 10(3) transits per year, thus enabling it to survey a large fraction of the bright (J<11) hot-Jupiters and warm sub-Neptunes TESS is expected to find. The James Webb Space Telescope (JWST) could be used to perform detailed atmospheric characterization of the most interesting transiting targets (transit, eclipse, andwhen possiblephase-resolved spectroscopy). TESS is also expected to discover a few temperate terrestrial planets transiting nearby M-Dwarfs. Characterizing these worlds will be time-intensive: JWST will need months to provide tantalizing constraints on the presence of an atmosphere, planetary rotational state, clouds, and greenhouse gases. Future flagship missions should be designed to provide better constraints on the habitability of M-Dwarf temperate terrestrial planets. C1 [Cowan, N. B.] Amherst Coll, Amherst, MA 01002 USA. [Greene, T.; Mandell, A. M.] NASA, Ames Res Ctr, Mountain View, CA 94035 USA. [Angerhausen, D.; Clampin, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Batalha, N. E.] Penn State Univ, State Coll, PA 16801 USA. [Colon, K.] Lehigh Univ, Bethlehem, PA 18015 USA. [Crossfield, I. J. M.] Univ Arizona, Tucson, AZ 85721 USA. [Fortney, J. J.] Univ Calif Santa Cruz, Santa Cruz, CA 95064 USA. [Gaudi, B. S.] Ohio State Univ, Columbus, OH 43210 USA. [Harrington, J.] Univ Cent Florida, Orlando, FL 32816 USA. [Iro, N.] Univ Hamburg, Hamburg, Germany. [Lillie, C. F.] Lillie Consulting, Houston, TX 77008 USA. [Linsky, J. L.] Univ Colorado, Boulder, CO 80309 USA. [Lopez-Morales, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Stevenson, K. B.] Univ Chicago, Chicago, IL 60637 USA. RP Cowan, NB (reprint author), Amherst Coll, Amherst, MA 01002 USA. EM ncowan@amherst.edu RI Harrington, Joseph/E-6250-2011; OI Harrington, Joseph/0000-0002-8955-8531 NR 136 TC 17 Z9 17 U1 1 U2 16 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6280 EI 1538-3873 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD MAR PY 2015 VL 127 IS 949 BP 311 EP 327 DI 10.1086/680855 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CE4BC UT WOS:000351774600008 ER PT J AU Rahman, IA Stewart, SE Zamora, S AF Rahman, Imran A. Stewart, Sarah E. Zamora, Samuel TI The youngest ctenocystoids from the Upper Ordovician of the United Kingdom and the evolution of the bilateral body plan in echinoderms SO ACTA PALAEONTOLOGICA POLONICA LA English DT Editorial Material DE Echinodermata; Ctenocystoidea; evolution; bilateral symmetry; body plans; Ordovician; United Kingdom ID PALEOZOIC ECHINODERMS; DIVERSIFICATION; PHYLOGENY; SYMMETRY; FOSSILS; FAUNAS AB During the early Palaeozoic, echinoderm body plans were much more diverse than they are today, displaying four distinct types of symmetry. This included the bilateral ctenocystoids, which were long thought to be restricted to the Cambrian. Here, we describe a new species of ctenocystoid from the Upper Ordovician of Scotland (Conollia sporranoides sp. nov.). This allows us to revise the genus Conollia, which was previously based on a single poorly-known species from the Upper Ordovician of Wales (Conollia staffordi). Both these species are characterized by a unique morphology consisting of an elongate-ovoid body covered in spines, which clearly distinguishes them from their better-known Cambrian relatives; they are interpreted as infaunal or semi-infaunal burrowers from deep-water environments. This indicates that the ctenocystoid body plan was not fixed early in the evolution of the group, and they most likely modified their structure as an adaptation to a new mode of life in the Ordovician. C1 [Rahman, Imran A.] Univ Bristol, Sch Earth Sci, Bristol BS8 1TQ, Avon, England. [Stewart, Sarah E.] Natl Museum Scotland, Dept Nat Sci, Edinburgh EH1 1JF, Midlothian, Scotland. [Zamora, Samuel] Smithsonian Inst, Dept Paleobiol, Natl Museum Nat Hist, Washington, DC 20013 USA. [Zamora, Samuel] Inst Geol & Minero Espana, Museo Geominero, Zaragoza 50006, Spain. RP Rahman, IA (reprint author), Univ Bristol, Sch Earth Sci, Life Sci Bldg,24 Tyndall Ave, Bristol BS8 1TQ, Avon, England. EM imran.rahman@bristol.ac.uk; sarah.stewart@nms.ac.uk; samuel@unizar.es RI Rahman, Imran/F-4224-2012 OI Rahman, Imran/0000-0001-6598-6534 NR 40 TC 0 Z9 0 U1 0 U2 3 PU INST PALEOBIOLOGII PAN PI WARSAW PA UL TWARDA 51/55, 00-818 WARSAW, POLAND SN 0567-7920 EI 1732-2421 J9 ACTA PALAEONTOL POL JI Acta Palaeontol. Pol. PD MAR PY 2015 VL 60 IS 1 BP 39 EP 48 DI 10.4202/app.00048.2013 PG 10 WC Paleontology SC Paleontology GA CD4UY UT WOS:000351081500004 ER PT J AU Roper, CFE Judkins, H Voss, NA Shea, E Dawe, E Ingrao, D Rothman, PL Roper, IH AF Roper, Clyde F. E. Judkins, Heather Voss, Nancy A. Shea, Elizabeth Dawe, Earl Ingrao, Debi Rothman, Paula L. Roper, Ingrid H. TI A compilation of recent records of the giant squid, Architeuthis dux (Steenstrup, 1857) (Cephalopoda) from the Western North Atlantic Ocean, Newfoundland to the Gulf of Mexico SO AMERICAN MALACOLOGICAL BULLETIN LA English DT Article DE cephalopod taxonomy; Mollusca ID GENUS ARCHITEUTHIS; WATERS; PREY AB This report provides information on 28 specimens of the giant squid, Architeuthis dux (Steenstrup 1857), discovered in the western North Atlantic Ocean between Newfoundland and the Gulf of Mexico. Some specimens have been reported in the press or popular literature, but others are recorded herein for the first time. Nominal architeuthid species are provided as well as tables listing repositories of types of nominal species, and repositories of non-type specimens from the study area. An extensive list of references of pertinent regional literature is provided, and recommendations for fixation and preservation are described. C1 [Roper, Clyde F. E.; Rothman, Paula L.; Roper, Ingrid H.] Smithsonian Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20013 USA. [Judkins, Heather] Univ S Florida, Dept Sci Biol, St Petersburg, FL 33701 USA. [Voss, Nancy A.] Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, Miami, FL 33149 USA. [Shea, Elizabeth] Delaware Museum Nat Hist, Dept Mollusks, Wilmington, DE 19807 USA. [Dawe, Earl] Fisheries & Oceans Canada, St John, NF A1C 5X1, Canada. [Ingrao, Debi] Mote Marine Lab, Sarasota, FL 34236 USA. RP Judkins, H (reprint author), Univ S Florida, Dept Sci Biol, 140 7th Ave S, St Petersburg, FL 33701 USA. EM Judkins@mail.usf.edu FU Mote Marine Laboratory FX The authors gratefully recognize the contributions of Michael J. Sweeney and Richard E. Young in the compilation of the nominal taxa tables. Michael Vecchione was instrumental in documenting specimens, as well as providing significant suggestions for revision of this manuscript. Glen Loates, a noted Canadian wildlife artist and Architeuthis enthusiast, was instrumental in providing the illustrations for this manuscript which the authors gratefully acknowledge. The authors also recognize Lisa Greene at the Bermuda Aquarium Museum and Zoo for her contributions to the specimen list. The first author is particularly grateful to Joerg Loetze, Director, Eagle Hill Institute, Steuben, Maine, for the opportunity to work and write in a retreat-like, academic setting. H. Judkins would like to acknowledge the University of South Florida St. Petersburg, Department of Biological Sciences and, in particular, Deby Cassill for her assistance in documenting these important specimens. D. Ingrao would like to thank the Mote Marine Laboratory volunteers and staff for their time and financial support. NR 84 TC 1 Z9 1 U1 7 U2 18 PU AMER MALACOLOGICAL SOC, INC PI WILMINGTON PA DELAWARE MUSEUM NATURAL HISTORY, BOX 3937, WILMINGTON, DE 19807-0937 USA SN 0740-2783 EI 2162-2698 J9 AM MALACOL BULL JI Am. Malacol. Bull. PD MAR PY 2015 VL 33 IS 1 BP 78 EP 88 PG 11 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA CD9KK UT WOS:000351417000008 ER PT J AU Kim, TW Christy, JH AF Kim, Tae Won Christy, John H. TI A mechanism for visual orientation may facilitate courtship in a fiddler crab SO ANIMAL BEHAVIOUR LA English DT Article DE courtship; fiddler crab; hood; orientation errors; sexual selection; visual beacon ID UCA-LACTEA; SEXUAL SELECTION; MATE CHOICE; FEMALE PREFERENCE; FOOD AVAILABILITY; MALE COMPETITION; PILLAR FUNCTION; SENSORY TRAP; OCYPODIDAE; BEEBEI AB Some social signals are sexually selected both by female mating preferences and by male-male competition for mates. Studies of the behavioural mechanisms that mediate responses to these signals provide insight into how sexual selection operates. Courting male fiddler crabs, Uca terpsichores, sometimes build large sand structures called hoods at the openings to their burrows. Hoods attract females to males' burrows for mating because they elicit landmark orientation, a behaviour that is selected by predation. Males also orient visually to their own hoods when errors are introduced experimentally into their nonvisual mechanism for path integration. These errors occur naturally when males move far from their burrows to court females or fight neighbours. Here we explored whether courting males also use hoods as visual beacons to the location of their burrow. Crabs that rely on path integration to orient to their burrow keep their lateral axis closely aligned with the bearing home. We therefore measured and compared the distances males moved from their burrows and the maximum deviations between males' body axes and home bearings for males that did and did not build hoods, males that had their hood removed and males that had a hood added to their burrow. Males with hoods did not range further from their burrows than those without hoods, but they exhibited greater maximum deviations between their body axes and the bearings to their burrows. Hoods may facilitate courtship by allowing males to move more freely than when they rely on nonvisual path integration alone. (C) 2014 The Authors. Published on behalf of The Association for the Study of Animal Behaviour by Elsevier Ltd. C1 [Kim, Tae Won] Korea Inst Ocean Sci & Technol, Ansan 426744, South Korea. [Kim, Tae Won] Univ Sci & Technol, Taejon, South Korea. [Christy, John H.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Kim, TW (reprint author), Korea Inst Ocean Sci & Technol, Haeanro 787, Ansan 426744, South Korea. EM ktwon@kiost.ac FU KIOST major project awards [PE99195, PE99247]; WWF YSESP - Panasonic Co. [PI55710] FX We thank the Smithsonian Tropical Research Institute, the Naos Laboratories and the Culebra Nature Centre for logistical support and are grateful to Seung Hee Gong for helping with the video analysis. This research was supported by KIOST major project awards (PE99195 and PE99247) and WWF YSESP (PI55710) funded by Panasonic Co. NR 37 TC 2 Z9 2 U1 3 U2 28 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 2015 VL 101 BP 61 EP 66 DI 10.1016/j.anbehav.2014.12.007 PG 6 WC Behavioral Sciences; Zoology SC Behavioral Sciences; Zoology GA CD3YR UT WOS:000351020200009 ER PT J AU Kuhn, AW Tedesco, M Laughinghouse, HD Flores, FC da Silvad, CD do Canto-Dorow, TS Tedesco, SB AF Kuhn, Andrielle Wouters Tedesco, Marlia Laughinghouse, Haywood Dail Flores, Fernanda Cramer da Silvad, Cristiane de Bona do Canto-Dorow, Thais Scotti Tedesco, Solange Bosio TI Mutagenic and antimutagenic effects of Eugenia uniflora L. by the Allium cepa L. test SO CARYOLOGIA LA English DT Article DE antimutagenic; antiproliferative; cell cycle; infusions; pitangueira ID MEDICINAL-PLANTS; CELL-CYCLE; INFUSIONS; ASTERACEAE; MYRTACEAE; EXTRACTS AB Eugenia uniflora (Surinam cherry tree) is an important species in traditional medicine and is used to decrease blood pressure and prevent heartburn, bronchitis, colic and stomachaches. The tealeaves have antirheumatic, anti-dysenteric, and febrifuge properties and are used to treat diabetes. This study aimed to assess the antiproliferative, mutagenic and antimutagenic effects of the leaves and fruits of E. uniflora through the Allium cepa test. The infusions were prepared using dried leaves (6.l(-1) and 24 gl(-1)) and the oil extraction was undertaken using hydrolyzation (0.25%, in ethanol). For juice preparation, fruit pulp with and without seeds was used. Allium cepa root tips were used for slide preparation following the squashing technique. Analysis of 500 cells for each bulb was undertaken, 250 of each root, summing 2500 cells per treatment, a total of 17,500 and 10,000 cells in the first and second experiments, respectively. The mitotic index was calculated and statistical analyses were performed. We found that the aqueous extract and oil of E. uniflora has mutagenic activity at low concentrations and the extract at a higher than average concentration can be considered antimutagenic. Furthermore, both juice extracts with and without seeds have anti-proliferative capacity. C1 [Kuhn, Andrielle Wouters; Tedesco, Marlia] Univ Fed Santa Maria, Ctr Ciencias Nat & Exatas, Dept Biol, Programa Posgrad Agrobiol, BR-97119900 Santa Maria, RS, Brazil. [Laughinghouse, Haywood Dail] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20560 USA. [Laughinghouse, Haywood Dail] Smith Coll, Dept Biol, Northampton, MA 01063 USA. [Flores, Fernanda Cramer; da Silvad, Cristiane de Bona] Univ Fed Santa Maria, Ctr Ciencias Saude, Programa Posgrad Ciencias Farmaceut, BR-97119900 Santa Maria, RS, Brazil. [do Canto-Dorow, Thais Scotti; Tedesco, Solange Bosio] Univ Fed Santa Maria, Ctr Ciencias Nat & Exatas, Dept Biol, Programa Posgrad Agrobiol, BR-97119900 Santa Maria, RS, Brazil. RP Laughinghouse, HD (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20560 USA. EM laughinghouseh@gmail.com RI Laughinghouse, Haywood/M-5836-2016 OI Laughinghouse, Haywood/0000-0003-1018-6948 FU Fundacao de Amparo a Pesquisa do Estado do Rio Grande do Sul (FAPERGS/CAPES); Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPq) FX This study was supported by Fundacao de Amparo a Pesquisa do Estado do Rio Grande do Sul (FAPERGS/CAPES) and Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPq) to whom we express our gratitude. NR 33 TC 1 Z9 1 U1 0 U2 7 PU UNIV FLORENCE BOTANY INST PI FLORENCE PA VIA LAMARMORA 4, 50121 FLORENCE, ITALY SN 0008-7114 EI 2165-5391 J9 CARYOLOGIA JI Caryologia PD MAR PY 2015 VL 68 IS 1 BP 25 EP 30 DI 10.1080/00087114.2014.998525 PG 6 WC Plant Sciences; Genetics & Heredity SC Plant Sciences; Genetics & Heredity GA CD9IU UT WOS:000351412600005 ER PT J AU Aiello, A AF Aiello, Annette TI ONCIDERES SERVILLE (COLEOPTERA: CERAMBYCIDAE) KEY TO TOO FEW: 34 SPECIES LOST SO COLEOPTERISTS BULLETIN LA English DT Editorial Material C1 Smithsonian Trop Res Inst, Panama City, Panama. RP Aiello, A (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Panama City, Panama. EM aielloa@si.edu NR 0 TC 0 Z9 1 U1 0 U2 2 PU COLEOPTERISTS SOC PI ATHENS PA UNIV GEORGIA, 413 BIOLOGICAL SCIENCES BUILDING, ATHENS, GA 30602-2603 USA SN 0010-065X EI 1938-4394 J9 COLEOPTS BULL JI Coleopt. Bull. PD MAR PY 2015 VL 69 IS 1 BP 60 EP 60 PG 1 WC Entomology SC Entomology GA CE0MH UT WOS:000351497700006 ER PT J AU Murphy, SJ Audino, LD Whitacre, J Eck, JL Wenzel, JW Queenborough, SA Comita, LS AF Murphy, Stephen J. Audino, Livia D. Whitacre, James Eck, Jenalle L. Wenzel, John W. Queenborough, Simon A. Comita, Liza S. TI Species associations structured by environment and land-use history promote beta-diversity in a temperate forest SO ECOLOGY LA English DT Article DE community assembly; environmental filtering; forest diversity; habitat association; multivariate regression tree analysis; spatial dependency; spatial eigenvector; variance partitioning ID CENTRAL NEW-ENGLAND; ECOLOGICAL VARIATION; PLANT-COMMUNITIES; VEGETATION; TREES; DYNAMICS; NICHE; MAINTENANCE; MECHANISMS; REGRESSION AB Patterns of diversity and community composition in forests are controlled by a combination of environmental factors, historical events, and stochastic or neutral mechanisms. Each of these processes has been linked to forest community assembly, but their combined contributions to alpha and beta-diversity in forests has not been well explored. Here we use variance partitioning to analyze 40000 individual trees of 49 species, collected within 137 ha of sampling area spread across a 900-ha temperate deciduous forest reserve in Pennsylvania to ask (1) To what extent is site-to-site variation in species richness and community composition of a temperate forest explained by measured environmental gradients and by spatial descriptors (used here to estimate dispersal-assembly or unmeasured, spatially structured processes)? (2) How does the incorporation of land-use history information increase the importance attributed to deterministic community assembly? and (3) How do the distributions and abundances of individual species within the community correlate with these factors? Environmental variables (i.e., topography, soils, and distance to stream), spatial descriptors (i.e., spatial eigenvectors derived from Cartesian coordinates), and land-use history variables (i.e., land-use type and intensity, forest age, and distance to road), explained about half of the variation in both species richness and community composition. Spatial descriptors explained the most variation, followed by measured environmental variables and then by land-use history. Individual species revealed variable responses to each of these sets of predictor variables. Several species were associated with stream habitats, and others were strictly delimited across opposing north- and south-facing slopes. Several species were also associated with areas that experienced recent (i.e., <100 years) human land-use impacts. These results indicate that deterministic factors, including environmental and land-use history variables, are important drivers of community response. The large amount of unexplained variation seen here (about 50%) is commonly observed in other such studies attempting to explain distribution and abundance patterns of plant communities. Determining whether such large fractions of unaccounted for variation are caused by a lack of sufficient data, or are an indication of stochastic features of forest communities globally, will remain an important challenge for ecologists in the future. C1 [Murphy, Stephen J.; Eck, Jenalle L.] Ohio State Univ, Dept Evolut Ecol & Organismal Biol, Columbus, OH 43210 USA. [Audino, Livia D.] Univ Fed Lavras, Dept Entomol, BR-37200000 Lavras, MG, Brazil. [Whitacre, James; Wenzel, John W.] Carnegie Museum Nat Hist, Powdermill Nat Reserve, Rector, PA 15677 USA. [Queenborough, Simon A.; Comita, Liza S.] Yale Univ, Sch Forestry & Environm Studies, New Haven, CT 06511 USA. [Comita, Liza S.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Murphy, SJ (reprint author), Ohio State Univ, Dept Evolut Ecol & Organismal Biol, 318 West 12th Ave, Columbus, OH 43210 USA. EM murphy.1132@osu.edu RI Audino, Livia/I-5182-2015; OI Whitacre, James/0000-0003-3464-9337 FU Heinz Endowments; Capes [PDSE 11219/12-2] FX The vegetation survey was made possible through a grant from the Heinz Endowments. We thank the field crews who conducted the survey, and Matthew Silveira for helping with Geographic Information Systems work. L. D. Audino thanks Capes for a doctorate scholarship (sandwich program; PDSE 11219/12-2). NR 65 TC 3 Z9 3 U1 6 U2 47 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0012-9658 EI 1939-9170 J9 ECOLOGY JI Ecology PD MAR PY 2015 VL 96 IS 3 BP 705 EP 715 DI 10.1890/14-0695.1 PG 11 WC Ecology SC Environmental Sciences & Ecology GA CD7MY UT WOS:000351275800011 PM 26236867 ER PT J AU Langin, KM Sillett, TS Funk, WC Morrison, SA Desrosiers, MA Ghalambor, CK AF Langin, Kathryn M. Sillett, T. Scott Funk, W. Chris Morrison, Scott A. Desrosiers, Michelle A. Ghalambor, Cameron K. TI Islands within an island: Repeated adaptive divergence in a single population SO EVOLUTION LA English DT Review DE Adaptation; Aphelocoma; gene flow; morphological evolution; natural selection; population structure ID SMALL SPATIAL SCALE; SANTA-CRUZ-ISLAND; SYMPATRIC SPECIATION; GENE FLOW; ECOLOGICAL SPECIATION; SCRUB-JAYS; MICROGEOGRAPHIC ADAPTATION; CONSERVATION BIOLOGY; NATURAL-SELECTION; COMPUTER-PROGRAM AB Physical barriers to gene flow were once viewed as prerequisites for adaptive evolutionary divergence. However, a growing body of theoretical and empirical work suggests that divergence can proceed within a single population. Here we document genetic structure and spatially replicated patterns of phenotypic divergence within a bird species endemic to 250 km(2) Santa Cruz Island, California, USA. Island scrub-jays (Aphelocoma insularis) in three separate stands of pine habitat had longer, shallower bills than jays in oak habitat, a pattern that mirrors adaptive differences between allopatric populations of the species' mainland congener. Variation in both bill measurements was heritable, and island scrub-jays mated nonrandomly with respect to bill morphology. The population was not panmictic; instead, we found a continuous pattern of isolation by distance across the east-west axis of the island, as well as a subtle genetic discontinuity across the boundary between the largest pine stand and adjacent oak habitat. The ecological factors that appear to have facilitated adaptive differentiation at such a fine scaleenvironmental heterogeneity and localized dispersalare ubiquitous in nature. These findings support recent arguments that microgeographic patterns of adaptive divergence may be more common than currently appreciated, even in mobile taxonomic groups like birds. C1 [Langin, Kathryn M.; Funk, W. Chris; Desrosiers, Michelle A.; Ghalambor, Cameron K.] Colorado State Univ, Dept Biol, Ft Collins, CO 80523 USA. [Langin, Kathryn M.; Funk, W. Chris; Ghalambor, Cameron K.] Colorado State Univ, Grad Degree Program Ecol, Ft Collins, CO 80523 USA. [Sillett, T. Scott] Natl Zool Pk, Migratory Bird Ctr, Smithsonian Conservat Biol Inst, Washington, DC 20013 USA. [Morrison, Scott A.] Nature Conservancy, San Francisco, CA 94105 USA. RP Langin, KM (reprint author), US Geol Survey, Ft Collins Sci Ctr, Ft Collins, CO 80526 USA. EM k.m.langin@gmail.com OI Langin, Kathryn/0000-0002-1799-1942 FU U.S. National Science Foundation [GRFP-2006037277, DDIG-1210421]; Nature Conservancy (TNC); U.S. National Park Service (NPS); Colorado State University; Smithsonian Institution; Queen's University FX We thank L. Angeloni, C. Benkman, L. Caldwell, A. Charmantier, K. Crooks, P. Grant, R. Grant, R. Greenberg, C. Handelsman, T. Lenormand, J. McCormack, M. Pesendorfer, E. Ruell, H. Sofaer, and two anonymous reviewers for helpful comments on the study and manuscript; the U.S. National Science Foundation (GRFP-2006037277, DDIG-1210421), The Nature Conservancy (TNC), the U.S. National Park Service (NPS), Colorado State University, the Smithsonian Institution, and Queen's University for funding; TNC, NPS, and the University of California Natural Reserve System's Santa Cruz Island Reserve for logistical support and access to Santa Cruz Island; and many field technicians for their assistance with data and sample collection. NR 101 TC 10 Z9 10 U1 10 U2 90 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0014-3820 EI 1558-5646 J9 EVOLUTION JI Evolution PD MAR PY 2015 VL 69 IS 3 BP 653 EP 665 DI 10.1111/evo.12610 PG 13 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA CD9VD UT WOS:000351446000008 PM 25645813 ER PT J AU Osada, N Oikawa, S Kitajima, K AF Osada, Noriyuki Oikawa, Shimpei Kitajima, Kaoru TI Implications of life span variation within a leaf cohort for evaluation of the optimal timing of leaf shedding SO FUNCTIONAL ECOLOGY LA English DT Article DE carbon balance; chronosequence; leaf survival; mean leaf longevity; optimal strategy; photosynthesis; photosynthetic nitrogen-use efficiency; repeated measurements ID NITROGEN USE EFFICIENCY; TROPICAL PIONEER TREE; PHOTOSYNTHETIC CAPACITY; CARBON GAIN; RAIN-FOREST; LEAVES; DYNAMICS; CANOPY; AGE; LONGEVITY AB Leaf life span (LLS) has been intensively studied as a key functional trait, and it is thought to have evolved and acclimates so as to optimize carbon balance or nitrogen use. However, empirical studies have produced inconsistent results in support of the theoretical predictions of optimal LLS. How rapidly daily carbon gain declines with leaf age is a critical parameter in the theories of optimal LLS, and it is often estimated from empirical data on the mean daily carbon gain of surviving leaves at each age class. We predict that such statistical approach should result in overestimation of daily carbon gain at the mean LLS, especially when LLS variation is large in the leaf cohort. This prediction is supported by simple simulations; daily carbon gain linearly declines to zero at the death of each individual leaf within a cohort (Case 1), and daily carbon gain linearly declines to zero at the cohort mean LLS (Case 2). In addition, variance in the initial carbon gain is considered, with the inverse relationship between the initial carbon gain and LLS but other assumptions are same as in the Case 1 (Case 3). Under the Cases 1 and 3, the mean daily carbon gain of surviving leaves at is always positive, and it increases with increasing LLS variance within a cohort. Under the Case 2, the mean daily carbon gain of surviving leaves at is zero regardless of variation in LLS, but this case is unrealistic as some leaves with negative carbon balance are assumed to survive for long-time when LLS variability is large. Published data on multiple species demonstrate a positive relationship of photosynthetic capacity at with LLS variability as predicted by our simulation under the Cases 1 and 3. This strongly suggests that the age-related decline of carbon gain may be underestimated in many previous studies that neglect within-cohort variation in LLS. In conclusion, we call attention to the importance of LLS variations within a leaf cohort, which should be considered in empirical test of the theories of optimal LLS. C1 [Osada, Noriyuki] Kyoto Univ, Field Sci Educ & Res Ctr, Kyoto 6068502, Japan. [Osada, Noriyuki] Hokkaido Univ, Field Sci Ctr Northern Biosphere, Tomakomai Res Stn, Tomakomai 0530035, Japan. [Oikawa, Shimpei] Ibaraki Univ, Coll Sci, Mito, Ibaraki 3100056, Japan. [Kitajima, Kaoru] Kyoto Univ, Grad Sch Agr, Kyoto 6068502, Japan. [Kitajima, Kaoru] Smithsonian Trop Res Inst, Balboa, Panama. RP Osada, N (reprint author), Kyoto Univ, Field Sci Educ & Res Ctr, Kyoto 6068502, Japan. EM osadada@fsc.hokudai.ac.jp FU Ministry of Education, Science, Sports and Culture of Japan [18770011, 21780140]; Nissan Foundation [08336] FX We thank two anonymous reviewers for helpful comments on the manuscript. This study was partly supported by a grant from the Ministry of Education, Science, Sports and Culture of Japan (18770011 and 21780140), and Nissan Foundation (08336). NR 38 TC 2 Z9 2 U1 2 U2 15 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0269-8463 EI 1365-2435 J9 FUNCT ECOL JI Funct. Ecol. PD MAR PY 2015 VL 29 IS 3 BP 308 EP 314 DI 10.1111/1365-2435.12326 PG 7 WC Ecology SC Environmental Sciences & Ecology GA CE1XO UT WOS:000351606400003 ER PT J AU Zweifler, LE Patel, MK Nociti, FH Wimer, HF Millan, JL Somerman, MJ Foster, BL AF Zweifler, Laura E. Patel, Mudita K. Nociti, Francisco H., Jr. Wimer, Helen F. Millan, Jose L. Somerman, Martha J. Foster, Brian L. TI Counter-regulatory phosphatases TNAP and NPP1 temporally regulate tooth root cementogenesis SO INTERNATIONAL JOURNAL OF ORAL SCIENCE LA English DT Article DE cementum; bone; ectonucleotide pyrophosphatase phosphodiesterase 1; periodontal ligament; progressive ankylosis protein; tissue-nonspecific alkaline phosphatase ID NONSPECIFIC ALKALINE-PHOSPHATASE; CEMENTOBLASTS IN-VITRO; PERIODONTAL-LIGAMENT; ACELLULAR CEMENTUM; PYROPHOSPHATASE PHOSPHODIESTERASE-1; INFANTILE HYPOPHOSPHATASIA; DOMINANT HYPOPHOSPHATASIA; SKELETAL MINERALIZATION; DENTIN MINERALIZATION; DEVELOPMENTAL BIOLOGY AB Cementum is critical for anchoring the insertion of periodontal ligament fibers to the tooth root. Several aspects of cementogenesis remain unclear, including differences between acellular cementum and cellular cementum, and between cementum and bone. Biomineralization is regulated by the ratio of inorganic phosphate (P-i) to mineral inhibitor pyrophosphate (PPi), where local P-i and PPi concentrations are controlled by phosphatases including tissue-nonspecific alkaline phosphatase (TNAP) and ectonucleotide pyrophosphatase/phosphodiesterase 1 (NPP1). The focus of this study was to define the roles of these phosphatases in cementogenesis. TNAP was associated with earliest cementoblasts near forming acellular and cellular cementum. With loss of TNAP in the Alpl null mouse, acellular cementum was inhibited, while cellular cementum production increased, albeit as hypomineralized cementoid. In contrast, NPP1 was detected in cementoblasts after acellular cementum formation, and at low levels around cellular cementum. Loss of NPP1 in the Enpp1 null mouse increased acellular cementum, with little effect on cellular cementum. Developmental patterns were recapitulated in a mouse model for acellular cementum regeneration, with early TNAP expression and later NPP1 expression. In vitro, cementoblasts expressed Alpl gene/protein early, whereas Enpp1 gene/protein expression was significantly induced only under mineralization conditions. These patterns were confirmed in human teeth, including widespread TNAP, and NPP1 restricted to cementoblasts lining acellular cementum. These studies suggest that early TNAP expression creates a low PPi environment promoting acellular cementum initiation, while later NPP1 expression increases PPi, restricting acellular cementum apposition. Alterations in PPi have little effect on cellular cementum formation, though matrix mineralization is affected. C1 [Zweifler, Laura E.; Patel, Mudita K.; Nociti, Francisco H., Jr.; Somerman, Martha J.; Foster, Brian L.] NIAMSD, NIAMS, NIH, Bethesda, MD 20892 USA. [Nociti, Francisco H., Jr.] Univ Estadual Campinas, Sch Dent, Div Periodont, Dept Prosthodont & Periodont, Piracicaba, Brazil. [Wimer, Helen F.] Smithsonian Inst, Natl Museum Amer Hist, Dept Vertebrate Zool, Washington, DC 20560 USA. [Millan, Jose L.] Sanford Burnham Med Res Inst, Sanford Childrens Hlth Res Ctr, La Jolla, CA USA. RP Foster, BL (reprint author), NIAMSD, NIAMS, NIH, Bldg 50 Room 4120, Bethesda, MD 20892 USA. EM brian.foster@nih.gov RI Nociti, Francisco/G-4907-2015; Foster, Brian/H-8375-2015 OI Foster, Brian/0000-0003-3444-0576 FU Intramural Research Program of the National Institute of Arthritis and Musculoskeletal and Skin Diseases (NIAMS) of the National Institutes of Health (NIH); NIH [JLM-DE12889, AR53102] FX This research was supported by the Intramural Research Program of the National Institute of Arthritis and Musculoskeletal and Skin Diseases (NIAMS) of the National Institutes of Health (NIH) and extramural NIH funding (JLM-DE12889 and AR53102). The authors thank Dr Thaisangela Rodrigues for her role in development and execution of the mouse periodontal defect model featured here and in a previous publication. NR 85 TC 6 Z9 6 U1 0 U2 3 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 1674-2818 EI 2049-3169 J9 INT J ORAL SCI JI Int. J. Oral Sci. PD MAR PY 2015 VL 7 IS 1 BP 27 EP 41 DI 10.1038/ijos.2014.62 PG 15 WC Dentistry, Oral Surgery & Medicine SC Dentistry, Oral Surgery & Medicine GA CD6HH UT WOS:000351189700006 PM 25504209 ER PT J AU Szczepanowska, HM Jha, D Mathia, TG AF Szczepanowska, H. M. Jha, D. Mathia, Th. G. TI Morphology and characterization of Dematiaceous fungi on a cellulose paper substrate using synchrotron X-ray microtomography, scanning electron microscopy and confocal laser scanning microscopy in the context of cultural heritage SO JOURNAL OF ANALYTICAL ATOMIC SPECTROMETRY LA English DT Article AB Dematiaceous (black pigmented) fungi interact with a cellular paper matrix growing on the surface and in paper bulk. Fungi-induced stains are one form of such interactions and are referred to as biodeterioration when applied to cultural heritage materials. The complexity of both paper and living systems, such as fungi, requires multi-scale analysis. The surface topography and spatial distribution of fungal monilioid hyphae, branched and un-branched chains and morphology of isodiametric enlargements of spores and yeast-like cells on the surface of paper were imaged by correlative microscopy, combining environmental scanning electron microscopy and imaging in backscattered electron mode (SEM-BSE) with confocal laser scanning microscopy (CLSM). The spherical fruiting bodies (perithecia) embedded in paper were not detected by CLSM, and ESEM provided data collected near the surface. Their interaction with paper was analyzed by 3D visualization using X-ray microtomography (X mu CT). Until now the fungi and paper interfaces in the matrix (bulk) of paper have not been analyzed using X mu CT. We present a novel method for investigating the interaction of fungal pigmented mycelia, spores and perithecia in the paper matrix using XmCT X and 3D visualization based on the X mu CT data. The tomographs were generated on the designated ID19 beam at ESRF, Grenoble, France. The ultimate purpose of this investigation was to understand the mechanisms of fungi and paper interactions in order to develop preservation strategies for cultural heritage, such as historic and artistic works on paper infested by fungi. C1 [Szczepanowska, H. M.] Smithsonian Inst, Museum Conservat Inst, Suitland, MD 20746 USA. [Jha, D.] Univ Copenhagen, Dept Chem, Nanosci Ctr, DK-2100 Copenhagen, Denmark. [Mathia, Th. G.] Ecole Cent Lyon, CNRS, Lab Tribol & Dynam Syst, F-69130 Ecully, France. RP Szczepanowska, HM (reprint author), Smithsonian Inst, Museum Conservat Inst, Suitland, MD 20746 USA. EM hszczepanowska1@gmail.com NR 22 TC 0 Z9 0 U1 4 U2 27 PU ROYAL SOC CHEMISTRY PI CAMBRIDGE PA THOMAS GRAHAM HOUSE, SCIENCE PARK, MILTON RD, CAMBRIDGE CB4 0WF, CAMBS, ENGLAND SN 0267-9477 EI 1364-5544 J9 J ANAL ATOM SPECTROM JI J. Anal. At. Spectrom. PD MAR 1 PY 2015 VL 30 IS 3 BP 651 EP 657 DI 10.1039/c4ja00337c PG 7 WC Chemistry, Analytical; Spectroscopy SC Chemistry; Spectroscopy GA CC8XB UT WOS:000350650800010 ER PT J AU Moskalik, P Smolec, R Kolenberg, K Molnar, L Kurtz, DW Szabo, R Benko, JM Nemec, JM Chadid, M Guggenberger, E Ngeow, CC Jeon, YB Kopacki, G Kanbur, SM AF Moskalik, P. Smolec, R. Kolenberg, K. Molnar, L. Kurtz, D. W. Szabo, R. Benko, J. M. Nemec, J. M. Chadid, M. Guggenberger, E. Ngeow, C. -C. Jeon, Y. -B. Kopacki, G. Kanbur, S. M. TI Kepler photometry of RRc stars: peculiar double-mode pulsations and period doubling SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE techniques: photometric; stars: horizontal branch; stars: oscillations; stars: variables: RR Lyrae ID GRAVITATIONAL LENSING EXPERIMENT.; LARGE-MAGELLANIC-CLOUD; OGLE-III CATALOG; LYRAE STARS; INITIAL CHARACTERISTICS; CLASSICAL CEPHEIDS; RADIAL-VELOCITIES; NONRADIAL MODES; GALACTIC BULGE; LIGHT CURVES AB We present the analysis of four first overtone RR Lyrae stars observed with the Kepler space telescope, based on data obtained over nearly 2.5 yr. All four stars are found to be multiperiodic. The strongest secondary mode with frequency f(2) has an amplitude of a few mmag, 20-45 times lower than the main radial mode with frequency f(1). The two oscillations have a period ratio of P-2/P-1 = 0.612-0.632 that cannot be reproduced by any two radial modes. Thus, the secondary mode is non-radial. Modes yielding similar period ratios have also recently been discovered in other variables of the RRc and RRd types. These objects form a homogenous group and constitute a new class of multimode RR Lyrae pulsators, analogous to a similar class of multimode classical Cepheids in the Magellanic Clouds. Because a secondary mode with P-2/P-1 similar to 0.61 is found in almost every RRc and RRd star observed from space, this form of multiperiodicity must be common. In all four Kepler RRc stars studied, we find subharmonics of f(2) at similar to 1/2f(2) and at similar to 3/2f(2). This is a signature of period doubling of the secondary oscillation, and is the first detection of period doubling in RRc stars. The amplitudes and phases of f(2) and its subharmonics are variable on a time-scale of 10-200 d. The dominant radial mode also shows variations on the same time-scale, but with much smaller amplitude. In three Kepler RRc stars we detect additional periodicities, with amplitudes below 1 mmag, that must correspond to non-radial g-modes. Such modes never before have been observed in RR Lyrae variables. C1 [Moskalik, P.; Smolec, R.] Copernicus Astron Ctr, PL-00716 Warsaw, Poland. [Kolenberg, K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kolenberg, K.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Heverlee, Belgium. [Molnar, L.; Szabo, R.; Benko, J. M.] MTA CSFK, Konkoly Observ, H-1121 Budapest, Hungary. [Molnar, L.] Univ West Hungary, Inst Math & Phys, H-9700 Szombathely, Hungary. [Kurtz, D. W.] Univ Cent Lancashire, Jeremiah Horrocks Inst, Preston PR1 2HE, Lancs, England. [Nemec, J. M.] Camosun Coll, Dept Phys & Astron, Victoria, BC V8P5J2, Canada. [Chadid, M.] Univ Nice Sophia Antipolis, Observ Cote Azur, UMR 7293, F-06108 Nice 02, France. [Guggenberger, E.] Max Planck Inst Sonnensyst Forsch, D-37077 Gottingen, Germany. [Guggenberger, E.] Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, DK-8000 Aarhus C, Denmark. [Ngeow, C. -C.] Natl Cent Univ, Grad Inst Astron, Jhongli 32001, Taiwan. [Jeon, Y. -B.] Korea Astron & Space Sci Inst, Taejon 305348, South Korea. [Kopacki, G.] Uniwersytetu Wroclawskie, Inst Astron, PL-51622 Wroclaw, Poland. [Kanbur, S. M.] SUNY Coll Oswego, Dept Phys, Oswego, NY 13126 USA. RP Moskalik, P (reprint author), Copernicus Astron Ctr, Ul Bartycka 18, PL-00716 Warsaw, Poland. EM pam@camk.edu.pl RI Smolec, Radoslaw/F-1435-2013; OI Smolec, Radoslaw/0000-0001-7217-4884; Szabo, Robert/0000-0002-3258-1909; Molnar, Laszlo/0000-0002-8159-1599 FU NASA's Science Mission Directorate; Polish NCN [DEC-2012/05/B/ST9/03932, 2011/03/B/ST9/02667]; 'Lendulet Young Researchers' Program of the Hungarian Academy of Sciences; Hungarian OTKA [K83790]; National Science Foundation [NSF PHY05-51164]; European Community [269194, 312844, 338251]; ESA PECS [4000110889/14/NL/NDe]; Ministry of Science and Technology (Taiwan) [MOST101-2112-M-008-017-MY3]; Korea Astronomy and Space Science Institute [2014-1-400-06]; Camosun College Faculty Association; [PIOF-GA-2009-255267] FX Funding for this Discovery mission was provided by NASA's Science Mission Directorate. The authors gratefully acknowledge the entire Kepler team, whose outstanding efforts have made these results possible. This research has been supported by the Polish NCN through grant no. DEC-2012/05/B/ST9/03932. It has also been supported by the 'Lendulet-2009 Young Researchers' Program of the Hungarian Academy of Sciences, the Hungarian OTKA grant K83790, the National Science Foundation grant no. NSF PHY05-51164, the European Community's Seventh Framework Programme (FP7/2007-2013) grants no. 269194 (IRSES/ASK), 312844 (SPACEINN) and 338251 (StellarAges), the ESA PECS Contract no. 4000110889/14/NL/NDe, the Ministry of Science and Technology (Taiwan) grant no. MOST101-2112-M-008-017-MY3, the Korea Astronomy and Space Science Institute Project no. 2014-1-400-06, supervised by the Ministry of Science, ICT and Future Planning and by the Polish NCN grant no. 2011/03/B/ST9/02667. KK is currently a Marie Curie Fellow, grateful for the support of grant PIOF-GA-2009-255267 (SAS-RRL). RSz acknowledges the University of Sydney IRCA grant. JMN wishes to thank the Camosun College Faculty Association for financial assistance. NR 76 TC 14 Z9 14 U1 0 U2 6 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAR 1 PY 2015 VL 447 IS 3 BP 2348 EP 2366 DI 10.1093/mnras/stu2561 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CC3TP UT WOS:000350273200022 ER PT J AU Hurley-Walker, N Johnston-Hollitt, M Ekers, R Hunstead, R Sadler, EM Hindson, L Hancock, P Bernardi, G Bowman, JD Briggs, F Cappallo, R Corey, B Deshpande, AA Emrich, D Gaensler, BM Goeke, R Greenhill, L Hazelton, BJ Hewitt, J Kaplan, DL Kasper, J Kratzenberg, E Lonsdale, C Lynch, M Mitchell, D McWhirter, R Morales, M Morgan, E Oberoi, D Offringa, A Ord, S Prabu, T Rogers, A Roshi, A Shankar, U Srivani, K Subrahmanyan, R Tingay, S Waterson, M Wayth, RB Webster, R Whitney, A Williams, A Williams, C AF Hurley-Walker, Natasha Johnston-Hollitt, Melanie Ekers, Ron Hunstead, Richard Sadler, Elaine M. Hindson, Luke Hancock, Paul Bernardi, Gianni Bowman, Judd D. Briggs, Frank Cappallo, Roger Corey, Brian Deshpande, Avinash A. Emrich, David Gaensler, Bryan M. Goeke, Robert Greenhill, Lincoln Hazelton, Bryna J. Hewitt, Jacqueline Kaplan, David L. Kasper, Justin Kratzenberg, Eric Lonsdale, Colin Lynch, Mervyn Mitchell, Daniel McWhirter, Russell Morales, Miguel Morgan, Edward Oberoi, Divya Offringa, Andre Ord, Stephen Prabu, Thiagaraj Rogers, Alan Roshi, Anish Shankar, Udaya Srivani, K. Subrahmanyan, Ravi Tingay, Steven Waterson, Mark Wayth, Randall B. Webster, Rachel Whitney, Alan Williams, Andrew Williams, Chris TI Serendipitous discovery of a dying Giant Radio Galaxy associated with NGC 1534, using the Murchison Widefield Array SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE techniques: interferometric; galaxies: active; galaxies: general; galaxies: individual:NGC 1534; radio continuum: galaxies ID ALL-SKY SURVEY; SAMPLE DEFINITION; DOMINATED HOST; SOURCE CATALOG; IMAGING SURVEY; SPIRAL GALAXY; SOUTHERN SKY; CLUSTERS; EMISSION; EVOLUTION AB Recent observations with the Murchison Widefield Array at 185 MHz have serendipitously unveiled a heretofore unknown giant and relatively nearby (z = 0.0178) radio galaxy associated with NGC 1534. The diffuse emission presented here is the first indication that NGC 1534 is one of a rare class of objects (along with NGC 5128 and NGC 612) in which a galaxy with a prominent dust lane hosts radio emission on scales of similar to 700 kpc. We present details of the radio emission along with a detailed comparison with other radio galaxies with discs. NGC 1534 is the lowest surface brightness radio galaxy known with an estimated scaled 1.4-GHz surface brightness of just 0.2 mJy arcmin(-2). The radio lobes have one of the steepest spectral indices yet observed: alpha = -2.1 +/- 0.1, and the core to lobe luminosity ratio is <0.1 per cent. We estimate the space density of this low brightness (dying) phase of radio galaxy evolution as 7 x 10(-7) Mpc(-3) and argue that normal AGN cannot spend more than 6 per cent of their lifetime in this phase if they all go through the same cycle. C1 [Hurley-Walker, Natasha; Ekers, Ron; Hancock, Paul; Emrich, David; Lynch, Mervyn; Ord, Stephen; Tingay, Steven; Waterson, Mark; Wayth, Randall B.; Williams, Andrew] Curtin Univ, Int Ctr Radio Astron Res, Bentley, WA 6102, Australia. [Johnston-Hollitt, Melanie; Hindson, Luke] Victoria Univ Wellington, Sch Chem Phys Sci, Wellington 6140, New Zealand. [Ekers, Ron; Mitchell, Daniel] CSIRO Astron & Space Sci, Marsfield, NSW 2122, Australia. [Hunstead, Richard; Sadler, Elaine M.; Gaensler, Bryan M.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia. [Hancock, Paul; Briggs, Frank; Gaensler, Bryan M.; Mitchell, Daniel; Offringa, Andre; Ord, Stephen; Subrahmanyan, Ravi; Tingay, Steven; Wayth, Randall B.; Webster, Rachel] ARC Ctr Excellence All Sky Astrophys CAASTRO Redf, Sydney, NSW 2016, Australia. [Bernardi, Gianni] SKA SA, ZA-7405 Pinelands, South Africa. [Bernardi, Gianni] Rhodes Univ, Dept Phys & Elect, ZA-6140 Grahamstown, South Africa. [Bernardi, Gianni; Greenhill, Lincoln; Kasper, Justin] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bowman, Judd D.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Briggs, Frank; Offringa, Andre; Waterson, Mark] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia. [Cappallo, Roger; Corey, Brian; Goeke, Robert; Kratzenberg, Eric; Lonsdale, Colin; McWhirter, Russell; Whitney, Alan] MIT Haystack Observ, Westford, MA 01886 USA. [Prabu, Thiagaraj; Shankar, Udaya; Srivani, K.; Subrahmanyan, Ravi] Raman Res Inst, Bangalore 560080, Karnataka, India. [Hazelton, Bryna J.; Morales, Miguel] Univ Washington, Dept Phys, Seattle, WA 98195 USA. [Hewitt, Jacqueline; Morgan, Edward; Williams, Chris] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Kaplan, David L.] Univ Wisconsin Milwaukee, Dept Phys, Milwaukee, WI 53201 USA. [Oberoi, Divya] Tata Inst Fundamental Res, Natl Ctr Radio Astrophys, Pune 411007, Maharashtra, India. [Roshi, Anish] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Roshi, Anish] Natl Radio Astron Observ, Greenbank, VA 22903 USA. [Webster, Rachel] Univ Melbourne, Sch Phys, Melbourne, Vic 3010, Australia. RP Hurley-Walker, N (reprint author), Curtin Univ, Int Ctr Radio Astron Res, Bentley, WA 6102, Australia. EM nhw@icrar.org RI Williams, Andrew/K-2931-2013; M, Manjunath/N-4000-2014; Deshpande, Avinash/D-4868-2012; Wayth, Randall/B-2444-2013; Hurley-Walker, Natasha/B-9520-2013; Emrich, David/B-7002-2013; Subrahmanyan, Ravi/D-4889-2012; OI Sadler, Elaine/0000-0002-1136-2555; Gaensler, Bryan/0000-0002-3382-9558; Williams, Andrew/0000-0001-9080-0105; M, Manjunath/0000-0001-8710-0730; Wayth, Randall/0000-0002-6995-4131; Hurley-Walker, Natasha/0000-0002-5119-4808; Emrich, David/0000-0002-4058-1837; Hancock, Paul/0000-0002-4203-2946 FU Marsden Fund; U.S. National Science Foundation [AST-0457585, PHY-0835713, CAREER-0847753, AST-0908884]; Australian Research Council (LIEF) [LE0775621, LE0882938]; U.S. Air Force Office of Scientific Research [FA9550-0510247]; Centre for All-sky Astrophysics (an Australian Research Council Centre of Excellence) [CE110001020]; Smithsonian Astrophysical Observatory; MIT School of Science; Raman Research Institute; Australian National University; Victoria University of Wellington from the New Zealand Ministry of Economic Development [MED-E1799]; Victoria University of Wellington from an IBM Shared University Research Grant [MED-E1799]; Australian Federal government via the Commonwealth Scientific and Industrial Research Organization (CSIRO); Australian Federal government via the National Collaborative Research Infrastructure Strategy; Education Investment Fund; Australia India Strategic Research Fund; Astronomy Australia Limited; NVIDIA at Harvard University; International Centre for Radio Astronomy Research (ICRAR), a Joint Venture of Curtin University; University of Western Australia - Western Australian State government; Space Telescope Science Institute under US Government [NAG W-2166]; UK Science and Engineering Research Council FX We thank Drs Leith Godfrey and Lakshmi Saripalli for useful discussions on properties of dying radio galaxies. MJ-H is supported in this work through the Marsden Fund administered by the Royal Society of New Zealand. This scientific work makes use of the Murchison Radio-astronomy Observatory, operated by CSIRO. We acknowledge the Wajarri Yamatji people as the traditional owners of the Observatory site. Support for the MWA comes from the U.S. National Science Foundation (grants AST-0457585, PHY-0835713, CAREER-0847753, and AST-0908884), the Australian Research Council (LIEF grants LE0775621 and LE0882938), the U.S. Air Force Office of Scientific Research (grant FA9550-0510247), and the Centre for All-sky Astrophysics (an Australian Research Council Centre of Excellence funded by grant CE110001020). Support is also provided by the Smithsonian Astrophysical Observatory, the MIT School of Science, the Raman Research Institute, the Australian National University, and the Victoria University of Wellington (via grant MED-E1799 from the New Zealand Ministry of Economic Development and an IBM Shared University Research Grant). The Australian Federal government provides additional support via the Commonwealth Scientific and Industrial Research Organization (CSIRO), National Collaborative Research Infrastructure Strategy, Education Investment Fund, and the Australia India Strategic Research Fund, and Astronomy Australia Limited, under contract to Curtin University. We acknowledge the iVEC Petabyte Data Store, the Initiative in Innovative Computing and the CUDA Center for Excellence sponsored by NVIDIA at Harvard University, and the International Centre for Radio Astronomy Research (ICRAR), a Joint Venture of Curtin University and The University of Western Australia, funded by the Western Australian State government. This research has made use of the National Aeronautics and Space Administration (NASA)/Infrared Processing and Analysis Center (IPAC) Infrared Science Archive and the NASA/IPAC Extragalactic Database (NED) which are operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. This research has also made use of NASA's Astrophysics Data System. The DSS was produced at the Space Telescope Science Institute under US Government grant NAG W-2166 and is based on photographic data obtained using The UK Schmidt Telescope. The UK Schmidt Telescope was operated by the Royal Observatory Edinburgh, with funding from the UK Science and Engineering Research Council, until 1988 June, and thereafter by the Anglo-Australian Observatory. Original plate material is copyright of the Royal Observatory Edinburgh and the Anglo-Australian Observatory. The plates were processed into the present compressed digital form with their permission. SuperCOSMOS Sky Survey material is based on photographic data originating from the UK, Palomar and ESO Schmidt telescopes and is provided by the Wide-Field Astronomy Unit, Institute for Astronomy, University of Edinburgh. NR 60 TC 10 Z9 10 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 2015 VL 447 IS 3 BP 2468 EP 2478 DI 10.1093/mnras/stu2570 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CC3TP UT WOS:000350273200031 ER PT J AU Torrey, P Snyder, GF Vogelsberger, M Hayward, CC Genel, S Sijacki, D Springel, V Hernquist, L Nelson, D Kriek, M Pillepich, A Sales, LV McBride, CK AF Torrey, Paul Snyder, Gregory F. Vogelsberger, Mark Hayward, Christopher C. Genel, Shy Sijacki, Debora Springel, Volker Hernquist, Lars Nelson, Dylan Kriek, Mariska Pillepich, Annalisa Sales, Laura V. McBride, Cameron K. TI Synthetic galaxy images and spectra from the Illustris simulation SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: numerical; astronomical data bases: miscellaneous; catalogues; galaxies: evolution; galaxies: formation; galaxies: photometry ID DARK-MATTER UNIVERSE; SMOOTHED PARTICLE HYDRODYNAMICS; STELLAR POPULATION SYNTHESIS; STAR-FORMING GALAXIES; LYMAN BREAK GALAXIES; PRESSURE-DOMINATED PHOTOIONIZATION; EMISSION-LINE DIAGNOSTICS; HIGH-REDSHIFT GALAXIES; BROAD-BAND PHOTOMETRY; COSMOLOGICAL SIMULATIONS AB We present our methods for generating a catalogue of 7000 synthetic images and 40 000 integrated spectra of redshift z = 0 galaxies from the Illustris simulation. The mock data products are produced by using stellar population synthesis models to assign spectral energy distributions (SED) to each star particle in the galaxies. The resulting synthetic images and integrated SEDs therefore properly reflect the spatial distribution, stellar metallicity distribution, and star formation history of the galaxies. From the synthetic data products, it is possible to produce monochromatic or colour-composite images, perform SED fitting, classify morphology, determine galaxy structural properties, and evaluate the impacts of galaxy viewing angle. The main contribution of this paper is to describe the production, format, and composition of the image catalogue that makes up the Illustris Simulation Observatory. As a demonstration of this resource, we derive galactic stellar mass estimates by applying the SED fitting code FAST to the synthetic galaxy products, and compare the derived stellar masses against the true stellar masses from the simulation. We find from this idealized experiment that systematic biases exist in the photometrically derived stellar mass values that can be reduced by using a fixed metallicity in conjunction with a minimum galaxy age restriction. C1 [Torrey, Paul; Hayward, Christopher C.; Genel, Shy; Hernquist, Lars; Nelson, Dylan; Pillepich, Annalisa; Sales, Laura V.; McBride, Cameron K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Torrey, Paul; Vogelsberger, Mark; Hayward, Christopher C.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Torrey, Paul] CALTECH, Pasadena, CA 91125 USA. [Snyder, Gregory F.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Hayward, Christopher C.; Springel, Volker] Heidelberger Inst Theoret Studien, D-69118 Heidelberg, Germany. [Sijacki, Debora] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Sijacki, Debora] Univ Cambridge, Kavli Inst Cosmol, Cambridge CB3 0HA, England. [Springel, Volker] Heidelberg Univ, ARI, Zentrum Astron, D-69120 Heidelberg, Germany. [Kriek, Mariska] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. RP Torrey, P (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM ptorrey@cfa.harvard.edu RI Hayward, Christopher/I-4756-2012; OI Hayward, Christopher/0000-0003-4073-3236; Torrey, Paul/0000-0002-5653-0786 FU HST [HST-AR-12856.01-A]; NASA through a grant from the Space Telescope Science Institute [12856]; NASA [NAS 5-26555, NNX12AC67G]; Klaus Tschira Foundation; National Science Foundation [PHY-1066293]; DFG Research Centre [SFB-881]; European Research Council [ERC-StG EXAGAL-308037]; NSF [AST-1312095]; FAS Division of Science, Research Computing Group at Harvard University FX We thank the referee for a constructive report which has helped to improve the quality of this paper. We thank Dave Sanders and Arjun Dey for helpful suggestions on this work. We thank Patrik Jonsson for his significant efforts to write, develop, and support the SUNRISE code. GS acknowledges support from the HST grants programme, number HST-AR-12856.01-A. Support for programme # 12856 (PI Lotz) was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. CCH is grateful to the Klaus Tschira Foundation for financial support and acknowledges the hospitality of the Aspen Center for Physics, which is supported by the National Science Foundation Grant No. PHY-1066293. VS acknowledges support by the DFG Research Centre SFB-881 The Milky Way System through project A1, and by the European Research Council under ERC-StG EXAGAL-308037. LH acknowledges support from NASA grant NNX12AC67G and NSF grant AST-1312095. The computations in this paper were run on the Odyssey cluster supported by the FAS Division of Science, Research Computing Group at Harvard University. We thank Paul Edmon and the FAS RC team for their technical support. NR 135 TC 26 Z9 26 U1 1 U2 3 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAR 1 PY 2015 VL 447 IS 3 BP 2753 EP 2771 DI 10.1093/mnras/stu2592 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CC3TP UT WOS:000350273200053 ER PT J AU Ivanova, MA Petaev, MI AF Ivanova, M. A. Petaev, M. I. TI Characteristics and origin of the components of the carbonaceous chondrite NWA 470 SO PETROLOGY LA English DT Article ID EARLY SOLAR-SYSTEM; CH CHONDRITES; METAL GRAINS; ISOTOPIC COMPOSITIONS; CONDENSATION; CR; CHONDRULES; ALH85085; CALCIUM; CLASSIFICATION AB For the first time, data are presented from a detailed investigation of all components of the NWA 470 CH-type carbonaceous chondrite. The meteorite's major characteristics are a high metal content with a solar Co/Ni ratio, a majority of chemically-zoned metal grains, cryptocrystalline chondrules, grossite- and hibonite-bearing refractory inclusions, the presence of SiO2 objects and the lack of a fine-grained matrix. The bulk chemical and isotope composition of oxygen in the meteorite is typical for CH chondrites. However, among all CH chondrites, NWA 470 is the most enriched in iron. Notable among the chondrite's components are refractory inclusions and chondrules of several different generations, which may have formed under either canonical nebular or dust-rich conditions. In general, the origin of refractory inclusions, SiO2 objects and zoned metal can be explained through fractional condensation with partial isolation of the condensates. Dark inclusions were probably included in the material of CH chondrites from a different parent body, similar in composition to CM chondrites. After mixing of these multiple types of material during accretion, the components of NWA 470 were not further affected by aqueous alteration or thermal metamorphic processes, and the components' primary characteristics have been preserved. C1 [Ivanova, M. A.] Russian Acad Sci, Vernadsky Inst Geochem & Analyt Chem, Moscow 119991, Russia. [Petaev, M. I.] Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA. [Petaev, M. I.] Harvard Smithsonian Ctr Astrophys, Dept Solar Stellar & Planetary Phys, Cambridge, MA 02138 USA. RP Ivanova, MA (reprint author), Russian Acad Sci, Vernadsky Inst Geochem & Analyt Chem, 19 Kosygin St, Moscow 119991, Russia. EM meteorite2000@mail.ru; mpetaev@fas.harvard.edu FU Presidium of the RAS [22] FX This investigation was performed with the support of Program no. 22 of the Presidium of the RAS. NR 44 TC 0 Z9 0 U1 1 U2 5 PU MAIK NAUKA/INTERPERIODICA/SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013-1578 USA SN 0869-5911 EI 1556-2085 J9 PETROLOGY+ JI Petrology PD MAR PY 2015 VL 23 IS 2 BP 150 EP 167 DI 10.1134/S0869591115020058 PG 18 WC Geosciences, Multidisciplinary; Mineralogy SC Geology; Mineralogy GA CD3QS UT WOS:000350995100004 ER PT J AU Duan, L Wen, J Yang, X Liu, PL Arslan, E Ertugrul, K Chang, ZY AF Duan, Lei Wen, Jun Yang, Xue Liu, Pei-Liang Arslan, Emine Ertugrul, Kuddisi Chang, Zhao-Yang TI Phylogeny of Hedysarum and tribe Hedysareae (Leguminosae: Papilionoideae) inferred from sequence data of ITS, matK, trnL-F and psbA-trnH SO TAXON LA English DT Article DE Caraganeae; Galegeae; Hedysareae; Hedysarum; Leguminosae; phylogeny ID WORLD ASTRAGALUS FABACEAE; NUCLEAR RIBOSOMAL DNA; MOLECULAR PHYLOGENY; CARAGANA LEGUMINOSAE; CHLOROPLAST-DNA; NORTH-AMERICA; SYSTEMATICS; INFERENCE; NRDNA; BIOGEOGRAPHY AB Based on sequence data of the nuclear ITS and plastid matK, trnL-F and psbA-trnH markers of 162 species (169 accessions), the relationships and monophyly of tribe Hedysareae and its close relatives were assessed, with special reference to the infrageneric phylogeny of Hedysarum. The results showed that Hedysareae sensu Lock is not monophyletic, and its relationships with tribe Galegeae are unclear. Tribe Galegeae is polyphyletic. Hedysareae sensu Lock includes two strongly supported clades: the Caraganean clade and the Hedysaroid clade. Tribe Caraganeae Ranjbar was supported to be recognized based on the Caraganean clade, but it is herein suggested to be re-circumscribed by excluding Chesneya and Gueldenstaedtia. Our results support treating the Hedysaroid clade as tribe Hedysareae, comprising nine genera: Alhagi, Corethrodendron, Ebenus, Eversmannia, Greuteria, Hedysarum, Onobrychis, Sulla and Taverniera. Hedysarum as delimited here consists of three main clades: the first clade (the mesic group) corresponds to H. sect. Hedysarum; the second clade (the xeric group) is the re-defined H. sect. Multicaulia, consisting of the core group of H. sect. Multicaulia plus the former genus Sartoria; and the third clade (the psychrophilic group) includes the monospecific H. sect. Stracheya (with H. tibeticum) and two species previously placed in H. sect. Multicaulia (H. kumaonense, H. lehmannianum). C1 [Duan, Lei; Liu, Pei-Liang; Chang, Zhao-Yang] Northwest A&F Univ, Coll Life Sci, Yangling 712100, Shaanxi, Peoples R China. [Wen, Jun] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA. [Yang, Xue] Kunming Univ, Sch Agr, Kunming 650204, Yunnan, Peoples R China. [Arslan, Emine; Ertugrul, Kuddisi] Selcuk Univ, Fac Sci, Dept Biol, TR-42031 Konya, Turkey. RP Chang, ZY (reprint author), Northwest A&F Univ, Coll Life Sci, Yangling 712100, Shaanxi, Peoples R China. EM wenj@si.edu; czybbg@nwsuaf.edu.cn RI Ertugrul, Kuddisi/A-1122-2016 OI Ertugrul, Kuddisi/0000-0002-6463-2918 FU Laboratories of Analytical Biology of the National Museum of Natural History (Smithsonian Institution); Natural Science Foundation of China [30270106, 30870155]; China Scholarship Council FX We thank three anonymous reviewers for constructive suggestions on the manuscript. We are grateful to the curators of the following herbaria who offered leaf samples, seeds or DNA samples: CS, F, K, KNYA, TURP, US, WUK, XJBI. We thank Gabriel Johnson, Matthew Kweskin, Ming-Qin Zhou, and Jian-Qiang Zhang for lab assistance; Natasha Crump for Russian literature translation; Robin Everly for literature search; and Martin F. Wojciechowski, Ying Feng and Shi-Min Duan for checking voucher information. The Laboratories of Analytical Biology of the National Museum of Natural History (Smithsonian Institution), the Natural Science Foundation of China (Project no. 30270106, 30870155), and the China Scholarship Council are gratefully acknowledged for financial support of the study. NR 108 TC 7 Z9 7 U1 1 U2 16 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 MAR PY 2015 VL 64 IS 1 BP 49 EP 64 PG 16 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA CD4XS UT WOS:000351090100005 ER PT J AU Olson, SL AF Olson, Storrs L. TI HISTORY, MORPHOLOGY, AND FOSSIL RECORD OF THE EXTINCT PUERTO RICAN PARAKEET PSITTACARA MAUGEI SOUANCE SO WILSON JOURNAL OF ORNITHOLOGY LA English DT Article DE Aratinga; Hispaniolan Parakeet; Mona Island; paleontology; Psittacidae; Psittacara chloroptera ID AVES AB The extinct Puerto Rican Parakeet (Psittacara maugei) has been known with certainty only from Mona Island and is usually regarded as a poorly defined subspecies of P. chloroptera of Hispaniola. Examination of skin specimens and comparison of skeletons with fossil and archeological material from Puerto Rico, show that Psitticara maugei is a fully distinct species from P. chloroptera, differing in plumage and particularly in bill morphology, such that a probable difference in diet is suggested. The main range of P. maugei was Puerto Rico, with the Mona Island population being only an isolated outlier. Extinction took place on Puerto Rico by the mid-1800s and on Mona Island shortly after 1892 possibly because of a combination of habitat destruction, persecution for crop depredations, and disease. Received 7 February 2014. Accepted 19 June 2014. C1 Natl Museum Nat Hist, Smithsonian Inst, Dept Vertebrate Zool, Washington, DC 20013 USA. RP Olson, SL (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Dept Vertebrate Zool, POB 37012, Washington, DC 20013 USA. EM olsons@si.edu NR 59 TC 2 Z9 2 U1 4 U2 10 PU WILSON ORNITHOLOGICAL SOC PI WACO PA 5400 BOSQUE BLVD, STE 680, WACO, TX 76710 USA SN 1559-4491 EI 1938-5447 J9 WILSON J ORNITHOL JI Wilson J. Ornithol. PD MAR PY 2015 VL 127 IS 1 BP 1 EP 12 PG 12 WC Ornithology SC Zoology GA CD9ZM UT WOS:000351460800001 ER PT J AU Gotanda, KM Sharpe, DMT De Leon, LF AF Gotanda, Kiyoko M. Sharpe, Diana M. T. De Leon, Luis F. TI Galapagos Mockingbird (Mimus parvulus) Preys on an Invasive Mammal SO WILSON JOURNAL OF ORNITHOLOGY LA English DT Article DE bashing; behavior; Galapagos; Mimus parvulus; predation; rodent ID BIRDS; ISLANDS AB Galapagos Mockingbirds (Mimus parvulus) are opportunistic feeders that have been observed engaging in a variety of unusual predatory behaviors. Here, we report on a specific behavior that we observed: a Galapagos Mockingbird preying on an invasive mammal by repeatedly hitting it on the ground. We discuss the reasons that the mockingbird might have engaged in this behavior and the potential implications this could have for native biodiversity and conservation on the Galapagos Islands. C1 [Gotanda, Kiyoko M.] McGill Univ, Redpath Museum, Montreal, PQ H3A 0C4, Canada. [Gotanda, Kiyoko M.] McGill Univ, Dept Biol, Montreal, PQ H3A 0C4, Canada. [Sharpe, Diana M. T.] Smithsonian Trop Res Inst, Naos Labs, Panama City, Panama. [De Leon, Luis F.] Inst Invest Cient & Serv Alta Tecnol INDICASAT AI, Ctr Biodiversidad & Descubrimiento Drogas, Panama City 5, Panama. RP Gotanda, KM (reprint author), McGill Univ, Redpath Museum, Montreal, PQ H3A 0C4, Canada. EM kiyoko.gotanda@mail.mcgill.ca FU Earthwatch Institute; Sigma Xi; National Science and Engineering Research Council of Canada; Les Fonds Quebecois de la Recherche sur la Nature et les Technologies (FQRNT); Sistema Nacional de Investigacion (SNI); Secretaria Nacional de Ciencia, Tecnologia e Innovacion (SENACYT) FX Logistical support and permits were provided by Galapagos National Park Service and the Charles Darwin Foundation. We thank R. Dowler, A. Goldman, and V. Millien for assistance in identifying the rodent from digital photographs of the mouse in several positions. Financial support was provided by Earthwatch Institute, Sigma Xi, the National Science and Engineering Research Council of Canada in the form of a Vanier scholarship for KMG, Les Fonds Quebecois de la Recherche sur la Nature et les Technologies (FQRNT) in the form of a post-doctoral scholarship to DS, and a grant from Sistema Nacional de Investigacion (SNI) and Secretaria Nacional de Ciencia, Tecnologia e Innovacion (SENACYT) to LFD. We gratefully acknowledge J. Podos (aka "Papa Pinzon") and A. Hendry for introducing us to research on the Galapagos Islands. NR 26 TC 0 Z9 0 U1 2 U2 10 PU WILSON ORNITHOLOGICAL SOC PI WACO PA 5400 BOSQUE BLVD, STE 680, WACO, TX 76710 USA SN 1559-4491 EI 1938-5447 J9 WILSON J ORNITHOL JI Wilson J. Ornithol. PD MAR PY 2015 VL 127 IS 1 BP 138 EP 141 PG 4 WC Ornithology SC Zoology GA CD9ZM UT WOS:000351460800020 ER PT J AU Gunay, F Alten, B Simsek, F Aldemir, A Linton, YM AF Gunay, Filiz Alten, Bulent Simsek, Fatih Aldemir, Adnan Linton, Yvonne-Marie TI Barcoding Turkish Culex mosquitoes to facilitate arbovirus vector incrimination studies reveals hidden diversity and new potential vectors SO ACTA TROPICA LA English DT Article DE DNA barcoding; Culex; Arbovirus; Vector; New records; Turkey ID WEST-NILE-VIRUS; ST-LOUIS ENCEPHALITIS; DIPTERA-CULICIDAE; JAPANESE ENCEPHALITIS; VERTICAL TRANSMISSION; MODESTUS FICALBI; SINDBIS VIRUS; GETAH VIRUS; TURKEY; CIRCULATION AB As a precursor to planned arboviral vector incrimination studies, an integrated systematics approach was adopted using morphology and DNA barcoding to examine the Culex fauna present in Turkey. The mitochondrial COI gene (658 bp) were sequenced from 185 specimens collected across 11 Turkish provinces, as well as from colony material. Although by morphology only 9 species were recognised, DNA barcoding recovered 13 distinct species including: Cx. (Barraudius) modestus, Cx. (Culex) laticinctus, Cx. (Cux.) mimeticus, Cx. (Cux.) perexiguus, Cx. (Cux.) pipiens, Cx. (Cux.) pipiens form molestus, Cx. (Cux.) quinquefasciatus, Cx. (Cux.) theilen, Cx. (Cux.) torrentium, Cx. (Cux.) tritaeniorhynchus and Cx. (Maillotia) hortensis. The taxon formerly identified as Cx. (Neoculex) territans was shown to comprise two distinct species, neither of which correspond to Cx. territans s.s. These include Cx. (Neo.) impudicus and another uncertain species, which may be Cx. (Neo.) europaeus or Cx. (Neo.) martinii (herein =Cx. (Neo.) sp. 1). Detailed examination of the Pipiens Group revealed Cx. pipiens, Cx. pipiens f. molestus and the widespread presence of the highly efficient West Nile virus vector Cx. quinquefasciatus for the first time. Four new country records are reported, increasing the Culex of Turkey to 15 recognised species and Cx. pipiens f. molestus. Anew taxonomic checklist is provided, annotated with respective vector competencies for transmission of arboviruses. (C) 2014 The Authors. Published by Elsevier B.V. C1 [Gunay, Filiz; Alten, Bulent] Hacettepe Univ, Fac Sci, Dept Biol, Ecol Sect,ESRL Labs, TR-06800 Beytepe, Turkey. [Simsek, Fatih] Adnan Menderes Univ, Fac Sci & Literature, Dept Biol, Div Ecol, TR-09010 Kepez Aydin, Turkey. [Aldemir, Adnan] Kafkas Univ, Fac Sci & Literature, Dept Biol, TR-36100 Kars, Turkey. [Linton, Yvonne-Marie] Walter Reed Army Inst Res, Entomol Branch, Silver Spring, MD USA. [Linton, Yvonne-Marie] Smithsonian Inst, Museum Support Ctr, Walter Reed Biosystemat Unit, Suitland, MD 20746 USA. [Linton, Yvonne-Marie] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20560 USA. [Linton, Yvonne-Marie] Uniformed Serv Univ Hlth Sci, Fac Preventat Med & Biometr, Bethesda, MD 20814 USA. RP Linton, YM (reprint author), Walter Reed Army Inst Res, Entomol, Walter Reed Biosystemat Unit, Smithsonian Inst Museum Support Ctr, MRC-534,4210 Silver Hill Rd, Suitland, MD 20746 USA. EM gunayf@gmail.com; kaynas@hacettepe.edu.tr; fsimsek@adu.edu.tr; LintonY@si.edu FU EU SYNTHESYS programme at the Natural History Museum, London; AFHSC-GEIS-Global Emerging Infections Surveillance and Response System, a Division of the Armed Forces Health Surveillance Center [PO327_14_WR]; EU [FP7-261504]; National Research Council (NRC) Research Associateship Award at the Walter Reed Army Institute of Research FX This study forms part of the PhD study of FG, and contributes to the wider objectives of the global Mosquito Barcoding Initiative (MBI), headed by YML and R.C. Wilkerson (Walter Reed Biosystematics Unit). We are thankful to Ms Hilal Bedir for assisting FG and YML in the field in August 2011 and to Dr Berna Demirci (both of Kafkas University, Kars, Turkey) for donations of Culex specimens. Some data reported in this manuscript was generated during a training period for FG funded through the EU SYNTHESYS programme at the Natural History Museum, London, with the remainder generated at the Laboratory of Analytical Biology, Smthsonian Institution, Washington, USA. Data was analysed and prepared for publication while YML, BA and FG held a project grant from AFHSC-GEIS-Global Emerging Infections Surveillance and Response System, a Division of the Armed Forces Health Surveillance Center (Project Grant Award PO327_14_WR to YML). Field studies were supported by EU grant FP7-261504 EDENext and is catalogued by the EDENext Steering Committee as EDENext-269. This manuscript was prepared whilst YML held a National Research Council (NRC) Research Associateship Award at the Walter Reed Army Institute of Research. The material to be published reflects the views of the authors and should not be construed to represent those of the US Department of the Army or the US Department of Defense. NR 83 TC 7 Z9 7 U1 5 U2 15 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0001-706X EI 1873-6254 J9 ACTA TROP JI Acta Trop. PD MAR PY 2015 VL 143 BP 112 EP 120 DI 10.1016/j.actatropica.2014.10.013 PG 9 WC Parasitology; Tropical Medicine SC Parasitology; Tropical Medicine GA CC7DB UT WOS:000350526800016 PM 25446171 ER PT J AU Abavandimwe, D Galbany, J Breuer, T Ndagijimana, F Stoinski, TS Mcfarlin, SC AF Abavandimwe, Didier Galbany, Jordi Breuer, Thomas Ndagijimana, Felix Stoinski, Tara S. Mcfarlin, Shannon C. TI Body growth in wild mountain gorillas (Gorilla beringei beringei) from Volcanoes National Park, Rwanda SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 84th Annual Meeting of the American-Association-of-Physical-Anthropologists CY MAR 25-28, 2015 CL St Louis, MO SP Amer Assoc Phys Anthropologists C1 [Abavandimwe, Didier; Ndagijimana, Felix; Stoinski, Tara S.] Dian Fossey Gorilla Fund Int, Karisoke Res Ctr, Ruhengeri, Rwanda. [Galbany, Jordi; Mcfarlin, Shannon C.] George Washington Univ, Anthropol, Washington, DC 20052 USA. [Galbany, Jordi; Mcfarlin, Shannon C.] George Washington Univ, Ctr Adv Study Hominid Paleobiol, Washington, DC 20052 USA. [Breuer, Thomas] Wildlife Conservat Soc, Mbeli Bai Study, Nouabale Ndoki Natl Pk, Sangha, Congo. [Stoinski, Tara S.] Zoo Atlanta, Primate Res, Washington, DC USA. [Mcfarlin, Shannon C.] Smithsonian Inst, Natl Museum Nat Hist, Div Mammals, Washington, DC 20560 USA. NR 0 TC 2 Z9 2 U1 2 U2 13 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0002-9483 EI 1096-8644 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PD MAR PY 2015 VL 156 SU 60 SI SI BP 65 EP 65 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA CC8CE UT WOS:000350594900002 ER PT J AU Cargill, TM AF Cargill, Tyler M. TI A bioarchaeological exploration of scorbutic cranial lesions and a proposed etiology SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 84th Annual Meeting of the American-Association-of-Physical-Anthropologists CY MAR 25-28, 2015 CL St Louis, MO SP Amer Assoc Phys Anthropologists C1 [Cargill, Tyler M.] Smithsonian Inst, Dept Anthropol, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 1 U2 1 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0002-9483 EI 1096-8644 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PD MAR PY 2015 VL 156 SU 60 SI SI BP 101 EP 101 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA CC8CE UT WOS:000350594900141 ER PT J AU Clark, AN Guatelli-Steinberg, D Hubbe, M Ferrell, R AF Clark, Allison N. Guatelli-Steinberg, Debbie Hubbe, Mark Ferrell, Rebecca TI Lateral enamel formation of anterior teeth and life history in New World monkeys SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 84th Annual Meeting of the American-Association-of-Physical-Anthropologists CY MAR 25-28, 2015 CL St Louis, MO SP Amer Assoc Phys Anthropologists C1 [Clark, Allison N.; Guatelli-Steinberg, Debbie; Hubbe, Mark] Ohio State Univ, Dept Anthropol, Columbus, OH 43210 USA. [Ferrell, Rebecca] Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0002-9483 EI 1096-8644 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PD MAR PY 2015 VL 156 SU 60 SI SI BP 105 EP 106 PG 2 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA CC8CE UT WOS:000350594900159 ER PT J AU Crofoot, MC Strandburg-Peshkin, A Farine, D AF Crofoot, Margaret C. Strandburg-Peshkin, Ariana Farine, Damien TI Simultaneous tracking of wild baboons reveals individual and social drivers of troop organization SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 84th Annual Meeting of the American-Association-of-Physical-Anthropologists CY MAR 25-28, 2015 CL St Louis, MO SP Amer Assoc Phys Anthropologists C1 [Crofoot, Margaret C.; Farine, Damien] Univ Calif Davis, Dept Anthropol, Davis, CA 95616 USA. [Crofoot, Margaret C.; Farine, Damien] Smithsonian Inst, Smithsonian Trop Res Inst, Washington, DC 20560 USA. [Farine, Damien] Univ Oxford, Edward Grey Inst Field Ornithol, Oxford OX1 2JD, England. [Strandburg-Peshkin, Ariana] Princeton Univ, Dept Ecol & Evolutionary, Princeton, NJ 08544 USA. NR 0 TC 0 Z9 0 U1 1 U2 3 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0002-9483 EI 1096-8644 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PD MAR PY 2015 VL 156 SU 60 SI SI BP 112 EP 112 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA CC8CE UT WOS:000350594900186 ER PT J AU Fernandez, A Hunt, DR AF Fernandez, Aileen Hunt, David R. TI Sex determination from the human sacrum: A re-assessment SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 84th Annual Meeting of the American-Association-of-Physical-Anthropologists CY MAR 25-28, 2015 CL St Louis, MO SP Amer Assoc Phys Anthropologists C1 [Fernandez, Aileen] Lehman Coll Cuny, Dept Anthropol, Bronx, NY USA. [Hunt, David R.] Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 1 U2 2 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0002-9483 EI 1096-8644 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PD MAR PY 2015 VL 156 SU 60 SI SI BP 132 EP 132 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA CC8CE UT WOS:000350594901025 ER PT J AU Guevara, EF Saltonstall, K Caccone, A Mundy, NI Bradley, BJ AF Guevara, Elaine F. Saltonstall, Kristin Caccone, Adalgisa Mundy, Nicholas I. Bradley, Brenda J. TI Examining the co-evolution of primates and angiosperms: Brazzein sweet proteins and gorilla taste receptors SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 84th Annual Meeting of the American-Association-of-Physical-Anthropologists CY MAR 25-28, 2015 CL St Louis, MO SP Amer Assoc Phys Anthropologists C1 [Guevara, Elaine F.; Bradley, Brenda J.] Yale Univ, Dept Anthropol, New Haven, CT 06520 USA. [Saltonstall, Kristin] Smithsonian Trop Res Inst, Balboa, Panama. [Caccone, Adalgisa] Yale Univ, Dept Ecol & Evolutionary Biol, New Haven, CT 06520 USA. [Mundy, Nicholas I.] Univ Cambridge, Dept Zool, Cambridge CB2 1TN, England. [Bradley, Brenda J.] George Washington Univ, Dept Anthropol, Washington, DC 20052 USA. NR 0 TC 0 Z9 0 U1 3 U2 13 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0002-9483 EI 1096-8644 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PD MAR PY 2015 VL 156 SU 60 SI SI BP 154 EP 154 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA CC8CE UT WOS:000350594901113 ER PT J AU Hunt, DR Dimichele, D AF Hunt, David R. Dimichele, Daniel TI Postcraniometric databank for the Robert J. Terry Collection: On-line access, data sharing, and discussion for measurement standardization SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 84th Annual Meeting of the American-Association-of-Physical-Anthropologists CY MAR 25-28, 2015 CL St Louis, MO SP Amer Assoc Phys Anthropologists C1 [Hunt, David R.; Dimichele, Daniel] Smithsonian Inst, Dept Anthropol, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0002-9483 EI 1096-8644 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PD MAR PY 2015 VL 156 SU 60 SI SI BP 173 EP 173 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA CC8CE UT WOS:000350594901189 ER PT J AU Jungers, WL Grine, FE Leakey, MG Leakey, L Brown, F Yang, DM Tocheri, MW AF Jungers, William L. Grine, Frederick E. Leakey, Meave G. Leakey, Louise Brown, Frank Yang, Deming Tocheri, Matthew W. TI New hominin fossils from Ileret (Kolom Odiet), Kenya SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 84th Annual Meeting of the American-Association-of-Physical-Anthropologists CY MAR 25-28, 2015 CL St Louis, MO SP Amer Assoc Phys Anthropologists C1 [Jungers, William L.] SUNY Stony Brook, Dept Anat Sci, Stony Brook, NY USA. [Grine, Frederick E.; Leakey, Meave G.; Leakey, Louise] SUNY Stony Brook, Dept Anthropol, Stony Brook, NY USA. [Leakey, Meave G.; Leakey, Louise] Turkana Basin Inst, Nairobi, Kenya. [Brown, Frank] Univ Utah, Dept Geol & Geophys, Salt Lake City, UT 84112 USA. [Yang, Deming] SUNY Stony Brook, IDPAS, Stony Brook, NY USA. [Tocheri, Matthew W.] Smithsonian Inst, Anthropol & Human Origins Program, Washington, DC 20560 USA. NR 0 TC 1 Z9 1 U1 1 U2 3 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0002-9483 EI 1096-8644 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PD MAR PY 2015 VL 156 SU 60 SI SI BP 181 EP 181 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA CC8CE UT WOS:000350594901221 ER PT J AU Killough, ML Hunt, D Eriksen, AB Stoinski, TS Bromage, TG Cranfield, MR Mudakikwa, A Mcfarlin, SC AF Killough, Meredith L. Hunt, David Eriksen, Amandine B. Stoinski, Tara S. Bromage, Timothy G. Cranfield, Michael R. Mudakikwa, Antoine Mcfarlin, Shannon C. TI Skeletal pathology in individually documented wild Virunga mountain gorillas SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 84th Annual Meeting of the American-Association-of-Physical-Anthropologists CY MAR 25-28, 2015 CL St Louis, MO SP Amer Assoc Phys Anthropologists C1 [Killough, Meredith L.] George Washington Univ, Dept Anthropol, Washington, DC 20052 USA. [Hunt, David] Smithsonian Inst, Natl Museum Nat Hist, Div Phys Anthropol, Washington, DC 20560 USA. [Eriksen, Amandine B.] SUNY Buffalo, Dept Anthropol, Buffalo, NY 14260 USA. [Stoinski, Tara S.] Dian Fossey Gorilla Fund Int, Atlanta, GA USA. [Stoinski, Tara S.] Zoo Atlanta, Atlanta, GA USA. [Bromage, Timothy G.] NYU, Coll Dent, Dept Biomat & Biomimet, New York, NY 10003 USA. [Cranfield, Michael R.] Univ Calif Davis, Mt Gorilla Vet Project, Davis, CA 95616 USA. [Cranfield, Michael R.] Baltimore Zoo, Baltimore, MD USA. [Mudakikwa, Antoine] Rwanda Dev Board, Dept Tourism & Conservat, Kigali, Rwanda. [Mcfarlin, Shannon C.] George Washington Univ, Dept Anthropol, Ctr Adv Study Hominid Paleobiol, Washington, DC 20052 USA. [Mcfarlin, Shannon C.] Smithsonian Inst, Natl Museum Nat Hist, Div Mammals, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 1 U2 3 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0002-9483 EI 1096-8644 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PD MAR PY 2015 VL 156 SU 60 SI SI BP 186 EP 187 PG 2 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA CC8CE UT WOS:000350594901243 ER PT J AU Lambert, PM Sholts, SB Erlandson, JM AF Lambert, Patricia M. Sholts, Sabrina B. Erlandson, Jon M. TI Life on the Santa Barbara Channel Islands, ca. 9,500 BP: Insights from the Dentition of Tuqan Man SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 84th Annual Meeting of the American-Association-of-Physical-Anthropologists CY MAR 25-28, 2015 CL St Louis, MO SP Amer Assoc Phys Anthropologists C1 [Lambert, Patricia M.] Utah State Univ, Anthropol Program, Logan, UT 84322 USA. [Sholts, Sabrina B.] Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20560 USA. [Erlandson, Jon M.] Univ Oregon, Dept Anthropol, Eugene, OR 97403 USA. NR 0 TC 0 Z9 0 U1 2 U2 15 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0002-9483 EI 1096-8644 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PD MAR PY 2015 VL 156 SU 60 SI SI BP 197 EP 198 PG 2 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA CC8CE UT WOS:000350594901286 ER PT J AU Pobiner, B AF Pobiner, Briana TI The Smithsonian's Human Origins Program: Broadening and deepening public engagement with human evolution through social media SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 84th Annual Meeting of the American-Association-of-Physical-Anthropologists CY MAR 25-28, 2015 CL St Louis, MO SP Amer Assoc Phys Anthropologists C1 [Pobiner, Briana] Smithsonian Inst, Dept Anthropol, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 1 U2 2 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0002-9483 EI 1096-8644 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PD MAR PY 2015 VL 156 SU 60 SI SI BP 254 EP 254 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA CC8CE UT WOS:000350594901511 ER PT J AU Renner, ER Subiaul, F AF Renner, Elizabeth R. Subiaul, Francys TI Individual, Observational, and Imitation Learning in Orangutans SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 84th Annual Meeting of the American-Association-of-Physical-Anthropologists CY MAR 25-28, 2015 CL St Louis, MO SP Amer Assoc Phys Anthropologists C1 [Renner, Elizabeth R.; Subiaul, Francys] George Washington Univ, Dept Anthropol, Washington, DC 20052 USA. [Subiaul, Francys] George Washington Univ, Dept Speech & Hearing Sci, Washington, DC 20052 USA. [Subiaul, Francys] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 7 U2 15 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0002-9483 EI 1096-8644 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PD MAR PY 2015 VL 156 SU 60 SI SI BP 265 EP 265 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA CC8CE UT WOS:000350594901554 ER PT J AU Richmond, BG Roach, NT Hatala, KG Ostrofsky, K Behrensmeyer, AK Bobe, R Braun, DR Reeves, J Kiura, P Villmoare, B AF Richmond, Brian G. Roach, Neil T. Hatala, Kevin G. Ostrofsky, Kelly Behrensmeyer, Anna K. Bobe, Rene Braun, David R. Reeves, Jonathan Kiura, Purity Villmoare, Brian TI What can footprint assemblages tell us about early hominin habitat preferences and social behavior? SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 84th Annual Meeting of the American-Association-of-Physical-Anthropologists CY MAR 25-28, 2015 CL St Louis, MO SP Amer Assoc Phys Anthropologists C1 [Richmond, Brian G.; Roach, Neil T.] Amer Museum Nat Hist, Div Anthropol, New York, NY 10024 USA. [Richmond, Brian G.; Roach, Neil T.; Hatala, Kevin G.; Ostrofsky, Kelly; Bobe, Rene; Braun, David R.; Reeves, Jonathan] George Washington Univ, Ctr Adv Study Hominid Paleobiol, Washington, DC 20052 USA. [Hatala, Kevin G.] Max Planck Inst Evolutionary Anthropol, Dept Human Evolut, Leipzig, Germany. [Behrensmeyer, Anna K.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. [Kiura, Purity] Natl Museums Kenya, Archaeol Dept, Nairobi, Kenya. [Villmoare, Brian] Univ Nevada Las Vegas, Dept Anthropol, Las Vegas, NV USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0002-9483 EI 1096-8644 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PD MAR PY 2015 VL 156 SU 60 SI SI BP 266 EP 267 PG 2 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA CC8CE UT WOS:000350594901560 ER PT J AU Schwarcz, HP Stafford, T Chisholm, BS Burchell, M Knyf, M Owsley, DW AF Schwarcz, Henry P. Stafford, Thomas, Jr. Chisholm, Brian S. Burchell, Meghan Knyf, Martin Owsley, Douglas W. TI Kennewick Man: paleodiet, and the people of the Pacific Northwest Coast SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 84th Annual Meeting of the American-Association-of-Physical-Anthropologists CY MAR 25-28, 2015 CL St Louis, MO SP Amer Assoc Phys Anthropologists C1 [Schwarcz, Henry P.; Knyf, Martin] McMaster Univ, Sch Geog & Earth Sci, Hamilton, ON, Canada. [Stafford, Thomas, Jr.] Univ Aarhus, Dept Phys & Astron, Aarhus, Denmark. [Chisholm, Brian S.] Univ British Columbia, Dept Anthropol, Vancouver, BC V5Z 1M9, Canada. [Burchell, Meghan] Mem Univ Newfoundland, Dept Archaeol, St John, NF, Canada. [Owsley, Douglas W.] Smithsonian Inst, Dept Anthropol, US Natl Museum Nat Hist, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 2 U2 6 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0002-9483 EI 1096-8644 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PD MAR PY 2015 VL 156 SU 60 SI SI BP 281 EP 282 PG 2 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA CC8CE UT WOS:000350594902045 ER PT J AU Sherwood, KD Owsley, DW Bruwelheide, KS Rouse, SL Hurlbert, DE AF Sherwood, Kate D. Owsley, Douglas W. Bruwelheide, Kari S. Rouse, Stephen L. Hurlbert, Donald E. TI Basketmakers revealed: Physical, CT, and 3D analyses of mummified human remains from the southwest SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 84th Annual Meeting of the American-Association-of-Physical-Anthropologists CY MAR 25-28, 2015 CL St Louis, MO SP Amer Assoc Phys Anthropologists C1 [Sherwood, Kate D.; Owsley, Douglas W.; Bruwelheide, Kari S.; Rouse, Stephen L.; Hurlbert, Donald E.] Smithsonian Inst, Dept Anthropol, Natl Museum Nat Hist, Washington, DC 20560 USA. [Sherwood, Kate D.] Univ North Carolina Wilmington, Dept Anthropol, Wilmington, NC USA. [Hurlbert, Donald E.] Smithsonian Inst, Natl Museum Nat Hist Imaging, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 1 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0002-9483 EI 1096-8644 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PD MAR PY 2015 VL 156 SU 60 SI SI BP 287 EP 287 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA CC8CE UT WOS:000350594902066 ER PT J AU Thompson, RC Allam, AH Lombardi, GP Wann, LS Sutherland, ML Sutherland, JD Zink, A Soliman, MA Frohlich, B Monge, JM Vallodolid, CM Cox, SE Abd El-Maksoud, G Badr, I Miyamoto, M Nured-Din, AEH Watson, L Michalik, D King, SI Narula, J Finch, CE Thomas, GS AF Thompson, Randall C. Allam, Adel H. Lombardi, Guido P. Wann, L. Samuel Sutherland, M. Linda Sutherland, James D. Zink, Albert Soliman, Muhammad Al-Tohamy Frohlich, Bruno Monge, Janet M. Vallodolid, Clide M. Cox, Samantha E. Abd El-Maksoud, Gomaa Badr, Ibrahim Miyamoto, Michael Nured-Din, Abd El-Halim Watson, Luchia Michalik, David King, Samantha I. Narula, Jagat Finch, Caleb E. Thomas, Gregory S. TI CT Evidence of Atherosclerosis in Ancient Mummies: The Horus Study of 220 Mummies from 5 Continents SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 84th Annual Meeting of the American-Association-of-Physical-Anthropologists CY MAR 25-28, 2015 CL St Louis, MO SP Amer Assoc Phys Anthropologists C1 [Thompson, Randall C.; King, Samantha I.] Mid Amer Heart Inst, Dept Cardiovasc Dis, Kansas City, MO 64111 USA. [Allam, Adel H.] Al Azhar Med Sch, Dept Cardiovasc Dis, Cairo, Egypt. [Lombardi, Guido P.] Univ Peruana Cayetano Heredia, Dept Paleopathol, Lima, Peru. [Wann, L. Samuel] St Marys Healthcare, Dept Cardiovasc Dis, Milwaukee, WI USA. [Sutherland, M. Linda] Newport Diagnost Ctr, Dept Radiol, Newport Beach, CA USA. [Sutherland, James D.] South Coast Radiol Med Grp, Dept Radiol, Laguna Hills, CA USA. [Zink, Albert] European Acad Bolzano Bozen EURAC, Inst Mummies & Iceman, Bolzano, Italy. [Soliman, Muhammad Al-Tohamy; Nured-Din, Abd El-Halim] Natl Res Ctr, Dept Preservat, Giza, Egypt. [Monge, Janet M.; Cox, Samantha E.] Univ Penn, Museum Archeol & Anthropol, Dept Archaeol, Philadelphia, PA 19104 USA. [Vallodolid, Clide M.] Museo Sitio Puruchuco Antro Jimenez Borja, Lima, Peru. [Cox, Samantha E.] Univ Cambridge, Dept Archaeol, Cambridge CB2 3DZ, England. [Abd El-Maksoud, Gomaa] Cairo Univ, Dept Preservat, Cairo, Egypt. [Badr, Ibrahim] Inst Restorat, Dept Preservat, Alexandria, Egypt. [Miyamoto, Michael] Mission Internal Med Grp, Dept Cardiovasc Dis, Mission Viejo, CA USA. [Watson, Luchia] Univ Peruana Cayetano Heredia, Dept Archaeol, Lima, Peru. [Michalik, David; Thomas, Gregory S.] Long Beach Mem Med Ctr, Dept Cardiovasc Dis, Los Angeles, CA USA. [Narula, Jagat] Mt Sinai Med Ctr, Dept Cardiovasc Dis, New York, NY 10029 USA. [Finch, Caleb E.] Univ So Calif, Dept Biol & Aging, Los Angeles, CA USA. [Frohlich, Bruno] Smithsonian Inst, Dept Archaeol, Washington, DC 20560 USA. RI Zink, Albert/P-4024-2015 OI Zink, Albert/0000-0002-1461-747X NR 0 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0002-9483 EI 1096-8644 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PD MAR PY 2015 VL 156 SU 60 SI SI BP 305 EP 305 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA CC8CE UT WOS:000350594902136 ER PT J AU Zink, AR Wann, S Thompson, RC Keller, A Maixner, F Allam, AH Finch, CE Frohlich, B Lombardi, GP Sutherland, ML Sutherland, JD Watson, L Cox, SL Miyamoto, MI Narula, J Stewart, AF Krause, J Thomas, GS AF Zink, Albert R. Wann, Samuel Thompson, Randall C. Keller, Andreas Maixner, Frank Allam, Adel H. Finch, Caleb E. Frohlich, Bruno Lombardi, Guido P. Sutherland, M. Linda Sutherland, James D. Watson, Lucia Cox, Samantha L. Miyamoto, Michael I. Narula, Jagat Stewart, Alexandre F. Krause, Johannes Thomas, Gregory S. TI The Genetic Background of Atherosclerosis in Ancient Mummies SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 84th Annual Meeting of the American-Association-of-Physical-Anthropologists CY MAR 25-28, 2015 CL St Louis, MO SP Amer Assoc Phys Anthropologists C1 [Zink, Albert R.; Maixner, Frank] European Acad EURAC, Inst Mummies & Iceman, Bolzano, Italy. [Thompson, Randall C.] Univ Missouri Kansas City, St Lukes Mid Amer Heart Inst, Kansas City, MO USA. [Keller, Andreas] Univ Saarland, Dept Clin Bioinformat, D-66123 Saarbrucken, Germany. [Allam, Adel H.] Al Azhar Univ, Sch Med, Cairo, Egypt. [Finch, Caleb E.] Univ So Calif, Davis Sch Gerontol, Los Angeles, CA 90089 USA. [Frohlich, Bruno] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. [Lombardi, Guido P.] Univ Peruana Cayetano Heredia, Catedra Pedro Weiss, San Martin De Porres, Peru. [Sutherland, M. Linda] Newport Diagnost Ctr, Newport Beach, CA USA. [Sutherland, James D.] Med Ctr Laguna Hills, Saddleback Mem, Laguna Hills, CA USA. [Watson, Lucia] Univ Nacl Autonoma Mexico, Mexico City 04510, DF, Mexico. [Cox, Samantha L.] Univ Cambridge, Dept Archaeol, Cambridge CB2 1TN, England. [Miyamoto, Michael I.] Miss Viejo, Miss Heritage Med Grp, Mission Viejo, CA USA. [Narula, Jagat] Icahn Sch Med Mt Sinai, Zena & Michael A Wiener Cardiovasc Inst, New York, NY 10029 USA. [Stewart, Alexandre F.] Univ Ottawa, Inst Heart, John & Jennifer Ruddy Canadian Cardiovasc Genet C, Ottawa, ON K1N 6N5, Canada. [Krause, Johannes] Univ Tubingen, Inst Archaeol Sci, Tubingen, Germany. [Thomas, Gregory S.] Univ Calif Irvine, Long Beach Mem, MemorialCare Heart & Vasc Inst, Irvine, CA USA. RI Krause, Johannes/E-6640-2015; Zink, Albert/P-4024-2015 OI Krause, Johannes/0000-0001-5475-4690; Zink, Albert/0000-0002-1461-747X NR 0 TC 0 Z9 0 U1 0 U2 5 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0002-9483 EI 1096-8644 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PD MAR PY 2015 VL 156 SU 60 SI SI BP 332 EP 333 PG 2 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA CC8CE UT WOS:000350594902242 ER PT J AU Drabent, A Hoeft, M Pizzo, RF Bonafede, A van Weeren, RJ Klein, U AF Drabent, A. Hoeft, M. Pizzo, R. F. Bonafede, A. van Weeren, R. J. Klein, U. TI Diffuse radio emission in the complex merging galaxy cluster Abell 2069 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE magnetic fields; radiation mechanisms: non-thermal; turbulence; galaxies: clusters: individual: Abell 2069; galaxies: clusters: intracluster medium ID CORONA BOREALIS SUPERCLUSTER; COOLING FLOW CLUSTERS; COSMIC-RAY PROTONS; GAMMA-RAY; COMA CLUSTER; SKY SURVEY; NONTHERMAL EMISSION; SCALING RELATIONS; NORRIS SURVEY; MINI-HALOS AB Context. Galaxy clusters with signs of a recent merger in many cases show extended diffuse radio features. This emission originates from relativistic electrons that suffer synchrotron losses due to the intracluster magnetic field. The mechanisms of particle acceleration and the properties of the magnetic field are still poorly understood. Aims. We search for diffuse radio emission in galaxy clusters. Here, we study the complex galaxy cluster Abell 2069, for which X-ray observations indicate a recent merger. Methods. We investigate the cluster's radio continuum emission by deep Westerbork Synthesis Radio Telescope (WSRT) observations at 346 MHz and Giant Metrewave Radio Telescope (GMRT) observations at 322 MHz. Results. We find an extended diffuse radio feature roughly coinciding with the main component of the cluster. We classify this emission as a radio halo and estimate its lower limit flux density at 25 +/- 9 mJy. Moreover, we find a second extended diffuse source located at the cluster's companion and estimate its flux density at 15 +/- 2 mJy. We speculate that this is a small halo or a mini-halo. If true, this cluster is the first example of a double-halo in a single galaxy cluster. C1 [Drabent, A.; Hoeft, M.] Thuringer Landessternwarte TLS, D-07778 Tautenburg, Germany. [Pizzo, R. F.] ASTRON Netherlands Inst Radio Astron, NL-7991 PD Dwingeloo, Netherlands. [Bonafede, A.] Hamburger Sternwarte, D-21029 Hamburg, Germany. [van Weeren, R. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Klein, U.] Univ Bonn, Argelander Inst Radioastron, D-53121 Bonn, Germany. RP Drabent, A (reprint author), Thuringer Landessternwarte TLS, Sternwarte 5, D-07778 Tautenburg, Germany. EM alex@tls-tautenburg.de OI van Weeren, Reinout/0000-0002-0587-1660 FU DFG, in the framework of the DFG Forschergruppe [1254]; NASA - Chandra X-ray Center [PF2-130104]; NASA [NAS8-03060]; Alfred P. Sloan Foundation; National Science Foundation; US Department of Energy Office of Science FX The authors thank the anonymous referee for useful comments and suggestions which have significantly improved the manuscript. M.H. and U.K. acknowledge financial support by the DFG, in the framework of the DFG Forschergruppe 1254 "Magnetisation of Interstellar and Intergalactic Media: The Prospects of Low-Frequency Radio Observations". R.J.W. is supported by NASA through the Einstein Postdoctoral grant number PF2-130104 awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. This research has made use of data obtained from the Chandra Data Archive and the Chandra Source Catalog, and software provided by the Chandra X-ray Center (CXC) in the application packages CIAO, ChIPS, and Sherpa. Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the US Department of Energy Office of Science. SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration. NR 46 TC 1 Z9 1 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAR PY 2015 VL 575 AR A8 DI 10.1051/0004-6361/201424828 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CC3LA UT WOS:000350249100008 ER PT J AU Garsden, H Girard, JN Starck, JL Corbel, S Tasse, C Woiselle, A McKean, JP van Amesfoort, AS Anderson, J Avruch, IM Beck, R Bentum, MJ Best, P Breitling, F Broderick, J Bruggen, M Butcher, HR Ciardi, B de Gasperin, F de Geus, E de Vos, M Duscha, S Eisloffel, J Engels, D Falcke, H Fallows, RA Fender, R Ferrari, C Frieswijk, W Garrett, MA Griessmeier, J Gunst, AW Hassall, TE Heald, G Hoeft, M Horandel, J van der Horst, A Juette, E Karastergiou, A Kondratiev, VI Kramer, M Kuniyoshi, M Kuper, G Mann, G Markoff, S McFadden, R McKay-Bukowski, D Mulcahy, DD Munk, H Norden, MJ Orru, E Paas, H Pandey-Pommier, M Pandey, VN Pietka, G Pizzo, R Polatidis, AG Renting, A Rottgering, H Rowlinson, A Schwarz, D Sluman, J Smirnov, O Stappers, BW Steinmetz, M Stewart, A Swinbank, J Tagger, M Tang, Y Tasse, C Thoudam, S Toribio, C Vermeulen, R Vocks, C van Weeren, RJ Wijnholds, SJ Wise, MW Wucknitz, O Yatawatta, S Zarka, P Zensus, A AF Garsden, H. Girard, J. N. Starck, J. L. Corbel, S. Tasse, C. Woiselle, A. McKean, J. P. van Amesfoort, A. S. Anderson, J. Avruch, I. M. Beck, R. Bentum, M. J. Best, P. Breitling, F. Broderick, J. Brueggen, M. Butcher, H. R. Ciardi, B. de Gasperin, F. de Geus, E. de Vos, M. Duscha, S. Eisloeffel, J. Engels, D. Falcke, H. Fallows, R. A. Fender, R. Ferrari, C. Frieswijk, W. Garrett, M. A. Griessmeier, J. Gunst, A. W. Hassall, T. E. Heald, G. Hoeft, M. Hoerandel, J. van der Horst, A. Juette, E. Karastergiou, A. Kondratiev, V. I. Kramer, M. Kuniyoshi, M. Kuper, G. Mann, G. Markoff, S. McFadden, R. McKay-Bukowski, D. Mulcahy, D. D. Munk, H. Norden, M. J. Orru, E. Paas, H. Pandey-Pommier, M. Pandey, V. N. Pietka, G. Pizzo, R. Polatidis, A. G. Renting, A. Roettgering, H. Rowlinson, A. Schwarz, D. Sluman, J. Smirnov, O. Stappers, B. W. Steinmetz, M. Stewart, A. Swinbank, J. Tagger, M. Tang, Y. Tasse, C. Thoudam, S. Toribio, C. Vermeulen, R. Vocks, C. van Weeren, R. J. Wijnholds, S. J. Wise, M. W. Wucknitz, O. Yatawatta, S. Zarka, P. Zensus, A. TI LOFAR sparse image reconstruction SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE techniques: interferometric; methods: numerical; techniques: image processing ID UNDERSTANDING RADIO POLARIMETRY; W-PROJECTION ALGORITHM; INTERFEROMETRIC IMAGES; APERTURE SYNTHESIS; WIDE-FIELD; DECONVOLUTION; CALIBRATION; ASTRONOMY; SYSTEM; ARRAY AB Context. The LOw Frequency ARray (LOFAR) radio telescope is a giant digital phased array interferometer with multiple antennas distributed in Europe. It provides discrete sets of Fourier components of the sky brightness. Recovering the original brightness distribution with aperture synthesis forms an inverse problem that can be solved by various deconvolution and minimization methods. Aims. Recent papers have established a clear link between the discrete nature of radio interferometry measurement and the "compressed sensing" (CS) theory, which supports sparse reconstruction methods to form an image from the measured visibilities. Empowered by proximal theory, CS offers a sound framework for efficient global minimization and sparse data representation using fast algorithms. Combined with instrumental direction-dependent effects (DDE) in the scope of a real instrument, we developed and validated a new method based on this framework. Methods. We implemented a Sparse reconstruction method in the standard LOFAR imaging tool and compared the photometric and resolution performance of this new imager with that of CLEAN based methods (CLEAN and MS CLEAN) with simulated and real LOFAR data. Results. We show that 0 sparse reconstruction performs as well as CLEAN in recovering the flux of point sources; performs much better on extended objects (the root mean square error is reduced by a factor of up to 10): and iii) provides a solution with an effective angular resolution 2-3 times better than the CLEAN images. Conclusions. Sparse recovery gives a correct photometry on high dynamic and wide-field images and improved realistic structures of extended sources (of simulated and real LOFAR datasets), This sparse reconstruction method is compatible with modern interferometric imagers that handle DDE corrections (A- and W-projections) required for current and future instruments such as LOFAR and SKA. C1 [Garsden, H.; Girard, J. N.; Starck, J. L.; Corbel, S.; Woiselle, A.] Univ Paris 07, Lab AIM, CNRS, CEA Saclay,DSM,IRFU,SAp, F-91191 Gif Sur Yvette, France. [Tasse, C.] Rhodes Univ, Dept Phys & Elect, ZA-6140 Grahamstown, South Africa. [Tasse, C.] SKA South Africa, ZA-7405 Phielands, South Africa. [Woiselle, A.] Sagem Safran, F-75512 Paris 15, France. [McKean, J. P.; van Amesfoort, A. S.; Bentum, M. J.; de Geus, E.; de Vos, M.; Duscha, S.; Falcke, H.; Fallows, R. A.; Frieswijk, W.; Garrett, M. A.; Gunst, A. W.; Heald, G.; Kondratiev, V. I.; Kuper, G.; Mann, G.; McFadden, R.; Munk, H.; Norden, M. J.; Orru, E.; Pandey, V. N.; Pizzo, R.; Polatidis, A. G.; Renting, A.; Sluman, J.; Tang, Y.; Toribio, C.; Vermeulen, R.; Wijnholds, S. J.; Wise, M. W.; Yatawatta, S.] Netherlands Inst Radio Astron ASTRON, NL-7990 AA Dwingeloo, Netherlands. [Anderson, J.] Deutsch GeoForschungsZentrum GFZ, Helmholtz Zentrum Potsdam, Dept Geodesy & Remote Sensing 1, D-14473 Potsdam, Germany. [Breitling, F.; Mann, G.; Steinmetz, M.; Vocks, C.] Leibniz Inst Astrophys Potsdam AIP, D-14482 Potsdam, Germany. [Avruch, I. M.] SRON Netherlands Inst Space Res, NL-9700 AV Groningen, Netherlands. [Avruch, I. M.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Beck, R.; Kramer, M.; Kuniyoshi, M.; Mulcahy, D. D.; Wucknitz, O.; Zensus, A.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Bentum, M. J.] Univ Twente, NL-7522 Enschede, Netherlands. [Best, P.] Univ Edinburgh, Inst Astron, Royal Observ Edinburgh, Edinburgh EH9 3HJ, Midlothian, Scotland. [Broderick, J.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Brueggen, M.; de Gasperin, F.] Univ Hamburg, D-21029 Hamburg, Germany. [Butcher, H. R.] Australian Natl Univ, Res Sch Astron & Astrophys, Mt Stromlo Obs, Weston, ACT 2611, Australia. [Ciardi, B.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [de Geus, E.] SmarterVision BV, NL-9401 JX Assen, Netherlands. [Eisloeffel, J.] Thuringer Landessternwarte, D-07778 Tautenburg, Germany. [Engels, D.] Hamburger Sternwarte, D-21029 Hamburg, Germany. [Falcke, H.; Hoerandel, J.; Thoudam, S.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6500 GL Nijmegen, Netherlands. [Fender, R.; Karastergiou, A.; Pietka, G.; Stewart, A.] Univ Oxford, Astrophys, Oxford OX1 3RH, England. [Ferrari, C.] Univ Nice Sophia Antipolis, Observ Cote Azur, CNRS, Lab Lagrange,UMR7293, F-06189 Nice, France. [Garrett, M. A.; Roettgering, H.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Griessmeier, J.; Tagger, M.] Univ Orleans, LPC2E, CNRS, F-45071 Orleans 2, France. [Griessmeier, J.] Univ Orleans, OSUC, USR 704, Stn Radioastron Nancay,Obsev Paris CNRS INSU, F-18330 Nancay, France. [Hassall, T. E.; Kramer, M.; Stappers, B. W.] Univ Manchester, Sch Phys & Astron, Jodrell Bank, Ctr Astrophys, Manchester M13 9PL, Lancs, England. [van der Horst, A.; Markoff, S.; Rowlinson, A.; Swinbank, J.; Wise, M. W.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands. [Juette, E.] Ruhr Univ Bochum, Astron Inst, D-44780 Bochum, Germany. [Kondratiev, V. I.] Lebedev Phys Inst, Ctr Astro Space, Moscow 117997, Russia. [McKay-Bukowski, D.] Univ Oulu, Sodankyla Geophys Observ, Sodankyla 99600, Finland. [McKay-Bukowski, D.] STFC Rutherford Appleton Lab, Didcot OX11 0QX, Oxon, England. [Paas, H.] Univ Groningen, CIT, NL-9700 CA Groningen, Netherlands. [Pandey-Pommier, M.] Observ Lyon, Ctr Rech Astrophys Lyon, F-69561 St Genis Laval, France. [Schwarz, D.] Univ Bielefeld, Fak Phys, D-33615 Bielefeld, Germany. [Tasse, C.; Zarka, P.] Observ Paris, UMR CNRS 8109, LESIA, F-92195 Meudon, France. [van Weeren, R. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Girard, JN (reprint author), Univ Paris 07, Lab AIM, CNRS, CEA Saclay,DSM,IRFU,SAp, F-91191 Gif Sur Yvette, France. EM julien.girard@cea.fr RI Tagger, Michel/O-6615-2014; Ciardi, Benedetta/N-7625-2015; Kondratiev, Vladislav/N-1105-2015; Yatawatta, Sarod/E-6037-2013; OI Tagger, Michel/0000-0003-2962-3220; Kondratiev, Vladislav/0000-0001-8864-7471; Swinbank, John/0000-0001-9445-1846; Yatawatta, Sarod/0000-0001-5619-4017; de Gasperin, Francesco/0000-0003-4439-2627; Starck, Jean-Luc/0000-0003-2177-7794; Horandel, Jorg/0000-0001-6604-547X; van Weeren, Reinout/0000-0002-0587-1660 FU UnivEarthS Labex program of Sorbonne Paris Cite [ANR-10-LABX-0023, ANR-11-IDEX-0005-02]; European Research Council [ERC-228261]; Agence Nationale de la Recherche [ANR-09-JCJC-0001-01] FX H.G. and J.N.G. were responsible for the implementation of the CS code in the LOFAR imager (AWimager), J.N.G. wrote most of the article and performed all the scientific validation on simulated and real data. J.L.S. and S.C. conducted the research, supplied support. C.S. libraries, and wrote the independent version (SASIR) of the code. C.T. participated to the implementation of AWimager for LOFAR. A.W. wrote the preliminary version of the independent code. J.P.M. provided the LOFAR Cygnus A dataset. The other co-authors are part of the LOFAR builders list. We would like to thank all co-authors and the anonymous referee for their active contribution and/or insightful comments and reviews. We acknowledge the financial support from the UnivEarthS Labex program of Sorbonne Paris Cite (ANR-10-LABX-0023 and ANR-11-IDEX-0005-02) and from the European Research Council grant SparseAstro (ERC-228261). LOFAR, the Low Frequency Array designed and constructed by ASTRON, has facilities in several countries, that are owned by various parties (each with their own funding sources), and that are collectively operated by the International LOFAR Telescope (ILT) foundation under a joint scientific policy. C.F. acknowledges financial support by the Agence Nationale de la Recherche through grant ANR-09-JCJC-0001-01. VLA data of 3C 405 come from the online NRAO Archive (the National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc.). NR 63 TC 12 Z9 12 U1 1 U2 11 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 PY 2015 VL 575 AR A90 DI 10.1051/0004-6361/201424504 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CC3LA UT WOS:000350249100090 ER PT J AU Grazian, A Fontana, A Santini, P Dunlop, JS Ferguson, HC Castellano, M Amorin, R Ashby, MLN Barro, G Behroozi, P Boutsia, K Caputi, KI Chary, RR Dekel, A Dickinson, ME Faber, SM Fazio, GG Finkelstein, SL Galametz, A Giallongo, E Giavalisco, M Grogin, NA Guo, Y Kocevski, D Koekemoer, AM Koo, DC Lee, KS Lu, Y Merlin, E Mobasher, B Nonino, M Papovich, C Paris, D Pentericci, L Reddy, N Renzini, A Salmon, B Salvato, M Sommariva, V Song, M Vanzella, E AF Grazian, A. Fontana, A. Santini, P. Dunlop, J. S. Ferguson, H. C. Castellano, M. Amorin, R. Ashby, M. L. N. Barro, G. Behroozi, P. Boutsia, K. Caputi, K. I. Chary, R. R. Dekel, A. Dickinson, M. E. Faber, S. M. Fazio, G. G. Finkelstein, S. L. Galametz, A. Giallongo, E. Giavalisco, M. Grogin, N. A. Guo, Y. Kocevski, D. Koekemoer, A. M. Koo, D. C. Lee, K. -S. Lu, Y. Merlin, E. Mobasher, B. Nonino, M. Papovich, C. Paris, D. Pentericci, L. Reddy, N. Renzini, A. Salmon, B. Salvato, M. Sommariva, V. Song, M. Vanzella, E. TI The galaxy stellar mass function at 3.5 <= z <= 7.5 in the CANDELS/UDS, GOODS-South, and HUDF fields SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: luminosity function, mass function; galaxies: distances and redshifts; galaxies: evolution; galaxies: high-redshift ID STAR-FORMATION RATES; LYMAN BREAK GALAXIES; ORIGINS DEEP SURVEY; EXTRAGALACTIC LEGACY SURVEY; ACTIVE GALACTIC NUCLEI; HIGH-REDSHIFT GALAXIES; GIANT BRANCH STARS; LUMINOSITY FUNCTION; QUIESCENT GALAXIES; FORMATION HISTORY AB Context. The form and evolution of the galaxy stellar mass function (GSMF) at high redshifts provide crucial information on star formation history and mass assembly in the young Universe, close or even prior to the epoch of reionization. Aims. We used the unique combination of deep optical/near-infrared/mid-infrared imaging provided by HST, Spitzer, and the VLT in the CANDELS-UDS. GOODS-South, and HUDF fields to determine the GSMF over the redshift range 3.5 <= z <= 7.5. Methods. We used the LIST WEC3/IR near-infrared imaging from CANDELS and HUDF09, reaching H similar or equal to 27-28.5 over a total area of 369 arcmin(2), in combination with associated deep usT ACS optical data, deep Spitzer IRAC imaging from the SEDS programme, and deep Y and K-band VI l Hawk-I images from the ElliGS programme, to select a galaxy sample with high-quality photometric redshifts. These have been calibrated with more than 150 spectroscopic redshifts in the range 3.5 <= z <= 7.5, resulting in an overall precision of sigma(z)/(1 + z) similar to 0.037. With this database we have determined the low-mass end of the high-redshift GSMF with unprecedented precision, reaching down to masses as low as M* similar to 10(9) M-circle dot at z = 4 and similar to 6 x 10(9) M-circle dot at z = 7. Results. We find that the GSMF at 3.5 <= z <= 7.5 depends only slightly on the recipes adopted to measure the stellar masses, namely the photometric redshifts, the star formation histories, the nebular contribution, or the presence of AGN in the parent sample. The low-mass end of the GSMF is steeper than has been found at lower redshifts, but appears to be unchanged over the redshift range probed here. Meanwhile the high-mass end of the GSMF appears to evolve primarily in density, although there is also some evidence of evolution in characteristic mass. Our results are very different from previous mass function estimates based on converting UV galaxy luminosity functions into mass functions via tight mass-to-light relations. Integrating our evolving GSMF over mass, we find that the growth of stellar mass density is barely consistent with the time-integral of the star formation rate (lensity over cosmic time at z > 4. Conclusions. These results confirm the unique synergy of the CANDELS+HUDF, and SIDS surveys for the discovery and study of moderate/low-mass galaxies at high iredshifts, and reaffirm the importance of space-based infrared selection for the unbiased measurement of the evolving GSMF in the young Universe. C1 [Grazian, A.; Fontana, A.; Santini, P.; Castellano, M.; Amorin, R.; Boutsia, K.; Merlin, E.; Paris, D.; Pentericci, L.] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy. [Dunlop, J. S.] Univ Edinburgh, Inst Astron, SUPA, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland. [Ferguson, H. C.; Behroozi, P.; Grogin, N. A.; Koekemoer, A. M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Ashby, M. L. N.; Fazio, G. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Barro, G.; Faber, S. M.; Guo, Y.; Koo, D. C.] Univ Calif Santa Cruz, UCO Lick Observ, Santa Cruz, CA 95064 USA. [Caputi, K. I.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Chary, R. R.] CALTECH, Pasadena, CA 91125 USA. [Dekel, A.] Hebrew Univ Jerusalem, Racah Inst Phys, Ctr Astrophys & Planetary Sci, IL-91904 Jerusalem, Israel. [Dickinson, M. E.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Finkelstein, S. L.; Song, M.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Galametz, A.; Salvato, M.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Giavalisco, M.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Kocevski, D.] Univ Kentucky, Dept Phys & Astron, Lexington, KY 40506 USA. [Lee, K. -S.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Lu, Y.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, Stanford, CA 94305 USA. [Lu, Y.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Mobasher, B.; Reddy, N.] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA. [Nonino, M.] Osserv Astron Trieste, INAF, I-34131 Trieste, Italy. [Papovich, C.; Salmon, B.] Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamenta, College Stn, TX 77843 USA. [Renzini, A.] Osserv Astron Padova, INAF, I-35122 Padua, Italy. [Sommariva, V.] Univ Bologna, Dept Phys & Astron DIFA, I-40127 Bologna, Italy. [Vanzella, E.] Osservatorio Astron Bologna, INAF, Bologna, Italy. RP Grazian, A (reprint author), Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy. EM andrea.grazian@oa-roma.inaf.it OI Giallongo, Emanuele/0000-0003-0734-1273; Castellano, Marco/0000-0001-9875-8263; Nonino, Mario/0000-0001-6342-9662; Vanzella, Eros/0000-0002-5057-135X; Santini, Paola/0000-0002-9334-8705; Amorin, Ricardo O./0000-0001-5758-1000; Koekemoer, Anton/0000-0002-6610-2048 FU ASI-INAF [I/009/10/0]; NASA [NAS5-26555]; NASA; NASA by JPL/Caltech; EC [312725]; Royal Society; ERC FX We warmly thank the referee for her/his constructive report. We acknowledge financial contribution from the agreement ASI-INAF I/009/10/0. This work is based on observations taken by the CANDELS Multi-Cycle Treasury Program with the NASA/ESA HST, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Observations were also carried out using the Very Large Telescope at the LSO Paranal Observatory under Programme IDs LP186.A-0898, LP181.A-0717, LP168.A-0485, ID 170.A-0788, ID 181.A-0485, ID 283.A-5052 and the ESO Science Archive under Programme IDs 60.A-9284, 67.A-0249, 71.A-0584, 73.A-0564, 68.A-0563, 69.A-0539, 70.A-0048, 64.O-0643, 66.A-0572, 68.A-0544, 164.O-0561, 163.N-0210, 85.A-0961 and 60.A-9120. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. A.F. and J.S.D. acknowledge the contribution of the EC FP7 SPACE project ASTRODEEP (Ref. No: 312725). J.S.D. also acknowledges the support of the Royal Society via a Wolfson Research Merit Award, and the support of the ERC through an Advanced Grant. NR 101 TC 41 Z9 41 U1 1 U2 3 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAR PY 2015 VL 575 AR A96 DI 10.1051/0004-6361/201424750 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CC3LA UT WOS:000350249100096 ER PT J AU Gusdorf, A Riquelme, D Anderl, S Eisloffel, J Codella, C Gomez-Ruiz, AI Graf, UU Kristensen, LE Leurini, S Parise, B Requena-Torres, MA Ricken, O Gusten, R AF Gusdorf, A. Riquelme, D. Anderl, S. Eisloeffel, J. Codella, C. Gomez-Ruiz, A. I. Graf, U. U. Kristensen, L. E. Leurini, S. Parise, B. Requena-Torres, M. A. Ricken, O. Guesten, R. TI Impacts of pure shocks in the BHR71 bipolar outflow SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: formation; ISM: jets and outflows; ISM: individual objects: BHR71; submillimeter: ISM; infrared: ISM; shock waves ID STAR-FORMING REGIONS; MOLECULAR LINE EMISSION; YOUNG STELLAR OBJECTS; TIME DIGIT HERSCHEL; LOW-MASS PROTOSTARS; HIGH-J CO; SMALL DARK CLOUDS; KEY PROGRAM; MAGNETOHYDRODYNAMIC SHOCKS; HETERODYNE INSTRUMENT AB Context. During the formation of a star, material is ejected along powerful jets that impact the ambient material. This outflow regulates star formation by e.g. inducing turbulence and heating the surrounding gas. Understanding the associated shocks is therefore essential to the study of star formation. Aims. We present comparisons of shock models with CO, H-2, and SiO observations in a "pure" shock position in the BHR71 bipolar outflow. These comparisons provide an insight into the shock and pre-shock characteristics, and allow us to understand the energetic and chemical feedback of star formation on Galactic scales. Methods. New CO (J(up) = 16, 11, 7, 6, 4, 3) observations from the shocked regions with the SOFIA and APEX telescopes are presented and combined with earlier H-2 and SiO data (from the Spitzer and APEX telescopes). The integrated intensities are compared to a grid of models that were obtained from a magneto-hydrodynamical shock code, which calculates the dynamical and chemical structure of these regions combined with a radiative transfer module based on the "large velocity gradient" approximation. Results. The CO emission leads us to update the conclusions of our previous shock analysis: pre-shock densities of 10(4) cm(-3) and shock velocities around 20-25 km s(-1) are still constrained, but older ages are inferred (similar to 4000 years). Conclusions. We evaluate the contribution of shocks to the excitation of CO around forming stars. The SiO observations are compatible with a scenario where less than 4% of the pre-shock SiO belongs to the grain mantles. We infer outflow parameters: a mass of 1.8 x 10(-2) M-circle dot was measured in our beam, in which a momentum of 0.4 M-circle dot km s(-1) is dissipated, corresponding to an energy of 4.2 x 10(43) erg. We analyse the energetics of the outflow species by species. Comparing our results with previous studies highlights their dependence on the method: H-2 observations only are not sufficient to evaluate the mass of outflows. C1 [Gusdorf, A.] PSL Res Univ, CNRS, Ecole Normale Super, LERMA,Observ Paris,UMR 8112, F-75014 Paris, France. [Gusdorf, A.] Univ Paris 06, Sorbonne Univ, UMR 8112, LERMA, F-75005 Paris, France. [Riquelme, D.; Gomez-Ruiz, A. I.; Leurini, S.; Requena-Torres, M. A.; Ricken, O.; Guesten, R.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Anderl, S.] Univ Grenoble Alpes, IPAG, F-38000 Grenoble, France. [Anderl, S.] CNRS, IPAG, F-38000 Grenoble, France. [Eisloeffel, J.] Thuringer Landessternwarte, D-07778 Tautenburg, Germany. [Codella, C.] INAF, Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. [Graf, U. U.] Univ Cologne, KOSMA, Phys Inst 1, D-50937 Cologne, Germany. [Kristensen, L. E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Parise, B.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. RP Gusdorf, A (reprint author), PSL Res Univ, CNRS, Ecole Normale Super, LERMA,Observ Paris,UMR 8112, F-75014 Paris, France. EM antoine.gusdorf@lra.ens.fr RI Kristensen, Lars/F-4774-2011; OI Kristensen, Lars/0000-0003-1159-3721; Codella, Claudio/0000-0003-1514-3074 FU NASA [NAS2-97001]; Deutsches SOFIA Institut, under DLR [50 OK 0901]; French Agence Nationale de la Recherche [ANR-09- BLAN-0231-01]; CNRS programme "Physique et Chimie du Milieu Interstellaire" FX We thank the anonymous referee for comments that helped to improve the quality of this work. We thank the SOFIA operations and the GREAT instrument teams, whose support has been essential for the GREAT accomplishments, and the DSI telescope engineering team. Based [in part] on observations made with the NASA/DLR Stratospheric Observatory for Infrared Astronomy. SOFIA Science Mission Operations are conducted jointly by the Universities Space Research Association, Inc., under NASA contract NAS2-97001, and the Deutsches SOFIA Institut, under DLR contract 50 OK 0901. This work was partly funded by grant ANR-09- BLAN-0231-01 from the French Agence Nationale de la Recherche as part of the SCHISM project. It was also partly supported by the CNRS programme "Physique et Chimie du Milieu Interstellaire". NR 95 TC 6 Z9 6 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAR PY 2015 VL 575 AR A98 DI 10.1051/0004-6361/201425142 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CC3LA UT WOS:000350249100098 ER PT J AU Hoeijmakers, HJ de Kok, RJ Snellen, IAG Brogi, M Birkby, JL Schwarz, H AF Hoeijmakers, H. J. de Kok, R. J. Snellen, I. A. G. Brogi, M. Birkby, J. L. Schwarz, H. TI A search for TiO in the optical high-resolution transmission spectrum of HD 209458b: Hindrance due to inaccuracies in the line database SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE line: identification; molecular data; planets and satellites: atmospheres; methods: observational ID TAU BOOTIS B; MU-M; THERMAL INVERSION; CARBON-MONOXIDE; ORBITAL MOTION; WATER-VAPOR; ATMOSPHERE; ABSORPTION; SPECTROSCOPY; PLANETS AB Context. The spectral signature of an exoplanet can be separated from the spectrum of its host star using high-resolution spectroscopy. During these observations, the radial component of the planet's orbital velocity changes, resulting in a significant Doppler shift that allows its spectral features to be extracted. Aims. In this work, we aim to detect TiO in the optical transmission spectrum of HD 209458b. Gaseous TiO has been suggested as the cause of the thermal inversion layer invoked to explain the dayside spectrum of this planet. Methods. We used archival data from the 8.2 m Subaru telescope taken with the High Dispersion Spectrograph of a transit of HD209458b in 2002. We created model transmission spectra that include absorption by TiO, and cross-correlated them with the residual spectral data after removal of the dominating stellar absorption features. We subsequently co-added the correlation signal in time, taking the change in Doppler shift due to the orbit of the planet into account. Results. We detect no significant cross-correlation signal due to TiO, though artificial injection of our template spectra into the data indicates a sensitivity down to a volume-mixing ratio of similar to 10(-10). However, cross-correlating the template spectra with a HARPS spectrum of Barnard's star yields only a weak wavelength-dependent correlation, even though Barnard's star is an M4V dwarf that exhibits clear TiO absorption. We infer that the TiO line list poorly matches the real positions of TiO lines at spectral resolutions of similar to 100 000. Similar line lists are also used in the PHOENIX and Kurucz stellar atmosphere suites and we show that their synthetic M-dwarf spectra also correlate poorly with the HARPS spectra of Barnard's star and five other M dwarfs. We conclude that the lack of an accurate TiO line list is currently critically hampering this high-resolution retrieval technique. C1 [Hoeijmakers, H. J.; de Kok, R. J.; Snellen, I. A. G.; Brogi, M.; Birkby, J. L.; Schwarz, H.] Leiden Univ, Leiden Observ, NL-2333 CA Leiden, Netherlands. [de Kok, R. J.] SRON Netherlands Inst Space Res, SRON, NL-3584 CA Utrecht, Netherlands. [Birkby, J. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Hoeijmakers, HJ (reprint author), Leiden Univ, Leiden Observ, Niels Bohrweg 2, NL-2333 CA Leiden, Netherlands. EM hoeijmakers@strw.leidenuniv.nl FU Netherlands Organisation for Scientific Research (NWO) [639.043.107]; Leiden Observatory Huygens Fellowship; NASA; NASA through Hubble Fellowship - Space Telescope Science Institute [HST-HF2-51336] FX This work is part of the research programmes PEPSci and VICI 639.043.107, which are financed by the Netherlands Organisation for Scientific Research (NWO), and was also supported by the Leiden Observatory Huygens Fellowship. This work was performed in part under contract with the California Institute of Technology (Caltech)/Jet Propulsion Laboratory (JPL) funded by NASA through the Sagan Fellowship Program executed by the NASA Exoplanet Science Institute. Support for this work was provided in part by NASA through Hubble Fellowship grant HST-HF2-51336 awarded by the Space Telescope Science Institute. Also, this research has made use of the Exoplanet Orbit Database and the Exoplanet Data Explorer at exoplanets. org. Finally, we would like to thank Leigh Fetcher, Jaemin Lee and Patrick Irwin for providing the TiO line-list needed to perform this analysis. NR 40 TC 15 Z9 15 U1 0 U2 4 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAR PY 2015 VL 575 AR A20 DI 10.1051/0004-6361/201424794 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CC3LA UT WOS:000350249100020 ER PT J AU Podigachoski, P Barthel, PD Haas, M Leipski, C Wilkes, B Kuraszkiewicz, J Westhues, C Willner, SP Ashby, MLN Chini, R Clements, DL Fazio, GG Labiano, A Lawrence, C Meisenheimer, K Peletier, RF Siebenmorgen, R Kleijn, GV AF Podigachoski, P. Barthel, P. D. Haas, M. Leipski, C. Wilkes, B. Kuraszkiewicz, J. Westhues, C. Willner, S. P. Ashby, M. L. N. Chini, R. Clements, D. L. Fazio, G. G. Labiano, A. Lawrence, C. Meisenheimer, K. Peletier, R. F. Siebenmorgen, R. Kleijn, G. Verdoes TI Star formation in z > 1 3CR host galaxies as seen by Herschel SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: active; galaxies: high-redshift; galaxies: star formation; infrared: galaxies ID ACTIVE GALACTIC NUCLEI; SPECTRAL ENERGY-DISTRIBUTIONS; REDSHIFT RADIO GALAXIES; SPITZER-SPACE-TELESCOPE; FAR-INFRARED PROPERTIES; OLD STELLAR POPULATIONS; CLUMPY TORUS MODELS; SUBMILLIMETER GALAXIES; DUST EMISSION; BLACK-HOLE AB We present Herschel (PACS and SPIRE) far-infrared (FIR) photometry of a complete sample of z > 1 3CR sources, from the Herschel guaranteed time project The Herschel Legacy of distant radio-loud AGN. Combining these with existing Spitzer photometric data, we perform an infrared (1.12) spectral energy distribution (SED) analysis of these landmark objects in extragalactic research to study the star formation in the hosts of some of the brightest active galactic nuclei (A(iN) known at any epoch. Accounting for the contribution from an AGN-powered warm dust component to the IR SED, about 40% of our objects undergo episodes of prodigious. ULIRG-strength star formation, with rates of hundreds of solar masses per year, coeval with the growth of the central supermassive black hole. Median SEDs imply that the quasar and radio galaxy hosts have similar FIR properties, in agreement with the orientation-based unification for radio-loud AGN. The star-forming properties of the AGN hosts are similar to those of the general population of equally massive non-AGN galaxies at comparable redshifts, thus there is no strong evidence of universal quenching of star formation (negative feedback) within this sample. Massive galaxies at high redshift may be forming stars prodigiously, regardless of whether their superm.assive black holes are accreting or not. C1 [Podigachoski, P.; Barthel, P. D.; Peletier, R. F.; Kleijn, G. Verdoes] Univ Groningen, Kapteyn Astron Inst, NL-9747 AD Groningen, Netherlands. [Haas, M.; Westhues, C.; Chini, R.] Ruhr Univ Bochum, Astron Inst, D-44801 Bochum, Germany. [Leipski, C.; Meisenheimer, K.] MPIA, D-69117 Heidelberg, Germany. [Wilkes, B.; Kuraszkiewicz, J.; Willner, S. P.; Ashby, M. L. N.; Fazio, G. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Clements, D. L.] Univ London Imperial Coll Sci Technol & Med, Astrophys Grp, Blackett Lab, London SW7 2AZ, England. [Labiano, A.] ETH, Inst Astron, Dept Phys, CH-8093 Zurich, Switzerland. [Lawrence, C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Siebenmorgen, R.] European So Observ, D-85748 Garching, Germany. RP Podigachoski, P (reprint author), Univ Groningen, Kapteyn Astron Inst, NL-9747 AD Groningen, Netherlands. EM podigachoski@astro.rug.nl FU Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO); Akademie der Wissenschaften und der Kunste Nordrhein-Westfalen; Deutsches Zentrum fur Luft-und Raumfahrt (DLR); Thales Alenia Space (Cannes); BMVIT (Austria); ESA-PRODEX (Belgium); CEA/CNES (France); DLR (Germany); ASI/INAF (Italy); CICYT/MCYT (Spain); CSA (Canada); NAOC (China); CEA (France); CNES (France); CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK); UKSA (UK); NASA (USA); NASA; National Aeronautics and Space Administration FX The authors acknowledge the expert referee for useful comments which improved the paper, and thank Giulia Rodighiero for kindly providing the PEP data from the deep GOODS South Odd. P.P. acknowledges the Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO) for a Ph.D. fellowship. M.H. and C.W. are supported by the Akademie der Wissenschaften und der Kunste Nordrhein-Westfalen and by Deutsches Zentrum fur Luft-und Raumfahrt (DLR). The Herschel spacecraft was designed, built, tested, and launched under a contract to ESA managed by the Herschel/Planck Project team by an industrial consortium under the overall responsibility of the prime contractor Thales Alenia Space (Cannes), and including Astrium (Friedrichshafen) responsible for the payload module and for system testing at spacecraft level, Thales Alenia Space (Turin) responsible for the service module, and Astrium (Toulouse) responsible for the telescope, with in excess of a hundred subcontractors. PACS has been developed by a consortium of institutes led by MPE (Germany) and including UVIE (Austria); KU Leuven, CSL, IMEC (Belgium); CEA, LAM (France); MPIA (Germany); INAF-IFSI/OAA/OAP/OAT, LENS, SISSA (Italy); IAC (Spain). This development has been supported by the funding agencies BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI/INAF (Italy), and CICYT/MCYT (Spain). SPIRE has been developed by a consortium of institutes led by Cardiff University (UK) and including Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); and Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK); and NASA (USA). HIPE is a joint development by the Herschel Science Ground Segment Consortium, consisting of ESA, the NASA Herschel Science Center, and the HIFI, PACS and SPIRE consortia. This work is partly 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 research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This research made use of APLpy, an open-source plotting package for Python hosted at http://aplpy.github.com NR 106 TC 15 Z9 15 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 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAR PY 2015 VL 575 AR UNSP A80 DI 10.1051/0004-6361/201425137 PG 28 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CC3LA UT WOS:000350249100080 ER PT J AU Schellenberger, G Reiprich, TH Lovisari, L Nevalainen, J David, L AF Schellenberger, G. Reiprich, T. H. Lovisari, L. Nevalainen, J. David, L. TI XMM-Newton and Chandra cross-calibration using HIFLUGCS galaxy clusters SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE X-rays: galaxies: clusters; instrumentation: miscellaneous; galaxies: clusters: intracluster medium; techniques: spectroscopic ID X-RAY LUMINOSITY; SCALING RELATIONS; MASS FUNCTION; SOLAR; ABUNDANCES; SAMPLE; EMISSION; ABSORPTION; COSMOLOGY; ELEMENTS AB Context. Robust X-ray temperature measurements of the intracluster medium (ICM) of galaxy clusters require an accurate energydependent effective area calibration. Since the hot gas X-ray emission of galaxy clusters does not vary on relevant timescales, they are excellent cross-calibration targets. Moreover, cosmological constraints from clusters rely on accurate gravitational mass estimates, which in X-rays strongly depend on cluster gas temperature measurements. Therefore, systematic calibration differences may result in biased, instrument-dependent cosmological constraints. This is of special interest in light of the tension between the Planck results of the primary temperature anisotropies of the cosmic microwave background (CMB) and Sunyaev-Zel'dovich-plus-X-ray cluster-count analyses. Aims. We quantify in detail the systematics and uncertainties of the cross-calibration of the effective area between five X-ray instruments, EPIC-MOS1/MOS2/PN onboard XMM-Newton and ACIS-I/S onboard Chandra, and the influence on temperature measurements. Furthermore, we assess the impact of the cross-calibration uncertainties on cosmology. Methods. Using the HIFLUGCS sample, consisting of the 64 X-ray brightest galaxy clusters, we constrain the ICM temperatures through spectral fitting in the same, mostly isothermal regions and compare the different instruments. We use the stacked residual ratio method to evaluate the cross-calibration uncertainties between the instruments as a function of energy. Our work is an extension to a previous one using X-ray clusters by the International Astronomical Consortium for High Energy Calibration (IACHEC) and is carried out in the context of IACHEC. Results. Performing spectral fitting in the full energy band, (0 : 7-7) keV, as is typical of the analysis of cluster spectra, we find that best-fit temperatures determined with XMM-Newton/EPIC are significantly lower than Chandra/ACIS temperatures. This confirms the previous IACHEC results obtained with older calibrations with high precision. The difference increases with temperature, and we quantify this dependence with a fitting formula. For instance, at a cluster temperature of 10 keV, EPIC temperatures are on average 23% lower than ACIS temperatures. We also find systematic differences between the three XMM-Newton/EPIC instruments, with the PN detector typically estimating the lowest temperatures. Testing the cross-calibration of the energy-dependence of the effective areas in the soft and hard energy bands, (0 : 7-2) keV and (2-7) keV, respectively, we confirm the previously indicated relatively good agreement between all instruments in the hard and the systematic differences in the soft band. We provide scaling relations to convert between the different instruments based on the effective area, gas temperature, and hydrostatic mass. We demonstrate that effects like multitemperature structure and different relative sensitivities of the instruments at certain energy bands cannot explain the observed differences. We conclude that using XMM-Newton / EPIC instead of Chandra / ACIS to derive full energy band temperature profiles for cluster mass determination results in an 8% shift toward lower Omega(M) values and < 1% change of sigma(8) values in a cosmological analysis of a complete sample of galaxy clusters. Such a shift alone is insufficient to significantly alleviate the tension between Planck CMB primary anisotropies and Sunyaev-Zel'dovich-plus-XMM-Newton cosmological constraints. C1 [Schellenberger, G.; Reiprich, T. H.; Lovisari, L.] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany. [Nevalainen, J.] Tartu Observ, EE-61602 Toravere, Estonia. [Nevalainen, J.] Univ Helsinki, Dept Phys, Dynamicum, Helsinki 00014, Finland. [David, L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA. RP Schellenberger, G (reprint author), Univ Bonn, Argelander Inst Astron, Hugel 71, D-53121 Bonn, Germany. EM gerrit@uni-bonn.de FU German Research Association (DFG) [RE 1462/6]; DFG through Heisenberg grant [RE 1462/5]; DFG [LO 2009/1-1]; German Aerospace Agency (DLR); Ministry of Economy and Technology (BMWi) [50 OR 1102]; Estonian Research Council [PUT 246] FX The authors would like to thank Douglas Applegate, Matteo Guainazzi and Fabio Gastaldello for helpful discussions. G.S., L.L., and T.H.R. acknowledge support by the German Research Association (DFG) through grant RE 1462/6. T.H.R. acknowledges support by the DFG through Heisenberg grant RE 1462/5. L.L. acknowledges support by the DFG through grant LO 2009/1-1 and by the German Aerospace Agency (DLR) with funds from the Ministry of Economy and Technology (BMWi) through grant 50 OR 1102. J.N. acknowledges a PUT 246 grant from Estonian Research Council. NR 39 TC 27 Z9 27 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 MAR PY 2015 VL 575 AR A30 DI 10.1051/0004-6361/201424085 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CC3LA UT WOS:000350249100030 ER PT J AU Sudar, D Skokic, I Brajsa, R Saar, SH AF Sudar, D. Skokic, I. Brajsa, R. Saar, S. H. TI Steps towards a high precision solar rotation profile: Results from SDO/AIA coronal bright point data SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE Sun: rotation; Sun: corona; Sun: activity ID SOHO-EIT IMAGES; MICHELSON DOPPLER IMAGER; SMALL MAGNETIC FEATURES; DIFFERENTIAL ROTATION; SUNSPOT GROUPS; AUTOMATIC METHODS; MOUNT-WILSON; SUN; VELOCITY; OSCILLATIONS AB Context. Coronal bright points (CBP) are ubiquitous small brightenings in the solar corona associated with small magnetic bipoles. Aims. We derive the solar differential rotation profile by tracing the motions of CBPs detected by the Atmospheric Imaging Assembly (AIA) instrument aboard the Solar Dynamics Observatory (SDO). We also investigate problems related to the detection of CBPs resulting from instrument and detection algorithm limitations. Methods. To determine the positions and identification of CBPs we used a segmentation algorithm. A linear fit of their central meridian distance and latitude vs time was used to derive velocities. Results. We obtained 906 velocity measurements in a time interval of only 2 days. The differential rotation profile can be expressed as omega(rot) = (14 degrees.47 +/- 0 degrees.10 + (0 degrees.6 +/- 1 degrees.0) sin(2)(b) + (-4 degrees.7 +/- 1 degrees.7) sin(4)(b)) d(-1). Our result is in agreement with other work and it comes with reasonable errors in spite of the very short time interval used. This was made possible by the higher sensitivity and resolution of the AIA instrument compared to similar equipment as well as high cadence. The segmentation algorithm also played a crucial role by detecting so many CBPs, which reduced the errors to a reasonable level. Conclusions. Data and methods presented in this paper show a great potential for obtaining very accurate velocity profiles, both for rotation and meridional motion and, consequently, Reynolds stresses. The amount of CBP data that could be obtained from this instrument should also provide a great opportunity to study changes of velocity patterns with a temporal resolution of only a few months. Other possibilities are studies of evolution of CBPs and proper motions of magnetic elements on the Sun. C1 [Sudar, D.; Brajsa, R.] Univ Zagreb, Fac Geodesy, Hvar Observ, Zagreb 10000, Croatia. [Skokic, I.] Cybrotech Ltd, Zagreb 10000, Croatia. [Saar, S. H.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Sudar, D (reprint author), Univ Zagreb, Fac Geodesy, Hvar Observ, Kaciceva 26, Zagreb 10000, Croatia. EM davor.sudar@gmail.com FU European Commission [284461, 312495]; FP7 Capacities Programme; Croatian Science Foundation [6212]; NASA [NNX09AB03G]; Lockheed-Martin [SP02H1701R] FX This work has received funding from the European Commission FP7 project eHEROES (284461, 2012-2015) and SOLARNET project (312495, 2013-2017) which is an Integrated Infrastructure Initiative (I3) supported by FP7 Capacities Programme. It was also supported by the Croatian Science Foundation under the project 6212 Solar and Stellar Variability. SS was supported by NASA Grant NNX09AB03G to the Smithsonian Astrophysical Observatory and contract SP02H1701R from Lockheed-Martin to SAO. We would like to thank the SDO/AIA science teams for providing the observations. We would also like to thank Veronique Delouille and Alexander Engell for valuable help in the preparation of this work. NR 57 TC 4 Z9 4 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 MAR PY 2015 VL 575 AR A63 DI 10.1051/0004-6361/201424929 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CC3LA UT WOS:000350249100063 ER PT J AU Turner, BL Yavitt, JB Harms, KE Garcia, MN Wright, SJ AF Turner, Benjamin L. Yavitt, Joseph B. Harms, Kyle E. Garcia, Milton N. Joseph Wright, S. TI Seasonal changes in soil organic matter after a decade of nutrient addition in a lowland tropical forest SO BIOGEOCHEMISTRY LA English DT Article DE Carbon; Gigante Peninsula; Nitrogen; Panama; Phosphorus; Soil microbial biomass ID BELOW-GROUND CARBON; RAIN-FOREST; MICROBIAL BIOMASS; MOIST FOREST; ATMOSPHERIC CO2; WET FOREST; PHOSPHORUS; NITROGEN; LITTERFALL; PANAMA AB Soil organic matter is an important pool of carbon and nutrients in tropical forests. The majority of this pool is assumed to be relatively stable and to turn over slowly over decades to centuries, although changes in nutrient status can influence soil organic matter on shorter timescales. We measured carbon, nitrogen, and phosphorus concentrations in soil organic matter and leaf litter over an annual cycle in a long-term nutrient addition experiment in lowland tropical rain forest in the Republic of Panama. Total soil carbon was not affected by a decade of factorial combinations of nitrogen, phosphorus, or potassium. Nitrogen addition increased leaf litter nitrogen concentration by 7 % but did not affect total soil nitrogen. Phosphorus addition doubled the leaf litter phosphorus concentration and increased soil organic phosphorus by 50 %. Surprisingly, concentrations of carbon, nitrogen, and phosphorus in soil organic matter declined markedly during the four-month dry season, and then recovered rapidly during the following wet season. Between the end of the wet season and the late dry season, total soil carbon declined by 16 %, total nitrogen by 9 %, and organic phosphorus by between 19 % in control plots and 25 % in phosphorus addition plots. The decline in carbon and nitrogen was too great to be explained by changes in litter fall, bulk density, or the soil microbial biomass. However, a major proportion of the dry-season decline in soil organic phosphorus was explained by a corresponding decline in the soil microbial biomass. These results have important implications for our understanding of the stability and turnover of organic matter in tropical forest soils, because they demonstrate that a considerable fraction of the soil organic matter is seasonally transient, despite the overall pool being relatively insensitive to long-term changes in nutrient status. C1 [Turner, Benjamin L.; Garcia, Milton N.; Joseph Wright, S.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Yavitt, Joseph B.] Cornell Univ, Dept Nat Resources, Ithaca, NY 14853 USA. [Harms, Kyle E.] Louisiana State Univ, Dept Biol Sci, Baton Rouge, LA 70803 USA. 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; Wright, Stuart/M-3311-2013 OI Turner, Benjamin/0000-0002-6585-0722; Wright, Stuart/0000-0003-4260-5676 NR 63 TC 5 Z9 5 U1 4 U2 44 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0168-2563 EI 1573-515X J9 BIOGEOCHEMISTRY JI Biogeochemistry PD MAR PY 2015 VL 123 IS 1-2 BP 221 EP 235 DI 10.1007/s10533-014-0064-1 PG 15 WC Environmental Sciences; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Geology GA CC9GC UT WOS:000350675300014 ER PT J AU Tarvin, RD Bermudez, CS Briggs, VS Warkentin, KM AF Tarvin, Rebecca D. Silva Bermudez, Catalina Briggs, Venetia S. Warkentin, Karen M. TI Carry-over Effects of Size at Metamorphosis in Red-eyed Treefrogs: Higher Survival but Slower Growth of Larger Metamorphs SO BIOTROPICA LA English DT Article DE Agalychnis callidryas; complex life cycle; foraging; juvenile behavior; optimal metamorphic timing; Panama; phenotypic plasticity; trade-off ID FROGS RANA-SYLVATICA; COMPLEX LIFE-CYCLES; AGALYCHNIS-CALLIDRYAS; PREDATION RISK; TRADE-OFF; PHENOTYPIC PLASTICITY; DIGESTIVE PLASTICITY; LARVAL DEVELOPMENT; HISTORY TRAITS; COMMON FROG AB Most animals have complex life histories, composed of a series of ecologically distinct stages, and the transitions between stages are often plastic. Anurans are models for research on complex life cycles. Many species exhibit plastic timing of and size at metamorphosis, due to both environmental constraints on larval growth and development and adaptive plastic responses to environmental variation. Models predicting optimal timing of metamorphosis balance cost/benefit ratios across stages, assuming that size affects growth and mortality rates in each stage. Much research has documented such effects in the larval period, but we lack an equal understanding of juvenile growth and mortality. Here, we examine how variation in size at metamorphosis in the Neotropical red-eyed treefrog, Agalychnis callidryas, affects post-metamorphic growth, foraging, and behavior in the lab as well as growth and survival in the field. Surprisingly, many individuals lost mass for weeks after metamorphosis. In the lab, larger metamorphs lost more mass following metamorphosis, ate similar amounts, had lower food conversion efficiencies, and grew more slowly after mass loss ceased than did smaller ones. In field cages larger metamorphs were more likely to survive than smaller ones; just one froglet died in the lab. Our data suggest that size-specific differences in physiology and behavior influence these trends. Comparing across species and studies, large size at metamorphosis generally confers higher survival; size effects on growth rates vary substantially among species, in both magnitude and direction, but may be stronger in the tropics. C1 [Tarvin, Rebecca D.; Briggs, Venetia S.; Warkentin, Karen M.] Boston Univ, Dept Biol, Boston, MA 02215 USA. [Tarvin, Rebecca D.] Univ Texas Austin, Dept Integrat Biol, Austin, TX 78712 USA. [Silva Bermudez, Catalina] Univ Los Andes, Bogota, Colombia. [Warkentin, Karen M.] Smithsonian Trop Res Inst, Balboa, Panama. RP Tarvin, RD (reprint author), Boston Univ, Dept Biol, 5 Cummington Mall, Boston, MA 02215 USA. EM rdtarvin@gmail.com FU US National Science Foundation [DEB-0716923, DEB-0717220]; Boston University and its Undergraduate Research Opportunities Program; Smithsonian Tropical Research Institute FX We thank the Smithsonian Tropical Research Institute for use of their facilities and logistical support and the Panamanian Autoridad Nacional del Ambiente for permission to conduct this research (SE/A-32-09, SE/A-73/09). We thank Hayley McLeod, Isaac Smith, Sergio Gonzalez, Alex Lebron, Chris Asquith, and Justin Touchon for help rearing tadpoles and Sarah Bouchard, James Vonesh, Chris Schneider, and Michael Mahometa for advice. This research was funded by the US National Science Foundation (DEB-0716923 to KMW and DEB-0717220 to J. Vonesh), Boston University and its Undergraduate Research Opportunities Program, and the Smithsonian Tropical Research Institute. NR 62 TC 7 Z9 7 U1 2 U2 19 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0006-3606 EI 1744-7429 J9 BIOTROPICA JI Biotropica PD MAR PY 2015 VL 47 IS 2 BP 218 EP 226 DI 10.1111/btp.12198 PG 9 WC Ecology SC Environmental Sciences & Ecology GA CD3LU UT WOS:000350980800010 ER PT J AU Stellaccio, A AF Stellaccio, Anthony TI Finding the Words in Karin Karinson's Sculpture SO CERAMICS-ART AND PERCEPTION LA English DT Article C1 Natl Museum African Art, Smithsonian, Washington, DC 20560 USA. RP Stellaccio, A (reprint author), Natl Museum African Art, Smithsonian, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU CERAMIC ART PI SHERIDAN PA 23 NORTH SCOTT ST, STE 19, SHERIDAN, WYOMING 82801 USA SN 1035-1841 J9 CERAMICS-ART PERCEPT JI Ceramics-Art Percept. PD MAR-MAY PY 2015 IS 99 BP 46 EP 49 PG 4 WC Art SC Art GA CD1LB UT WOS:000350835300012 ER PT J AU Hallworth, MT Sillett, TS Van Wilgenburg, SL Hobson, KA Marra, PP AF Hallworth, Michael T. Sillett, T. Scott Van Wilgenburg, Steven L. Hobson, Keith A. Marra, Peter P. TI Migratory connectivity of a Neotropical migratory songbird revealed by archival light-level geolocators SO ECOLOGICAL APPLICATIONS LA English DT Article DE Bayesian; Caribbean basin; conservation biogeography; geo-logger; migration; movement ecology; Ovenbird (Seiurus aurocapilla); probability of origin; spatial distribution ID AERIAL INSECTIVORE; MIGRANT SONGBIRD; SPRING MIGRATION; WILSONIA-PUSILLA; STABLE-ISOTOPES; WINTER; BIRDS; POPULATION; ABUNDANCE; TRACKING AB Understanding migratory connectivity is critical for interpreting population dynamics, seasonal interactions, and for the implementation of conservation strategies of migratory species. We evaluated the migratory connectivity of a Neotropical migratory songbird, the Ovenbird (Seiurus aurocapilla) using archival light-level geolocators deployed at two breeding and four nonbreeding locations while incorporating Ovenbird abundance as prior information using Bayes' Rule. We also included band recoveries submitted to the United States Geological Survey's Bird Banding Laboratory to assess connectivity of areas where geolocators were not deployed. We created a probabilistic map of origin for each capture site and mapped spring migration routes between nonbreeding and breeding locations. We found a complete separation of eastern and western populations of Ovenbirds throughout the annual cycle. Breeding Ovenbirds from western Canada spent the nonbreeding season throughout Central America and migrated through central North America during spring migration. Birds breeding in the northeastern United States were distributed throughout the central Greater Antilles in the Caribbean and migrated through eastern North America during spring migration. Fall migration routes were not included because the timing of migration coincided with fall equinox when latitudinal estimates are unreliable. However, longitudinal estimates suggest no overlap between eastern and western populations during fall migration. Ovenbirds with geolocators attached in Jamaica bred in the northeastern United States with the highest posterior probability of origin found in Massachusetts, while Ovenbirds captured in Florida and Puerto Rico bred primarily in the mid-Atlantic. Incorporating Ovenbird abundance as a prior into geolocator estimates decreased the area of origin by 90.37% +/- 1.05% (mean +/- SE) for the breeding season and 62.30% +/- 1.69% for the nonbreeding season, compared to geolocator estimates alone. Ovenbirds exhibited strong migratory connectivity between breeding and nonbreeding season, which has important implications for various aspects of the ecology, evolution, and conservation. C1 [Hallworth, Michael T.; Sillett, T. Scott; Marra, Peter P.] Natl Zool Pk, Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Washington, DC 20013 USA. [Hallworth, Michael T.] George Mason Univ, Coll Sci, Fairfax, VA 22030 USA. [Van Wilgenburg, Steven L.; Hobson, Keith A.] Environm Canada, Saskatoon, SK S7N 3H5, Canada. [Van Wilgenburg, Steven L.] Environm Canada, Saskatoon, SK S7N 0X4, Canada. RP Hallworth, MT (reprint author), Natl Zool Pk, Smithsonian Conservat Biol Inst, Migratory Bird Ctr, MRC 5503, Washington, DC 20013 USA. EM mhallwor@masonlive.gmu.edu FU U.S. National Science Foundation; Smithsonian Institution's Bond Fund; American Ornithologists' Union; Environment Canada; Cosmos Scholars FX We acknowledge N. Cooper, W. Garcia, M. Thomas, C. Tonra, R. Reitsma, D. Narango, R. Terrill, J. Gautreaux, L. Rowse, and L. Pop for assisting in field work. We thank R. Harvey and J. Avecedo for generously donating accommodations during field work. The manuscript was improved by comments from two anonymous reviewers. We thank the individuals who submitted eBird checklists and/or conducted Breeding Bird Surveys. Field work in Canada was facilitated by a research permit and accommodations provided by Parks Canada (Prince Albert National Park) to K. A. Hobson. J. Smith provided helpful insight on the use of NDVI maps. Funding was provided by grants from the U.S. National Science Foundation's Long-term Research in Environmental Biology program (P. P. Marra, T. S. Sillett), the Smithsonian Institution's Bond Fund (M. T. Hallworth and P. P. Marra), Cosmos Scholars (M. T. Hallworth), and the American Ornithologists' Union (M. T. Hallworth). Funding for the Canadian component of the study was provided by an operating grant to K. A. Hobson from Environment Canada. NR 56 TC 9 Z9 10 U1 4 U2 58 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1051-0761 EI 1939-5582 J9 ECOL APPL JI Ecol. Appl. PD MAR PY 2015 VL 25 IS 2 BP 336 EP 347 DI 10.1890/14-0195.1 PG 12 WC Ecology; Environmental Sciences SC Environmental Sciences & Ecology GA CC7OA UT WOS:000350556400003 PM 26263658 ER PT J AU Young, HS McCauley, DJ Dirzo, R Goheen, JR Agwanda, B Brook, C Otarola-Castillo, E Ferguson, AW Kinyua, SN McDonough, MM Palmer, TM Pringle, RM Young, TP Helgen, KM AF Young, Hillary S. McCauley, Douglas J. Dirzo, Rodolfo Goheen, Jacob R. Agwanda, Bernard Brook, Cara Otarola-Castillo, Erik Ferguson, Adam W. Kinyua, Stephen N. McDonough, Molly M. Palmer, Todd M. Pringle, Robert M. Young, Truman P. Helgen, Kristofer M. TI Context-dependent effects of large-wildlife declines on small-mammal communities in central Kenya SO ECOLOGICAL APPLICATIONS LA English DT Article DE community structure; defaunation; diversity; East Africa; environmental gradients; exclosure experiment; land-use change; species richness ID AFRICAN SAVANNA; POPULATION DECLINES; LARGE HERBIVORES; LAND-USE; NATIONAL-PARK; EAST-AFRICA; RODENT; DIVERSITY; DYNAMICS; RAINFALL AB Many species of large wildlife have declined drastically worldwide. These reductions often lead to profound shifts in the ecology of entire communities and ecosystems. However, the effects of these large-wildlife declines on other taxa likely hinge upon both underlying abiotic properties of these systems and on the types of secondary anthropogenic changes associated with wildlife loss, making impacts difficult to predict. To better understand how these important contextual factors determine the consequences of large-wildlife declines on other animals in a community, we examined the effects of three common forms of large-wildlife loss (removal without replacement [using fences], removal followed by replacement with domestic stock, and removal accompanied by crop agricultural use) on small-mammal abundance, diversity, and community composition, in landscapes that varied in several abiotic attributes (rainfall, soil fertility, land-use intensity) in central Kenya. We found that small-mammal communities were indeed heavily impacted by all forms of large-wildlife decline, showing, on average: (1) higher densities, (2) lower species richness per site, and (3) different species assemblages in sites from which large wildlife were removed. However, the nature and magnitude of these effects were strongly context dependent. Rainfall, type of land-use change, and the interaction of these two factors were key predictors of both the magnitude and type of responses of small mammals. The strongest effects, particularly abundance responses, tended to be observed in low-rainfall areas. Whereas isolated wildlife removal primarily led to increased small-mammal abundance, wildlife removal associated with secondary uses (agriculture, domestic stock) had much more variable effects on abundance and stronger impacts on diversity and composition. Collectively, these results (1) highlight the importance of context in determining the impacts of large-wildlife decline on small-mammal communities, (2) emphasize the challenges in extrapolating results from controlled experimental studies to predict the effects of wildlife declines that are accompanied by secondary land-uses, and (3) suggest that, because of the context-dependent nature of the responses to large-wildlife decline, large-wildlife status alone cannot be reliably used to predict small-mammal community changes. C1 [Young, Hillary S.; McCauley, Douglas J.] Univ Calif Santa Barbara, Dept Ecol Evolut & Marine Biol, Santa Barbara, CA 93106 USA. [Young, Hillary S.; McDonough, Molly M.; Helgen, Kristofer M.] Smithsonian Inst, Div Mammals, Natl Museum Nat Hist, Washington, DC 20013 USA. [Young, Hillary S.; Goheen, Jacob R.; Kinyua, Stephen N.; Palmer, Todd M.; Pringle, Robert M.; Young, Truman P.] Mpala Res Ctr, Nanyuki, Kenya. [Young, Hillary S.; Dirzo, Rodolfo] Stanford Univ, Dept Biol, Stanford, CA 94305 USA. [Goheen, Jacob R.] Univ Wyoming, Dept Zool & Physiol, Laramie, WY 82071 USA. [Goheen, Jacob R.] Univ Wyoming, Dept Bot, Laramie, WY 82071 USA. [Agwanda, Bernard] Natl Museums Kenya, Mammal Sect, Nairobi, Kenya. [Brook, Cara; Pringle, Robert M.] Princeton Univ, Dept Ecol & Evolutionary Biol, Princeton, NJ 08544 USA. [Otarola-Castillo, Erik] Harvard Univ, Dept Human Evolutionary Biol, Cambridge, MA 02138 USA. [Ferguson, Adam W.; McDonough, Molly M.] Texas Tech Univ, Dept Biol Sci, Lubbock, TX 79409 USA. [Palmer, Todd M.] Univ Florida, Dept Biol, Gainesville, FL 32611 USA. [Young, Truman P.] Univ Calif Davis, Dept Plant Sci, Davis, CA 95616 USA. RP Young, HS (reprint author), Univ Calif Santa Barbara, Dept Ecol Evolut & Marine Biol, Santa Barbara, CA 93106 USA. EM hillary.young@lifesci.ucsb.edu FU James Smithson Fund of the Smithsonian Institution; National Geographic Society [4691-91, 8846-10, 9106-12]; National Science Foundation [LTREB BSR-97-07477, 03-16402, 08-16453, DEB-09-09670]; Natural Sciences and Engineering Council of Canada; African Elephant Program of the U.S. Fish and Wildlife Service [98210-0-G563]; Woods Institute for the Environment; Smithsonian Barcoding Network Grant; Smithsonian Institution Women's Committee (SWC) [22, 44] FX We thank Jack Silanje, Peter Lokeny, Everlyn Ndinda, Stephen Nyaga, Frederick Erii, Margaret Kinnaird, John Lochikuya, Matthew Namoni, Jackson Ekadeli, Abdikadir Ali Hassan, Simon Lima, Patrick Etelej, Anne Adelson, and Pasha Feinberg for their assistance throughout this project. We also thank the Kenyan Government, Kenya Wildlife Service, National Museums Kenya, Mpala Research Centre, Ol Jogi Ranch, Ol Pejeta Ranch, Segera Ranch, Ol Maisor Ranch, and the Lekiji, Il Motiok, Koija, Lododo, Narok, Il Polei, Thome, Marura, and Kimugandura communities for their assistance in facilitating this research. Financial support for this project came from the James Smithson Fund of the Smithsonian Institution, the National Geographic Society (Grants 4691-91, 8846-10, 9106-12), National Science Foundation (LTREB BSR-97- 07477, 03-16402, 08-16453, DEB-09-09670), Natural Sciences and Engineering Council of Canada, African Elephant Program of the U.S. Fish and Wildlife Service (98210-0-G563), Woods Institute for the Environment, Smithsonian Barcoding Network Grant, and Smithsonian Institution Women's Committee (SWC No. 22 and No. 44). We also thank the National Sciences and Engineering Research Council of Canada, the University of Wyoming, the University of Florida, the Princeton Enviromental Institute's Grand Challenges Initiative, and the National Geographic Society (9291-13). We thank Tim Caro, Tim O'Brien, and two anonymous reviewers for their thoughtful comments on earlier versions of the manuscript. All small-mammal trapping and sampling was undertaken in accordance with institutional animal care and use permits (Smithsonian Institution IACUC permit No. 2009-04) and the guidelines of the American Society of Mammalogists for the use of wild mammals in research (Sikes et al. 2011). We thank S. Miller, L. Helgen, C. France, A. Driskell, D. Lunde, J. Ososky, L. Cattaneo, A. Hintz, and H. Kafka for assistance at the Smithsonian. NR 79 TC 9 Z9 9 U1 5 U2 51 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 2015 VL 25 IS 2 BP 348 EP 360 DI 10.1890/14-0995.1 PG 13 WC Ecology; Environmental Sciences SC Environmental Sciences & Ecology GA CC7OA UT WOS:000350556400004 PM 26263659 ER PT J AU Kettenring, KM Whigham, DF Hazelton, ELG Gallagher, SK Weiner, HM AF Kettenring, Karin M. Whigham, Dennis F. Hazelton, Eric L. G. Gallagher, Sally K. Weiner, Heather M. TI Biotic resistance, disturbance, and mode of colonization impact the invasion of a widespread, introduced wetland grass SO ECOLOGICAL APPLICATIONS LA English DT Article DE asexual and sexual reproduction; biotic resistance; Chesapeake Bay; colonization; common reed; Distichlis spicata; disturbance; Iva frutescens; Phragmites australis; plant invasions; Schoenoplectus americanus; Spartina patens ID REED PHRAGMITES-AUSTRALIS; LIFE HISTORY STAGES; SALT-MARSH PLANTS; COMMON REED; GENETIC DIVERSITY; CHESAPEAKE BAY; NORTH-AMERICA; SPARTINA-ALTERNIFLORA; CALIFORNIA GRASSLAND; OXYGEN AVAILABILITY AB Disturbance and biotic resistance are important factors driving plant invasions, but how these factors interact for plants with different modes of colonization (i.e., sexual and asexual) is unclear. We evaluated factors influencing the invasion of nonnative Phragmites australis, which has been rapidly expanding in brackish tidal wetlands in Chesapeake Bay. We conducted a survey of naturally occurring small-scale disturbances (removal of vegetation and/or sediment deposition) across four plant communities; determined the effects of small-scale disturbance and biotic resistance on P. australis seedling and rhizome emergence; and tested the effects of size and frequency of small-scale disturbances on seedling emergence and survival of transplanted seedlings. The results of our study demonstrate that the invasion window for seeds is in disturbed areas in high-marsh plant communities that flood less frequently; seedling emergence in undisturbed areas was negligible. Establishment of shoots from rhizome segments was low in all plant communities. Disturbance size and frequency had no significant impact on seed germination and seedling survival. Our findings provide evidence that small-scale within-wetland disturbances are important for the invasion of the nonnative lineage of P. australis by seeds in brackish tidal wetlands in Chesapeake Bay. Efforts to reduce disturbances, large and small, in wetlands can be used to limit P. australis invasion by seed, but invasion by rhizome is still likely to occur across many plant communities irrespective of the presence of disturbance. C1 [Kettenring, Karin M.; Hazelton, Eric L. G.] Utah State Univ, Ctr Ecol, Logan, UT 84322 USA. [Kettenring, Karin M.; Hazelton, Eric L. G.] Utah State Univ, Dept Watershed Sci, Logan, UT 84322 USA. [Kettenring, Karin M.; Whigham, Dennis F.; Hazelton, Eric L. G.; Gallagher, Sally K.; Weiner, Heather M.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Kettenring, KM (reprint author), Utah State Univ, Ctr Ecol, Logan, UT 84322 USA. EM karin.kettenring@usu.edu OI Whigham, Dennis/0000-0003-1488-820X NR 80 TC 7 Z9 7 U1 9 U2 58 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 2015 VL 25 IS 2 BP 466 EP 480 DI 10.1890/14-0434.1 PG 15 WC Ecology; Environmental Sciences SC Environmental Sciences & Ecology GA CC7OA UT WOS:000350556400013 PM 26263668 ER PT J AU Turner, BL Laliberte, E AF Turner, Benjamin L. Laliberte, Etienne TI Soil Development and Nutrient Availability Along a 2 Million-Year Coastal Dune Chronosequence Under Species-Rich Mediterranean Shrubland in Southwestern Australia SO ECOSYSTEMS LA English DT Article DE chronosequence; ecosystem development; pedogenesis; nutrients; phosphorus; nitrogen ID TERM ECOSYSTEM DEVELOPMENT; SOUTH-WESTERN AUSTRALIA; SEA-LEVEL CHANGE; NEW-ZEALAND; PLANT DIVERSITY; ACQUISITION STRATEGIES; PHOSPHORUS FRACTIONS; FOREST SOILS; YELLOW SAND; PERTH BASIN AB Soil chronosequences provide valuable model systems to investigate pedogenesis and associated effects of nutrient availability on biological communities. However, long-term chronosequences occurring under seasonally dry climates remain scarce. We assessed soil development and nutrient dynamics along the Jurien Bay chronosequence, a 2 million-year sequence of coastal dunes in southwestern Australia. The chronosequence is significant because it occurs in a Mediterranean climate and supports hyperdiverse shrublands within a global biodiversity hotspot. Young soils formed during the Holocene (< 6,500 years old) are strongly alkaline and contain abundant carbonate, which is leached from the profile within a few thousand years. Middle Pleistocene soils (ca 120,000-500,000 years old) are yellow decalcified sands with residual iron oxide coatings on quartz grains over a petrocalcic horizon that occurs at increasing depth as soils age. Early Pleistocene soils (> 2,000,000 years old) are completely leached of iron oxides and consist of bleached quartz sand several meters deep. Changes in soil organic matter and nutrient status along the Jurien Bay chronosequence are consistent with patterns observed along other long-term chronosequences and correspond closely to expectations of the Walker and Syers (1976) model of biogeochemical change during pedogenesis. Organic carbon and nitrogen (N) accumulate rapidly to maximum amounts in intermediate-aged Holocene dunes and then decline as soils age. In contrast, total phosphorus (P) declines continuously along the chronosequence to extremely low levels after 2 million years of pedogenesis, eventually representing some of the lowest P soils globally. Ratios of soil organic carbon to P and N to P increase continuously along the chronosequence, consistent with a shift from N limitation on young soils to extreme P limitation on old soils. Phosphorus fractionation by sequential extraction reveals a rapid decline in primary and non-occluded phosphate and an increase in organic and occluded P as soils age. Concentrations of extractable (that is, readily bioavailable) N and P, as well as exchangeable cations, are greatest in Holocene dunes and decline to low levels in Pleistocene dunes. Extractable micronutrient concentrations were generally very low and varied little across the chronosequence. We conclude that the Jurien Bay chronosequence is an important example of changing patterns of nutrient limitation linked to long-term soil and ecosystem development under a Mediterranean climate. C1 [Turner, Benjamin L.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Laliberte, Etienne] Univ Western Australia, Sch Plant Biol, Perth, WA 6009, Australia. RP Turner, BL (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Ancon, Panama. EM TurnerBL@si.edu RI Laliberte, Etienne/B-6855-2008; Turner, Benjamin/E-5940-2011 OI Laliberte, Etienne/0000-0002-3167-2622; Turner, Benjamin/0000-0002-6585-0722 FU Australian Research Council [DE120100352]; University of Western Australia FX Funding was provided by a Discovery Early Career Researcher Award (DE120100352) from the Australian Research Council and a Research Collaboration Award from The University of Western Australia (both to EL). The authors thank Dayana Agudo, Pedro Arauz, Aleksandra Bielnicka, and Paola Escobar for laboratory support; and Felipe Albornoz, Patrick Hayes, Hans Lambers, Kenny Png, Francois Teste, Karl-Heinz Wyrwoll, and Graham Zemunik for assistance in the field. Figure 1 was created using base maps provided by the Department of Agriculture and Food of Western Australia. NR 102 TC 12 Z9 12 U1 8 U2 49 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1432-9840 EI 1435-0629 J9 ECOSYSTEMS JI Ecosystems PD MAR PY 2015 VL 18 IS 2 BP 287 EP 309 DI 10.1007/s10021-014-9830-0 PG 23 WC Ecology SC Environmental Sciences & Ecology GA CD2CC UT WOS:000350880400009 ER PT J AU Siegal-Willott, JL Jensen, N Kim, D Taliaferro, D Blankenship, T Malinsky, B Murray, S Eiden, MV Xu, WQ AF Siegal-Willott, Jessica L. Jensen, Nathaniel Kim, David Taliaferro, Dwayne Blankenship, Tiffany Malinsky, Becky Murray, Suzan Eiden, Maribeth V. Xu, Wenqin TI EVALUATION OF CAPTIVE GIBBONS (HYLOBATES SPP., NOMASCUS SPP., SYMPHALANGUS SPP.) IN NORTH AMERICAN ZOOLOGICAL INSTITUTIONS FOR GIBBON APE LEUKEMIA VIRUS (GALV) SO JOURNAL OF ZOO AND WILDLIFE MEDICINE LA English DT Article DE Gibbon; Hylobates; leukemia; Nomascus; retrovirus; Symphalangus ID C-TYPE VIRUS; HALLS ISLAND; RETROVIRUS; SEQUENCES; ONCOGENICITY; INFECTIONS; CATS AB This study evaluated 79 captive gibbons (Hylobates, Nomascus, and Symphalangus spp.) within 30 North American zoological institutions for evidence of exposure to and possible infection with gibbon ape leukemia virus (GALV). Enzyme-linked immunosorbent assays (ELISAs) on gibbon serum samples revealed the presence of antibodies against GALV antigens in 28% of animals, indicating previous exposure or possibly protective immunity to GALV. Virus detection in gibbon blood or serum using polymerase chain reaction (PCR) or co-culture of gibbon peripheral blood mononuclear cells with human cells was negative for all samples submitted. The majority (19/27, 70%) of animals with reported health conditions were clinically healthy at the time of sample collection. Historically accrued clinical data were used to assess association of diseases in gibbons antibody positive for GALV. The results suggest captive gibbons could mount an immune response to GALV and show no evidence of infection. There was no association with neoplastic conditions in seropositive animals. The potential role of gibbons as a reservoir for GALV and the role of GALV as an epizoonotic-zoonotic agent or as a contributor to gibbon ape morbidity and mortality are not substantiated by the study findings. C1 [Siegal-Willott, Jessica L.; Murray, Suzan] Smithsonian Inst, Natl Zool Pk, Dept Wildlife Hlth Serv, Washington, DC 20008 USA. [Malinsky, Becky] Smithsonian Inst, Natl Zool Pk, Anim Programs, Washington, DC 20008 USA. [Jensen, Nathaniel; Kim, David; Taliaferro, Dwayne; Blankenship, Tiffany; Eiden, Maribeth V.; Xu, Wenqin] NIMH, Sect Directed Gene Transfer, Lab Cellular & Mol Regulat, NIH, Bethesda, MD 20892 USA. RP Xu, WQ (reprint author), NIMH, Sect Directed Gene Transfer, Lab Cellular & Mol Regulat, NIH, Bethesda, MD 20892 USA. EM xuwenqin@mail.nih.gov FU National Institute of Mental Health FX The authors thank Jim Nagle and Debbie Kauffmann at the National Institute of Neurological Disorders and Stroke sequencing facility (National Institutes of Health) for sequencing. We are grateful to Kristen Kluska for her editorial help. The authors also acknowledge the valuable information obtained in conversations with the late Alan Mootnick, whose broad knowledge of gibbon conservation practices in the United States was greatly appreciated. The authors thank Jay Petersen (gibbon Species Survival Plan coordinator) and Lisa Stevens (curator of primates, National Zoological Park) for their assistance with sample collection. The authors thank all of the participating institutions and their associated staff, including Binder Park Zoo, Birmingham Zoo, Blank Park Zoo, Brookfield Zoological Society, Dallas Zoo, Denver Zoo, Detroit Zoo, Fort Wayne Children's Zoo, Great Plains Zoo, Indianapolis Zoo, Jackson Zoological Park, Jacksonville Zoo, Los Angeles Zoo, Little Rock Zoo, Lion Country Safari Zoo, Nebraska Zoo, Phoenix Zoo, Pueblo Zoo, Rio Grande Zoo, Roger Williams Park Zoo, Sacramento Zoo, San Diego Zoo Safari Park, Seneca Park Zoo, Smithsonian Institution's National Zoological Park, Tulsa Zoo, Turtle Back Zoo, Utica Zoo, Woodland Park Zoo, and Zoo New England. This work was supported by the National Institute of Mental Health intramural funding. NR 28 TC 2 Z9 2 U1 1 U2 8 PU AMER ASSOC ZOO VETERINARIANS PI YULEE PA 581705 WHITE OAK ROAD, YULEE, FL 32097 USA SN 1042-7260 EI 1937-2825 J9 J ZOO WILDLIFE MED JI J. Zoo Wildl. Med. PD MAR PY 2015 VL 46 IS 1 BP 27 EP 33 DI 10.1638/2014-0034R.1 PG 7 WC Veterinary Sciences SC Veterinary Sciences GA CD2CG UT WOS:000350880800004 PM 25831573 ER PT J AU Luque, J AF Luque, Javier TI THE OLDEST HIGHER TRUE CRABS (CRUSTACEA: DECAPODA: BRACHYURA): INSIGHTS FROM THE EARLY CRETACEOUS OF THE AMERICAS SO PALAEONTOLOGY LA English DT Article DE Americas; crab; Early Cretaceous; Eubrachyura; evolution; neotropics ID PHYLOGENETIC ANALYSIS; CLASSIFICATION; PODOTREMATA; HOMOLOIDEA; RANINOIDA; FAMILIES AB Despite the extensive fossil record of higher crabs (Eubrachyura) from Late Cretaceous and Cenozoic rocks worldwide, their Early Cretaceous occurrences are scarce and fragmentary, obscuring our understanding of their early evolution. Until now, representatives of only two families of eubrachyuran-like crabs were known from the Early Cretaceous: Componocancridae and Tepexicarcinidae fam. nov., both monospecific lineages from the Albian (110-100Ma) of North and Central America, respectively. The discovery of Telamonocarcinus antiquus sp. nov. (Telamonocarcinidae) from the early Albian of Colombia, South America (110Ma), increases to three the number of known Early Cretaceous eubrachyuran-like families. The ages and geographical distributions of the oldest eubrachyuran-like taxa (i.e. Componocancridae, Telamonocarcinidae and Tepexicarcinidae fam. nov.) suggest that the oldest higher true crabs might have originated in the Americas; that they were already morphologically diverse by the late Early Cretaceous; and that their most recent common ancestor must be rooted in the Early Cretaceous, or even the Late Jurassic. C1 [Luque, Javier] Univ Alberta, Dept Biol Sci, Edmonton, AB T6G 2E9, Canada. [Luque, Javier] Smithsonian Trop Res Inst, Balboa 084303092, Panama. RP Luque, J (reprint author), Univ Alberta, Dept Biol Sci, Edmonton, AB T6G 2E9, Canada. EM luque@ualberta.ca OI Luque, Javier/0000-0002-4391-5951 FU STRI, Panama; University of Alberta, Canada; Natural Science and Engineering Research Council of Canada; NSERC; Canada Graduate Scholarship (NSERC CGS-D); Fondo Corrigan-ACGGP-ARES Grant; Discovery Grant [A7245] FX Funding for this research was provided by Carlos Jaramillo (STRI, Panama), A. Richard Palmer (University of Alberta, Canada), a Natural Science and Engineering Research Council of Canada, NSERC, Discovery Grant A7245 to ARP, and a Canada Graduate Scholarship (NSERC CGS-D) and Fondo Corrigan-ACGGP-ARES Grant to JL. Special thanks to Jorge Moreno (University of Nebraska-Lincoln, USA) who discovered the holotype of Telamonocarcinus antiquus and Alexis Rojas (FLMNH, USA) for valuable field assistance; Luis Felipe Guarin for providing field facilities and permission to collect on his property; Fernando Etayo, Roberto Terraza and Diana Montoya (Colombian Geological Survey), for field support and information regarding the stratigraphic position of the material studied; Kecia Kerr (STRI, Panama), Rodney Feldmann and Carrie Schweitzer (Kent State University, USA), for intellectual support and providing literature items; Alessandro Garassino (Museo di Storia Naturale, Italy), Hiroaki Karasawa (Mizunami Fossil Museum, Japan) and John E. Simes (GNS Science, New Zealand), for providing images of different type specimens herein illustrated. Jose Arenas (Colombian Geological Survey, Colombia) provided the export permits. My deepest thanks to Rodney Feldmann (Kent State University, USA), Barry van Bakel (Oertijdmuseum De Groene Poort, Boxtel, the Netherlands) and editors John W.M. Jagt and Sally Thomas, for valuable suggestions that improved the final manuscript. NR 66 TC 6 Z9 6 U1 0 U2 3 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0031-0239 EI 1475-4983 J9 PALAEONTOLOGY JI Paleontology PD MAR PY 2015 VL 58 IS 2 BP 251 EP 263 DI 10.1111/pala.12135 PG 13 WC Paleontology SC Paleontology GA CD0HW UT WOS:000350752400005 ER PT J AU Power, ML AF Power, M. L. TI The milk microbiome SO AMERICAN JOURNAL OF HUMAN BIOLOGY LA English DT Meeting Abstract C1 [Power, M. L.] Natl Zool Pk, Smithsonian Conservat Biol Inst, Nutr Lab, Conservat Ecol Ctr, Washington, DC USA. NR 0 TC 0 Z9 0 U1 1 U2 4 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1042-0533 EI 1520-6300 J9 AM J HUM BIOL JI Am. J. Hum. Biol. PD MAR-APR PY 2015 VL 27 IS 2 BP 283 EP 283 PG 1 WC Anthropology; Biology SC Anthropology; Life Sciences & Biomedicine - Other Topics GA CC6KH UT WOS:000350473300082 ER PT J AU Chaput, DL Hansel, CM Burgos, WD Santelli, CM AF Chaput, Dominique L. Hansel, Colleen M. Burgos, William D. Santelli, Cara M. TI Profiling Microbial Communities in Manganese Remediation Systems Treating Coal Mine Drainage SO APPLIED AND ENVIRONMENTAL MICROBIOLOGY LA English DT Article ID RICE FIELD SUBSOILS; MN(II) OXIDATION; BACTERIAL COMMUNITIES; MN(II)-OXIDIZING BACTERIA; SUPEROXIDE-PRODUCTION; PASSIVE TREATMENT; FUNGI; OXIDES; ALGAE; WATER AB Water discharging from abandoned coal mines can contain extremely high manganese levels. Removing this metal is an ongoing challenge. Passive Mn(II) removal beds (MRBs) contain microorganisms that oxidize soluble Mn(II) to insoluble Mn(III/IV) minerals, but system performance is unpredictable. Using amplicon pyrosequencing, we profiled the bacterial, fungal, algal, and archaeal communities in four MRBs, performing at different levels, in Pennsylvania to determine whether they differed among MRBs and from surrounding soil and to establish the relative abundance of known Mn(II) oxidizers. Archaea were not detected; PCRs with archaeal primers returned only nontarget bacterial sequences. Fungal taxonomic profiles differed starkly between sites that remove the majority of influent Mn and those that do not, with the former being dominated by Ascomycota (mostly Dothideomycetes) and the latter by Basidiomycota (almost entirely Agaricomycetes). Taxonomic profiles for the other groups did not differ significantly between MRBs, but operational taxonomic unit-based analyses showed significant clustering by MRB with all three groups (P < 0.05). Soil samples clustered separately from MRBs in all groups except fungi, whose soil samples clustered loosely with their respective MRB. Known Mn(II) oxidizers accounted for a minor proportion of bacterial sequences (up to 0.20%) but a greater proportion of fungal sequences (up to 14.78%). MRB communities are more diverse than previously thought, and more organisms may be capable of Mn(II) oxidation than are currently known. C1 [Chaput, Dominique L.; Santelli, Cara M.] Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. [Hansel, Colleen M.] Woods Hole Oceanog Inst, Dept Marine Chem & Geochem, Woods Hole, MA 02543 USA. [Burgos, William D.] Penn State Univ, Dept Civil & Environm Engn, University Pk, PA 16802 USA. RP Santelli, CM (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. EM santellic@si.edu OI Chaput, Dominique/0000-0002-9736-2619; Santelli, Cara/0000-0001-8617-0008 FU Smithsonian Postdoctoral Fellowship; National Science Foundation [EAR-1249489, CBET-1336496]; Smithsonian Scholarly Studies and Next-Generation Sequencing grants FX This project was funded by Smithsonian Scholarly Studies and Next-Generation Sequencing grants to C.M.S., by a Smithsonian Postdoctoral Fellowship to D.L.C., and by the National Science Foundation, grant numbers EAR-1249489 (awarded to C.M.H.) and CBET-1336496 (awarded to C.M.H. and C.M.S.). NR 67 TC 8 Z9 8 U1 3 U2 41 PU AMER SOC MICROBIOLOGY PI WASHINGTON PA 1752 N ST NW, WASHINGTON, DC 20036-2904 USA SN 0099-2240 EI 1098-5336 J9 APPL ENVIRON MICROB JI Appl. Environ. Microbiol. PD MAR PY 2015 VL 81 IS 6 BP 2189 EP 2198 DI 10.1128/AEM.03643-14 PG 10 WC Biotechnology & Applied Microbiology; Microbiology SC Biotechnology & Applied Microbiology; Microbiology GA CC7NM UT WOS:000350554800035 PM 25595765 ER PT J AU Barnard, R Garcia, MR Murray, SS AF Barnard, R. Garcia, M. R. Murray, S. S. TI SWIFT REVEALS A similar to 5.7 DAY SUPER-ORBITAL PERIOD IN THE M31 GLOBULAR CLUSTER X-RAY BINARY XB158 SO ASTROPHYSICAL JOURNAL LA English DT Article DE X-rays: binaries; X-rays: general ID UPDATED SURVEY; VW HYDRI; STARS; M-31; STABILITY; BO-158 AB The M31 globular cluster X-ray binary XB158 (a.k.a. Bo 158) exhibits intensity dips on a 2.78 hr period in some observations, but not others. The short period suggests a low mass ratio, and an asymmetric, precessing disk due to additional tidal torques from the donor star since the disk crosses the 3:1 resonance. Previous theoretical three-dimensional smoothed particle hydrodynamical modeling suggested a super-orbital disk precession period 29 +/- 1 times the orbital period, i.e., similar to 81 +/- 3 hr. We conducted a Swift monitoring campaign of 30 observations over similar to 1 month in order to search for evidence of such a super-orbital period. Fitting the 0.3-10 keV Swift X-Ray Telescope luminosity light curve with a sinusoid yielded a period of 5.65 +/- 0.05 days, and a > 5 sigma improvement in chi(2) over the best fit constant intensity model. A Lomb-Scargle periodogram revealed that periods of 5.4-5.8 days were detected at a > 3 sigma level, with a peak at 5.6 days. We consider this strong evidence for a 5.65 day super-orbital period, similar to 70% longer than the predicted period. The 0.3-10 keV luminosity varied by a factor of similar to 5, consistent with variations seen in long-term monitoring from Chandra. We conclude that other X-ray binaries exhibiting similar long-term behavior are likely to also be X-ray binaries with low mass ratios and super-orbital periods. C1 [Barnard, R.; Garcia, M. R.; Murray, S. S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Murray, S. S.] Johns Hopkins Univ, Baltimore, MD 21218 USA. RP Barnard, R (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. FU Swift [NNX13AJ76G] FX We thank the anonymous referees for suggesting improvements to this work, in particular for prompting a more rigorous estimation of the super-orbital period. We thank the Swift team for making this work possible. This work was funded by Swift grant NNX13AJ76G. NR 25 TC 1 Z9 1 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 2015 VL 801 IS 1 AR 65 DI 10.1088/0004-637X/801/1/65 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CC6PR UT WOS:000350488700065 ER PT J AU Guidorzi, C Dichiara, S Frontera, F Margutti, R Baldeschi, A Amati, L AF Guidorzi, C. Dichiara, S. Frontera, F. Margutti, R. Baldeschi, A. Amati, L. TI A COMMON STOCHASTIC PROCESS RULES GAMMA-RAY BURST PROMPT EMISSION AND X-RAY FLARES SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma-ray burst: general; methods: statistical ID WAITING-TIME DISTRIBUTION; SELF-ORGANIZED CRITICALITY; POWER-DENSITY SPECTRUM; INTERNAL-SHOCK MODEL; STATISTICAL PROPERTIES; QUIESCENT TIMES; CENTRAL ENGINE; SOLAR-FLARES; TEMPORAL PROPERTIES; ACCRETION DISK AB Prompt gamma-ray and early X-ray afterglow emissions in gamma-ray bursts (GRBs) are characterized by a bursty behavior and are often interspersed with long quiescent times. There is compelling evidence that X-ray flares are linked to prompt gamma-rays. However, the physical mechanism that leads to the complex temporal distribution of gamma-ray pulses and X-ray flares is not understood. Here we show that the waiting time distribution (WTD) of pulses and flares exhibits a power-law tail extending over four decades with an index of about two and can be the manifestation of a common time-dependent Poisson process. This result is robust and is obtained on different catalogs. Surprisingly, GRBs with many (>= 8) gamma-ray pulses are very unlikely to be accompanied by X-ray flares after the end of the prompt emission (3.1 sigma Gaussian confidence). These results are consistent with a simple interpretation: a hyperaccreting disk breaks up into one or a few groups of fragments, each of which is independently accreted with the same probability per unit time. Prompt gamma-rays and late X-ray flares are nothing but different fragments being accreted at the beginning and at the end, respectively, following the very same stochastic process and likely the same mechanism. C1 [Guidorzi, C.; Dichiara, S.; Frontera, F.; Baldeschi, A.] Univ Ferrara, Dept Phys & Earth Sci, I-44122 Ferrara, Italy. [Frontera, F.; Amati, L.] INAF IASF Bologna, I-40129 Bologna, Italy. [Margutti, R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Guidorzi, C (reprint author), Univ Ferrara, Dept Phys & Earth Sci, Via Saragat 1, I-44122 Ferrara, Italy. RI Amati, Lorenzo/N-5586-2015; OI Amati, Lorenzo/0000-0001-5355-7388; Margutti, Raffaella/0000-0003-4768-7586 FU PRIN MIUR project on "Gamma-ray bursts: From progenitors to physics of the prompt emission process" [Prot. 2009 ERC3HT] FX We are grateful to the anonymous referee for a constructive and insightful review. The PRIN MIUR project on "Gamma-ray bursts: From progenitors to physics of the prompt emission process," P.I. F. Frontera (Prot. 2009 ERC3HT), is acknowledged. NR 88 TC 7 Z9 8 U1 1 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 2015 VL 801 IS 1 AR 57 DI 10.1088/0004-637X/801/1/57 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CC6PR UT WOS:000350488700057 ER PT J AU Hernitschek, N Rix, HW Bovy, J Morganson, E AF Hernitschek, Nina Rix, Hans-Walter Bovy, Jo Morganson, Eric TI ESTIMATING BLACK HOLE MASSES IN HUNDREDS OF QUASARS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: photometry; quasars: supermassive black holes ID DIGITAL-SKY-SURVEY; ACTIVE GALACTIC NUCLEI; RADIUS-LUMINOSITY RELATIONSHIP; DAMPED RANDOM-WALK; LINE REGION SIZES; REVERBERATION LAGS; DATA RELEASE; STRIPE 82; VARIABILITY; GALAXIES AB We explore the practical feasibility of active galactic nucleus (AGN) broadband reverberation mapping and present first results. We lay out and apply a rigorous approach for the stochastic reverberation mapping of unevenly sampled multi-broadband flux measurements, assuming that the broad-line region (BLR) line flux is contributing up to 15% in some bands, and is directly constrained by one spectroscopical epoch. The approach describes variations of the observed flux as the continuum, modeled as a stochastic Gaussian process, and emission line contribution, modeled as a scaled, smoothed, and delayed version of the continuum. This approach can be used not only to interpolate in time between measurements, but also to determine confidence limits on continuum-line emission delays. This approach is applied to Sloan Digital Sky Survey observations in Stripe 82 (S82), providing flux measurements that are precise to 2% at similar to 60 epochs over similar to 10 yr. The strong annual variations in the epoch sampling prove a serious limitation in practice. In addition, suitable redshift ranges must be identified where strong, broad emission lines contribute to one filter, but not to another. By generating and evaluating problem-specific mock data, we verify that S82-like data can constrain tau(delay) for a simple transfer function model. In application to real data, we estimate tdelay for 323 AGNs with 0.225 < z < 0.846, combining information for different objects through the ensemble-scaling relationships for BLR size and black hole mass. Our analysis tentatively indicates a 1.7 times larger BLR size of Ha and Mg II compared to Kaspi et al. and Vestergaard, but the seasonal data sampling casts doubt on the robustness of the inference. C1 [Hernitschek, Nina; Rix, Hans-Walter] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Bovy, Jo] Inst Adv Study, Sch Nat Sci, Princeton, NJ 08540 USA. [Morganson, Eric] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Hernitschek, N (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. EM hernitschek@mpia-hd.mpg.de OI Bovy, Jo/0000-0001-6855-442X; Hernitschek, Nina/0000-0003-1681-0430 FU European Research Council under European Union's Seventh Framework Programme (FP 7) ERC [321035]; NASA grant from Space Telescope Science Institute [HST-HF-51285.01]; Association of Universities for Research in Astronomy, Incorporated, under NASA [NAS5-26555] FX The research leading to these results received funding from the European Research Council under the European Union's Seventh Framework Programme (FP 7) ERC Grant Agreement No. [321035]. Jo Bovy was supported by NASA through Hubble Fellowship grant HST-HF-51285.01 from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. NR 50 TC 3 Z9 3 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 MAR 1 PY 2015 VL 801 IS 1 AR 45 DI 10.1088/0004-637X/801/1/45 PG 31 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CC6PR UT WOS:000350488700045 ER PT J AU MacGregor, MA Wilner, DJ Andrews, SM Hughes, AM AF MacGregor, Meredith A. Wilner, David J. Andrews, Sean M. Hughes, A. Meredith TI RESOLVED MILLIMETER EMISSION FROM THE HD 15115 DEBRIS DISK SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; stars: individual (HD 15115); submillimeter: planetary systems ID INTERSTELLAR-MEDIUM; STELLAR ENCOUNTERS; DUST PROPERTIES; AU MICROSCOPII; GAS; DYNAMICS; SYSTEM; BELT; WAVELENGTHS; CANDIDATES AB We have used the Submillimeter Array (SMA) to make 1.3 mm observations of the debris disk surrounding HD 15115, an F-type star with a putative membership in the beta Pictoris moving group. This nearly edge-on debris disk shows an extreme asymmetry in optical scattered light, with an extent almost two times larger to the west of the star than to the east (originally dubbed the "Blue Needle"). The SMA observations reveal resolved emission that we model as a circumstellar belt of thermal dust emission. This belt extends to a radius of similar to 110 AU, coincident with the break in the scattered light profile convincingly seen on the western side of the disk. This outer edge location is consistent with the presence of an underlying population of dust-producing planetesimals undergoing a collisional cascade, as hypothesized in "birth ring" theory. In addition, the millimeter emission shows a similar to 3 sigma feature aligned with the asymmetric western extension of the scattered light disk. If this millimeter extension is real, then mechanisms for asymmetry that affect only small grains, such as interactions with interstellar gas, are disfavored. This tentative feature might be explained by secular perturbations to grain orbits introduced by neutral gas drag, as previously invoked to explain asymmetric morphologies of other, similar debris disks. C1 [MacGregor, Meredith A.; Wilner, David J.; Andrews, Sean M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hughes, A. Meredith] Wesleyan Univ, Dept Astron, Van Vleck Observ, Middletown, CT 06459 USA. RP MacGregor, MA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI MacGregor, Meredith/0000-0001-7891-8143 FU National Science Foundation Graduate Research Fellowship [DGE1144152] FX We thank Paul Kalas for providing the Hubble Space Telescope image in Figure 1. M.A.M acknowledges support from a National Science Foundation Graduate Research Fellowship (DGE1144152). We thank Katherine Rosenfeld, Til Birnstiel and John Debes for helpful conversations. NR 46 TC 6 Z9 6 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 2015 VL 801 IS 1 AR 59 DI 10.1088/0004-637X/801/1/59 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CC6PR UT WOS:000350488700059 ER PT J AU Muirhead, PS Mann, AW Vanderburg, A Morton, TD Kraus, A Ireland, M Swift, JJ Feiden, GA Gaidos, E Gazak, JZ AF Muirhead, Philip S. Mann, Andrew W. Vanderburg, Andrew Morton, Timothy D. Kraus, Adam Ireland, Michael Swift, Jonathan J. Feiden, Gregory A. Gaidos, Eric Gazak, J. Zachary TI KEPLER-445, KEPLER-446 AND THE OCCURRENCE OF COMPACT MULTIPLES ORBITING MID-M DWARF STARS SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; stars: fundamental parameters; stars: individual (KOI-2704, KOI-2842, Kepler-42, Barnard's Star); stars: late-type; stars: low-mass ID DIGITAL SKY SURVEY; EARTH GJ 1214B; K-BAND SPECTRA; OPTICAL APERTURE-SYNTHESIS; POTENTIAL TRANSIT SIGNALS; GIANT PLANET OCCURRENCE; SOLAR-TYPE STARS; LOW MASS STARS; DATA RELEASE; HOST-STARS AB We confirm and characterize the exoplanetary systems Kepler-445 and Kepler-446: two mid-M dwarf stars, each with multiple, small, short-period transiting planets. Kepler-445 is a metal-rich ([ Fe/H] = + 0.25 0.10) M4 dwarf with three transiting planets, and Kepler-446 is a metal-poor ([ Fe/H] = -0.30 0.10) M4 dwarf also with three transiting planets. Kepler-445c is similar toGJ 1214b: both in planetary radius and the properties of the host star. The Kepler-446 system is similar to the Kepler-42 system: both are metal-poor with large galactic space velocities and three short-period, likely rocky transiting planets that were initially assigned erroneously large planet-to-star radius ratios. We independently determined stellar parameters from spectroscopy and searched for and fitted the transit light curves for the planets, imposing a strict prior on stellar density in order to remove correlations between the fitted impact parameter and planet-to-star radius ratio for short-duration transits. Combining Kepler-445, Kepler-446, and Kepler-42, and isolating all mid-M dwarf stars observed by Kepler with the precision necessary to detect similar systems, we calculate that 21+ 7 -5 % of mid-M dwarf stars host compact multiples ( multiple planets with periods of less than 10 days) for a wide range of metallicities. We suggest that the inferred planet masses for these systems support highly efficient accretion of protoplanetary disk metals by mid-M dwarf protoplanets. C1 [Muirhead, Philip S.] Boston Univ, Dept Astron, Boston, MA 02215 USA. [Mann, Andrew W.; Kraus, Adam] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Vanderburg, Andrew] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Morton, Timothy D.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Ireland, Michael] Australian Natl Univ, Canberra, ACT 2611, Australia. [Swift, Jonathan J.] CALTECH, Dept Astrophys, Pasadena, CA 91125 USA. [Feiden, Gregory A.] Uppsala Univ, Dept Phys & Astron, SW-75120 Uppsala, Sweden. [Gaidos, Eric] Univ Hawaii Manoa, Dept Geol & Geophys, Honolulu, HI 96822 USA. [Gazak, J. Zachary] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. RP Muirhead, PS (reprint author), Boston Univ, Dept Astron, 725 Commonwealth Ave, Boston, MA 02215 USA. EM philipm@bu.edu RI Feiden, Gregory/F-1505-2015; Muirhead, Philip/H-2273-2014 OI Feiden, Gregory/0000-0002-2012-7215; Muirhead, Philip/0000-0002-0638-8822 NR 128 TC 14 Z9 14 U1 1 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 2015 VL 801 IS 1 AR 18 DI 10.1088/0004-637X/801/1/18 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CC6PR UT WOS:000350488700018 ER PT J AU Schaefer, L Sasselov, D AF Schaefer, Laura Sasselov, Dimitar TI THE PERSISTENCE OF OCEANS ON EARTH-LIKE PLANETS: INSIGHTS FROM THE DEEP-WATER CYCLE SO ASTROPHYSICAL JOURNAL LA English DT Article DE convection; planets and satellites: oceans; planets and satellites: tectonics; planets and satellites: terrestrial planets ID SUPER-EARTHS; UPPER-MANTLE; TERRESTRIAL PLANETS; DEPENDENT VISCOSITY; THERMAL EVOLUTION; SPACE-TELESCOPE; PLATE-TECTONICS; CONVECTION; ATMOSPHERE; RHEOLOGY AB In this paper we present a series of models for the deep-water cycle on super-Earths experiencing plate tectonics. The deep-water cycle can be modeled through parameterized convection models coupled with a volatile recycling model. The convection of the silicate mantle is linked to the volatile cycle through the water-dependent viscosity. Important differences in surface water content are found for different parameterizations of convection. Surface oceans are smaller and more persistent for single layer convection, rather than convection by boundary layer instability. Smaller planets have initially larger oceans but also return that water to the mantle more rapidly than larger planets. Super-Earths may therefore be less habitable in their early years than smaller planets, but their habitability (assuming stable surface conditions) will persist much longer. C1 [Schaefer, Laura; Sasselov, Dimitar] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Schaefer, L (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM lschaefer@cfa.harvard.edu OI Schaefer, Laura/0000-0003-2915-5025 NR 55 TC 9 Z9 9 U1 2 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 MAR 1 PY 2015 VL 801 IS 1 AR 40 DI 10.1088/0004-637X/801/1/40 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CC6PR UT WOS:000350488700040 ER PT J AU France, K McCray, R Fransson, C Larsson, J Frank, KA Burrows, DN Challis, P Kirshner, RP Chevalier, RA Garnavich, P Heng, K Lawrence, SS Lundqvist, P Smith, N Sonneborn, G AF France, Kevin McCray, Richard Fransson, Claes Larsson, Josefin Frank, Kari A. Burrows, David N. Challis, Peter Kirshner, Robert P. Chevalier, Roger A. Garnavich, Peter Heng, Kevin Lawrence, Stephen S. Lundqvist, Peter Smith, Nathan Sonneborn, George TI MAPPING HIGH-VELOCITY H alpha AND Ly alpha EMISSION FROM SUPERNOVA 1987A SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE circumstellar matter; shock waves; supernovae: individual (SN 1987A) ID SN 1987A; REMNANT 1987A; SN-1987A; RING; NEBULA; SHOCK; TWIN; GAS AB We present new Hubble Space Telescope images of high-velocity H alpha and Ly alpha emission in the outer debris of SN 1987 A. The Ha images are dominated by emission from hydrogen atoms crossing the reverse shock (RS). For the first time we observe emission from the RS surface well above and below the equatorial. ring (ER), suggesting a bipolar or conical structure perpendicular to the ring plane. Using the H alpha imaging, we measure the mass flux of hydrogen atoms crossing the RS front, in the velocity intervals (-7500 < V-obs < -2800 km s(-1)) and (1000 < V-obs < 7500 km s(-1)), (M)(H) over dot = 1.2 x 10(-3) M-circle dot yr(-1). We also present the first Ly alpha imaging of the whole remnant and new Chandra X-ray observations. Comparing the spatial distribution of the Ly alpha and X-ray emission, we observe that the majority of the high-velocity Ly alpha emission originates interior to the ER. The observed Ly alpha/H alpha photon ratio, < R(L alpha/H alpha)> approximate to 17, is significantly higher than the theoretically predicted ratio of approximate to 5 for neutral atoms crossing the RS front. We attribute this excess to Ly alpha emission produced by X-ray heating of the outer debris. The spatial orientation of the Ly alpha and X-ray emission suggests that X-ray heating of the outer debris is the dominant Ly alpha production mechanism in SN 1987 A at this phase in its evolution. C1 [France, Kevin] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80309 USA. [France, Kevin] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. [McCray, Richard] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Fransson, Claes; Lundqvist, Peter] Stockholm Univ, Oskar Klein Ctr, Dept Astron, SE-10691 Stockholm, Sweden. [Larsson, Josefin] KTH, Dept Phys, SE-10691 Stockholm, Sweden. [Larsson, Josefin] AlbaNova, Oskar Klein Ctr, SE-10691 Stockholm, Sweden. [Frank, Kari A.; Burrows, David N.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Challis, Peter; Kirshner, Robert P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Chevalier, Roger A.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Garnavich, Peter] Univ Notre Dame, Notre Dame, IN 46556 USA. [Heng, Kevin] Univ Bern, Ctr Space & Habitabil, CH-3012 Bern, Switzerland. [Lawrence, Stephen S.] Hofstra Univ, Dept Phys & Astron, Hempstead, NY 11549 USA. [Smith, Nathan] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Sonneborn, George] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP France, K (reprint author), Univ Colorado, Lab Atmospher & Space Phys, 392 UCB, Boulder, CO 80309 USA. EM kevin.france@colorado.edu FU Cycle SAINTS program [13401, 13405] FX The HST observations presented here were acquired as part of the Cycle SAINTS program (13401 and 13405). NR 16 TC 5 Z9 5 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD MAR 1 PY 2015 VL 801 IS 1 AR L16 DI 10.1088/2041-8205/801/1/L16 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CC3QB UT WOS:000350262900016 ER PT J AU Teske, JK Ghezzi, L Cunha, K Smith, VV Schuler, SC Bergemann, M AF Teske, Johanna K. Ghezzi, Luan Cunha, Katia Smith, Verne V. Schuler, Simon C. Bergemann, Maria TI ABUNDANCE DIFFERENCES BETWEEN EXOPLANET BINARY HOST STARS XO-2N AND XO-2S-DEPENDENCE ON STELLAR PARAMETERS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE planets and satellites: formation; planets and satellites: individual (XO-2); stars: abundances; stars: atmospheres ID GAS GIANT PLANETS; CONDENSATION TEMPERATURE; DETAILED ABUNDANCES; WIDE BINARIES; DEBRIS DISKS; METALLICITY; SYSTEM; COMPONENTS; ACCRETION; SILICON AB The chemical composition of exoplanet host stars is an important factor in understanding the formation and characteristics of their orbiting planets. The best example of this to date is the planet-metallicity correlation. Other proposed correlations are thus far less robust, in part due to uncertainty in the chemical history of stars pre- and post-planet formation. Binary host stars of similar type present an opportunity to isolate the effects of planets on host star abundances. Here we present a differential elemental abundance analysis of the XO-2 stellar binary, in which both G9 stars host giant planets, one of which is transiting. Building on our previous work, we report 16 elemental abundances and compare the Delta(XO-2N-XO-S) values to elemental condensation temperatures. The Delta(N-S) values and slopes with condensation temperature resulting from four different pairs of stellar parameters are compared to explore the effects of changing the relative temperature and gravity of the stars. We find that most of the abundance differences between the stars depend on the chosen stellar parameters, but that Fe, Si, and potentially Ni are consistently enhanced in XO-2N regardless of the chosen stellar parameters. This study emphasizes the power of binary host star abundance analysis for probing the effects of giant planet formation, but also illustrates the potentially large uncertainties in abundance differences and slopes induced by changes in stellar temperature and gravity. C1 [Teske, Johanna K.] Carnegie DTM, Washington, DC 20015 USA. [Ghezzi, Luan] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Cunha, Katia] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Cunha, Katia] Observ Nacl, BR-20921400 Rio De Janeiro, RJ, Brazil. [Smith, Verne V.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Schuler, Simon C.] Univ Tampa, Tampa, FL 33606 USA. [Bergemann, Maria] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Teske, Johanna K.] Carnegie Observ, Pasadena, CA USA. RP Teske, JK (reprint author), Carnegie DTM, 5241 Broad Branch Rd NW, Washington, DC 20015 USA. EM jteske@carnegiescience.edu NR 42 TC 13 Z9 13 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 1 PY 2015 VL 801 IS 1 AR L10 DI 10.1088/2041-8205/801/1/L10 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CC3QB UT WOS:000350262900010 ER PT J AU Tepolt, CK AF Tepolt, C. K. TI Adaptation in marine invasion: a genetic perspective SO BIOLOGICAL INVASIONS LA English DT Article; Proceedings Paper CT Workshop on Molecular Tools for Monitoring Marine Invasive Species CY SEP 12-14, 2012 CL Lecce, ITALY DE Adaptation; Genetics; Marine invasion; Next-generation sequencing; Selection ID SNAIL LITTORINA-SAXATILIS; MUSSELS GENUS MYTILUS; SPECIES DISTRIBUTION MODELS; BRYOZOAN BUGULA-NERITINA; HERRING CLUPEA-HARENGUS; EUROPEAN GREEN CRAB; CLIMATE-CHANGE; LOCAL ADAPTATION; POPULATION GENOMICS; BIOLOGICAL INVASIONS AB Genetic adaptation-heritable changes that alter an organism's performance-may facilitate invasion at several scales, but is seldom considered in predicting and managing marine invasions. However, a growing body of research-largely based on emerging genetic approaches-suggests that adaptation is possible and potentially widespread in the marine realm. Here, I review evidence for adaptation in marine invasion, considering both quantitative and genetic studies. Quantitative studies, which consider trait-based differences between populations or individuals without directly examining genetic makeup, have suggested local adaptation in several high-profile species. This implies that invasion risk may not be constant from population to population within a species, a key assumption of most invasion models. However, in many quantitative studies, the effects of heritable adaptive changes may be confounded with the effects of plasticity. Molecular approaches can help disentangle these effects, and studies at the genomic level are beginning to elucidate the specific genetic patterns and pathways underlying adaptation in invasion. While studies at this scale are currently rare in the marine invasion literature, they are likely to become increasingly prevalent-and useful-now that next-generation sequencing approaches have become tractable in non-model systems. Both traditional and emerging genetic approaches can improve our understanding of adaptation in marine invasions, and can aid managers in making accurate predictions of invasion spread and risk. C1 [Tepolt, C. K.] Stanford Univ, Hopkins Marine Stn, Pacific Grove, CA 93950 USA. RP Tepolt, CK (reprint author), Smithsonian Environm Res Ctr, 647 Contees Wharf Rd, Edgewater, MD 21037 USA. EM carolyn.tepolt@gmail.com FU Stanford Center for Computational, Evolutionary, and Human Genomics; CONISMA; Italian National Interuniversity Consortium for Marine Sciences; European Community's Seventh Framework Programme (FP7) for the project VECTORS FX I wish to thank Drs. Steve Palumbi and George Somero and two anonymous reviewers for their insightful comments on previous versions of this manuscript, and Drs. Alison Haupt and John Darling for their helpful overview of some of the tables. I was supported by a fellowship from the Stanford Center for Computational, Evolutionary, and Human Genomics; I greatly appreciate their support. The publication of this paper is supported by CONISMA, the Italian National Interuniversity Consortium for Marine Sciences, which received funding from the European Community's Seventh Framework Programme (FP7/2007-2013) for the project VECTORS (http://www.marine-vectors.eu). This paper stems from the International workshop MOLTOOLS (Molecular Tools for Monitoring Marine Invasive Species), held in Lecce, Italy, in September 2012. NR 128 TC 6 Z9 6 U1 6 U2 57 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 1387-3547 EI 1573-1464 J9 BIOL INVASIONS JI Biol. Invasions PD MAR PY 2015 VL 17 IS 3 SI SI BP 887 EP 903 DI 10.1007/s10530-014-0825-8 PG 17 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA CC9GI UT WOS:000350675900006 ER PT J AU Gamfeldt, L Lefcheck, JS Byrnes, JEK Cardinale, BJ Duffy, JE Griffin, JN AF Gamfeldt, Lars Lefcheck, Jonathan S. Byrnes, Jarrett E. K. Cardinale, Bradley J. Duffy, J. Emmett Griffin, John N. TI Marine biodiversity and ecosystem functioning: what's known and what's next? SO OIKOS LA English DT Review ID PREDATOR-PREY INTERACTIONS; SPECIES RICHNESS; CONSUMER DIVERSITY; GRAZER DIVERSITY; CLIMATE-CHANGE; FOOD-WEB; TROPHIC COMPLEXITY; MULTIPLE FUNCTIONS; BIOMASS PRODUCTION; FUTURE CHALLENGES AB Marine ecosystems are experiencing rapid and pervasive changes in biodiversity and species composition. Understanding the ecosystem consequences of these changes is critical to effectively managing these systems. Over the last several years, numerous experimental manipulations of species richness have been performed, yet existing quantitative syntheses have focused on a just a subset of processes measured in experiments and, as such, have not summarized the full data available from marine systems. Here, we present the results of a meta-analysis of 110 marine experiments from 42 studies that manipulated the species richness of organisms across a range of taxa and trophic levels and analysed the consequences for various ecosystem processes (categorised as production, consumption or biogeochemical fluxes). Our results show that, generally, mixtures of species tend to enhance levels of ecosystem function relative to the average component species in monoculture, but have no effect or a negative effect on functioning relative to the highest- performing' species. These results are largely consistent with those from other syntheses, and extend conclusions to ecological functions that are commonly measured in the marine realm (e.g. nutrient release from sediment bioturbation). For experiments that manipulated three or more levels of richness, we attempted to discern the functional form of the biodiversity-ecosystem functioning relationship. We found that, for response variables related to consumption, a power-function best described the relationship, which is also consistent with previous findings. However, we identified a linear relationship between richness and production. Combined, our results suggest that changes in the number of species will, on average, tend to alter the functioning of marine ecosystems. We outline several research frontiers that will allow us to more fully understand how, why, and when diversity may drive the functioning of marine ecosystems. Synthesis The oceans host an incredible number and variety of species. However, human activities are driving rapid changes in the marine environment. It is imperative we understand ecosystem consequences of any associated loss of species. We summarized data from 110 experiments that manipulated species diversity and evaluated resulting changes to a range of ecosystem responses. We show that losing species, on average, decreases productivity, growth, and a myriad of other processes related to how marine organisms capture and utilize resources. Finally, we suggest that the loss of species may have stronger consequences for some processes than others. C1 [Gamfeldt, Lars] Univ Gothenburg, Dept Biol & Environm Sci, SE-40530 Gothenburg, Sweden. [Lefcheck, Jonathan S.] Coll William & Mary, Virginia Inst Marine Sci, Dept Biol Sci, Gloucester Point, VA 23062 USA. [Byrnes, Jarrett E. K.] Univ Massachusetts, Dept Biol, Boston, MA 02125 USA. [Cardinale, Bradley J.] Univ Michigan, Sch Nat Resources & Environm, Ann Arbor, MI 48109 USA. [Duffy, J. Emmett] Smithsonian Inst, Tennenbaum Marine Observ Network, Washington, DC 20013 USA. [Griffin, John N.] Swansea Univ, Dept Biosci, Swansea SA2 8PP, W Glam, Wales. RP Gamfeldt, L (reprint author), Univ Gothenburg, Dept Biol & Environm Sci, Box 461, SE-40530 Gothenburg, Sweden. EM lars.gamfeldt@gu.se OI Byrnes, Jarrett/0000-0002-9791-9472; Lefcheck, Jonathan/0000-0002-8787-1786 FU Swedish Research Council VR [621-2009-5457]; NSF [OCE-1031061, DEB-1046121] FX This work is part of the NCEAS working group 'Biodiversity and the functioning of ecosystems: translating results from model experiments into functional reality'. Support for NCEAS comes from Univ. of California Santa Barbara and the National Science Foundation. Mary O'Connor and Lisandro Benedetti-Cecchi provided valuable feedback on earlier drafts. LG was supported by grant 621-2009-5457 from the Swedish Research Council VR. JED had support from NSF OCE-1031061; BJC had support from NSF DEB-1046121. NR 144 TC 25 Z9 25 U1 28 U2 150 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0030-1299 EI 1600-0706 J9 OIKOS JI Oikos PD MAR PY 2015 VL 124 IS 3 BP 252 EP 265 DI 10.1111/oik.01549 PG 14 WC Ecology SC Environmental Sciences & Ecology GA CC6GG UT WOS:000350462700002 ER PT J AU Thomas, BC Neale, PJ Snyder, BR AF Thomas, Brian C. Neale, Patrick J. Snyder, Brock R. TI Solar Irradiance Changes and Photobiological Effects at Earth's Surface Following Astrophysical Ionizing Radiation Events SO ASTROBIOLOGY LA English DT Article ID GAMMA-RAY BURSTS; BIOLOGICAL WEIGHTING FUNCTION; ULTRAVIOLET-B RADIATION; OZONE DEPLETION; COSMIC-RAYS; ACTION SPECTRUM; CLIMATE-CHANGE; HIGHER-PLANTS; UV; PHOTOSYNTHESIS AB Astrophysical ionizing radiation events have been recognized as a potential threat to life on Earth, primarily through depletion of stratospheric ozone and subsequent increase in surface-level solar ultraviolet radiation. Simulations of the atmospheric effects of a variety of events (such as supernovae, gamma-ray bursts, and solar proton events) have been previously published, along with estimates of biological damage at Earth's surface. In this work, we employed the Tropospheric Ultraviolet and Visible (TUV) radiative transfer model to expand and improve calculations of surface-level irradiance and biological impacts following an ionizing radiation event. We considered changes in surface-level UVB, UVA, and photosynthetically active radiation (visible light) for clear-sky conditions and fixed aerosol parameter values. We also considered a wide range of biological effects on organisms ranging from humans to phytoplankton. We found that past work overestimated UVB irradiance but that relative estimates for increase in exposure to DNA-damaging radiation are still similar to our improved calculations. We also found that the intensity of biologically damaging radiation varies widely with organism and specific impact considered; these results have implications for biosphere-level damage following astrophysical ionizing radiation events. When considering changes in surface-level visible light irradiance, we found that, contrary to previous assumptions, a decrease in irradiance is only present for a short time in very limited geographical areas; instead we found a net increase for most of the modeled time-space region. This result has implications for proposed climate changes associated with ionizing radiation events. Key Words: UV radiation-Supernovae-Extinctions-Radiative transfer. Astrobiology 15, 207-220. C1 [Thomas, Brian C.; Snyder, Brock R.] Washburn Univ, Dept Phys & Astron, Topeka, KS 66604 USA. [Neale, Patrick J.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Thomas, BC (reprint author), Washburn Univ, Dept Phys & Astron, 1700 SW Coll Ave, Topeka, KS 66604 USA. EM brian.thomas@washburn.edu OI Thomas, Brian/0000-0001-9091-0830 FU National Aeronautics and Space Administration through the Astrobiology: Exobiology and Evolutionary Biology Program [NNX09AM85G, NNX14AK22G] FX The authors thank Sasha Madronich for assistance with using and modifying the TUV code. This work has been supported by the National Aeronautics and Space Administration under grant Nos. NNX09AM85G and NNX14AK22G, through the Astrobiology: Exobiology and Evolutionary Biology Program. Computational time for this work was provided by the High Performance Computing Environment (HiPACE) at Washburn University; thanks to Steve Black for assistance with computing resources. The authors thank two anonymous reviewers for helpful comments that improved the manuscript. NR 67 TC 8 Z9 8 U1 1 U2 15 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 1 PY 2015 VL 15 IS 3 BP 207 EP 220 DI 10.1089/ast.2014.1224 PG 14 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA CD0ZU UT WOS:000350804100003 PM 25692406 ER PT J AU Martinsen, ES Brightman, H Fleischer, RC AF Martinsen, E. S. Brightman, H. Fleischer, R. C. TI Fecal samples fail in PCR-based diagnosis of malaria parasite infection in birds SO CONSERVATION GENETICS RESOURCES LA English DT Article DE Avian malaria parasites; Fecal diagnostics; Haemosporidians ID PLASMODIUM AB Malaria parasites are common in wild vertebrates on all warm continents and have recently been isolated from wild apes by non-invasive fecal sampling. Here, we examined the utility of fecal samples for malaria parasite detection in wild birds. We collected both blood and fecal samples from 56 birds sampled in the field, extracted DNA from all samples using various methods, and screened all samples using sensitive PCR-based methods. We found 35 birds to be positive for malaria parasite infection (genera Plasmodium and Parahaemoproteus) using blood samples while no fecal samples revealed a positive infection. These results suggest that malaria parasites cannot be efficiently detected from fecal samples of birds and that blood sampling is still necessary for the study of the malaria parasites of wild bird populations. C1 [Martinsen, E. S.; Brightman, H.; Fleischer, R. C.] Natl Zool Pk, Smithsonian Conservat Biol Inst, Ctr Conservat & Evolutionary Genet, Washington, DC 20013 USA. RP Martinsen, ES (reprint author), Natl Zool Pk, Smithsonian Conservat Biol Inst, Ctr Conservat & Evolutionary Genet, POB 37012,MRC5503, Washington, DC 20013 USA. EM ellensarah.martinsen@gmail.com FU National Science Foundation [NSF 0905964]; Morris Animal Foundation FX We thank Nancy Rotzel McInerney for logistical support. The work was funded by Grants from the National Science Foundation to E. S. Martinsen (NSF 0905964), and the Morris Animal Foundation to R. C. Fleischer and E. S. Martinsen. NR 8 TC 1 Z9 1 U1 3 U2 9 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 1877-7252 EI 1877-7260 J9 CONSERV GENET RESOUR JI Conserv. Genet. Resour. PD MAR PY 2015 VL 7 IS 1 BP 15 EP 17 DI 10.1007/s12686-014-0297-2 PG 3 WC Biodiversity Conservation; Genetics & Heredity SC Biodiversity & Conservation; Genetics & Heredity GA CB8UW UT WOS:000349908000005 ER PT J AU Pelayo-Villamil, P Guisande, C Vari, RP Manjarres-Hernandez, A Garcia-Rosello, E Gonzalez-Dacosta, J Heine, J Vilas, LG Patti, B Quinci, EM Jimenez, LF Granado-Lorencio, C Tedesco, PA Lobo, JM AF Pelayo-Villamil, Patricia Guisande, Castor Vari, Richard P. Manjarres-Hernandez, Ana Garcia-Rosello, Emilio Gonzalez-Dacosta, Jacinto Heine, Juergen Gonzalez Vilas, Luis Patti, Bernardo Maria Quinci, Enza Fernanda Jimenez, Luz Granado-Lorencio, Carlos Tedesco, Pablo A. Lobo, Jorge M. TI Global diversity patterns of freshwater fishes - potential victims of their own success SO DIVERSITY AND DISTRIBUTIONS LA English DT Article DE Description curve; freshwater fish species richness; geographical rarity; historical factors; world distribution ID SPECIES RICHNESS; HISTORICAL BIOGEOGRAPHY; CONSERVATION; BIODIVERSITY; CLIMATE; PERFORMANCE; CONGRUENT; ENDEMISM; RANGES; MODELS AB AimTo examine the pattern and cumulative curve of descriptions of freshwater fishes world-wide, the geographical biases in the available information on that fauna, the relationship between species richness and geographical rarity of such fishes, as well as to assess the relative contributions of different environmental factors on these variables. LocationGlobal. MethodsModestR was used to summarize the geographical distribution of freshwater fish species using information available from data-based geographical records. The first-order jackknife richness estimator was used to estimate the completeness of such data in all terrestrial 1-degree cells world-wide. An -shape procedure was used to build range maps capable of providing relatively accurate species richness and geographical rarity values for each grid cell. We also examined the explanatory capacity of a high number of environmental variables using multiple regressions and Support Vector Machine. ResultsCumulative species description curves show that a high number of species of freshwater fishes remain to be discovered. Completeness values indicate that only 199 one-degree grid cells, mainly located in eastern North America and Europe, could be considered as having relatively accurate inventories. Range maps provide species richness values that are positively and significantly related to those resulting from the first-order jackknife richness estimator. The relationship between species richness and geographical rarity is triangular, so that these species-rich cells are those with a higher proportion of distributionally rare species. Species richness is predicted by climatic and/or productivity variables but geographical rarity is not. Main conclusionsIn general, species-rich tropical areas harbour a higher number of narrowly distributed species although comparatively species-poor subtropical cells may also contain narrowly distributed species. Historical factors may help to explain the faunistic composition of these latter areas; a supposition also supported by the low predictive capacity of climatic and productivity variables on geographical rarity values. C1 [Pelayo-Villamil, Patricia; Fernanda Jimenez, Luz] Univ Antioquia, Grp Ictiol, Medellin 1226, Colombia. [Guisande, Castor; Gonzalez Vilas, Luis] Univ Vigo, Fac Ciencias, Vigo 36200, Spain. [Vari, Richard P.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA. [Manjarres-Hernandez, Ana] Univ Nacl Colombia, Inst Amazon Invest IMANI, Leticia 215, Colombia. [Garcia-Rosello, Emilio; Gonzalez-Dacosta, Jacinto; Heine, Juergen] Univ Vigo, Dept Informat, Vigo 36310, Spain. [Patti, Bernardo; Maria Quinci, Enza] CNR, UO Capo Granitola, Ist Ambiente Marino Costiero, I-91021 Campobello Di Mazara, TP, Italy. [Granado-Lorencio, Carlos] Univ Seville, Fac Biol, Dept Biol Vegetal & Ecol, Seville, Spain. [Tedesco, Pablo A.] IRD 207 CNRS 7208 UPMC MNHN, UMR Biol Organismes & Ecosyst Aquat UMR BOREA, Museum Natl Hist Nat, Dept Milieux & Peuplements Aquat, F-75231 Paris, France. [Lobo, Jorge M.] Museo Nacl Ciencias Nat CSIC, Dept Biogeog & Cambio Global, Madrid 28006, Spain. RP Guisande, C (reprint author), Univ Vigo, Fac Ciencias, Vigo 36200, Spain. EM castor@uvigo.es RI Lobo, Jorge/E-2309-2013; Tedesco, Pablo/F-7088-2013 OI Lobo, Jorge/0000-0002-3152-4769; Tedesco, Pablo/0000-0001-5972-5928 FU ENDESA FX We thank ENDESA for technical and financial support, and Juliana Herrera and Almudena Blanco for their great assistance in searching for records of species occurrences. NR 64 TC 6 Z9 7 U1 2 U2 33 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1366-9516 EI 1472-4642 J9 DIVERS DISTRIB JI Divers. Distrib. PD MAR PY 2015 VL 21 IS 3 BP 345 EP 356 DI 10.1111/ddi.12271 PG 12 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA CB9RN UT WOS:000349970100010 ER PT J AU Kaspari, M Clay, NA Lucas, J Yanoviak, SP Kay, A AF Kaspari, Michael Clay, Natalie A. Lucas, Jane Yanoviak, Stephen P. Kay, Adam TI Thermal adaptation generates a diversity of thermal limits in a rainforest ant community SO GLOBAL CHANGE BIOLOGY LA English DT Article DE ants; boundary layer; canopy; community; ectotherms; thermal limits; tropical forest; understory ID BODY-SIZE; TERRESTRIAL ECTOTHERMS; GLOBAL ANALYSIS; CLIMATE-CHANGE; TEMPERATURE; TOLERANCE; LATITUDE; HEAT; PHYSIOLOGY; DROSOPHILA AB The Thermal Adaptation Hypothesis posits that the warmer, aseasonal tropics generates populations with higher and narrower thermal limits. It has largely been tested among populations across latitudes. However, considerable thermal heterogeneity exists within ecosystems: across 31 trees in a Panama rainforest, surfaces exposed to sun were 8 degrees C warmer and varied more in temperature than surfaces in the litter below. Tiny ectotherms are confined to surfaces and are variously submerged in these superheated boundary layer environments. We quantified the surface CTmin and CT(max)s (surface temperatures at which individuals grew torpid and lost motor control, respectively) of 88 ant species from this forest; they ranged in average mass from 0.01 to 57mg. Larger ants had broader thermal tolerances. Then, for 26 of these species we again tested body CT(max)s using a thermal dry bath to eliminate boundary layer effects: body size correlations observed previously disappeared. In both experiments, consistent with Thermal Adaptation, CT(max)s of canopy ants averaged 3.5-5 degrees C higher than populations that nested in the shade of the understory. We impaled thermocouples in taxidermy mounts to further quantify the factors shaping operative temperatures for four ant species representing the top third (1-30mg) of the size distribution. Extrapolations suggest the smallest 2/3rds of species reach thermal equilibrium in <10s. Moreover, the large ants that walk above the convective superheated surface air also showed more net heating by solar radiation, with operative temperatures up to 4 degrees C higher than surrounding air. The thermal environments of this Panama rainforest generate a range of CTmax subsuming 74% of those previously recorded for ant populations worldwide. The Thermal Adaptation Hypothesis can be a powerful tool in predicting diversity of thermal limits within communities. Boundary layer temperatures are likely key to predicting the future of Earth's tiny terrestrial ectotherm populations. C1 [Kaspari, Michael; Clay, Natalie A.] Univ Oklahoma, Dept Biol, Grad Program Ecol & Evolut, Norman, OK 73019 USA. [Clay, Natalie A.] Smithsonian Trop Res Inst, Balboa, Panama. [Lucas, Jane; Kay, Adam] Univ St Thomas, Dept Biol, St Paul, MN 55105 USA. [Yanoviak, Stephen P.] Univ Louisville, Dept Biol, Louisville, KY 40292 USA. RP Kaspari, M (reprint author), Univ Oklahoma, Dept Biol, Grad Program Ecol & Evolut, Norman, OK 73019 USA. EM mkaspari@ou.edu OI Kaspari, Michael/0000-0002-9717-5768 FU NSF [DEB 0842038, EF 1065844] FX Amanda Winters and Dana Frederick provided invaluable help in the field. John Longino, and three anonymous reviewers provided helpful comments on an earlier draft. Funding was provided by grants from the NSF (DEB 0842038) to A.D. Kay and M. Kaspari and (EF 1065844) to M. Kaspari. AntWeb graciously provided ant images in Figure 6. NR 78 TC 25 Z9 25 U1 9 U2 58 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1354-1013 EI 1365-2486 J9 GLOBAL CHANGE BIOL JI Glob. Change Biol. PD MAR PY 2015 VL 21 IS 3 BP 1092 EP 1102 DI 10.1111/gcb.12750 PG 11 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA CB8QS UT WOS:000349896400008 PM 25242246 ER PT J AU Zabin, CJ AF Zabin, Chela J. TI Patterns of adult abundance vary with recruitment of an invasive barnacle species on Oahu, Hawaii SO JOURNAL OF EXPERIMENTAL MARINE BIOLOGY AND ECOLOGY LA English DT Article DE Competition; Pre-settlement factors; Post-settlement factors; Chthamalus proteus; Nesochthamalus intertextus; Amphibalanus reticulatus ID LARVAL HABITAT SELECTION; POSTSETTLEMENT MORTALITY; CHTHAMALID BARNACLES; BALANUS-RETICULATUS; INTERTIDAL BARNACLE; ATLANTIC BARNACLE; KANEOHE BAY; SETTLEMENT; COMPETITION; CIRRIPEDIA AB The ability of non-native species to establish and spread is an interplay between the characteristics of the recipient ecosystem (e.g., biotic resistance) and the characteristics of the invading species (e.g., if it is a habitat generalist, fast-growing, highly fecund). In the Hawaiian Islands, the successful establishment and high impacts of many non-native species have been attributed to a disjunct flora and fauna that results in resources that can be readily exploited. Along these lines, the speed with which the Caribbean-Atlantic barnacle Chthamalus proteus became widespread in Hawaii has been attributed to the availability of settlement space in the intertidal zone. I investigated the relative importance of competition and recruitment in regulating the abundance of C proteus at three sites on the island of Oahu. Recruitment of C. proteus and other barnacle species mirrored adult abundance. Competition with adult barnacles did not appear to be a factor at two sites. At a third site, where recruitment was the highest, competition between C proteus and an early invader, Amphibalanus reticulatus, in the form of space pre-emption was occurring, apparently mediated-at least in part by the preference of A. reticulatus to settle near conspecifics. C proteus and the native barnacle Nesochthamalus intertextus displayed no such settlement preference. Earlier studies linked differences in recruitment rates of barnacles and other invertebrate species on Oahu to differences in circulation patterns that bring offshore waters into shore at some sites and hold near-shore water flowing out of lagoons and harbors close to shore in others. The present study adds to a growing body of work that suggests that while the relative importance of pre-settlement vs. post-settlement factors to invasion success varies with location, knowledge of local oceanographic conditions could help predict the spread of non-native marine species. Published by Elsevier B.V. C1 [Zabin, Chela J.] Univ Hawaii Manoa, Dept Zool & Ecol, Evolut & Conservat Biol Program, Honolulu, HI 96822 USA. RP Zabin, CJ (reprint author), Univ Calif Davis, Smithsonian Environm Res Ctr, 3152 Paradise Dr, Tiburon, CA 94920 USA. FU National Science Foundation [0232016]; Graduate Teaching Fellowship in K-12 Education; Edmondson Research Fund; Ecology, Evolution and Conservation Biology program at the University of Hawaii; National Oceanic and Atmospheric Administration [R/AN-1]; University of Hawaii Sea Grant College Program, SOEST from a NOAA Office of Sea Grant, Department of Commerce [NA86RG0041, UNIHI-SEAGRANT-JC-00-34] FX I thank Andrew Altieri, Blu Forman, Vanessa Fread, Stacy Pang, Alan Parsa, and the members of the Hadfield Laboratory at Kewalo Marine Laboratory for the field assistance and Blu Forman for the assistance with graphics. Advice on experimental design and statistical analyses was provided by Andrew D. Taylor and Andrew L Chang. I also thank Edwin D. Grosholz, Peter T. Raimondi, the members of the Smithsonian Environmental Research Center's laboratory in Tiburon, CA and an anonymous reviewer for the discussions and suggestions that improved this manuscript. This research was supported by a National Science Foundation (0232016) Graduate Teaching Fellowship in K-12 Education, the Edmondson Research Fund, and the Ecology, Evolution and Conservation Biology program at the University of Hawaii (awarded to the author). This study was also funded in part by a grant from the National Oceanic and Atmospheric Administration, Project #R/AN-1, which is sponsored by the University of Hawaii Sea Grant College Program, SOEST, under Institutional Grant No. NA86RG0041 from a NOAA Office of Sea Grant, Department of Commerce to Michael G. Hadfield (UNIHI-SEAGRANT-JC-00-34). The views expressed herein are those of the author and do not necessarily reflect those of NOAA or any of its subagencies. [SS] NR 65 TC 0 Z9 0 U1 2 U2 19 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0022-0981 EI 1879-1697 J9 J EXP MAR BIOL ECOL JI J. Exp. Mar. Biol. Ecol. PD MAR PY 2015 VL 464 BP 44 EP 51 DI 10.1016/j.jembe.2014.12.009 PG 8 WC Ecology; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA CB6IK UT WOS:000349730500006 ER PT J AU Pimiento, C Nifong, JC Hunter, ME Monaco, E Silliman, BR AF Pimiento, Catalina Nifong, James C. Hunter, Margaret E. Monaco, Eric Silliman, Brian R. TI Habitat use patterns of the invasive red lionfish Pterois volitans: a comparison between mangrove and reef systems in San Salvador, Bahamas SO MARINE ECOLOGY-AN EVOLUTIONARY PERSPECTIVE LA English DT Article DE Apex predator; feeding habits; isotopic niche; nursery habitat; predator-prey interactions ID INDO-PACIFIC LIONFISH; STABLE-ISOTOPE RATIOS; CORAL-REEFS; MILES; INVERTEBRATES; COMMUNITIES; RECRUITMENT; ASSUMPTIONS; ESTUARINE; PREDATION AB The Indo-Pacific red lionfish Pterois volitans is widespread both in its native and its non-native habitats. The rapid invasion of this top predator has had a marked negative effect on fish populations in the Western Atlantic and the Caribbean. It is now well documented that lionfish are invading many tropical and sub-tropical habitats. However, there are fewer data available on the change in lionfish abundance over time and the variation of body size and diet across habitats. A recent study in San Salvador, Bahamas, found body size differences between individuals from mangrove and reef systems. That study further suggested that ontogenetic investigation of habitat use patterns could help clarify whether lionfish are using the mangrove areas of San Salvador as nurseries. The aim of the present study is to determine temporal trends in lionfish relative abundance in mangrove and reef systems in San Salvador, and to further assess whether there is evidence suggesting an ontogenetic shift from mangroves to reef areas. Accordingly, we collected lionfish from mangrove and reef habitats and calculated catch per unit effort (a proxy for relative abundance), compared body size distributions across these two systems, and employed a combination of stable isotope, stomach content, and genetic analyses of prey, to evaluate differences in lionfish trophic interactions and habitat use patterns. Our results show that populations may have increased in San Salvador during the last 4 years, and that there is a strong similarity in body size between habitats, stark differences in prey items, and no apparent overlap in the use of habitat and/or food resources. These results suggest that there is not evidence an for ontogenetic shift from mangroves to reefs, and support other studies that propose lionfish are opportunistic forages with little movement across habitats. C1 [Pimiento, Catalina; Nifong, James C.; Monaco, Eric; Silliman, Brian R.] Univ Florida, Dept Biol, Gainesville, FL 32611 USA. [Pimiento, Catalina] Univ Florida, Florida Museum Nat Hist, Gainesville, FL 32611 USA. [Pimiento, Catalina] Smithsonian Trop Res Inst, Balboa, Panama. [Hunter, Margaret E.] US Geol Survey, Southeast Ecol Sci Ctr, Gainesville, FL USA. RP Pimiento, C (reprint author), Univ Florida, Dept Biol, POB 110600, Gainesville, FL 32611 USA. EM pimientoc@ufl.edu RI Nifong, James/D-4137-2015 OI Nifong, James/0000-0003-3607-0441 NR 51 TC 2 Z9 3 U1 10 U2 72 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0173-9565 EI 1439-0485 J9 MAR ECOL-EVOL PERSP JI Mar. Ecol.-Evol. Persp. PD MAR PY 2015 VL 36 IS 1 BP 28 EP 37 DI 10.1111/maec.12114 PG 10 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA CB7CK UT WOS:000349783500003 ER PT J AU Slot, M Kitajima, K AF Slot, Martijn Kitajima, Kaoru TI General patterns of acclimation of leaf respiration to elevated temperatures across biomes and plant types SO OECOLOGIA LA English DT Article DE Climate change; Global patterns; Meta-analysis; Plant ecophysiology; Warming ID PINUS-TAEDA SEEDLINGS; THERMAL-ACCLIMATION; DARK RESPIRATION; GROWTH TEMPERATURE; NIGHTTIME TEMPERATURES; SEASONAL-VARIATION; MOUNTAIN PASSES; TROPICAL FOREST; CO2 EXCHANGE; NEEDLE AGE AB Respiration is instrumental for survival and growth of plants, but increasing costs of maintenance processes with warming have the potential to change the balance between photosynthetic carbon uptake and respiratory carbon release from leaves. Climate warming may cause substantial increases of leaf respiratory carbon fluxes, which would further impact the carbon balance of terrestrial vegetation. However, downregulation of respiratory physiology via thermal acclimation may mitigate this impact. We have conducted a meta-analysis with data collected from 43 independent studies to assess quantitatively the thermal acclimation capacity of leaf dark respiration to warming of terrestrial plant species from across the globe. In total, 282 temperature contrasts were included in the meta-analysis, representing 103 species of forbs, graminoids, shrubs, trees and lianas native to arctic, boreal, temperate and tropical ecosystems. Acclimation to warming was found to decrease respiration at a set temperature in the majority of the observations, regardless of the biome of origin and growth form, but respiration was not completely homeostatic across temperatures in the majority of cases. Leaves that developed at a new temperature had a greater capacity for acclimation than those transferred to a new temperature. We conclude that leaf respiration of most terrestrial plants can acclimate to gradual warming, potentially reducing the magnitude of the positive feedback between climate and the carbon cycle in a warming world. More empirical data are, however, needed to improve our understanding of interspecific variation in thermal acclimation capacity, and to better predict patterns in respiratory carbon fluxes both within and across biomes in the face of ongoing global warming. C1 [Slot, Martijn; Kitajima, Kaoru] Univ Florida, Dept Biol, Gainesville, FL 32611 USA. [Slot, Martijn; Kitajima, Kaoru] Smithsonian Trop Res Inst, Panama City, Panama. [Kitajima, Kaoru] Kyoto Univ, Grad Sch Agr, Kyoto 6068502, Japan. RP Slot, M (reprint author), Univ Florida, Dept Biol, Gainesville, FL 32611 USA. EM martijnslot78@gmail.com FU National Science Foundation-Integrated Organismal Systems Grant [1051789]; Smithsonian Tropical Research Institute FOREST-GEO post-doctoral research fellowship FX We gratefully acknowledge three anonymous reviewers for their comments on an earlier version of this paper. Financial support came from National Science Foundation-Integrated Organismal Systems Grant 1051789 (KK) and a Smithsonian Tropical Research Institute FOREST-GEO post-doctoral research fellowship (MS). NR 74 TC 19 Z9 19 U1 13 U2 92 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0029-8549 EI 1432-1939 J9 OECOLOGIA JI Oecologia PD MAR PY 2015 VL 177 IS 3 BP 885 EP 900 DI 10.1007/s00442-014-3159-4 PG 16 WC Ecology SC Environmental Sciences & Ecology GA CC0NV UT WOS:000350033500023 PM 25481817 ER PT J AU Candek, K Kuntner, M AF Candek, Klemen Kuntner, Matjaz TI DNA barcoding gap: reliable species identification over morphological and geographical scales SO MOLECULAR ECOLOGY RESOURCES LA English DT Article DE barcoding gap; biogeography; CO1; DNA barcodes; morphology; spiders ID IDENTIFYING SPIDERS; EVOLUTIONARY RATES; ANALYSES REVEAL; DELIMITATION; DISTANCE; PHYLOGENIES; ARANEAE; SYSTEM; ERRORS; MISIDENTIFICATION AB The philosophical basis and utility of DNA barcoding have been a subject of numerous debates. While most literature embraces it, some studies continue to question its use in dipterans, butterflies and marine gastropods. Here, we explore the utility of DNA barcoding in identifying spider species that vary in taxonomic affiliation, morphological diagnosibility and geographic distribution. Our first test searched for a barcoding gap' by comparing intra- and interspecific means, medians and overlap in more than 75000 computed Kimura 2-parameter (K2P) genetic distances in three families. Our second test compared K2P distances of congeneric species with high vs. low morphological distinctness in 20 genera of 11 families. Our third test explored the effect of enlarging geographical sampling area at a continental scale on genetic variability in DNA barcodes within 20 species of nine families. Our results generally point towards a high utility of DNA barcodes in identifying spider species. However, the size of the barcoding gap strongly depends on taxonomic groups and practices. It is becoming critical to define the barcoding gap statistically more consistently and to document its variation over taxonomic scales. Our results support models of independent patterns of morphological and molecular evolution by showing that DNA barcodes are effective in species identification regardless of their morphological diagnosibility. We also show that DNA barcodes represent an effective tool for identifying spider species over geographic scales, yet their variation contains useful biogeographic information. C1 [Candek, Klemen; Kuntner, Matjaz] Slovenian Acad Sci & Arts, Ctr Sci Res, Inst Biol, Ljubljana 1000, Slovenia. [Kuntner, Matjaz] Hubei Univ, Coll Life Sci, Ctr Behav Ecol & Evolut, Wuhan 430062, Peoples R China. [Kuntner, Matjaz] Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Candek, K (reprint author), Slovenian Acad Sci & Arts, Ctr Sci Res, Inst Biol, Novi Trg 2, Ljubljana 1000, Slovenia. EM klemen.candek@gmail.com FU Slovenian Research Agency [P1-0236, MR-2013]; Swiss Contribution [C1536-1 1T440013] FX This research was supported by the Slovenian Research Agency (Grants P1-0236 and MR-2013) and a Swiss Contribution to the enlarged EU grant (C1536-1 1T440013). For help or discussions, we thank Ingi Agnarsson, Andrej Blejec, Cene Fiser, Rok Kostanjsek, Tjasa Lokovsek, Ren-Chung Cheng, Matjaz Gregoric and Simona Kralj-Fiser. We also thank Vincent Nijman and two anonymous reviewers for helpful suggestions. NR 77 TC 14 Z9 14 U1 6 U2 84 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1755-098X EI 1755-0998 J9 MOL ECOL RESOUR JI Mol. Ecol. Resour. PD MAR PY 2015 VL 15 IS 2 BP 268 EP 277 DI 10.1111/1755-0998.12304 PG 10 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA CB7PE UT WOS:000349819000005 PM 25042335 ER PT J AU Chen, J Zhao, JT Erickson, DL Xia, NH Kress, WJ AF Chen, Juan Zhao, Jietang Erickson, David L. Xia, Nianhe Kress, W. John TI Testing DNA barcodes in closely related species of Curcuma (Zingiberaceae) from Myanmar and China SO MOLECULAR ECOLOGY RESOURCES LA English DT Article DE chloroplast region; DNA barcoding; ITS2; species identification ID LAND PLANTS; CHROMOSOME-NUMBERS; IDENTIFICATION; L.; PHYLOGENY; DIVERGENCE; MORPHOLOGY; FABACEAE; SUCCESS; MARKERS AB The genus Curcuma L. is commonly used as spices, medicines, dyes and ornamentals. Owing to its economic significance and lack of clear-cut morphological differences between species, this genus is an ideal case for developing DNA barcodes. In this study, four chloroplast DNA regions (matK, rbcL, trnH-psbA and trnL-F) and one nuclear region (ITS2) were generated for 44 Curcuma species and five species from closely related genera, represented by 96 samples. PCR amplification success rate, intra- and inter-specific genetic distance variation and the correct identification percentage were taken into account to assess candidate barcode regions. PCR and sequence success rate were high in matK (89.7%), rbcL (100%), trnH-psbA (100%), trnL-F (95.7%) and ITS2 (82.6%) regions. The results further showed that four candidate chloroplast barcoding regions (matK, rbcL, trnH-psbA and trnL-F) yield no barcode gaps, indicating that the genus Curcuma represents a challenging group for DNA barcoding. The ITS2 region presented large interspecific variation and provided the highest correct identification rates (46.7%) based on BLASTClust method among the five regions. However, the ITS2 only provided 7.9% based on NJ tree method. An increase in discriminatory power needs the development of more variable markers. C1 [Chen, Juan; Xia, Nianhe] Chinese Acad Sci, Key Lab Plant Resources Conservat & Sustainable U, South China Bot Garden, Guangzhou 510650, Guangdong, Peoples R China. [Zhao, Jietang] South China Agr Univ, Coll Hort, Guangzhou 510642, Guangdong, Peoples R China. [Erickson, David L.; Kress, W. John] Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, MRC 166, Washington, DC 20013 USA. RP Kress, WJ (reprint author), Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, MRC 166, POB 37012, Washington, DC 20013 USA. EM kressj@si.edu FU Chinese Scholarship Council; Smithsonian's National Museum of Natural History; Chinese Scholarship Council [2010491001]; National Natural Science Foundation of China [31170185, 31200161] FX The authors thank the Chinese Scholarship Council and Smithsonian's National Museum of Natural History for their support. We thank Prof. De-Lin Wu, South China Botanical Garden, the Chinese Academy of Sciences, for help with species identifications. We also thank the Smithsonian's Laboratories of Analytical Biology for their help with laboratory work. This research work was supported by the Research Fund from the Chinese Scholarship Council (File no. 2010491001). It was also supported by National Natural Science Foundation of China (Grant no. 31170185 and no. 31200161). We also thank the reviewers who commented on the draft. NR 61 TC 8 Z9 9 U1 4 U2 41 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1755-098X EI 1755-0998 J9 MOL ECOL RESOUR JI Mol. Ecol. Resour. PD MAR PY 2015 VL 15 IS 2 BP 337 EP 348 DI 10.1111/1755-0998.12319 PG 12 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA CB7PE UT WOS:000349819000012 PM 25158042 ER PT J AU Grigson, PS Colechio, EM Power, ML Schulkin, J Norgren, R AF Grigson, P. S. Colechio, E. M. Power, M. L. Schulkin, J. Norgren, R. TI Parabrachial lesions in rats disrupt sodium appetite induced by furosemide but not by calcium deprivation SO PHYSIOLOGY & BEHAVIOR LA English DT Article DE Mineral appetite; Parabrachial; Calcium depletion; Sodium depletion ID TYMPANI NERVE RESPONSES; TASTE-AVERSION; PARATHYROIDECTOMIZED RATS; GUSTATORY LESIONS; NUCLEUS LESIONS; SALT APPETITE; DEFICIENCY; PREFERENCE; INCREASES; INGESTION AB An appetite for CaCl2 and NaCl occurs in young rats after they are fed a diet lacking Ca or Na, respectively. Bilateral lesions of the parabrachial nuclei (PBN) disrupt normal taste aversion learning and essentially eliminate the expression of sodium appetite. Here we tested whether similar lesions of the PBN would disrupt the calcium-deprivation-induced appetite for CaCl2 or NaCl. Controls and rats with PBN lesions failed to exhibit a calcium-deprivation-induced appetite for CaCl2. Nevertheless, both groups did exhibit a significant calcium-deprivation-induced appetite for 0.5 M NaCl. Thus, while damage to the second central gustatory relay in the PBN disrupts the appetite for 0.5 M NaCl induced by furosemide, deoxycorticosterone acetate, and polyethylene glycol, the sodium appetite induced by dietary CaCl2 depletion remains intact. (C) 2015 Elsevier Inc. All rights reserved. C1 [Grigson, P. S.; Colechio, E. M.; Norgren, R.] Penn State Univ, Coll Med, Dept Neural & Behav Sci, Hershey, PA 17033 USA. [Power, M. L.] Natl Zool Pk, Nutr Lab, Washington, DC 20013 USA. [Power, M. L.] Natl Zool Pk, Conservat Ecol Ctr, Smithsonian Conservat Biol Inst, Washington, DC 20013 USA. [Schulkin, J.] Georgetown Univ, Dept Neurosci, Washington, DC 20057 USA. RP Grigson, PS (reprint author), Penn State Univ, Coll Med, Dept Neural & Behav Sci, 500 Univ Dr, Hershey, PA 17033 USA. EM psg6@psu.edu; emc231@psu.edu; mpower@acog.org; Jschulkin@acog.org; rxn5@psu.edu OI Power, Michael/0000-0002-6120-3528; Grigson, Patricia/0000-0002-4252-7332 FU NIH [DC05435, DC00240, DA012473, DA009815] FX Han Li performed the surgery, Nelli Horvath collected the data, Kathy Matyas and Nelli Horvath did the histology, and Erin Handly assisted with Fig. 1. They each have our thanks. We also thank Sarah Ballard for her careful editorial assistance. This work was supported by the NIH (DC05435, DC00240, DA012473 and DA009815). NR 42 TC 0 Z9 0 U1 0 U2 1 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0031-9384 J9 PHYSIOL BEHAV JI Physiol. Behav. PD MAR 1 PY 2015 VL 140 BP 172 EP 179 DI 10.1016/j.physbeh.2014.11.070 PG 8 WC Psychology, Biological; Behavioral Sciences SC Psychology; Behavioral Sciences GA CB4HI UT WOS:000349588400023 PM 25540931 ER PT J AU Le Chat, G Issautier, K Zaslavsky, A Pantellini, F Meyer-Vernet, N Belheouane, S Maksimovic, M AF Le Chat, G. Issautier, K. Zaslavsky, A. Pantellini, F. Meyer-Vernet, N. Belheouane, S. Maksimovic, M. TI Effect of the Interplanetary Medium on Nanodust Observations by the Solar Terrestrial Relations Observatory SO SOLAR PHYSICS LA English DT Article DE Interplanetary dust; Nanodust; In situ dust detection; Radio antennas; STEREO/WAVES; Solar wind; Coronal mass ejections ID SPACED DATA; DUST; SPACECRAFT; ANTENNAS AB Dust particles provide an important part of the matter composing the interplanetary medium; their mass flux at 1 AU is similar to that of the solar wind. Dust grains of nanometer size-scale can be detected using radio and plasma wave instruments because they move at roughly the solar wind speed. The high-velocity impact of a dust particle generates a small crater on the spacecraft: the dust particle and the crater material are vaporized. This produces a plasma cloud whose associated electrical charge induces an electric pulse measured with radio and plasma instruments. Since their first detection in the interplanetary medium, nanodust particles have been routinely measured using the Solar Terrestrial Relations Observatory/WAVES experiment [S/WAVES]. We present the nanodust properties measured using S/WAVES/Low Frequency Receiver [LFR] observations between 2007 and 2013, and for the first time present evidence of coronal mass ejection interaction with the nanodust, leading to a higher nanodust flux measured at 1 AU. Finally, possible influences of the inner planets on the nanodust flux are presented and discussed. C1 [Le Chat, G.; Issautier, K.; Zaslavsky, A.; Pantellini, F.; Meyer-Vernet, N.; Belheouane, S.; Maksimovic, M.] Univ Paris Diderot, Univ Paris 06, CNRS, LESIA Observ Paris, F-92195 Meudon, France. [Le Chat, G.] NASA, Lunar Sci Inst, Moffett Field, CA USA. [Le Chat, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MD USA. RP Le Chat, G (reprint author), Univ Paris Diderot, Univ Paris 06, CNRS, LESIA Observ Paris, 5 Pl Jules Janssen, F-92195 Meudon, France. EM gaetan.lechat@obspm.fr FU CNES; CNRS; NASA [NAS5-00132] FX We thank the team who designed and built the S/WAVES instrument. The S/WAVES data used here are produced by an international consortium of the Observatoire de Paris (France), the University of Minnesota (USA), the University of California Berkeley (USA), and NASA Goddard Space Flight Center (USA). The French contribution is funded by CNES and CNRS, and the USA institutions are funded by NASA. We thank the STEREO PLASTIC Investigation (A.B. Galvin, PI) and NASA Contract NAS5-00132 for providing the proton data, and the STEREO IMPACT (J. Luhman, PI) for providing the magnetic field data. NR 23 TC 2 Z9 2 U1 3 U2 7 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 EI 1573-093X J9 SOL PHYS JI Sol. Phys. PD MAR PY 2015 VL 290 IS 3 BP 933 EP 942 DI 10.1007/s11207-015-0651-x PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CB8TF UT WOS:000349903300017 ER PT J AU Garcia-Rosello, E Guisande, C Manjarres-Hernandez, A Gonzalez-Dacosta, J Heine, J Pelayo-Villamil, P Gonzalez-Vilas, L Vari, RP Vaamonde, A Granado-Lorencio, C Lobo, JM AF Garcia-Rosello, Emilio Guisande, Castor Manjarres-Hernandez, Ana Gonzalez-Dacosta, Jacinto Heine, Juergen Pelayo-Villamil, Patricia Gonzalez-Vilas, Luis Vari, Richard P. Vaamonde, Antonio Granado-Lorencio, Carlos Lobo, Jorge M. TI Can we derive macroecological patterns from primary Global Biodiversity Information Facility data? SO GLOBAL ECOLOGY AND BIOGEOGRAPHY LA English DT Article DE Distribution models; GBIF; macroecological patterns; marine fishes; point-to-grid; range maps; Rapoport' rule ID SPECIES DISTRIBUTION MODELS; RANGE MAPS; GEOGRAPHICAL-DISTRIBUTION; LATITUDINAL GRADIENTS; SOFTWARE TOOL; RICHNESS; DIVERSITY; DISTRIBUTIONS; CONSERVATION; MODESTR AB AimTo determine whether the method used to build distributional maps from raw data influences the representation of two principal macroecological patterns: the latitudinal gradient in species richness and the latitudinal variation in range sizes (Rapoport's rule). LocationWorld-wide. MethodsAll available distribution data from the Global Biodiversity Information Facility (GBIF) for those fish species that are members of orders of fishes with only marine representatives in each order were extracted and cleaned so as to compare four different procedures: point-to-grid (GBIF maps), range maps applying an -shape [GBIF-extent of occurrence (EOO) maps], the MaxEnt method of species distribution modelling (GBIF-MaxEnt maps) and the MaxEnt method but restricted to the area delimited by the -shape (GBIF-MaxEnt-restricted maps). ResultsThe location of hotspots and the latitudinal gradient in species richness or range sizes are relatively similar in the four procedures. GBIF-EOO maps and most GBIF-MaxEnt-maps provide overestimations of species richness when compared with those present in a priori well-surveyed cells. GBIF-EOO maps seem to provide more reasonable world macroecological patterns. MaxEnt can erroneously predict the presence of species in environmentally similar cells of another hemisphere or in other regions that lie outside the range of the species. Limiting this overpredictive capacity, as in the case of GBIF-MaxEnt-restricted maps, seems to mimic the frequency of observations derived from a simple point-to-grid procedure, with the utility of this procedure consequently being limited. Main conclusionsIn studies of macroecological patterns at a global scale, the simple -shape method seems to be a more parsimonious option for extrapolating species distributions from primary data than are distribution models performed indiscriminately and automatically with MaxEnt. GBIF data may be used in macroecological patterns if original data are cleaned, autocorrelation is corrected and species richness figures do not constitute obvious underestimations. Efforts therefore should focus on improving the number and quality of records that can serve as the source of primary data in macroecological studies. C1 [Garcia-Rosello, Emilio; Gonzalez-Dacosta, Jacinto; Heine, Juergen] Univ Vigo, Dept Informat, Vigo 36310, Spain. [Guisande, Castor; Gonzalez-Vilas, Luis] Univ Vigo, Fac Ciencias Mar, Vigo 36310, Spain. [Manjarres-Hernandez, Ana] Univ Nacl Colombia, Inst Amazon Invest IMANI, Leticia, Colombia. [Pelayo-Villamil, Patricia] Univ Antioquia, Grp Ictiol, Medellin 1226, Colombia. [Vari, Richard P.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA. [Vaamonde, Antonio] Univ Vigo, Fac CCEE & Empresariales, Dept Estadist & Invest Operat, Vigo 36208, Spain. [Granado-Lorencio, Carlos] Univ Seville, Fac Biol, Dept Biol Vegetal & Ecol, E-41012 Seville, Spain. [Lobo, Jorge M.] Museo Nacl Ciencias Nat CSIC, Dept Biogeog & Cambio Global, Madrid 28006, Spain. RP Guisande, C (reprint author), Univ Vigo, Fac Ciencias Mar, Campus Lagoas Marcosende S-N, Vigo 36310, Spain. EM castor@uvigo.es RI Lobo, Jorge/E-2309-2013 OI Lobo, Jorge/0000-0002-3152-4769 FU ENDESA FX We thank ENDESA for technical and financial support. NR 50 TC 6 Z9 7 U1 2 U2 41 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 2015 VL 24 IS 3 BP 335 EP 347 DI 10.1111/geb.12260 PG 13 WC Ecology; Geography, Physical SC Environmental Sciences & Ecology; Physical Geography GA CB1MK UT WOS:000349391600007 ER PT J AU Carry, B Matter, A Scheirich, P Pravec, P Molnar, L Mottola, S Carbognani, A Jehin, E Marciniak, A Binzel, RP Demeo, FE Birlan, M Delbo, M Barbotin, E Behrend, R Bonnardeau, M Colas, F Farissier, P Fauvaud, M Fauvaud, S Gillier, C Gillon, M Hellmich, S Hirsch, R Leroy, A Manfroid, J Montier, J Morelle, E Richard, F Sobkowiak, K Strajnic, J Vachier, F AF Carry, B. Matter, A. Scheirich, P. Pravec, P. Molnar, L. Mottola, S. Carbognani, A. Jehin, E. Marciniak, A. Binzel, R. P. DeMeo, F. E. Birlan, M. Delbo, M. Barbotin, E. Behrend, R. Bonnardeau, M. Colas, F. Farissier, P. Fauvaud, M. Fauvaud, S. Gillier, C. Gillon, M. Hellmich, S. Hirsch, R. Leroy, A. Manfroid, J. Montier, J. Morelle, E. Richard, F. Sobkowiak, K. Strajnic, J. Vachier, F. TI The small binary asteroid (939) Isberga SO ICARUS LA English DT Article DE Asteroids, dynamics; Satellites of asteroids; Orbit determination ID NEAR-EARTH ASTEROIDS; MAIN-BELT ASTEROIDS; INTERFEROMETRIC OBSERVATIONS; IRRADIATION EXPERIMENTS; DENSITY; MIDI; SURFACES; POPULATION; SIMULATION; METEORITES AB In understanding the composition and internal structure of asteroids, their density is perhaps the most diagnostic quantity. We aim here at characterizing the surface composition, mutual orbit, size, mass, and density of the small main-belt binary asteroid (939) Isberga. For that, we conduct a suite of multi-technique observations, including optical lightcurves over many epochs, near-infrared spectroscopy, and interferometry in the thermal infrared. We develop a simple geometric model of binary systems to analyze the interferometric data in combination with the results of the lightcurve modeling. From spectroscopy, we classify lbserga as a Sq-type asteroid, consistent with the albedo of 0.14(-006)(+009), (all uncertainties are reported as 3-sigma-range) we determine (average albedo of S-types is 0.197 +/- 0.153, see Pravec et al. (Pravec et al. [2012]. Icarus 221, 365-387). Lightcurve analysis reveals that the mutual orbit has a period of 26.6304 +/- 0.0001 h, is close to circular (eccentricity lower than 0.1), and has pole coordinates within 7 degrees of (225 degrees, +86 degrees) in Ecliptic J2000, implying a low obliquity of 1.5(-1.5)(+6.0) deg. The combined analysis of lightcurves and interferometric data allows us to determine the dimension of the system and we find volume-equivalent diameters of 12.4(-1.2)(+2.5) km and 3.6(-0.3)(+0.7) km for Isberga and its satellite, circling each other on a 33 km wide orbit. Their density is assumed equal and found to be 2.91(-2.01)(+1.72) g cm(-3), lower than that of the associated ordinary chondrite meteorites, suggesting the presence of some macroporosity, but typical of S-types of the same size range (Carry [2012]. Planet. Space Sci. 73, 98-118). The present study is the first direct measurement of the size of a small main-belt binary. Although the interferometric observations of Isberga are at the edge of MIDI capabilities, the method described here is applicable to others suites of instruments (e.g., LBT, ALMA). (C) 2014 Elsevier Inc. All rights reserved. C1 [Carry, B.; Birlan, M.; Colas, F.; Vachier, F.] Univ Lille 1, IMCCE, Observ Paris, Univ Paris 06,CNRS,UMR8028, F-75014 Paris, France. [Carry, B.] ESA, European Space Astron Ctr, Madrid 28691, Spain. [Matter, A.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Matter, A.] Univ Grenoble 1, CNRS, INSU, IPAG,UMR 5274, F-38041 Grenoble, France. [Scheirich, P.; Pravec, P.] Acad Sci Czech Republic, Astron Inst, CZ-25165 Ondrejov, Czech Republic. [Molnar, L.] Calvin Coll, Dept Phys & Astron, Grand Rapids, MI 49546 USA. [Mottola, S.; Hellmich, S.] Deutsch Zentrum Luft & Raumfahrt DLR, D-12489 Berlin, Germany. [Delbo, M.] Observ Cote Azur, CNRS, UNS, Lab Lagrange, F-06304 Nice 04, France. [Binzel, R. P.; DeMeo, F. E.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. [DeMeo, F. E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Jehin, E.; Gillon, M.; Manfroid, J.] Univ Liege, Inst Astrophys & Geophys, B-4000 Liege, Belgium. [Marciniak, A.; Hirsch, R.; Sobkowiak, K.] Adam Mickiewicz Univ, Astron Observ Inst, Fac Phys, PL-60286 Poznan, Poland. [Carbognani, A.] Astron Observ Autonomous Reg Aosta Valley, I-11020 Nus, Aosta, Italy. [Behrend, R.] Observ Geneva, CH-1290 Sauverny, Switzerland. [Farissier, P.; Gillier, C.] CALA, F-69120 Vaulx En Velin, France. [Fauvaud, M.; Fauvaud, S.] Observ Bois Bardon, F-16110 Taponnat, France. [Fauvaud, M.; Fauvaud, S.; Richard, F.] Assoc T60, F-31400 Toulouse, France. RP Carry, B (reprint author), Univ Lille 1, IMCCE, Observ Paris, Univ Paris 06,CNRS,UMR8028, 77 Av Denfert Rochereau, F-75014 Paris, France. EM bcarry@imcce.fr RI Pravec, Petr/G-9037-2014; Scheirich, Peter/H-4331-2014; BIRLAN, Mirel/B-5283-2011 OI Scheirich, Peter/0000-0001-8518-9532; FU Grant Agency of the Czech Republic [P209/12/0229]; Centre National d'Etudes Spatiales (CNES); Belgian Fund for Scientific Research (Fonds National de la Recherche Scientifique, F.R.S.-FNRS); National Aeronautics and Space Administration, Office of Space Science, Planetary Astronomy Program [NCC 5-538]; NASA [09-NEOO009-0001, NNX12AL26G]; National Science Foundation [0506716, 0907766]; Hubble Fellowship [HST-HF-51319.01-A]; [RVO 67985815] FX We acknowledge support from the Faculty of the European Space Astronomy Centre (ESAC) for the visits of M. Delbo and A. "Momo" Matter. The work by P.S. and P.P. was supported by the Grant Agency of the Czech Republic, Grant P209/12/0229, and by Program RVO 67985815. A. Matter acknowledges financial support from the Centre National d'Etudes Spatiales (CNES). TRAPPIST is a project funded by the Belgian Fund for Scientific Research (Fonds National de la Recherche Scientifique, F.R.S.-FNRS) E. Jehin and M. Gillon are FNRS Research Associates, and Jean Manfroid is Research Director of the FNRS. Part of the data utilized in this publication were obtained and made available by the MIT-UH-IRTF Joint Campaign for NEO Reconnaissance. The IRTF is operated by the University of Hawaii under Cooperative Agreement No. NCC 5-538 with the National Aeronautics and Space Administration, Office of Space Science, Planetary Astronomy Program. The MIT component of this work is supported by NASA Grant 09-NEOO009-0001, and by the National Science Foundation under Grant Nos. 0506716 and 0907766. F.E.D. acknowledges funding from NASA under Grant No. NNX12AL26G and Hubble Fellowship Grant HST-HF-51319.01-A. Any opinions, findings, and conclusions or recommendations expressed in this material are those of the authors and do not necessarily reflect the views of NASA or the National Science Foundation. This research utilizes spectra acquired by Jeffery F. Bell with the NASA RELAB facility at Brown University. NR 56 TC 2 Z9 2 U1 1 U2 5 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD MAR 1 PY 2015 VL 248 BP 516 EP 525 DI 10.1016/j.icarus.2014.11.002 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AZ7PR UT WOS:000348411000035 ER PT J AU Schaepman, ME Jehle, M Hueni, A D'Odorico, P Damm, A Weyerrnann, J Schneider, FD Laurent, V Popp, C Seidel, FC Lenhard, K Gege, P Kuchler, C Brazile, J Kohler, P De Vos, L Meuleman, K Meynart, R Schlapfer, D Kneubuhler, M Itten, KI AF Schaepman, Michael E. Jehle, Michael Hueni, Andreas D'Odorico, Petra Damm, Alexander Weyerrnann, Jurg Schneider, Fabian D. Laurent, Valerie Popp, Christoph Seidel, Felix C. Lenhard, Karim Gege, Peter Kuechler, Christoph Brazile, Jason Kohler, Peter De Vos, Lieve Meuleman, Koen Meynart, Roland Schlaepfer, Daniel Kneubuhler, Mathias Itten, Klaus I. TI Advanced radiometry measurements and Earth science applications with the Airborne Prism Experiment (APEX) SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Imaging spectroscopy; Earth observation; APEX; Calibration; Processing; Validation; Earth science applications ID PUSHBROOM IMAGING SPECTROMETER; INDUCED CHLOROPHYLL FLUORESCENCE; REMOTELY-SENSED DATA; RADIANCE DATA; VEGETATION INDEXES; SPECTROSCOPY DATA; SURFACE ALBEDO; LAND-COVER; PERFORMANCE; RETRIEVAL AB We present the Airborne Prism Experiment (APEX), its calibration and subsequent radiometric measurements as well as Earth science applications derived from this data. APEX is a dispersive pushbroom imaging spectrometer covering the solar reflected wavelength range between 372 and 2540 nm with nominal 312 (max. 532) spectral bands. APEX is calibrated using a combination of laboratory, in-flight and vicarious calibration approaches. These are complemented by using a forward and inverse radiative transfer modeling approach, suitable to further validate APEX data. We establish traceability of APEX radiances to a primary calibration standard, including uncertainty analysis. We also discuss the instrument simulation process ranging from initial specifications to performance validation. In a second part, we present Earth science applications using APEX. They include geometric and atmospheric compensated as well as reflectance anisotropy minimized Level 2 data. Further, we discuss retrieval of aerosol optical depth as well as vertical column density of NOx, a radiance data-based coupled canopy atmosphere model, and finally measuring sun-induced chlorophyll fluorescence (Fs) and infer plant pigment content. The results report on all APEX specifications including validation. APEX radiances are traceable to a primary standard with <4% uncertainty and with an average SNR of >625 for all spectral bands. Radiance based vicarious calibration is traceable to a secondary standard with <= 65% uncertainty. Except for inferring plant pigment content, all applications are validated using in-situ measurement approaches and modeling. Even relatively broad APEX bands (FWHM of 6 nm at 760 nm) can assess Fs with modeling agreements as high as R-2 = 0.87 (relative RMSE = 27.76%). We conclude on the use of high resolution imaging spectrometers and suggest further development of imaging spectrometers supporting science grade spectroscopy measurements. (C) 2014 The Authors. Published by Elsevier Inc. C1 [Schaepman, Michael E.] Univ Zurich, Remote Sensing Labs, CH-8057 Zurich, Switzerland. [Schaepman, Michael E.; Jehle, Michael; Hueni, Andreas; D'Odorico, Petra; Damm, Alexander; Weyerrnann, Jurg; Schneider, Fabian D.; Laurent, Valerie; Kneubuhler, Mathias; Itten, Klaus I.] Univ Zurich, Remote Sensing Labs, CH-8057 Zurich, Switzerland. [Popp, Christoph] Smithsonian Inst, NMNH, Washington, DC 20013 USA. [Seidel, Felix C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Lenhard, Karim; Gege, Peter] Earth Observat Ctr, German Aerosp Ctr, D-82234 Oberpfaffenhofen, Wessling, Germany. [Kuechler, Christoph] RUAG Schweiz AG, RUAG Aviat, CH-6032 Emmenbrucke, Switzerland. [Brazile, Jason; Kohler, Peter] Netcetera AG, CH-8004 Zurich, Switzerland. [De Vos, Lieve] OIP Sensor Syst, B-9700 Oudenaarde, Belgium. [Meuleman, Koen] VITO, B-2400 Mol, Belgium. [Meynart, Roland] ESA ESTEC, NL-2201 AZ Noordwijk, Netherlands. [Schlaepfer, Daniel] ReSe Applicat Schlapfer, CH-9500 Wil, Switzerland. RP Schaepman, ME (reprint author), Univ Zurich, Remote Sensing Labs, Winterthurerstr 190, CH-8057 Zurich, Switzerland. EM michael.schaepman@geo.uzh.ch RI Kneubuehler, Mathias/D-1153-2010; Damm, Alexander/D-1160-2010; Schaepman, Michael/B-9213-2009; OI Kneubuehler, Mathias/0000-0002-6716-585X; Schaepman, Michael/0000-0002-9627-9565; Seidel, Felix/0000-0002-4282-2198; Hueni, Andreas/0000-0002-4283-2484 FU University of Zurich; ESA PRODEX [16298/02/NL/US, 15449/01/NL/Sfe]; Swiss National Science Foundation (SNSF); Belgian Science Policy Office (BELSPO); Swiss University Conference (SUK, KIP-SEON); University of Zurich Research Priority Program on 'Global Change and Biodiversity' (URPP GCB); Swiss Space Office (SSO); European Metrology Research Programme (EMRP) - EMRP within EURAMET; European Metrology Research Programme (EMRP) - European Union; ESA; German Aerospace Center (DLR) FX We thank the University of Zurich for continued funding and support to APEX. APEX is further supported through ESA, ESA PRODEX (16298/02/NL/US and 15449/01/NL/Sfe), the Swiss National Science Foundation (SNSF), the Belgian Science Policy Office (BELSPO), the Swiss University Conference (SUK, KIP-SEON), the University of Zurich Research Priority Program on 'Global Change and Biodiversity' (URPP GCB), the Swiss Space Office (SSO), the European Metrology Research Programme (EMRP, which is jointly funded by the EMRP participating countries within EURAMET and the European Union), and the German Aerospace Center (DLR). We thank former UZH APEX project managers Jens Nieke and Edoardo Alberti and former ESA APEX project managers Gerd Ulbrich, Jose Gaviras, and Hilde Schroeven-Deceuninck for their support. We thank the reviewers for helpful comments, allowing us to improve the manuscript NR 108 TC 27 Z9 27 U1 4 U2 31 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 1 PY 2015 VL 158 BP 207 EP 219 DI 10.1016/j.rse.2014.11.014 PG 13 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA CA4MR UT WOS:000348879100016 ER PT J AU Keuskamp, JA Hefting, MM Dingemans, BJJ Verhoeven, JTA Feller, IC AF Keuskamp, Joost A. Hefting, Mariet M. Dingemans, Bas J. J. Verhoeven, Jos T. A. Feller, Ilka C. TI Effects of nutrient enrichment on mangrove leaf litter decomposition SO SCIENCE OF THE TOTAL ENVIRONMENT LA English DT Article ID RHIZOPHORA-MANGLE; NITROGEN; ECOSYSTEMS; CARBON; PHOSPHORUS; FOREST; DYNAMICS; QUALITY; HERBIVORY; LIGNIN AB Nutrient enrichment of mangroves, a common phenomenon along densely populated coastlines, may negatively affect mangrove ecosystems by modifying internal carbon and nutrient cycling. The decomposition of litter exerts a strong influence on these processes and is potentially modified by eutrophication. This-study describes effects of N and P enrichment on litter decomposition rate and mineralisation/immobilisation patterns. By making use of reciprocal litter transplantation experiments among fertiliser treatments, it was tested if nutrient addition primarily acts on the primary producers (i.e. changes in litter quantity and quality) or on the microbial decomposers (i.e. changes in nutrient limitation for decomposition). Measurements were done in two mangrove forests where primary production was either limited by N or by P, which had been subject to at least 5 years of experimental N and P fertilisation. Results of this study indicated that decomposers were always N-limited regardless of the limitation of the primary producers. This leads to a differential nutrient limitation between decomposers and primary producers in sites where mangrove production was P-limited. In these sites, fertilisation with P caused litter quality to change, resulting in a higher decomposition rate. This study shows that direct effects of fertilisation on decomposition through an effect on decomposer nutrient availability might be non-significant, while the indirect effects through modifying litter quality might be quite substantial in mangroves. Our results show no indication that eutrophication increases decomposition without stimulating primary production. Therefore we do not expect a decline in carbon sequestration as a result of eutrophication of mangrove ecosystems. (C) 2014 Elsevier B.V. All rights reserved. C1 [Keuskamp, Joost A.; Hefting, Mariet M.; Dingemans, Bas J. J.; Verhoeven, Jos T. A.] Univ Utrecht, Dept Biol, NL-3584 CH Utrecht, Netherlands. [Feller, Ilka C.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Keuskamp, JA (reprint author), Univ Utrecht, Dept Biol, Padualaan 8, NL-3584 CH Utrecht, Netherlands. EM j.a.keuskamp@uu.nl; m.m.hefting@uu.nl; b.j.j.dingemans@uu.nl; j.t.a.verhoeven@uu.nl; feller@serc.si.edu RI Hefting, Mariet /L-9682-2016; OI Hefting, Mariet /0000-0002-3852-7532; Feller, Ilka/0000-0002-6391-1608 NR 46 TC 4 Z9 6 U1 16 U2 111 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0048-9697 EI 1879-1026 J9 SCI TOTAL ENVIRON JI Sci. Total Environ. PD MAR 1 PY 2015 VL 508 BP 402 EP 410 DI 10.1016/j.scitotenv.2014.11.092 PG 9 WC Environmental Sciences SC Environmental Sciences & Ecology GA CA8TZ UT WOS:000349195100044 PM 25497680 ER PT J AU Holzwarth, F Ruger, N Wirth, C AF Holzwarth, Frederic Rueger, Nadja Wirth, Christian TI Taking a closer look: disentangling effects of functional diversity on ecosystem functions with a trait-based model across hierarchy and time SO ROYAL SOCIETY OPEN SCIENCE LA English DT Article DE biodiversity and ecosystem functioning; functional composition; hierarchical trait influence; forest succession; trait-based modelling; LPJ-GUESS ID DYNAMIC VEGETATION MODEL; SPECIES RICHNESS; FOREST DIVERSITY; BIODIVERSITY EXPERIMENTS; PRIMARY PRODUCTIVITY; COMMUNITY ECOLOGY; TREE PRODUCTIVITY; CURRENT KNOWLEDGE; WATER-BALANCE; PLANT TRAITS AB Biodiversity and ecosystem functioning (BEF) research has progressed from the detection of relationships to elucidating their drivers and underlying mechanisms. In this context, replacing taxonomic predictors by trait-based measures of functional composition (FC)-bridging functions of species and of ecosystems-is a widely used approach. The inherent challenge of trait-based approaches is the multi-faceted, dynamic and hierarchical nature of trait influence: (i) traits may act via different facets of their distribution in a community, (ii) their influence may change over time and (iii) traits may influence processes at different levels of the natural hierarchy of organization. Here, we made use of the forest ecosystem model 'LPJ-GUESS' parametrized with empirical trait data, which creates output of individual performance, community assembly, stand-level states and processes. To address the three challenges, we resolved the dynamics of the top-level ecosystem function 'annual biomass change' hierarchically into its various component processes (growth, leaf and root turnover, recruitment and mortality) and states (stand structures, water stress) and traced the influence of different facets of FC along this hierarchy in a path analysis. We found an independent influence of functional richness, dissimilarity and identity on ecosystem states and processes and hence biomass change. Biodiversity effects were only positive during early succession and later turned negative. Unexpectedly, resource acquisition (growth, recruitment) and conservation (mortality, turnover) played an equally important role throughout the succession. These results add to a mechanistic understanding of biodiversity effects and place a caveat on simplistic approaches omitting hierarchical levels when analysing BEF relationships. They support the view that BEF relationships experience dramatic shifts over successional time that should be acknowledged in mechanistic theories. C1 [Holzwarth, Frederic; Wirth, Christian] Univ Leipzig, Inst Biol, AG Spezielle Bot & Funkt Biodiversitat, Johannisallee 21, D-04103 Leipzig, Germany. [Rueger, Nadja; Wirth, Christian] German Ctr Integrat Biodivers Res iDiv, D-04103 Leipzig, Germany. [Rueger, Nadja] Smithsonian Trop Res Inst, Balboa Ancon, Panama. RP Holzwarth, F (reprint author), Univ Leipzig, Inst Biol, AG Spezielle Bot & Funkt Biodiversitat, Johannisallee 21, D-04103 Leipzig, Germany. EM frederic.holzwarth@uni-leipzig.de RI Ruger, Nadja/J-6393-2015 OI Ruger, Nadja/0000-0003-2371-4172 FU Max Planck Society; DFG Priority Programme 1374 'Infrastructure-Biodiversity-Exploratories' [WI 2045/7-1]; University of Leipzig; Deutsche Forschungsgemeinschaft DFG [RU 1536/3-1]; DFG-Forschungszentrum 'German Centre for Integrative Biodiversity Research (iDiv) Halle-Jena-Leipzig' FX F.H. was funded by the Max Planck Society (www.bgc-jena.mpg.de), the DFG Priority Programme 1374 'Infrastructure-Biodiversity-Exploratories' (WI 2045/7-1) (www.dfg.de) and the University of Leipzig (www.uni-leipzig.de). N.R. was funded by a research grant from Deutsche Forschungsgemeinschaft DFG (RU 1536/3-1) (www.dfg.de). C.W. and N.R. were supported by the DFG-Forschungszentrum 'German Centre for Integrative Biodiversity Research (iDiv) Halle-Jena-Leipzig' (www.idiv-biodiversity.de). The funders had no role in study design, data collection and analysis, decision to publish or preparation of the manuscript. NR 83 TC 3 Z9 3 U1 4 U2 11 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 2054-5703 J9 ROY SOC OPEN SCI JI R. Soc. Open Sci. PD MAR PY 2015 VL 2 IS 3 AR 140541 DI 10.1098/rsos.140541 PG 19 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA DO7LV UT WOS:000377965000010 PM 26064620 ER PT J AU Graves, GR AF Graves, Gary R. TI SWIMMING BLACK-CROWNED NIGHT-HERONS (NYCTICORAX NYCTICORAX) KLEPTOPARASITIZE AMERICAN COOTS (FULICA AMERICANA) SO SOUTHWESTERN NATURALIST LA English DT Article ID EGRETS AB I observed black-crowned night-herons (Nycticorax nycticorax) swimming and kleptoparasitizing American coots (Fulica americana) at an artificial lake in Pinal County, Arizona. This appears to be the first record of interspecific kleptoparasitism by a swimming ardeid. C1 [Graves, Gary R.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, MRC-116,POB 37012, Washington, DC 20013 USA. [Graves, Gary R.] Univ Copenhagen, Natl Museum Denmark, Ctr Macroecol Evolut & Climate, DK-2100 Copenhagen O, Denmark. RP Graves, GR (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, MRC-116,POB 37012, Washington, DC 20013 USA. EM gravesg@si.edu FU Alexander Wetmore Fund of the Smithsonian Institution; Smoketree Trust FX I thank the Alexander Wetmore Fund of the Smithsonian Institution and the Smoketree Trust for funding and three anonymous reviewers for helpful comments. NR 10 TC 0 Z9 0 U1 1 U2 1 PU SOUTHWESTERN ASSOC NATURALISTS PI SAN MARCOS PA SOUTHWEST TEXAS STATE UNIV, DEPT BIOLOGY, 601 UNIVERSITY DR, SAN MARCOS, TX 78666 USA SN 0038-4909 EI 1943-6262 J9 SOUTHWEST NAT JI Southw. Natural. PD MAR PY 2015 VL 60 IS 1 BP 130 EP 131 DI 10.1894/MCG-11.1 PG 4 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA DE8NQ UT WOS:000370893200023 ER PT J AU Tremblay, SE Ord, SM Bhat, NDR Tingay, SJ Crosse, B Pallot, D Oronsaye, SI Bernardi, G Bowman, JD Briggs, F Cappallo, RJ Corey, BE Deshpande, AA Emrich, D Goeke, R Greenhill, LJ Hazelton, BJ Johnston-Hollitt, M Kaplan, DL Kasper, JC Kratzenberg, E Lonsdale, CJ Lynch, MJ McWhirter, SR Mitchell, DA Morales, MF Morgan, E Oberoi, D Prabu, T Rogers, AEE Roshi, A Shankar, NU Srivani, KS Subrahmanyan, R Waterson, M Wayth, RB Webster, RL Whitney, AR Williams, A Williams, CL AF Tremblay, S. E. Ord, S. M. Bhat, N. D. R. Tingay, S. J. Crosse, B. Pallot, D. Oronsaye, S. I. Bernardi, G. Bowman, J. D. Briggs, F. Cappallo, R. J. Corey, B. E. Deshpande, A. A. Emrich, D. Goeke, R. Greenhill, L. J. Hazelton, B. J. Johnston-Hollitt, M. Kaplan, D. L. Kasper, J. C. Kratzenberg, E. Lonsdale, C. J. Lynch, M. J. McWhirter, S. R. Mitchell, D. A. Morales, M. F. Morgan, E. Oberoi, D. Prabu, T. Rogers, A. E. E. Roshi, A. Shankar, N. Udaya Srivani, K. S. Subrahmanyan, R. Waterson, M. Wayth, R. B. Webster, R. L. Whitney, A. R. Williams, A. Williams, C. L. TI The High Time and Frequency Resolution Capabilities of the Murchison Widefield Array SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF AUSTRALIA LA English DT Article DE instrumentation: interferometers; pulsars: general; radio continuum: general; Sun: radio radiation; techniques: radar astronomy ID CRAB GIANT PULSES; FAST RADIO-BURSTS; PROTOTYPE; PULSARS; LOFAR; MHZ AB The science cases for incorporating high time resolution capabilities into modern radio telescopes are as numerous as they are compelling. Science targets range from exotic sources such as pulsars, to our Sun, to recently detected possible extragalactic bursts of radio emission, the so-called fast radio bursts (FRBs). Originally conceived purely as an imaging telescope, the initial design of the Murchison Widefield Array (MWA) did not include the ability to access high time and frequency resolution voltage data. However, the flexibility of the MWA's software correlator allowed an off-the-shelf solution for adding this capability. This paper describes the system that records the 100 mu s and 10 kHz resolution voltage data from the MWA. Example science applications, where this capability is critical, are presented, as well as accompanying commissioning results from this mode to demonstrate verification. C1 [Tremblay, S. E.; Ord, S. M.; Bhat, N. D. R.; Tingay, S. J.; Crosse, B.; Pallot, D.; Oronsaye, S. I.; Emrich, D.; Lynch, M. J.; Waterson, M.; Wayth, R. B.; Williams, A.] Curtin Univ, Int Ctr Radio Astron Res, Bentley, WA 6102, Australia. [Tremblay, S. E.; Ord, S. M.; Bhat, N. D. R.; Tingay, S. J.; Oronsaye, S. I.; Mitchell, D. A.; Subrahmanyan, R.; Wayth, R. B.; Webster, R. L.] ARC Ctr Excellence All Sky Astrophys CAASTRO, Redfern, NSW 2016, Australia. [Bernardi, G.] SKA SA, ZA-7405 Pinelands, South Africa. [Bernardi, G.] Rhodes Univ, Dept Phys & Elect, ZA-6140 Grahamstown, South Africa. [Bernardi, G.; Greenhill, L. J.; Kasper, J. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bowman, J. D.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Briggs, F.; Waterson, M.] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia. [Cappallo, R. J.; Corey, B. E.; Kratzenberg, E.; Lonsdale, C. J.; McWhirter, S. R.; Rogers, A. E. E.; Whitney, A. R.] MIT, Haystack Observ, Westford, MA 01886 USA. [Deshpande, A. A.; Prabu, T.; Shankar, N. Udaya; Srivani, K. S.; Subrahmanyan, R.] Raman Res Inst, Bangalore 560080, Karnataka, India. [Goeke, R.; Morgan, E.; Williams, C. L.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Hazelton, B. J.; Morales, M. F.] Univ Washington, Dept Phys, Seattle, WA 98195 USA. [Johnston-Hollitt, M.] Victoria Univ Wellington, Sch Chem & Phys Sci, Wellington 6140, New Zealand. [Kaplan, D. L.] Univ Wisconsin, Dept Phys, Milwaukee, WI 53201 USA. [Kasper, J. C.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Mitchell, D. A.] CSIRO Astron & Space Sci CASS, Epping, NSW 1710, Australia. [Oberoi, D.] Tata Inst Fundamental Res, Natl Ctr Radio Astrophys, Pune 411007, Maharashtra, India. [Roshi, A.] Natl Radio Astron Observ, Charlottesville, VA USA. [Roshi, A.] Natl Radio Astron Observ, Greenbank, VA USA. [Waterson, M.] Jodrell Bank Observ, SKA Org, Macclesfield SK11 9DL, Cheshire, England. [Webster, R. L.] Univ Melbourne, Sch Phys, Parkville, Vic 3010, Australia. RP Tremblay, SE (reprint author), Curtin Univ, Int Ctr Radio Astron Res, Bentley, WA 6102, Australia. EM steven.tremblay@curtin.edu.au RI Williams, Andrew/K-2931-2013; M, Manjunath/N-4000-2014; Deshpande, Avinash/D-4868-2012; Udayashankar , N/D-4901-2012; Wayth, Randall/B-2444-2013; Emrich, David/B-7002-2013; Subrahmanyan, Ravi/D-4889-2012 OI Williams, Andrew/0000-0001-9080-0105; M, Manjunath/0000-0001-8710-0730; Wayth, Randall/0000-0002-6995-4131; Emrich, David/0000-0002-4058-1837; FU U.S. National Science Foundation [AST-0457585, PHY-0835713, CAREER-0847753, AST-0908884]; Australian Research Council (LIEF) [LE0775621, LE0882938]; U.S. Air Force Office of Scientific Research [FA9550-0510247]; Centre for All-sky Astrophysics (an Australian Research Council Centre of Excellence) [CE110001020]; Smithsonian Astrophysical Observatory; MIT School of Science; Raman Research Institute; Australian National University; Victoria University of Wellington (New Zealand Ministry of Economic Development and an IBM Shared University Research Grant) [MED-E1799]; Commonwealth Scientific and Industrial Research Organisation (CSIRO); National Collaborative Research Infrastructure Strategy; Education Investment Fund; Australia India Strategic Research Fund; Astronomy Australia Limited; NVIDIA at Harvard University; International Centre for Radio Astronomy Research (ICRAR); Joint Venture of Curtin University; University of Western Australia - Western Australian State government; Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO) [CE110001020]; NSF [AST-1412421] FX This scientific work makes use of the Murchison Radio-astronomy Observatory, operated by CSIRO. We acknowledge the Wajarri Yamatji people as the traditional owners of the Observatory site. Support for the MWA comes from the U.S. National Science Foundation (grants AST-0457585, PHY-0835713, CAREER-0847753, and AST-0908884), the Australian Research Council (LIEF grants LE0775621 and LE0882938), the U.S. Air Force Office of Scientific Research (grant FA9550-0510247), and the Centre for All-sky Astrophysics (an Australian Research Council Centre of Excellence funded by grant CE110001020). Support is also provided by the Smithsonian Astrophysical Observatory, the MIT School of Science, the Raman Research Institute, the Australian National University, and the Victoria University of Wellington (via grant MED-E1799 from the New Zealand Ministry of Economic Development and an IBM Shared University Research Grant). The Australian Federal government provides additional support via the Commonwealth Scientific and Industrial Research Organisation (CSIRO), National Collaborative Research Infrastructure Strategy, Education Investment Fund, and the Australia India Strategic Research Fund, and Astronomy Australia Limited, under contract to Curtin University. We acknowledge the iVEC Petabyte Data Store, the Initiative in Innovative Computing and the CUDA Center for Excellence sponsored by NVIDIA at Harvard University, and the International Centre for Radio Astronomy Research (ICRAR), a Joint Venture of Curtin University and The University of Western Australia, funded by the Western Australian State government. This research was conducted by the Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO), through project number CE110001020. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. DLK was partially funded by NSF grant AST-1412421. NR 36 TC 6 Z9 6 U1 0 U2 5 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 1323-3580 EI 1448-6083 J9 PUBL ASTRON SOC AUST JI Publ. Astron. Soc. Aust. PD FEB 26 PY 2015 VL 32 DI 10.1017/pasa.2015.6 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CC3EH UT WOS:000350227700001 ER PT J AU Huang, YM Rueda, LM AF Huang, Yiau-Min Rueda, Leopoldo M. TI Pictorial Keys to the Species of the Subgenera Albuginosus and Aedimorphus (Grjebinei and Apicoannulatus Groups) of the Genus Aedes Meigen in the Afrotropical Region (Diptera: Culicidae) SO ZOOTAXA LA English DT Article DE Culicidae; mosquitoes; identification key; Africa ID ALLIED TAXA DIPTERA; LIFE STAGES; MORPHOLOGICAL DATA; AEDINI DIPTERA; CLASSIFICATION; PHYLOGENY; OCHLEROTATUS AB Nine species of the subgenus Albuginosus, one species of the subgenus Aedimorphus Grjebinei Group and two species of the subgenus Aedimorphus Apicoannulatus Group of the genus Aedes Meigen in the Afrotropical Region are treated in three pictorial keys based on diagnostic morphological features. C1 [Huang, Yiau-Min] Smithsonian Inst, Dept Entomol, Washington, DC 20013 USA. [Rueda, Leopoldo M.] Walter Reed Army Inst Res, Walter Reed Biosystemat Unit, Entomol Branch, Silver Spring, MD 20910 USA. RP Huang, YM (reprint author), Smithsonian Inst, Dept Entomol, POB 37012,MSC C1109,MRC 534, Washington, DC 20013 USA. EM huangy@si.edu; ruedapol@si.edu NR 27 TC 1 Z9 1 U1 0 U2 2 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD FEB 26 PY 2015 VL 3925 IS 1 BP 25 EP 36 PG 12 WC Zoology SC Zoology GA CB9VN UT WOS:000349981700002 PM 25781728 ER PT J AU Aplin, LM Farine, DR Morand-Ferron, J Cockburn, A Thornton, A Sheldon, BC AF Aplin, Lucy M. Farine, Damien R. Morand-Ferron, Julie Cockburn, Andrew Thornton, Alex Sheldon, Ben C. TI Experimentally induced innovations lead to persistent culture via conformity in wild birds SO NATURE LA English DT Article ID TRANSMISSION; CHIMPANZEES; DYNAMICS AB In human societies, cultural norms arise when behaviours are transmitted through social networks via high-fidelity social learning'. However, a paucity of experimental studies has meant that there is no comparable understanding of the process by which socially transmitted behaviours might spread and persist in animal populations'''. Here we show experimental evidence of the establishment of foraging traditions in a wild bird population. We introduced alternative novel foraging techniques into replicated wild sub-populations of great tits (Parus major) and used automated tracking to map the diffusion, establishment and long-term persistence of the seeded innovations. Furthermore, we used social network analysis to examine the social factors that influenced diffusion dynamics. From only two trained birds in each sub-population, the information spread rapidly through social network ties, to reach an average of 75% of individuals, with a total of 414 knowledgeable individuals performing 57,909 solutions over all replicates. The sub-populations were heavily biased towards using the technique that was originally introduced, resulting in established local traditions that were stable over two generations, despite a high population turnover. Finally, we demonstrate a strong effect of social conformity, with individuals disproportionately adopting the most frequent local variant when first acquiring an innovation, and continuing to favour social information over personal information. Cultural conformity is thought to be a key factor in the evolution of complex culture in humans''. In providing the first experimental demonstration of conformity in a wild non-primate, and of cultural norms in foraging techniques in any wild animal, our results suggest a much broader taxonomic occurrence of such an apparently complex cultural behaviour. C1 [Aplin, Lucy M.; Farine, Damien R.; Sheldon, Ben C.] Univ Oxford, Dept Zool, Edward Grey Inst, Oxford OX1 3PS, England. [Aplin, Lucy M.; Cockburn, Andrew] Australian Natl Univ, Res Sch Biol, Dept Evolut Ecol & Genet, Canberra, ACT 2600, Australia. [Farine, Damien R.] Univ Calif Davis, Dept Anthropol, Davis, CA 95616 USA. [Farine, Damien R.] Smithsonian Trop Res Inst, Ancon 9100, Panama. [Morand-Ferron, Julie] Univ Ottawa, Dept Biol, Ottawa, ON K1N 9B2, Canada. [Thornton, Alex] Univ Exeter, Ctr Ecol & Conservat, Dept Biosci, Penryn TR10 9EZ, England. [Sheldon, Ben C.] Uppsala Univ, Dept Ecol & Genet, S-75236 Uppsala, Sweden. RP Aplin, LM (reprint author), Univ Oxford, Dept Zool, Edward Grey Inst, Oxford OX1 3PS, England. EM lucy.aplin@zoo.ox.ac.uk RI Sheldon, Ben/A-8056-2010; Cockburn, Andrew/A-4864-2008; OI Sheldon, Ben/0000-0002-5240-7828; Farine, Damien/0000-0003-2208-7613; Morand-Ferron, Julie/0000-0001-5186-7710 FU BBSRC [BB/L006081/1, BB/H021817/1]; ERC [AdG 250164]; Australian Postgraduate Award FX This project was supported by grants from the BBSRC (BB/L006081/1) and the ERC (AdG 250164) to B.C.S., who was also supported by a visiting professorship at Uppsala University. L.M.A. was also supported by an Australian Postgraduate Award; and AT., by a BBSRC David Phillips Fellowship (BB/H021817/1). The EGI social networks group, S. Lang and K. McMahon provided assistance in the field, and M. Whitaker produced electronic components for the puzzle boxes. NR 30 TC 67 Z9 68 U1 26 U2 156 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 26 PY 2015 VL 518 IS 7540 BP 538 EP 541 DI 10.1038/nature13998 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CC1JP UT WOS:000350097300047 PM 25470065 ER PT J AU Hagedorn, M Farrell, A Carter, V Zuchowicz, N Johnston, E Padilla-Gamino, J Gunasekera, S Paul, V AF Hagedorn, Mary Farrell, Ann Carter, Virginia Zuchowicz, Nikolas Johnston, Erika Padilla-Gamino, Jacqueline Gunasekera, Sarath Paul, Valerie TI Effects of Toxic Compounds in Montipora capitata on Exogenous and Endogenous Zooxanthellae Performance and Fertilization Success SO PLOS ONE LA English DT Article ID CORAL GONIOPORA-TENUIDENS; CYTOTOXIC DIACETYLENES; SCLERACTINIAN CORALS; CHEMICAL DEFENSES; HAWAIIAN CORALS; CLIMATE-CHANGE; REEF CRISIS; EGGS; SETTLEMENT; DIGITATA AB Studies have identified chemicals within the stony coral genus Montipora that have significant biological activities. For example, Montiporic acids A and B and other compounds have been isolated fromthe adult tissue and eggs of Montipora spp. and have displayed antimicrobial activity and cytotoxicity in cultured cells. The ecological role of these toxic compounds is currently unclear. This study examines the role these toxins play in reproduction. Toxins were found in the eggs and larvae of the coral Montipora capitata. Releasing these toxins by crushing both the eggs and larvae resulted in irreversible inhibition of photosynthesis in endogenous and exogenous zooxanthellae within minutes. Moreover, these toxins were stable, as frozen storage of eggs and larvae did not affect toxicity. Photosynthetic competency of Porites compressa zooxanthellae treated with either frozen or fresh, crushed eggs was inhibited similarly (P > 0.05, ANCOVA). Addition of toxic eggs plugs to live P. compressa fragments caused complete tissue necrosis under the exposed area on the fragments within 1 week. Small volumes of M. capitata crushed eggs added to sperm suspensions reduced in vitro fertilization success by killing the sperm. After 30 min, untreated sperm maintained 90 +/- 1.9% SEM motility while those treated with crushed eggs were rendered immotile, 4 +/- 1.4% SEM. Flow cytometry indicated membrane disruption of the immotile sperm. Fertilization success using untreated sperm was 79 +/- 4% SEM, whereas the success rate dropped significantly after exposure to the crushed eggs, 1.3 +/- 0% SEM. Unlike the eggs and the larvae, M. capitata sperm did not reduce the photosynthetic competency of P. compressa zooxanthellae, suggesting the sperm was nontoxic. The identity of the toxins, cellular mechanism of action, advantage of the toxins for M. capitata and their role on the reef are still unknown. C1 [Hagedorn, Mary; Farrell, Ann; Carter, Virginia; Zuchowicz, Nikolas] Smithsonian Inst, Natl Zool Pk, Smithsonian Conservat Biol Inst, Dept Reprod Sci, Washington, DC 20008 USA. [Hagedorn, Mary; Farrell, Ann; Carter, Virginia; Zuchowicz, Nikolas; Johnston, Erika; Padilla-Gamino, Jacqueline] Univ Hawaii, Hawaii Inst Marine Biol, Kaneohe, HI USA. [Gunasekera, Sarath; Paul, Valerie] Smithsonian Marine Stn, Ft Pierce, FL USA. RP Hagedorn, M (reprint author), Smithsonian Inst, Natl Zool Pk, Smithsonian Conservat Biol Inst, Dept Reprod Sci, Washington, DC 20008 USA. EM hagedornm@si.edu FU Roddenberry Foundation; Anela Kolohe Foundation; Hawaii Community Foundation; Taronga Conservation Society Australia FX These experiments were funded through grants from the Roddenberry Foundation (http://roddenberryfoundation.org/), the Anela Kolohe Foundation, Hawaii Community Foundation (www.hawaiicommunityfoundation.org) and the Taronga Conservation Society Australia (http://taronga.org.au/conservation). No individuals were employed or contracted by the funders (other than the named authors), played any role in: study design, data collection and analysis, decision to publish, or preparation of the manuscript. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 37 TC 2 Z9 2 U1 3 U2 17 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD FEB 25 PY 2015 VL 10 IS 2 AR e0118364 DI 10.1371/journal.pone.0118364 PG 17 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CC2IM UT WOS:000350168700067 PM 25714606 ER PT J AU Hofman, CA Rick, TC Hawkins, MTR Funk, WC Ralls, K Boser, CL Collins, PW Coonan, T King, JL Morrison, SA Newsome, SD Sillett, TS Fleischer, RC Maldonado, JE AF Hofman, Courtney A. Rick, Torben C. Hawkins, Melissa T. R. Funk, W. Chris Ralls, Katherine Boser, Christina L. Collins, Paul W. Coonan, Tim King, Julie L. Morrison, Scott A. Newsome, Seth D. Sillett, T. Scott Fleischer, Robert C. Maldonado, Jesus E. TI Mitochondrial Genomes Suggest Rapid Evolution of Dwarf California Channel Islands Foxes (Urocyon littoralis) SO PLOS ONE LA English DT Article ID PHYLOGENETIC ANALYSIS; MOLECULAR EVOLUTION; GENETIC DIVERSITY; MAMMALS; DOMESTICATION; PLEISTOCENE; POPULATIONS; QUATERNARY; SELECTION; HISTORY AB Island endemics are typically differentiated from their mainland progenitors in behavior, morphology, and genetics, often resulting from long-term evolutionary change. To examine mechanisms for the origins of island endemism, we present a phylogeographic analysis of whole mitochondrial genomes from the endangered island fox (Urocyon littoralis), endemic to California's Channel Islands, and mainland gray foxes (U. cinereoargenteus). Previous genetic studies suggested that foxes first appeared on the islands > 16,000 years ago, before human arrival (similar to 13,000 cal BP), while archaeological and paleontological data supported a colonization > 7000 cal BP. Our results are consistent with initial fox colonization of the northern islands probably by rafting or human introduction similar to 9200-7100 years ago, followed quickly by human translocation of foxes from the northern to southern Channel Islands. Mitogenomes indicate that island foxes are monophyletic and most closely related to gray foxes from northern California that likely experienced a Holocene climate-induced range shift. Our data document rapid morphological evolution of island foxes (in similar to 2000 years or less). Despite evidence for bottlenecks, island foxes have generated and maintained multiple mitochondrial haplotypes. This study highlights the intertwined evolutionary history of island foxes and humans, and illustrates a new approach for investigating the evolutionary histories of other island endemics. C1 [Hofman, Courtney A.] Univ Maryland, Dept Anthropol, College Pk, MD 20742 USA. [Hofman, Courtney A.; Rick, Torben C.] Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Program Human Ecol & Archaeobiol, Washington, DC 20560 USA. [Hofman, Courtney A.; Hawkins, Melissa T. R.; Ralls, Katherine; Fleischer, Robert C.; Maldonado, Jesus E.] Smithsonian Inst, Natl Zool Pk, Smithsonian Conservat Biol Inst, Ctr Conservat & Evolutionary Genet, Washington, DC 20008 USA. [Hawkins, Melissa T. R.; Maldonado, Jesus E.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA. [Funk, W. Chris] Colorado State Univ, Dept Biol, Grad Degree Program Ecol, Ft Collins, CO 80523 USA. [Boser, Christina L.; Morrison, Scott A.] Nature Conservancy, San Francisco, CA USA. [Collins, Paul W.] Santa Barbara Museum Nat Hist, Dept Vertebrate Zool, Santa Barbara, CA USA. [Coonan, Tim] Channel Isl Natl Pk, Natl Pk Serv, Ventura, CA USA. [King, Julie L.] Catalina Isl Conservancy, Avalon, CA USA. [Newsome, Seth D.] Univ New Mexico, Dept Biol, Albuquerque, NM 87131 USA. [Sillett, T. Scott] Smithsonian Inst, Natl Zool Pk, Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Washington, DC 20008 USA. RP Hofman, CA (reprint author), Univ Maryland, Dept Anthropol, College Pk, MD 20742 USA. EM hofmanc@si.edu OI Hofman, Courtney/0000-0002-6808-3370 FU Smithsonian Grand Challenges Consortia; Cosmos Club Foundation; Amazon Web Services Education Research Grant; National Museum of Natural History; National Science Foundation Dissertation Improvement Grant [BCS-1338773] FX This research was funded by the Smithsonian Grand Challenges Consortia (CAH, JEM, TCR, RCF, TSS, KR), the Cosmos Club Foundation (CAH), an Amazon Web Services Education Research Grant (CAH), a National Museum of Natural History small grant (CAH, TR, JEM), and the National Science Foundation Dissertation Improvement Grant (CAH) (BCS-1338773). Roche 454 Life Sciences (RCF, JEM, CAH) provided support with lab equipment and reagents that greatly enhanced the initial phase of this research. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 57 TC 9 Z9 9 U1 9 U2 73 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD FEB 25 PY 2015 VL 10 IS 2 AR e0118240 DI 10.1371/journal.pone.0118240 PG 15 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CC2IM UT WOS:000350168700059 PM 25714775 ER PT J AU Amador-Vargas, S Gronenberg, W Wcislo, WT Mueller, U AF Amador-Vargas, Sabrina Gronenberg, Wulfila Wcislo, William T. Mueller, Ulrich TI Specialization and group size: brain and behavioural correlates of colony size in ants lacking morphological castes SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE division of labour; task specialization; brain anatomy; acacia ants; Pseudomyrmex spinicola ID DIVISION-OF-LABOR; MUSHROOM BODIES; TASK ALLOCATION; SOCIAL BRAIN; EVOLUTION; COMPLEXITY; PLASTICITY; ALLOMETRY; AGE; HYMENOPTERA AB Group size in both multicellular organisms and animal societies can correlate with the degree of division of labour. For ants, the task specialization hypothesis (TSH) proposes that increased behavioural specialization enabled by larger group size corresponds to anatomical specialization of worker brains. Alternatively, the social brain hypothesis proposes that increased levels of social stimuli in larger colonies lead to enlarged brain regions in all workers, regardless of their task specialization. We tested these hypotheses in acacia ants (Pseudomyrmex spinicola), which exhibit behavioural but not morphological task specialization. In wild colonies, we marked, followed and tested ant workers involved in foraging tasks on the leaves (leaf-ants) and in defensive tasks on the host tree trunk (trunk-ants). Task specialization increased with colony size, especially in defensive tasks. The relationship between colony size and brain region volume was task-dependent, supporting the TSH. Specifically, as colony size increased, the relative size of regions within the mushroom bodies of the brain decreased in trunk-ants but increased in leaf-ants; those regions play important roles in learning and memory. Our findings suggest that workers specialized in defence may have reduced learning abilities relative to leaf-ants; these inferences remain to be tested. In societies with monomorphic workers, brain polymorphism enhanced by group size could be a mechanism by which division of labour is achieved. C1 [Amador-Vargas, Sabrina; Mueller, Ulrich] Univ Texas Austin, Sect Integrat Biol, Austin, TX 78712 USA. [Amador-Vargas, Sabrina; Wcislo, William T.] Smithsonian Trop Res Inst, Balboa, Panama. [Gronenberg, Wulfila] Univ Arizona, Dept Neurosci, Tucson, AZ 85721 USA. RP Amador-Vargas, S (reprint author), Univ Texas Austin, Sect Integrat Biol, 1 Univ Stn C0990, Austin, TX 78712 USA. EM samadorv@utexas.edu FU STRI short-term fellowship; NSF-DDIG; EEB grant; NSF [IOS-0920138]; Wheeler Lost Pines Endowment from the University of Texas at Austin FX This research was supported by an STRI short-term fellowship, NSF-DDIG and EEB grant to S.A.-V.; NSF award IOS-0920138 to U.M.; and the Wheeler Lost Pines Endowment from the University of Texas at Austin. NR 52 TC 5 Z9 5 U1 6 U2 37 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 22 PY 2015 VL 282 IS 1801 AR UNSP 20142502 DI 10.1098/rspb.2014.2502 PG 8 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA CC1BU UT WOS:000350077000016 PM 25567649 ER PT J AU Modesto, SP Scott, DM MacDougall, MJ Sues, HD Evans, DC Reisz, RR AF Modesto, Sean P. Scott, Diane M. MacDougall, Mark J. Sues, Hans-Dieter Evans, David C. Reisz, Robert R. TI The oldest parareptile and the early diversification of reptiles SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE carboniferous; diversification; evolution; parareptile ID SOUTH-AFRICA; PROCOLOPHON-TRIGONICEPS; POSTCRANIAL SKELETON; SP-NOV; OSTEOLOGY; OKLAHOMA; PERSPECTIVE; LIMB AB Amniotes, tetrapods that evolved the cleidoic egg and thus independence from aquatic larval stages, appeared ca 314 Ma during the Coal Age. The rapid diversification of amniotes and other tetrapods over the course of the Late Carboniferous period was recently attributed to the fragmentation of coal-swamp rainforests ca 307 Ma. However, the amniote fossil record during the Carboniferous is relatively sparse, with ca 33% of the diversity represented by single specimens for each species. We describe here a new species of reptilian amniote that was collected from uppermost Carboniferous rocks of Prince Edward Island, Canada. Erpetonyx arsenaultorum gen. et sp. nov. is a new parareptile distinguished by 29 presacral vertebrae and autapomorphies of the carpus. Phylogenetic analyses of parareptiles reveal E. arsenaultorum as the closest relative of bolosaurids. Stratigraphic calibration of our results indicates that parareptiles begantheir evolutionary radiation before the close of the Carboniferous Period, and that the diversity of end-Carboniferous reptiles is 80% greater than suggested by previous work. Latest Carboniferous reptiles were still half as diverse as synapsid amniotes, a disparity that may be attributable to preservational biases, to collecting biases, to the origin of herbivory in tetrapocls or any combination of these factors. C1 [Modesto, Sean P.] Cape Breton Univ, Dept Biol, Sydney, NS B1P 6L2, Canada. [Scott, Diane M.; MacDougall, Mark J.; Reisz, Robert R.] Univ Toronto, Dept Biol, Mississauga, ON L5L 1C6, Canada. [Sues, Hans-Dieter] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. [Evans, David C.] Royal Ontario Museum, Dept Nat Hist, Toronto, ON M5S 2C6, Canada. RP Reisz, RR (reprint author), Univ Toronto, Dept Biol, Mississauga, ON L5L 1C6, Canada. EM robert.reisz@utoronto.ca FU Discovery Grants from the Natural Sciences and Engineering Research Council (NSERC) of Canada; New Opportunities Fund Award from the Canadian Foundation for Innovation (CFI); Nova Scotia Research and Innovation Trust FX This research was supported by Discovery Grants from the Natural Sciences and Engineering Research Council (NSERC) of Canada to S.P.M., R.R.R. and D.C.E. The first author was also supported by a New Opportunities Fund Award from the Canadian Foundation for Innovation (CFI), and by a grant from the Nova Scotia Research and Innovation Trust. NR 46 TC 2 Z9 2 U1 4 U2 27 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 22 PY 2015 VL 282 IS 1801 AR 20141912 DI 10.1098/rspb.2014.1912 PG 9 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA CC1BU UT WOS:000350077000007 PM 25589601 ER PT J AU Monna, A Seitz, S Zitrin, A Geller, MJ Grillo, C Mercurio, A Greisel, N Halkola, A Suyu, SH Postman, M Rosati, P Balestra, I Biviano, A Coe, D Fabricant, DG Hwang, HS Koekemoer, A AF Monna, A. Seitz, S. Zitrin, A. Geller, M. J. Grillo, C. Mercurio, A. Greisel, N. Halkola, A. Suyu, S. H. Postman, M. Rosati, P. Balestra, I. Biviano, A. Coe, D. Fabricant, D. G. Hwang, H. S. Koekemoer, A. TI Constraining the galaxy mass content in the core of A383 using velocity dispersion measurements for individual cluster members SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE gravitational lensing: strong; galaxies: clusters: general; galaxies: clusters: individual: A383; galaxies: haloes; dark matter ID DARK-MATTER HALOS; HIGH-DENSITY ENVIRONMENTS; TELESCOPE LENSING SURVEY; DEEP-FIELD-NORTH; LINE-OF-SIGHT; ELLIPTIC GALAXIES; PHOTOMETRIC REDSHIFTS; LEGACY SURVEY; ABELL 383; HUBBLE AB We use velocity dispersion measurements of 21 individual cluster members in the core of Abell 383, obtained with Multiple Mirror Telescope Hectospec, to separate the galaxy and the smooth dark halo (DH) lensing contributions. While lensing usually constrains the overall, projected mass density, the innovative use of velocity dispersion measurements as a proxy for masses of individual cluster members breaks inherent degeneracies and allows us to (a) refine the constraints on single galaxy masses and on the galaxy mass-to-light scaling relation and, as a result, (b) refine the constraints on the DM-only map, a high-end goal of lens modelling. The knowledge of cluster member velocity dispersions improves the fit by 17 per cent in terms of the image reproduction chi(2), or 20 per cent in terms of the rms. The constraints on the mass parameters improve by similar to 10 per cent for the DH, while for the galaxy component, they are refined correspondingly by similar to 50 per cent, including the galaxy halo truncation radius. For an L* galaxy with M-B* = -20.96, for example, we obtain best-fitting truncation radius r(tr)* = 20.5(-6.7)(+9.6) kpc and velocity dispersion sigma* = 324 +/- 17 km s(-1). Moreover, by performing the surface brightness reconstruction of the southern giant arc, we improve the constraints on r(tr) of two nearby cluster members, which have measured velocity dispersions, by more than similar to 30 per cent. We estimate the stripped mass for these two galaxies, getting results that are consistent with numerical simulations. In the future, we plan to apply this analysis to other galaxy clusters for which velocity dispersions of member galaxies are available. C1 [Monna, A.; Seitz, S.; Greisel, N.] Univ Observ Munich, D-81679 Munich, Germany. [Monna, A.; Seitz, S.; Greisel, N.; Balestra, I.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Zitrin, A.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Geller, M. J.; Fabricant, D. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Grillo, C.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark. [Mercurio, A.] INAF Osservatorio Astron Capodimonte, I-80131 Naples, Italy. [Halkola, A.] Med Univ Lubeck, Inst Med Engn, D-23562 Lubeck, Germany. [Suyu, S. H.] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Postman, M.; Coe, D.; Koekemoer, A.] Space Telescope Sci Inst, Baltimore, MD 21208 USA. [Rosati, P.] Univ Ferrara, Dipartimento Fis & Sci Terra, I-44122 Ferrara, Italy. [Balestra, I.; Biviano, A.] INAF Osservatorio Astron Trieste, I-34143 Trieste, Italy. [Hwang, H. S.] Korea Inst Adv Study, Seoul 130722, South Korea. RP Monna, A (reprint author), Univ Observ Munich, Scheinerstr 1, D-81679 Munich, Germany. EM anna.monna@gmail.com RI Grillo, Claudio/E-6223-2015; OI Grillo, Claudio/0000-0002-5926-7143; Greisel, Natascha/0000-0002-4907-6247; Balestra, Italo/0000-0001-9660-894X; Biviano, Andrea/0000-0002-0857-0732; Koekemoer, Anton/0000-0002-6610-2048 FU Transregional Collaborative Research Centre TRR 33 - The Dark Universe and the DFG cluster of excellence 'Origin and Structure of the Universe; NASA [NAS 5-26555]; CLASH Multi-Cycle Treasury Program [GO-12065]; DNRF; NASA - STScI [HST-HF-51334.01-A] FX This work is supported by the Transregional Collaborative Research Centre TRR 33 - The Dark Universe and the DFG cluster of excellence 'Origin and Structure of the Universe. The CLASH Multi-Cycle Treasury Program (GO-12065) is based on observations made with the NASA/ESA Hubble Space Telescope. The Space Telescope Science Institute is operated by the Association of Universities for Research in Astronomy, Inc. under NASA contract NAS 5-26555. The Dark Cosmology Centre is funded by the DNRF. Support for AZ is provided by NASA through Hubble Fellowship grant #HST-HF-51334.01-A awarded by STScI. The Smithsonian Institution supports the research of DGF, MJG, and HSH. We thank Daniel Gruen for his contribution to the improvement of the text. NR 77 TC 5 Z9 5 U1 2 U2 4 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB 21 PY 2015 VL 447 IS 2 BP 1224 EP 1241 DI 10.1093/mnras/stu2534 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CC3TM UT WOS:000350272900016 ER PT J AU Novak, M Smolcic, V Civano, F Bondi, M Ciliegi, P Wang, XW Loeb, A Banfield, J Bourke, S Elvis, M Hallinan, G Intema, HT Klockner, HR Mooley, K Navarrete, F AF Novak, Mladen Smolcic, Vernesa Civano, Francesca Bondi, Marco Ciliegi, Paolo Wang, Xiawei Loeb, Abraham Banfield, Julie Bourke, Stephen Elvis, Martin Hallinan, Gregg Intema, Huib T. Kloeckner, Hans-Rainer Mooley, Kunal Navarrete, Felipe TI New insights from deep VLA data on the potentially recoiling black hole CID-42 in the COSMOS field SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: active; galaxies: individual: CID-42; galaxies: interactions; galaxies: nuclei; radio continuum: galaxies ID ACTIVE GALACTIC NUCLEUS; PROBE WMAP OBSERVATIONS; RADIATION RECOIL; GALAXY MERGERS; SOURCE CATALOG; QUASAR; SDSS; CONSTRAINTS; EVOLUTION; PROJECT AB We present deep 3-GHz Karl G. Jansky Very Large Array (VLA) observations of the potentially recoiling black hole CID-42 in the Cosmic Evolution Survey (COSMOS) field. This galaxy shows two optical nuclei in the Hubble Space Telescope/Advanced Camera for Surveys (HST/ACS) image and a large velocity offset of approximate to 1300 km s(-1) between the broad and narrow H beta emission line although the spectrum is not spacially resolved (Civano et al. 2010). The new 3 GHz VLA data have a bandwidth of 2 GHz and to correctly interpret the flux densities imaging was done with two different methods: multiscale multifrequency (MSMF) synthesis and spectral windows (SPWs) stacking. The final resolutions and sensitivities of these maps are 0.7 arcsec with rms = 4.6 mu Jy beam(-1) and 0.9 arcsec with rms = 4.8 mu Jy beam(-1), respectively. With a 7 sigma detection, we find that the entire observed 3-GHz radio emission can be associated with the south-eastern component of CID-42, coincident with the detected X-ray emission. We use our 3 GHz data combined with other radio data from the literature ranging from 320 MHz to 9 GHz, which include the VLA, Very Long Baseline Array (VLBA) and Giant Metrewave Radio Telescope (GMRT) data, to construct a radio synchrotron spectrum of CID-42. The radio spectrum suggests a type I unobscured radio-quiet flat-spectrum active galactic nucleus (AGN) in the south-eastern component which may be surrounded by a more extended region of old synchrotron electron population or shocks generated by the outflow from the supermassive black hole (SMBH). Our data are consistent with the recoiling black hole picture but cannot rule out the presence of an obscured and radio-quiet SMBH in the north-western component. C1 [Novak, Mladen; Smolcic, Vernesa] Univ Zagreb, Dept Phys, Zagreb 10002, Croatia. [Civano, Francesca] Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA. [Civano, Francesca] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Bondi, Marco] INAF Ist Radioastron Bologna, I-40129 Bologna, Italy. [Ciliegi, Paolo] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy. [Wang, Xiawei; Loeb, Abraham] Harvard Univ, Dept Astron, Cambridge, MA 02138 USA. [Banfield, Julie] CSIRO Australia Telescope Natl Facil, Epping, NSW 1710, Australia. [Banfield, Julie] Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. [Bourke, Stephen; Hallinan, Gregg; Mooley, Kunal] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Elvis, Martin] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Intema, Huib T.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Kloeckner, Hans-Rainer] Univ Oxford, Subdept Astrophys, Oxford OX1 3RH, England. [Kloeckner, Hans-Rainer] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Navarrete, Felipe] Argelander Inst Astron, D-53121 Bonn, Germany. RP Novak, M (reprint author), Univ Zagreb, Dept Phys, Bijenicka Cesta 32, Zagreb 10002, Croatia. EM mlnovak@phy.hr RI Intema, Huib/D-1438-2012; OI Intema, Huib/0000-0002-5880-2730; Ciliegi, Paolo/0000-0002-0447-4620 FU European Union [337595] FX We thank the anonymous referee for providing helpful comments which improved the paper. This research was funded by the European Union's Seventh Framework programme under grant agreement 337595 (ERC Starting Grant, CoSMass). The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. NR 48 TC 6 Z9 6 U1 2 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 21 PY 2015 VL 447 IS 2 BP 1282 EP 1288 DI 10.1093/mnras/stu2473 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CC3TM UT WOS:000350272900020 ER PT J AU Joseph, TD Maccarone, TJ Kraft, RP Sivakoff, GR AF Joseph, T. D. Maccarone, T. J. Kraft, R. P. Sivakoff, G. R. TI Deep Chandra observations of the NGC 4472 globular cluster black hole XMMU 122939.7+075333: short-term variability from the first globular cluster black hole binary SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: individual: NGC 4472; X-rays: binaries ID X-RAY SOURCES; LMC X-4; RZ 2109; NGC-4472; EMISSION; ECCENTRICITY; SPECTROSCOPY; CATALOG; OBJECTS; SAMPLE AB In this paper, we discuss the luminosity modulations and spectral analysis results of the recent deep observations of XMMU 122939.7+075333, the first black hole discovered in a globular cluster. The source has been detected many times, typically with L-X > 10(39) erg s(-1), but in a 2010 observation had faded to L-X similar to 10(38) erg s(-1). In our 2011 observations, it has rebrightened to L-X similar to 2 x 10(39) erg s(-1). This significant increase in luminosity over a relatively short time period is not consistent with the idea that the long-term flux modulations displayed by XMMU 122939.7+075333 are caused by the Kozai mechanism alone as had previously been suggested. Instead, given that the source shows 'spiky' behaviour in its light curve, it seems likely that the faintness in 2010 was a result of a short observation that did not catch any bright epochs. We also find that when the source is brighter than average, it has an excess of soft (<0.7 keV) photons. The spectral analysis reveals strong, albeit model-dependent, evidence of emission from highly ionized oxygen (O VIII) when the source is brighter than average. C1 [Joseph, T. D.] Univ Cape Town, ZA-7701 Rondebosch, South Africa. [Joseph, T. D.; Maccarone, T. J.] Univ Southampton, Southampton SO17 1BJ, Hants, England. [Joseph, T. D.; Kraft, R. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Maccarone, T. J.] Texas Tech Univ, Lubbock, TX 79409 USA. [Sivakoff, G. R.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2E1, Canada. RP Joseph, TD (reprint author), Univ Cape Town, ZA-7701 Rondebosch, South Africa. EM tana@ast.uct.ac.za RI Sivakoff, Gregory/G-9602-2011 OI Sivakoff, Gregory/0000-0001-6682-916X FU Stobie-SALT studentship - NRF of South Africa; Stobie-SALT studentship - British Council; Stobie-SALT studentship - University of Southampton; National Aeronautics and Space Administration [GO1-12160X]; NSERC FX TDJ acknowledges support from a Stobie-SALT studentship, funded jointly by the NRF of South Africa, the British Council and the University of Southampton. 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 CHIPS, etc. This material is based upon work supported by the National Aeronautics and Space Administration under Grant No. GO1-12160X. GRS acknowledges the support of an NSERC Discovery Grant. TDJ would also like to thank Texas Tech University for its hospitality while this work was being finished. Lastly, the authors would like to thank Daniel Plant, Pablo Cassatella, Joey Neilsen, Matthew Middleton, and Dominic Walton for their assistance and useful comments. NR 37 TC 1 Z9 1 U1 0 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB 21 PY 2015 VL 447 IS 2 BP 1460 EP 1470 DI 10.1093/mnras/stu2523 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CC3TM UT WOS:000350272900037 ER PT J AU Mocz, P Guo, XY AF Mocz, Philip Guo, Xinyi TI Interpreting MAD within multiple accretion regimes SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; black hole physics; galaxies: jets ID ACTIVE GALACTIC NUCLEI; SUPERMASSIVE BLACK-HOLES; ADVECTION-DOMINATED ACCRETION; MAGNETOHYDRODYNAMIC SIMULATIONS; RELATIVISTIC JETS; RADIO-SOURCES; KINETIC POWER; AGN; FLOWS; DISKS AB General relativistic magnetohydrodynamic (GRMHD) simulations of accreting black holes in the radiatively inefficient regime show that systems with sufficient magnetic poloidal flux become magnetically arrested disc (MAD) systems, with a well-defined relationship between the magnetic flux and the mass accretion rate. Recently, Zamaninasab et al. report that the jet magnetic flux and accretion disc luminosity are tightly correlated over 7 orders of magnitude for a sample of 76 radio-loud active galaxies, concluding that the data are explained by the MAD mode of accretion. Their analysis assumes radiatively efficient accretion, and their sample consists primarily of radiatively efficient sources, while GRMHD simulations of MAD thus far have been carried out in the radiatively inefficient regime. We propose a model to interpret MAD systems in the context of multiple accretion regimes, and apply it to the sample in Zamaninasab et al., along with additional radiatively inefficient sources from archival data. We show that most of the radiatively inefficient radio-loud galaxies are consistent with being MAD systems. Assuming the MAD relationship found in radiatively inefficient simulations holds at other accretion regimes, a significant fraction of our sample can be candidates for MAD systems. Future GRMHD simulations have yet to verify the validity of this assumption. C1 [Mocz, Philip; Guo, Xinyi] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Mocz, P (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM pmocz@cfa.harvard.edu OI Mocz, Philip/0000-0001-6631-2566 FU National Science Foundation [DGE-1144152]; NASA [NNX14AB47G] FX The authors would like to thank Ramesh Narayan and Alexander Tchekhovskoy for helpful discussions, and Andy Fabian, Pierre Christian, Fernando Becerra, and the anonymous referee for valuable comments on the manuscript. This material is based upon work supported by the National Science Foundation Graduate Research Fellowship under grant no. DGE-1144152 (PM) and NASA grant NNX14AB47G (XG). NR 53 TC 4 Z9 4 U1 1 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB 21 PY 2015 VL 447 IS 2 BP 1498 EP 1503 DI 10.1093/mnras/stu2555 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CC3TM UT WOS:000350272900041 ER PT J AU Zapata, LA Palau, A Galvan-Madrid, R Rodriguez, LF Garay, G Moran, JM Franco-Hernandez, R AF Zapata, Luis A. Palau, Aina Galvan-Madrid, Roberto Rodriguez, Luis F. Garay, Guido Moran, James M. Franco-Hernandez, Ramiro TI ALMA reveals a candidate hot and compact disc around the O-type protostar IRAS 16547-4247 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars: protostars; ISM: jets and outflows ID MASSIVE STAR-FORMATION; II REGIONS; ACCRETION; OUTFLOW; CORES; EMISSION; SYSTEM; AU; IRAS-16547-4247; SUBMILLIMETER AB We present high angular resolution (similar to 0.3 arcsec) submillimeter continuum (0.85 mm) and line observations of the O-type protostar IRAS 16547-4247 carried out with the Atacama Large Millimeter/Submillimeter Array (ALMA). In the 0.85 mm continuum band, the observations revealed two compact sources (with a separation of 2 arcsec), one of them associated with IRAS 16547-4247, and the other one to the west. Both sources are well-resolved angularly, revealing a clumpy structure. On the other hand, the line observations revealed a rich variety of molecular species related to both continuum sources. In particular, we found a large number of S-bearing molecules, such as the rare molecule methyl mercaptan (CH3SH). At scales larger than 10 000 au, molecules (e. g. SO2 or OCS) mostly with low-excitation temperatures in the upper states (E-k less than or similar to 300 K) are present in both millimeter continuum sources, and show a southeast-north-west velocity gradient of 7 kms(-1) over 3 arcsec (165 km s(-1) pc(-1)). We suggest that this gradient probably is produced by the thermal (free-free) jet emerging from this object with a similar orientation at the base. At much smaller scales (about 1000 au), molecules with high-excitation temperatures (E-k >= 500 K) are tracing a rotating structure elongated perpendicular to the orientation of the thermal jet, which we interpret as a candidate disc surrounding IRAS 16547-4247. The dynamical mass corresponding to the velocity gradient of the candidate to disc is about 20M(circle dot), which is consistent with the bolometric luminosity of IRAS 16547-4247. C1 [Zapata, Luis A.; Palau, Aina; Galvan-Madrid, Roberto; Rodriguez, Luis F.] Univ Nacl Autonoma Mexico, Ctr Radiostron & Astrofis, Morelia 58089, Michoacan, Mexico. [Galvan-Madrid, Roberto] European So Observ, D-85748 Garching, Germany. [Garay, Guido; Franco-Hernandez, Ramiro] Univ Chile, Dept Astron, Santiago, Chile. [Moran, James M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Zapata, LA (reprint author), Univ Nacl Autonoma Mexico, Ctr Radiostron & Astrofis, Morelia 58089, Michoacan, Mexico. EM lzapata@crya.unam.mx RI Garay, Guido/H-8840-2013; OI Garay, Guido/0000-0003-1649-7958; Moran, James/0000-0002-3882-4414 FU DGAPA; UNAM; CONACyT, Mexico; CONICYT [PFB-06] FX LAZ, AP, RG, and LFR acknowledge the financial support from DGAPA, UNAM, and CONACyT, Mexico. This paper makes use of ALMA data: ADS/JAO.ALMA#2011.0.00419.S. ALMA is a partnership of ESO (representing its member states), NSF (USA), and NINS (Japan), together with NRC (Canada), and NSC and ASIAA (Taiwan), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. GG acknowledges support from CONICYT project PFB-06. NR 34 TC 7 Z9 7 U1 0 U2 3 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB 21 PY 2015 VL 447 IS 2 BP 1826 EP 1833 DI 10.1093/mnras/stu2527 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CC3TM UT WOS:000350272900066 ER PT J AU Bird, S Haehnelt, M Neeleman, M Genel, S Vogelsberger, M Hernquist, L AF Bird, Simeon Haehnelt, Martin Neeleman, Marcel Genel, Shy Vogelsberger, Mark Hernquist, Lars TI Reproducing the kinematics of damped Lyman alpha systems SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: formation; intergalactic medium; cosmology: theory ID MASS-METALLICITY RELATION; GALAXY FORMATION MODELS; SIMILAR-TO 5; LY-ALPHA; COSMOLOGICAL SIMULATIONS; HYDRODYNAMICAL SIMULATIONS; ILLUSTRIS PROJECT; STELLAR FEEDBACK; HIGH-REDSHIFT; BLACK-HOLES AB We examine the kinematic structure of damped Lyman alpha systems (DLAs) in a series of cosmological hydrodynamic simulations using the AREPO code. We are able to match the distribution of velocity widths of associated low-ionization metal absorbers substantially better than earlier work. Our simulations produce a population of DLAs dominated by haloes with virial velocities around 70 km s(-1), consistent with a picture of relatively small, faint objects. In addition, we reproduce the observed correlation between velocity width and metallicity and the equivalent width distribution of Si II. Some discrepancies of moderate statistical significance remain; too many of our spectra show absorption concentrated at the edge of the profile and there are slight differences in the exact shape of the velocity width distribution. We show that the improvement over previous work is mostly due to our strong feedback from star formation and our detailed modelling of the metal ionization state. C1 [Bird, Simeon] Inst Adv Study, Princeton, NJ 08540 USA. [Haehnelt, Martin] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Neeleman, Marcel] Univ Calif San Diego, Dept Phys, La Jolla, CA 92093 USA. [Neeleman, Marcel] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA. [Genel, Shy; Hernquist, Lars] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Vogelsberger, Mark] MIT, MKI, Cambridge, MA 02139 USA. [Vogelsberger, Mark] MIT, Dept Phys, Cambridge, MA 02139 USA. RP Bird, S (reprint author), Inst Adv Study, 1 Einstein Dr, Princeton, NJ 08540 USA. EM sbird@andrew.cmu.edu FU National Science Foundation [AST-0907969]; W.M. Keck Foundation; NSF [AST-1109447]; FP7 ERC Advanced Grant Emergence [320596]; NASA ATP Award [NNX12AC67G]; NSF grant [AST-1312095] FX SB thanks Ryan Cooke, Edoardo Tescari, Andrew Pontzen, Rob Simcoe, and J. Xavier Prochaska for useful discussions, and Volker Springel for writing and allowing us to use the AREPO code. SB is supported by the National Science Foundation grant number AST-0907969, and the W.M. Keck Foundation. MN is supported by NSF grant AST-1109447. MGH acknowledges support from the FP7 ERC Advanced Grant Emergence-320596. LH is supported by NASA ATP Award NNX12AC67G and NSF grant AST-1312095. NR 52 TC 14 Z9 14 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB 21 PY 2015 VL 447 IS 2 BP 1834 EP 1846 DI 10.1093/mnras/stu2542 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CC3TM UT WOS:000350272900067 ER PT J AU Musaeva, A Koribalski, BS Farrell, SA Sadler, EM Servillat, M Jurek, R Lenc, E Starling, RLC Webb, NA Godet, O Combes, F Barret, D AF Musaeva, A. Koribalski, B. S. Farrell, S. A. Sadler, E. M. Servillat, M. Jurek, R. Lenc, E. Starling, R. L. C. Webb, N. A. Godet, O. Combes, F. Barret, D. TI H I study of the environment around ESO 243-49, the host galaxy of an intermediate-mass black hole SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE ISM: general; galaxies: individual: AM 0108-462; galaxies: individual: ESO 243-49; galaxies: individual: HLX-1 ID NEUTRAL-HYDROGEN CONTENT; STAR-FORMING GALAXIES; X-RAY SOURCES; OPTICAL COUNTERPART; INTERSTELLAR-MEDIUM; SCALING RELATIONS; VIRGO CLUSTER; RADIO-SOURCES; 1.4 GHZ; HLX-1 AB The lenticular galaxy ESO 243-49 hosts the ultraluminous X-ray source HLX-1, the best candidate intermediate-mass black hole (IMBH) currently known. The environments of IMBHs remain unknown, however, the proposed candidates include the nuclei of dwarf galaxies or globular clusters. Evidence at optical wavelengths points at HLX-1 being the remnant of an accreted dwarf galaxy. Here we report the Australia Telescope Compact Array radio observations of HI emission in and around ESO 243-49 searching for signatures of a recent merger event. No HI line emission is detected in ESO 243-49 with a 5 sigma upper limit on the HI gas mass of a few 10(8)M(circle dot). A likely reason for this non-detection is the cluster environment depleting ESO 243-49's H I gas reservoir. The upper limit is consistent with an interpretation of HLX-1 as a dwarf satellite of ESO 243-49, however, more sensitive observations are required for a detection. We detect similar to 5x10(8)M(circle dot) of HI gas in the peculiar spiral galaxy AM0108-462, located at a projected distance of similar to 170 kpc from ESO 243-49. This amount of HI gas is similar to 10 times less than in spiral galaxies with similar optical and near-infrared properties in the field, strengthening the conclusion that the cluster environment indeed depletes the HI gas reservoir of these two galaxies. Here we also report observations of AM 0108-462 in several optical and near-infrared bands using the Magellan 6.5-m telescopes, and archival X-ray and ultraviolet observations with XMM-Newton and Swift. These data combined with the HI line data suggest it is likely that AM 0108-462 is experiencing a merger event. C1 [Musaeva, A.; Farrell, S. A.; Sadler, E. M.; Lenc, E.] Univ Sydney, Sydney Inst Astron, Sch Phys, Redfern, NSW 2016, Australia. [Musaeva, A.; Lenc, E.] ARC Ctr Excellence All Sky Astrophys CAASTRO, Redfern, NSW 2016, Australia. [Musaeva, A.; Koribalski, B. S.; Jurek, R.] CSIRO Astron & Space Sci, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. [Servillat, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Servillat, M.] Univ Paris Diderot, CEA Saclay, CNRS, Lab AIM,CEA,DSM,IRFU,SAp, F-91191 Gif Sur Yvette, France. [Starling, R. L. C.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Webb, N. A.; Godet, O.; Barret, D.] Univ Toulouse, UPS, IRAP, F-31028 Toulouse 4, France. [Webb, N. A.; Godet, O.; Barret, D.] Inst Rech Astrophys & Planetol, CNRS, F-31028 Toulouse 4, France. [Combes, F.] Observ Paris, UMR 8112, LERMA, F-75014 Paris, France. RP Musaeva, A (reprint author), Univ Sydney, Sydney Inst Astron, Sch Phys, Redfern, NSW 2016, Australia. EM a.musaeva@physics.usyd.edu.au OI Koribalski, Baerbel/0000-0003-4351-993X; Sadler, Elaine/0000-0002-1136-2555; Lenc, Emil/0000-0002-9994-1593; Combes, Francoise/0000-0003-2658-7893 FU Commonwealth of Australia; Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO) [CE110001020]; ESA Member States; USA (NASA); National Aeronautics and Space Administration; National Science Foundation; Australian Research Council [DP110102889]; Royal Society Dorothy Hodgkin Fellowship FX The Australia Telescope Compact Array is part of the Australia Telescope National Facility which is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. Parts of this research were conducted by the Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO), through project number CE110001020. This work is also based on observations obtained with XMM-Newton [an ESA science mission with instruments and contributions directly funded by ESA Member States and the USA (NASA)], the 6.5-m Magellan telescopes located at Las Campanas Observatory, Chile, and made use of data from the Swift Archive. 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. SAF was the recipient of an Australian Research Council Postdoctoral Fellowship for part of this work, funded by grant DP110102889. RLCS is the recipient of a Royal Society Dorothy Hodgkin Fellowship. NR 56 TC 0 Z9 0 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 21 PY 2015 VL 447 IS 2 BP 1951 EP 1961 DI 10.1093/mnras/stu2606 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CC3TM UT WOS:000350272900077 ER PT J AU Battisti, AJ Calzetti, D Johnson, BD Elbaz, D AF Battisti, A. J. Calzetti, D. Johnson, B. D. Elbaz, D. TI CONTINUOUS MID-INFRARED STAR FORMATION RATE INDICATORS: DIAGNOSTICS FOR 0 < z < 3 STAR-FORMING GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: star formation; infrared: galaxies; stars: formation ID ACTIVE GALACTIC NUCLEI; SPECTRAL ENERGY-DISTRIBUTIONS; DIGITAL SKY SURVEY; MASS-METALLICITY RELATION; S(4)G IRAC 3.6; STELLAR MASS; QUIESCENT GALAXIES; FORMATION HISTORY; INFRARED TRACERS; H-ALPHA AB We present continuous, monochromatic star formation rate (SFR) indicators over the mid-infrared wavelength range of 6-70 mu m. We use a sample of 58 star-forming galaxies (SFGs) in the Spitzer-SDSS-GALEX Spectroscopic Survey at z < 0.2, for which there is a rich suite of multi-wavelength photometry and spectroscopy from the ultraviolet through to the infrared. The data from the Spitzer Infrared Spectrograph (IRS) of these galaxies, which spans 5-40 mu m, is anchored to their photometric counterparts. The spectral region between 40-70 mu m is interpolated using dust model fits to the IRS spectrum and Spitzer 70 and 160 mu m photometry. Since there are no sharp spectral features in this region, we expect these interpolations to be robust. This spectral range is calibrated as a SFR diagnostic using several reference SFR indicators to mitigate potential bias. Our band-specific continuous SFR indicators are found to be consistent with monochromatic calibrations in the local universe, as derived from Spitzer, WISE, and Herschel photometry. Our local composite template and continuous SFR diagnostics are made available for public use through the NASA/IPAC Infrared Science Archive (IRSA) and have typical dispersions of 30% or less. We discuss the validity and range of applicability for our SFR indicators in the context of unveiling the formation and evolution of galaxies. Additionally, in the era of the James Webb Space Telescope this will become a flexible tool, applicable to any SFG up to z similar to 3. C1 [Battisti, A. J.; Calzetti, D.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Johnson, B. D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Elbaz, D.] Univ Paris Diderot, CNRS, CEA DSM Irfu, Lab AIM Paris Saclay, F-91191 Gif Sur Yvette, France. RP Battisti, AJ (reprint author), Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. EM abattist@astro.umass.edu FU NASA ROSES Astrophysics Data Analysis Program [NNX13AF19G]; Alfred P. Sloan Foundation; National Science Foundation; US Department of Energy; National Aeronautics and Space Administration; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England; American Museum of Natural History; Astrophysical Institute Potsdam; University of Basel; University of Cambridge; Case Western Reserve University; University of Chicago; Drexel University; Fermilab; Institute for Advanced Study; Japan Participation Group; Johns Hopkins University; Joint Institute for Nuclear Astrophysics; Kavli Institute for Particle Astrophysics and Cosmology; Korean Scientist Group; Chinese Academy of Sciences (LAMOST); Los Alamos National Laboratory; Max Planck Institute for Astronomy (MPIA); Max Planck Institute for Astrophysics (MPA); New Mexico State University; Ohio State University; University of Pittsburgh; University of Portsmouth; Princeton University; United States Naval Observatory; University of Washington; California Institute of Technology under NASA [NAS5-98034]; NASA FX The authors thank the referee whose suggestions helped to clarify and improve the content of this work. We also thank the MIRI instrument team for providing the MIRI filter curves prior to their publication. AJB thanks K. Grasha, A. Kirkpatrick, A. Pope, and D. Marchesini for comments and discussion that improved the content of this paper. AJB and DC gratefully acknowledge partial support from the NASA ROSES Astrophysics Data Analysis Program, under program number NNX13AF19G. This research has made use of the NASA/IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration (NASA). This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. This work has made use of SDSS data. Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the US Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society and the Higher Education Funding Council for England. The SDSS website is http://sdss.org/. The SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions. The Participating Institutions are the American Museum of Natural History, Astrophysical Institute Potsdam, University of Basel, University of Cambridge, Case Western Reserve University, University of Chicago, Drexel University, Fermilab, the Institute for Advanced Study, the Japan Participation Group, Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology, the Korean Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory, the Max Planck Institute for Astronomy (MPIA), the Max Planck Institute for Astrophysics (MPA), New Mexico State University, Ohio State University, University of Pittsburgh, University of Portsmouth, Princeton University, the United States Naval Observatory and the University of Washington. This work is based on observations made with the NASA Galaxy Evolution Explorer. GALEX is operated for NASA by the California Institute of Technology under NASA contract NAS5-98034. This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the NASA. NR 78 TC 3 Z9 3 U1 2 U2 10 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2015 VL 800 IS 2 AR 143 DI 10.1088/0004-637X/800/2/143 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CB7CA UT WOS:000349782500066 ER PT J AU Blair, WP Winkler, PF Long, KS Whitmore, BC Kim, H Soria, R Kuntz, KD Plucinsky, PP Dopita, MA Stockdale, C AF Blair, William P. Winkler, P. Frank Long, Knox S. Whitmore, Bradley C. Kim, Hwihyun Soria, Roberto Kuntz, K. D. Plucinsky, Paul P. Dopita, Michael A. Stockdale, Christopher TI A NEWLY RECOGNIZED VERY YOUNG SUPERNOVA REMNANT IN M83* SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: individual (M83); galaxies: ISM; ISM: supernova remnants; supernovae: general ID SMALL-MAGELLANIC-CLOUD; CORE-COLLAPSE SUPERNOVAE; TIME OPTICAL-EMISSION; X-RAY; HISTORICAL SUPERNOVAE; 1E 0102.2-7219; M83; SPECTROSCOPY; EVOLUTION; SPECTRA AB As part of a spectroscopic survey of supernova remnant candidates in M83 using the Gemini-South telescope and Gemini Multi-Object Spectrograph, we have discovered one object whose spectrum shows very broad lines at H alpha, [OI] lambda lambda 6300, 6363, and [OIII] lambda lambda 4959, 5007, similar to those from other objects classified as "late time supernovae". Although six historical supernovae have been observed in M83 since 1923, none were seen at the location of this object. Hubble Space Telescope (HST) Wide Field Camera 3 images show a nearly unresolved emission source, while Chandra and ATCA data reveal a bright X-ray source and nonthermal radio source at the position. Objects in other galaxies showing similar spectra are only decades post-supernova, which raises the possibility that the supernova that created this object occurred during the last century but was missed. Using photometry of nearby stars from the HST data, we suggest the precursor was at least 17M(circle dot), and the presence of broad Ha in the spectrum makes a type II supernova likely. The supernova must predate the 1983 Very Large Array radio detection of the object. We suggest examination of archival images of M83 to search for evidence of the supernova event that gave rise to this object, and thus provide a precise age. C1 [Blair, William P.; Kuntz, K. D.] Johns Hopkins Univ, Henry A Rowland Dept Phys & Astron, Baltimore, MD 21218 USA. [Winkler, P. Frank] Middlebury Coll, Dept Phys, Middlebury, VT 05753 USA. [Winkler, P. Frank; Dopita, Michael A.] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia. [Long, Knox S.; Whitmore, Bradley C.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Kim, Hwihyun] Korea Astron & Space Sci Inst, Taejon 305438, South Korea. [Soria, Roberto] Curtin Univ, Int Ctr Radio Astron Res, Perth, WA 6845, Australia. [Plucinsky, Paul P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Dopita, Michael A.] King Abdulaziz Univ, Dept Astron, Jeddah 21413, Saudi Arabia. [Stockdale, Christopher] Marquette Univ, Dept Phys, Milwaukee, WI 53201 USA. RP Blair, WP (reprint author), Johns Hopkins Univ, Henry A Rowland Dept Phys & Astron, 3400 North Charles St, Baltimore, MD 21218 USA. EM wpb@pha.jhu.edu; winkler@middlebury.edu; long@stsci.edu; whitmore@stsci.edu; hwihyun@kasi.re.kr; roberto.soria@icrar.org; plucinsky@cfa.harvard.edu; christopher.stockdale@marquette.edu RI Dopita, Michael/P-5413-2014 OI Dopita, Michael/0000-0003-0922-4986 FU STScI grants [ID GO-12513]; National Aeronautics and Space Administration through Chandra [G01-12115]; NASA [NAS8-03060]; Center for Astrophysical Sciences at Johns Hopkins University; National Science Foundation [AST-0908566] FX We thank additional colleagues on the companion multi-wavelength surveys of M83 (Chandra, ATCA, and HST) for useful discussions. W.P.B. and P.F.W. acknowledge travel support from the National Optical Astronomy Observatory, as well as STScI grants under the umbrella program ID GO-12513 to Johns Hopkins University and Middlebury College, respectively. Support was also provided by the National Aeronautics and Space Administration through Chandra grant number G01-12115, issued by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of NASA under contract NAS8-03060. W.P.B. acknowledges support from the Dean of the Krieger School of Arts and Sciences and the Center for Astrophysical Sciences at Johns Hopkins University during this work. P.F.W. acknowledges additional support from the National Science Foundation through grant AST-0908566. NR 39 TC 0 Z9 0 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2015 VL 800 IS 2 AR 118 DI 10.1088/0004-637X/800/2/118 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CB7CA UT WOS:000349782500041 ER PT J AU Bogdan, A Goulding, AD AF Bogdan, Akos Goulding, Andy D. TI CONNECTING DARK MATTER HALOS WITH THE GALAXY CENTER AND THE SUPERMASSIVE BLACK HOLE SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: elliptical and lenticular, cD; galaxies: evolution; galaxies: halos; X-rays: galaxies; X-rays: ISM ID ACTIVE GALACTIC NUCLEI; DIGITAL-SKY-SURVEY; X-RAY BINARIES; STELLAR MASS; HOST GALAXY; FUNDAMENTAL RELATION; LUMINOSITY FUNCTIONS; VELOCITY DISPERSION; ELLIPTIC GALAXIES; SCALING RELATIONS AB Observational studies of nearby galaxies have demonstrated correlations between the mass of the central supermassive black holes (BHs) and properties of the host galaxies, notably the stellar bulge mass or central stellar velocity dispersion. Motivated by these correlations, the theoretical paradigm has emerged in which BHs and bulges coevolve. However, this picture was challenged by observational and theoretical studies, which hinted that the fundamental connection may be between BHs and dark matter halos, and not necessarily with their host galaxies. Based on a study of 3130 elliptical galaxies selected from the Sloan Digital and ROSAT All Sky Surveys we demonstrate that the central stellar velocity dispersion exhibits a significantly tighter correlation with the total gravitating mass, traced by the X-ray luminosity of the hot gas, than with the stellar mass. This hints that the central stellar velocity dispersion, and hence the central gravitational potential, may be the fundamental property of elliptical galaxies that is most tightly connected to the larger-scale dark matter halo. Furthermore, using the central stellar velocity dispersion as a surrogate for the BH mass, we find that in elliptical galaxies the inferred BH mass and inferred total gravitating mass within the virial radius (or within five effective radii) can be expressed as M-BH proportional to M-tot(1.6+0.6) (0.4) (or M-BH proportional to M-5reff(1.8+0.7) (-0.6)). These results are consistent with a picture in which the BH mass is directly set by the central stellar velocity dispersion, which, in turn, is determined by the total gravitating mass of the system. C1 [Bogdan, Akos; Goulding, Andy D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Goulding, Andy D.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. RP Bogdan, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM abogdan@cfa.harvard.edu FU Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy Office of Science; NASA through Einstein Postdoctoral Fellowship - CXC [PF1-120081]; NASA [NAS8-03060, AR3-14016X]; participating institutions FX The authors thank the anonymous referee for excellent and insightful suggestions that have greatly improved the paper and its discussions. The authors thank W. Forman, J. Greene, and R. Hickox for helpful discussions. This research has made use of data, software, and Web tools obtained from the High Energy Astrophysics Science Archive Research Center (HEASARC), a service of the Astrophysics Science Division at NASA/GSFC and of the Smithsonian Astrophysical Observatory's High Energy Astrophysics Division. This work makes use of data from the SDSS-III survey. Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the participating institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. The SDSS-III Web site is http://www.sdss3.org/. A.B. acknowledges support provided by NASA through Einstein Postdoctoral Fellowship grant number PF1-120081 awarded by the CXC, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. A.D.G. acknowledges funding from NASA grant AR3-14016X. NR 58 TC 6 Z9 6 U1 2 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 20 PY 2015 VL 800 IS 2 AR 124 DI 10.1088/0004-637X/800/2/124 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CB7CA UT WOS:000349782500047 ER PT J AU Dressing, CD Charbonneau, D Dumusque, X Gettel, S Pepe, F Cameron, AC Latham, DW Molinari, E Udry, S Affer, L Bonomo, AS Buchhave, LA Cosentino, R Figueira, P Fiorenzano, AFM Harutyunyan, A Haywood, RD Johnson, JA Lopez-Morales, M Lovis, C Malavolta, L Mayor, M Micela, G Motalebi, F Nascimbeni, V Phillips, DF Piotto, G Pollacco, D Queloz, D Rice, K Sasselov, D Segransan, D Sozzetti, A Szentgyorgyi, A Watson, C AF Dressing, Courtney D. Charbonneau, David Dumusque, Xavier Gettel, Sara Pepe, Francesco Cameron, Andrew Collier Latham, David W. Molinari, Emilio Udry, Stephane Affer, Laura Bonomo, Aldo S. Buchhave, Lars A. Cosentino, Rosario Figueira, Pedro Fiorenzano, Aldo F. M. Harutyunyan, Avet Haywood, Raphaelle D. Johnson, John Asher Lopez-Morales, Mercedes Lovis, Christophe Malavolta, Luca Mayor, Michel Micela, Giusi Motalebi, Fatemeh Nascimbeni, Valerio Phillips, David F. Piotto, Giampaolo Pollacco, Don Queloz, Didier Rice, Ken Sasselov, Dimitar Segransan, Damien Sozzetti, Alessandro Szentgyorgyi, Andrew Watson, Chris TI THE MASS OF Kepler-93b AND THE COMPOSITION OF TERRESTRIAL PLANETS SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; planets and satellites: composition; stars: individual (Kepler-93=KOI 69=KIC 3544595); techniques: radial velocities ID 100 EARTH MASSES; SUPER-EARTH; RADIUS RELATIONSHIPS; EXTRASOLAR PLANETS; SOLAR-SYSTEM; STARS; ABUNDANCES; TRANSITS; CATALOG; ORBITS AB Kepler-93b is a 1.478 +/- 0.019 R-circle plus planet with a 4.7 day period around a bright ( V = 10.2), astroseismically characterized host star with a mass of 0.911 +/- 0.033 M-circle dot and a radius of 0.919 +/- 0.011 R-circle dot. Based on 86 radial velocity observations obtained with the HARPS-N spectrograph on the Telescopio Nazionale Galileo and 32 archival Keck/HIRES observations, we present a precise mass estimate of 4.02 +/- 0.68 M-circle plus. The corresponding high density of 6.88 +/- 1.18 g cm(-3) is consistent with a rocky composition of primarily iron and magnesium silicate. We compare Kepler-93b to other dense planets with well-constrained parameters and find that between 1 and 6 M., all dense planets including the Earth and Venus are well-described by the same fixed ratio of iron to magnesium silicate. There are as of yet no examples of such planets with masses > 6 M-circle plus. All known planets in this mass regime have lower densities requiring significant fractions of volatiles or H/He gas. We also constrain the mass and period of the outer companion in the Kepler-93 system from the long-term radial velocity trend and archival adaptive optics images. As the sample of dense planets with well-constrained masses and radii continues to grow, we will be able to test whether the fixed compositional model found for the seven dense planets considered in this paper extends to the full population of 1-6 M-circle plus planets. C1 [Dressing, Courtney D.; Charbonneau, David; Dumusque, Xavier; Gettel, Sara; Latham, David W.; Buchhave, Lars A.; Johnson, John Asher; Lopez-Morales, Mercedes; Phillips, David F.; Sasselov, Dimitar; Szentgyorgyi, Andrew] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Pepe, Francesco; Udry, Stephane; Lovis, Christophe; Motalebi, Fatemeh; Queloz, Didier; Segransan, Damien] Univ Geneva, Astron Observ, CH-1290 Versoix, Switzerland. [Cameron, Andrew Collier; Haywood, Raphaelle D.] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland. [Molinari, Emilio; Cosentino, Rosario; Fiorenzano, Aldo F. M.; Harutyunyan, Avet] INAF Fdn Galileo Galilei, E-38712 Brena Baja, Spain. [Molinari, Emilio] INAF IASF Milano, I-20133 Milan, Italy. [Affer, Laura; Micela, Giusi] INAF Osservatorio Astron Palermo, I-90124 Palermo, Italy. [Bonomo, Aldo S.; Sozzetti, Alessandro] INAF Osservatorio Astrofis Torino, I-10025 Pino Torinese, Italy. [Buchhave, Lars A.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark. [Figueira, Pedro] Univ Porto, Ctr Astrofis, P-4150762 Oporto, Portugal. [Figueira, Pedro] Univ Porto, CAUP, Inst Astrofis & Ciencias Espaco, PT-4150762 Oporto, Portugal. [Malavolta, Luca; Piotto, Giampaolo] Univ Padua, Dipartimento Fis & Astron Galileo Galilei, I-35122 Padua, Italy. [Malavolta, Luca; Nascimbeni, Valerio; Piotto, Giampaolo] INAF Osservatorio Astron Padova, I-35122 Padua, Italy. [Pollacco, Don] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Queloz, Didier] Univ Cambridge, Cavendish Lab, Cambridge CB3 0HE, England. [Rice, Ken] Univ Edinburgh, Inst Astron, Royal Observ, SUPA, Edinburgh EH9 3HJ, Midlothian, Scotland. [Watson, Chris] Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland. RP Dressing, CD (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM cdressing@cfa.harvard.edu RI Figueira, Pedro/J-4916-2013; Rice, Ken/H-5084-2011; OI Piotto, Giampaolo/0000-0002-9937-6387; Figueira, Pedro/0000-0001-8504-283X; Rice, Ken/0000-0002-6379-9185; Micela, Giuseppina/0000-0002-9900-4751; Molinari, Emilio/0000-0002-1742-7735; Sozzetti, Alessandro/0000-0002-7504-365X; Cameron, Andrew/0000-0002-8863-7828; Buchhave, Lars A./0000-0003-1605-5666 FU Prodex Program of the Swiss Space Office (SSO); Harvard University Origin of Life Initiative (HUOLI); Scottish Universities Physics Alliance (SUPA); University of Geneva; Smithsonian Astrophysical Observatory (SAO); Italian National Astrophysical Institute (INAF); University of St. Andrews; Queen's University Belfast; University of Edinburgh; European Union Seventh Framework Programme (FP7) [313014]; National Science Foundation Graduate Research Fellowship; Swiss National Science Foundation (SNSF); Fundacao para a Ciencia e a Tecnologia (FCT) through Investigador FCT [IF/01037/2013]; FEDER funding through the program "Programa Operacional de Factores de Competitividade - COMPETE"; John Templeton Foundation FX The HARPS-N project was funded by the Prodex Program of the Swiss Space Office (SSO), the Harvard University Origin of Life Initiative (HUOLI), the Scottish Universities Physics Alliance (SUPA), the University of Geneva, the Smithsonian Astrophysical Observatory (SAO), and the Italian National Astrophysical Institute (INAF), University of St. Andrews, Queen's University Belfast, and University of Edinburgh. The research leading to these results has received funding from the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement No. 313014 (ETAEARTH). C.D. is supported by a National Science Foundation Graduate Research Fellowship. X.D. would like to thank the Swiss National Science Foundation (SNSF) for its support through an Early Postdoc Mobility fellowship. P.F. acknowledges support by Fundacao para a Ciencia e a Tecnologia (FCT) through Investigador FCT contracts of reference IF/01037/2013 and POPH/FSE (EC) by FEDER funding through the program "Programa Operacional de Factores de Competitividade - COMPETE." This publication was made possible through the support of a grant from the John Templeton Foundation. The opinions expressed in this publication are those of the authors and do not necessarily reflect the views of the John Templeton Foundation. NR 57 TC 53 Z9 53 U1 1 U2 12 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2015 VL 800 IS 2 AR 135 DI 10.1088/0004-637X/800/2/135 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CB7CA UT WOS:000349782500058 ER PT J AU Landi, E Testa, P AF Landi, E. Testa, P. TI NEON AND OXYGEN ABUNDANCES AND ABUNDANCE RATIO IN THE SOLAR CORONA SO ASTROPHYSICAL JOURNAL LA English DT Article DE solar wind; Sun: abundances; Sun: corona; Sun: evolution; Sun: UV radiation ID ION COMPOSITION SPECTROMETER; NON-WKB MODELS; B-TYPE STARS; CHEMICAL-COMPOSITION; HELIUM ABUNDANCE; SUMER TELESCOPE; ATOMIC DATABASE; EMISSION-LINES; NE/O ABUNDANCE; WIND AB In this work we determine the Ne/O abundance ratio from Solar and Heliospheric Observatory (SOHO)/Solar Ultraviolet Measurement of Emitted Radiation (SUMER) off-disk observations of quiescent streamers over the 1996-2008 period. We find that the Ne/O ratio is approximately constant over solar cycle 23 from 1996 to 2005, at a value of 0.099 +/- 0.017; this value is lower than the transition region determinations from the quiet Sun used to infer the neon photospheric abundance from the oxygen photospheric abundance. Also, the Ne/O ratio we determined from SUMER is in excellent agreement with in situ determinations from ACE/SWICS. In 2005-2008, the Ne/O abundance ratio increased with time and reached 0.25 +/- 0.05, following the same trend found in the slowest wind analyzed by ACE/SWICS. Further, we measure the absolute abundance in the corona for both oxygen and neon from the data set of 1996 November 22, obtaining A(o) = 8.99 +/- 0.04 and A(Ne) = 7.92 +/- 0.03, and we find that both elements are affected by the first ionization potential (FIP) effect, with oxygen being enhanced by a factor of 1.4-2.1 over its photospheric abundance, and neon being changed by a factor of 0.75 +/- 1.20. We conclude that the Ne/O ratio is not constant in the solar atmosphere, both in time and at different heights, and that it cannot be reliably used to infer the neon abundance in the photosphere. Also, we argue that the FIP effect was less effective during the minimum of solar cycle 24, and that the Ne/O = 0.25 +/- 0.05 value measured at that time is closer to the true photospheric value, leading to a neon photospheric abundance larger than assumed by approximate to 40%. We discuss the implications of these results for the solar abundance problem, for the FIP effect, and for the identification of the source regions of the solar wind. C1 [Landi, E.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Testa, P.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Landi, E (reprint author), Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. EM elandi@umich.edu FU NASA [NNX11AC20G, NNX10AF29G] FX The work of E.L. was supported by NASA grant NNX11AC20G; the work of P.T. is supported by NASA grants NNX11AC20G and NNX10AF29G. The authors warmly thank Klaus Wilhelm, Werner Curdt, and Udo Schuhle for their assistance in the evaluation of the uncertainties in SUMER line intensity ratios and Paul Shearer for sharing the Ne/O data from ACE/SWICS. The authors also warmly thank the referee, Katharina Lodders, for her comments that helped us to clarify and improve the paper. NR 65 TC 5 Z9 5 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2015 VL 800 IS 2 AR 110 DI 10.1088/0004-637X/800/2/110 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CB7CA UT WOS:000349782500033 ER PT J AU Lee, GH Hwang, HS Lee, MG Ko, J Sohn, J Shim, H Diaferio, A AF Lee, Gwang-Ho Hwang, Ho Seong Lee, Myung Gyoon Ko, Jongwan Sohn, Jubee Shim, Hyunjin Diaferio, Antonaldo TI GALAXY EVOLUTION IN THE MID-INFRARED GREEN VALLEY: A CASE OF THE A2199 SUPERCLUSTER SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: individual (A2199); galaxies: evolution; galaxies: groups: general infrared: galaxies ID DIGITAL SKY SURVEY; STAR-FORMING GALAXIES; SIMILAR-TO 1; INFRARED LUMINOSITY FUNCTION; ACTIVE GALACTIC NUCLEI; PANORAMIC H-ALPHA; MASS PROFILES; ENVIRONMENTAL DEPENDENCE; ELLIPTIC GALAXIES; FORMATION RATES AB We study the mid-infrared (MIR) properties of the galaxies in the A2199 supercluster at z = 0.03 to understand the star formation activity of galaxy groups and clusters in the supercluster environment. Using the Wide-field Infrared Survey Explorer data, we find no dependence of mass-normalized integrated star formation rates of galaxy groups/ clusters on their virial masses. We classify the supercluster galaxies into three classes in the MIR color-luminosity diagram: MIR blue cloud (massive, quiescent, and mostly early-type), MIR star-forming sequence (mostly latetype), and MIR green valley galaxies. These MIR green valley galaxies are distinguishable from the optical green valley galaxies in the sense that they belong to the optical red sequence. We find that the fraction of each MIR class does not depend on the virial mass of each group/cluster. We compare the cumulative distributions of surface galaxy number density and cluster/group-centric distance for the three MIR classes. MIR green valley galaxies show the distribution between MIR blue cloud and MIR star-forming (SF) sequence galaxies. However, if we fix galaxy morphology, early-and late-type MIR green valley galaxies show different distributions. Our results suggest a possible evolutionary scenario of these galaxies: (1) late-type MIR SF sequence galaxies. (2) late-type MIR green valley galaxies. (3) early-type MIR green valley galaxies. (4) early-type MIR blue cloud galaxies. In this sequence, the star formation of galaxies is quenched before the galaxies enter the MIR green valley, and then morphological transformation occurs in the MIR green valley. C1 [Lee, Gwang-Ho; Lee, Myung Gyoon; Sohn, Jubee] Seoul Natl Univ, Dept Phys & Astron, Seoul 151742, South Korea. [Hwang, Ho Seong] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Hwang, Ho Seong] Korea Inst Adv Study, Sch Phys, Seoul 130722, South Korea. [Ko, Jongwan] Korea Astron & Space Sci Inst, Taejon 305348, South Korea. [Shim, Hyunjin] Kyungpook Natl Univ, Dept Earth Sci Educ, Taegu, South Korea. [Diaferio, Antonaldo] Univ Turin, Dipartimento Fis, Turin, Italy. [Diaferio, Antonaldo] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy. RP Lee, GH (reprint author), Seoul Natl Univ, Dept Phys & Astron, 1 Gwanak Ro, Seoul 151742, South Korea. EM ghlee@astro.snu.ac.kr; mglee@astro.snu.ac.kr FU National Research Foundation of Korea (NRF) Grant - Korean Government (NRF-Fostering Core Leaders of the Future Basic Science Program); NRF grant - Korea Government (MEST) [2012R1A4A1028713]; Smithsonian Institution; Global Ph.D. Fellowship Program through an NRF - MEST [2011-0007215] FX We thank Margaret Geller for many helpful discussions. G.H.L. acknowledges the support by the National Research Foundation of Korea (NRF) Grant funded by the Korean Government (NRF-2012-Fostering Core Leaders of the Future Basic Science Program). M.G.L was supported by the NRF grant funded by the Korea Government (MEST; No. 2012R1A4A1028713). H.S.H. acknowledges the Smithsonian Institution for the support of his post-doctoral fellowship. J.S. was supported by the Global Ph.D. Fellowship Program through an NRF funded by the MEST (No. 2011-0007215). H.S. is supported by the Basic Science Research Program through the National Research Foundation of Korea (NRF) funded by the Ministry of Science, ICT & Future Planning (2014R1A1A1038088). A.D. acknowledges partial support from the INFN grant In-Dark and from the grant Progetti di Ateneo/CSP TO Call2 2012 0011 "Marco Polo" of the University of Torino. This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the U.S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSS Web site is http://www.sdss.org/. The SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions. The Participating Institutions are the American Museum of Natural History, Astrophysical Institute Potsdam, University of Basel, 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 (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, Ohio State University, University of Pittsburgh, University of Portsmouth, Princeton University, the United States Naval Observatory, and the University of Washington. NR 117 TC 6 Z9 6 U1 3 U2 12 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2015 VL 800 IS 2 AR 80 DI 10.1088/0004-637X/800/2/80 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CB7CA UT WOS:000349782500003 ER PT J AU Madsen, CA Tian, H DeLuca, EE AF Madsen, Chad A. Tian, Hui DeLuca, Edward E. TI OBSERVATIONS OF UMBRAL FLASHES AND RUNNING SUNSPOT WAVES WITH THE INTERFACE REGION IMAGING SPECTROGRAPH SO ASTROPHYSICAL JOURNAL LA English DT Article DE magnetohydrodynamics (MHD); plasmas; Sun: chromosphere; Sun: oscillations; Sun: transition region; Sun: UV radiation; waves ID HIGH-RESOLUTION OBSERVATIONS; PENUMBRAL WAVES; TRANSITION REGION; PROPAGATING WAVES; DYNAMIC FIBRILS; OSCILLATIONS; CHROMOSPHERE; ASSOCIATION; CORONA; SDO AB We present simultaneous, high-resolution, multi-temperature observations of running waves and umbral flashes in a sunspot with the Interface Region Imaging Spectrograph. We analyze intensity variations in slit-jaw images to investigate the relationship between running waves in the 1400 angstrom (Si IV/transition region) passband and umbral flashes in the 2796 angstrom (Mg II/chromosphere) passband. Using global wavelet analysis, we find that the dominant wave periods increase from approximately 150 s near the sunspot center to about 300 s in the penumbra in both passbands. This coincides extremely well with the radially increasing inclination of magnetic field lines observed with Solar Dynamics Observatory/Helioseismic and Magnetic Imager, suggesting that the waves are propagating vertically along the inclined field lines. Furthermore, apparent horizontal velocities for running waves decrease from about 12 km s(-1) in the umbra to about 4 kms(-1) in the penumbra which is predicted by the same inclined field geometry. Finally, we find that umbral flashes lead running waves in both the spatial and temporal domains. The former result is attributable to the inclined field geometry; however, the geometry does not predict the radially increasing time lag which is likely due to the opacity difference between the emission lines that dominate the two passbands. These results suggest that running waves and umbral flashes both originate from photospheric p-mode oscillations and are manifestations of upward-propagating slow magnetoacoustic modes at different altitudes and temperatures. The apparent trans-sunspot propagation of running waves is not real but rather an image of these upward-propagating modes traveling along field lines of radially increasing inclination. C1 [Madsen, Chad A.; Tian, Hui; DeLuca, Edward E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Madsen, Chad A.] Boston Univ, Ctr Space Phys, Boston, MA 02215 USA. RP Madsen, CA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM cmadsen@cfa.harvard.edu RI DeLuca, Edward/L-7534-2013 OI DeLuca, Edward/0000-0001-7416-2895 FU Norwegian Space Center (NSC, Norway) through an ESA PRODEX contract; LMSAL [8100002705, SP02J1701R] FX The authors thank Bernhard Fleck for helpful discussions. IRIS is a NASA small explorer mission developed and operated by Lockheed-Martin Solar and Astrophysics Laboratory (LMSAL) with mission operations executed at NASA Ames Research center and major contributions to downlink communications funded by the Norwegian Space Center (NSC, Norway) through an ESA PRODEX contract. This work is supported by contracts 8100002705 and SP02J1701R from LMSAL to Smithsonian Astrophysical Observatory (SAO). NR 46 TC 10 Z9 10 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2015 VL 800 IS 2 AR 129 DI 10.1088/0004-637X/800/2/129 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CB7CA UT WOS:000349782500052 ER PT J AU Montet, BT Johnson, JA Muirhead, PS Villar, A Vassallo, C Baranec, C Law, NM Riddle, R Marcy, GW Howard, AW Isaacson, H AF Montet, Benjamin T. Johnson, John Asher Muirhead, Philip S. Villar, Ashley Vassallo, Corinne Baranec, Christoph Law, Nicholas M. Riddle, Reed Marcy, Geoffrey W. Howard, Andrew W. Isaacson, Howard TI CHARACTERIZING THE COOL KOIs. VII. REFINED PHYSICAL PROPERTIES OF THE TRANSITING BROWN DWARF LHS 6343 C SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: general; brown dwarfs; stars: fundamental parameters; stars: individual (KIC 10002261); stars: late-type; stars: low-mass ID EXTRASOLAR GIANT PLANETS; JUPITER-MASS COMPANION; LASER ADAPTIVE OPTICS; KEPLER LIGHT-CURVE; K-BAND SPECTRA; ELLIPSOIDAL VARIATIONS; SOPHIE VELOCIMETRY; RADIAL-VELOCITY; SUBSTELLAR COMPANION; ECLIPSING BINARY AB We present an updated analysis of LHS 6343, a triple system in the Kepler field which consists of a brown dwarf transiting one member of a widely separated M+M binary system. By analyzing the full Kepler data set and 34 Keck/HIgh Resolution Echelle Spectrometer radial velocity observations, we measure both the observed transit depth and Doppler semiamplitude to 0.5% precision. With Robo-AO and Palomar/PHARO adaptive optics imaging as well as TripleSpec spectroscopy, we measure a model-dependent mass for LHS 6343 C of 62.1 +/- 1.2 M-Jup and a radius of 0.783 +/- 0.011 R-Jup. We detect the secondary eclipse in the Kepler data at 3.5 sigma, measuring e cos omega = 0.0228 +/- 0.0008. We also derive a method to measure the mass and radius of a star and transiting companion directly, without any direct reliance on stellar models. The mass and radius of both objects depend only on the orbital period, stellar density, reduced semimajor axis, Doppler semiamplitude, eccentricity, and inclination, as well as the knowledge that the primary star falls on the main sequence. With this method, we calculate a mass and radius for LHS 6343 C to a precision of 3% and 2%, respectively. C1 [Montet, Benjamin T.; Howard, Andrew W.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91106 USA. [Montet, Benjamin T.; Johnson, John Asher; Villar, Ashley] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Muirhead, Philip S.] Boston Univ, Dept Astron, Boston, MA 02215 USA. [Vassallo, Corinne] Univ Texas Austin, Dept Aerosp Engn & Engn Mech, Austin, TX 78712 USA. [Baranec, Christoph] Univ Hawaii Manoa, Inst Astron, Hilo, HI 96720 USA. [Law, Nicholas M.] Univ N Carolina, Dept Phys & Astron, Chapel Hill, NC 27599 USA. [Marcy, Geoffrey W.; Isaacson, Howard] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Howard, Andrew W.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. RP Montet, BT (reprint author), CALTECH, Cahill Ctr Astron & Astrophys, 1200 E Calif Blvd,MC 249-17, Pasadena, CA 91106 USA. EM btm@astro.caltech.edu RI Howard, Andrew/D-4148-2015; Muirhead, Philip/H-2273-2014; OI Howard, Andrew/0000-0001-8638-0320; Muirhead, Philip/0000-0002-0638-8822; Montet, Benjamin/0000-0001-7516-8308 FU W. M. Keck Foundation; Association of Universities for Research in Astronomy, Inc., under NASA [NAS5-26555]; NASA Office of Space Science [NNX13AC07G]; NASA Science Mission directorate; National Science Foundation Graduate Research Fellowship [DGE1144469]; David and Lucile Packard Foundation; Alfred P. Sloan Foundation; California Institute of Technology; Inter-University Centre for Astronomy and Astrophysics; National Science Foundation [AST-0906060, AST-0960343, AST-1207891]; Mount Cuba Astronomical Foundation FX The RV data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. We are grateful to the entire Kepler team, past and present. Their tireless efforts were all essential to the tremendous success of the mission and the future successes of K2.; Some of the data presented in this paper were obtained from the Mikulski Archive for Space Telescopes ( MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant NNX13AC07G and by other grants and contracts. This paper includes data collected by the Kepler mission. Funding for the Kepler mission is provided by the NASA Science Mission directorate.; B.T.M. is supported by the National Science Foundation Graduate Research Fellowship under grant No. DGE1144469. J.A.J. is supported by generous grants from the David and Lucile Packard Foundation and the Alfred P. Sloan Foundation. C.B. acknowledges support from the Alfred P. Sloan Foundation. The Robo-AO system is supported by collaborating partner institutions, the California Institute of Technology and the Inter-University Centre for Astronomy and Astrophysics, and by the National Science Foundation under grant Nos. AST-0906060, AST-0960343, and AST-1207891, by the Mount Cuba Astronomical Foundation, by a gift from Samuel Oschin. NR 67 TC 13 Z9 13 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2015 VL 800 IS 2 AR 134 DI 10.1088/0004-637X/800/2/134 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CB7CA UT WOS:000349782500057 ER PT J AU Newton, ER Charbonneau, D Irwin, J Mann, AW AF Newton, Elisabeth R. Charbonneau, David Irwin, Jonathan Mann, Andrew W. TI AN EMPIRICAL CALIBRATION TO ESTIMATE COOL DWARF FUNDAMENTAL PARAMETERS FROM H-BAND SPECTRA SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars: atmospheres; binaries: general; stars: fundamental parameters; stars: low-mass Supporting material: machine-readable tables ID LOW-MASS STARS; STELLAR EFFECTIVE TEMPERATURES; INFRARED FLUX METHOD; NEARBY M DWARFS; ANGULAR DIAMETERS; MAIN-SEQUENCE; SOLAR NEIGHBORHOOD; ECLIPSING BINARIES; CANDIDATE PLANETS; TRANSIT DETECTION AB Interferometric radius measurements provide a direct probe of the fundamental parameters of M dwarfs. However, interferometry is within reach for only a limited sample of nearby, bright stars. We use interferometrically measured radii, bolometric luminosities, and effective temperatures to develop new empirical calibrations based on low-resolution, near-infrared spectra. We find that H-band Mg and Al spectral features are good tracers of stellar properties, and derive functions that relate effective temperature, radius, and log luminosity to these features. The standard deviations in the residuals of our best fits are, respectively, 73 K, 0.027R(circle dot), and 0.049 dex (an 11% error on luminosity). Our calibrations are valid from mid K to midMdwarf stars, roughly corresponding to temperatures between 3100 and 4800 K. We apply our H-band relationships to M dwarfs targeted by the MEarth transiting planet survey and to the cool Kepler Objects of Interest (KOIs). We present spectral measurements and estimated stellar parameters for these stars. Parallaxes are also available for many of the MEarth targets, allowing us to independently validate our calibrations by demonstrating a clear relationship between our inferred parameters and the stars' absolute K magnitudes. We identify objects with magnitudes that are too bright for their inferred luminosities as candidate multiple systems. We also use our estimated luminosities to address the applicability of near-infrared metallicity calibrations to mid and late M dwarfs. The temperatures we infer for the KOIs agree remarkably well with those from the literature; however, our stellar radii are systematically larger than those presented in previous works that derive radii from model isochrones. This results in a mean planet radius that is 15% larger than one would infer using the stellar properties from recent catalogs. Our results confirm the derived parameters from previous in-depth studies of KOIs 961 (Kepler-42), 254 (Kepler-45), and 571 (Kepler-186), the latter of which hosts a rocky planet orbiting in its star's habitable zone. C1 [Newton, Elisabeth R.; Charbonneau, David; Irwin, Jonathan] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Mann, Andrew W.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. RP Newton, ER (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM enewton@cfa.harvard.edu OI Newton, Elisabeth/0000-0003-4150-841X FU National Science Foundation Graduate Research Fellowship; University of Texas at Austin; David and Lucille Packard Fellowship for Science and Engineering; National Science Foundation [AST-0807690, AST-1109468, AST-1004488]; John Templeton Foundation; NASA; NSF, NASAs Astrophysics Data System (ADS); SIMBAD database, operated at CDS, Strasbourg, France FX E.R.N. was supported throughout this work by a National Science Foundation Graduate Research Fellowship and A.W.M. by the Harlan J. Smith Fellowship from the University of Texas at Austin. The MEarth Team gratefully acknowledges funding from the David and Lucille Packard Fellowship for Science and Engineering (awarded to D.C.). This material is based upon work supported by the National Science Foundation under grants AST-0807690, AST-1109468, and AST-1004488 (Alan T. Waterman Award). This publication was made possible through the support of a grant from the John Templeton Foundation. The opinions expressed in this publication are those of the authors and do not necessarily reflect the views of the John Templeton Foundation. We thank Z. Berta-Thomspon, J. Dittmann, and P. Muirhead for helpful conversations and the anonymous referee for comments and suggestions that improved the paper. This work used observations from the Infrared Telescope Facility, which is operated by the University of Hawaii under Cooperative Agreement No. NNX-08AE38A with the National Aeronautics and Space Administration, Science Mission Directorate, Planetary Astronomy Program. This research has made extensive use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by NASA and the NSF, NASAs Astrophysics Data System (ADS), and the SIMBAD database, operated at CDS, Strasbourg, France. NR 77 TC 28 Z9 28 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2015 VL 800 IS 2 AR 85 DI 10.1088/0004-637X/800/2/85 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CB7CA UT WOS:000349782500008 ER PT J AU Ngo, H Knutson, HA Hinkley, S Crepp, JR Bechter, EB Batygin, K Howard, AW Johnson, JA Morton, TD Muirhead, PS AF Ngo, Henry Knutson, Heather A. Hinkley, Sasha Crepp, Justin R. Bechter, Eric B. Batygin, Konstantin Howard, Andrew W. Johnson, John A. Morton, Timothy D. Muirhead, Philip S. TI FRIENDS OF HOT JUPITERS. II. NO CORRESPONDENCE BETWEEN HOT-JUPITER SPIN-ORBIT MISALIGNMENT AND THE INCIDENCE OF DIRECTLY IMAGED STELLAR COMPANIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: close; binaries: eclipsing; methods: observational; planetary systems; planets and satellites: dynamical evolution and stability; techniques: high angular resolution ID SOLAR-TYPE STARS; PLANET-HOST STARS; GAS-GIANT PLANET; ROSSITER-MCLAUGHLIN OBSERVATIONS; TRANSITING EXTRASOLAR PLANET; HIERARCHICAL 3-BODY SYSTEMS; HIGH-PRECISION PHOTOMETRY; COLOR-MAGNITUDE DIAGRAMS; INTERNAL GRAVITY-WAVES; ECCENTRIC ORBIT AB Multi-star systems are common, yet little is known about a stellar companion's influence on the formation and evolution of planetary systems. For instance, stellar companions may have facilitated the inward migration of hot Jupiters toward to their present day positions. Many observed short-period gas giant planets also have orbits that are misaligned with respect to their star's spin axis, which has also been attributed to the presence of a massive outer companion on a non-coplanar orbit. We present the results of a multi-band direct imaging survey using Keck NIRC2 to measure the fraction of short-period gas giant planets found in multi-star systems. Over three years, we completed a survey of 50 targets ("Friends of Hot Jupiters") with 27 targets showing some signature of multi-body interaction (misaligned or eccentric orbits) and 23 targets in a control sample (well-aligned and circular orbits). We report the masses, projected separations, and confirmed common proper motion for the 19 stellar companions found around 17 stars. Correcting for survey incompleteness, we report companion fractions of 48% +/- 9%, 47% +/- 12%, and 51% +/- 13% in our total, misaligned/eccentric, and control samples, respectively. This total stellar companion fraction is 2.8s larger than the fraction of field stars with companions approximately 50-2000AU. We observe no correlation between misaligned/eccentric hot Jupiter systems and the incidence of stellar companions. Combining this result with our previous radial velocity survey, we determine that 72% +/- 16% of hot Jupiters are part of multi-planet and/or multi-star systems. C1 [Ngo, Henry; Knutson, Heather A.; Hinkley, Sasha; Batygin, Konstantin] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Hinkley, Sasha] Univ Exeter, Dept Phys & Astron, Exeter, Devon, England. [Crepp, Justin R.; Bechter, Eric B.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. [Howard, Andrew W.] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. [Johnson, John A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Morton, Timothy D.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Muirhead, Philip S.] Boston Univ, Dept Astron, Boston, MA 02215 USA. RP Ngo, H (reprint author), CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. EM hngo@caltech.edu RI Howard, Andrew/D-4148-2015; Muirhead, Philip/H-2273-2014; OI Howard, Andrew/0000-0001-8638-0320; Muirhead, Philip/0000-0002-0638-8822; Ngo, Henry/0000-0001-5172-4859 FU NASA [NNX14AD24G]; Natural Sciences and Engineering Research Council of Canada; David & Lucile Packard foundation; Alfred P. Sloan foundation FX This work was supported by NASA grant NNX14AD24G. H.N. is grateful for funding support from the Natural Sciences and Engineering Research Council of Canada. J.A.J. gratefully acknowledges support from generous fellowships from the David & Lucile Packard and Alfred P. Sloan foundations. We also thank Brendan Bowler for assistance with our common proper motion analysis and Rebekah Dawson and Cristobal Petrovich for helpful discussions. NR 157 TC 45 Z9 45 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2015 VL 800 IS 2 AR 138 DI 10.1088/0004-637X/800/2/138 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CB7CA UT WOS:000349782500061 ER PT J AU Nynka, M Hailey, CJ Zhang, S Morris, MM Zhao, JH Goss, M Bauer, FE Boggs, SE Craig, WW Christensen, FE Gotthelf, EV Harrison, FA Mori, K Perez, KM Stern, D Zhang, WW AF Nynka, Melania Hailey, Charles J. Zhang, Shuo Morris, Mark M. Zhao, Jun-Hui Goss, Miller Bauer, Franz E. Boggs, Stephen E. Craig, William W. Christensen, Finn E. Gotthelf, Eric V. Harrison, Fiona A. Mori, Kaya Perez, Kerstin M. Stern, Daniel Zhang, William W. TI G359.97-0.038: A HARD X-RAY FILAMENT ASSOCIATED WITH A SUPERNOVA SHELL-MOLECULAR CLOUD INTERACTION SO ASTROPHYSICAL JOURNAL LA English DT Article DE Galaxy: center ID SAGITTARIUS-A-EAST; PULSAR-WIND NEBULAE; LARGE ARRAY OBSERVATIONS; GALACTIC-CENTER REGION; HIGH-ENERGY EMISSION; 1720 MHZ MASERS; NONTHERMAL EMISSION; CIRCUMNUCLEAR DISK; SOURCE CATALOG; COSMIC-RAYS AB We present the first high-energy X-ray (>10 keV) observations of the non-thermal filament G359.97-0.038 using the Nuclear Spectroscopic Telescope Array (NuSTAR). This filament is one of approximately 20 X-ray filaments of unknown origin located in the central 20 pc region in the Galactic Center near Sgr A*. Its NuSTAR and Chandra broadband spectrum is characterized by a single power law with Gamma = 1.3 +/- 0.3 that extends from 2 to 50 keV, with an unabsorbed luminosity of 1.3 x 10(33) erg s(-1) (d/8 kpc)(2) in the 2-8 keV band. Despite possessing a cometary X-ray morphology that is typical of a pulsar wind nebula (PWN) in high-resolution Chandra imaging, our spatially resolved Chandra spectral analysis found no significant spectral softening along the filament as would be expected from particle synchrotron cooling. Coincident radio emission is detected using the Very Large Array at 5.5 and 8.3 GHz. We examine and subsequently discard a PWN or magnetic flux tube as the origin of G359.97-0.038. We use broadband spectral characteristics and a morphological analysis to show that G359.97-0.038 is likely an interaction site between the shell of Sgr A East and an adjacent molecular cloud. This is supported by CS molecular line spectroscopy and the presence of an OH maser. C1 [Nynka, Melania; Hailey, Charles J.; Zhang, Shuo; Gotthelf, Eric V.; Mori, Kaya; Perez, Kerstin M.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Morris, Mark M.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Zhao, Jun-Hui] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Goss, Miller] NRAO, Socorro, NM 87801 USA. [Bauer, Franz E.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Santiago 22, Chile. [Bauer, Franz E.] Millennium Inst Astrophys, Santiago, Chile. [Bauer, Franz E.] Space Sci Inst, Boulder, CO 80301 USA. [Boggs, Stephen E.; Craig, William W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Craig, William W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Christensen, Finn E.] Tech Univ Denmark, DTU Space Natl Space Inst, DK-2800 Lyngby, Denmark. [Harrison, Fiona A.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Zhang, William W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Nynka, M (reprint author), Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. RI Boggs, Steven/E-4170-2015 OI Boggs, Steven/0000-0001-9567-4224 FU NASA [NNG08FD60C]; National Aeronautics and Space Administration; CONICYT-Chile [Basal-CATA PFB-06/2007, FONDECYT 1141218, "EMBIGGEN" Anillo ACT1101]; Iniciativa Cientifica Milenio del Ministerio de Economia, Fomento y Turismo [IC120009] FX This work was supported under NASA contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. F.E.B. acknowledges support from CONICYT-Chile (Basal-CATA PFB-06/2007, FONDECYT 1141218, "EMBIGGEN" Anillo ACT1101), and Project IC120009 "Millennium Institute of Astrophysics (MAS)" funded by the Iniciativa Cientifica Milenio del Ministerio de Economia, Fomento y Turismo. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTAR-DAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). NR 54 TC 4 Z9 4 U1 1 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2015 VL 800 IS 2 AR 119 DI 10.1088/0004-637X/800/2/119 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CB7CA UT WOS:000349782500042 ER PT J AU Piso, AMA Youdin, AN Murray-Clay, RA AF Piso, Ana-Maria A. Youdin, Andrew N. Murray-Clay, Ruth A. TI MINIMUM CORE MASSES FOR GIANT PLANET FORMATION WITH REALISTIC EQUATIONS OF STATE AND OPACITIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE planets and satellites: atmospheres; planets and satellites: formation; planets and satellites: gaseous planets ID STELLAR ASTROPHYSICS MESA; ORTHO-PARA CONVERSION; PROTOPLANETARY DISKS; PROTOSTELLAR DISKS; GRAIN OPACITY; OF-STATE; CIRCUMSTELLAR DISKS; EXTRASOLAR PLANETS; MOLECULAR-HYDROGEN; GASEOUS ENVELOPE AB Giant planet formation by core accretion requires a core that is sufficiently massive to trigger runaway gas accretion in less than the typical lifetime of protoplanetary disks. We explore how the minimum required core mass, Mcrit, depends on a non-ideal equation of state (EOS) and on opacity changes due to grain growth across a range of stellocentric distances from 5-100AU. This minimum M-crit applies when planetesimal accretion does not substantially heat the atmosphere. Compared to an ideal gas polytrope, the inclusion of molecular hydrogen (H-2) dissociation and variable occupation of H-2 rotational states increases M-crit. Specifically, M-crit increases by a factor of similar to 2 if the H-2 spin isomers, ortho-and parahydrogen, are in thermal equilibrium, and by a factor of similar to 2-4 if the ortho-to-para ratio is fixed at 3: 1. Lower opacities due to grain growth reduce M-crit. For a standard disk model around a Solar mass star, we calculate M-crit similar to 8M(circle plus) at 5 Lambda U, decreasing to similar to 5M(circle plus) at 100AU, for a realistic EOS with an equilibrium ortho-to-para ratio and for grain growth to centimeter-sizes. If grain coagulation is taken into account, M-crit may further reduce by up to one order of magnitude. These results for the minimum critical core mass are useful for the interpretation of surveys that find exoplanets at a range of orbital distances. C1 [Piso, Ana-Maria A.; Murray-Clay, Ruth A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Youdin, Andrew N.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Murray-Clay, Ruth A.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. RP Piso, AMA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM apiso@cfa.harvard.edu FU NASA Astrophysics Theory Program; Origins of Solar Systems Program [NNX10AF35G]; Brinson Foundation FX We thank the referee for a helpful report. We thank Sean Andrews for providing us with the D'Alessio et al. (2001) opacity tables. We also thank Phil Arras, Eugene Chiang, and Steven Cranmer for useful conversations. A.N.Y. acknowledges support from NASA Astrophysics Theory Program and Origins of Solar Systems Program through grant NNX10AF35G. A.P. and R.M.C. acknowledge support from the Brinson Foundation. NR 69 TC 10 Z9 10 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2015 VL 800 IS 2 AR 82 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CB7CA UT WOS:000349782500005 ER PT J AU Ptak, A Hornschemeier, A Zezas, A Lehmer, B Yukita, M Wik, D Antoniou, V Argo, MK Ballo, L Bechtol, K Boggs, S Della Ceca, R Christensen, FE Craig, WW Hailey, CJ Harrison, FA Krivonos, R Maccarone, TJ Stern, D Tatum, M Venters, T Zhang, WW AF Ptak, A. Hornschemeier, A. Zezas, A. Lehmer, B. Yukita, M. Wik, D. Antoniou, V. Argo, M. K. Ballo, L. Bechtol, K. Boggs, S. Della Ceca, R. Christensen, F. E. Craig, W. W. Hailey, C. J. Harrison, F. A. Krivonos, R. Maccarone, T. J. Stern, D. Tatum, M. Venters, T. Zhang, W. W. TI A FOCUSED, HARD X-RAY LOOK AT ARP 299 WITH NuSTAR SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: individual (Arp 299); galaxies: starburst; X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; SUPERMASSIVE BLACK-HOLES; INFRARED GALAXIES; NGC 253; EMISSION; CHANDRA; MODEL; CONSTRAINTS; STARBURSTS; DISCOVERY AB We report on simultaneous observations of the local starburst system Arp 299 with NuSTAR and Chandra, which provides the first resolved images of this galaxy up to energies of similar to 45 keV. Fitting the 3-40 keV spectrum reveals a column density of N-H similar to 4 x 10(24) cm(-2), characteristic of a Compton-thick active galactic nucleus (AGN), and a 10-30 keV luminosity of 1.2 x 1043 erg s(-1). The hard X-rays detected by NuSTAR above 10 keV are centered on the western nucleus, Arp 299-B, which previous X-ray observations have shown to be the primary source of neutral Fe-K emission. Other X-ray sources, including Arp 299-A, the eastern nucleus also thought to harbor an AGN, as well as X-ray binaries, contribute less than or similar to 10% to the 10-20 keV emission from the Arp 299 system. The lack of significant emission above 10 keV other than that attributed to Arp 299-B suggests that: (1) any AGN in Arp 299-A must be heavily obscured (N-H > 10(24) cm(-2)) or have a much lower luminosity than Arp 299-B and (2) the extranuclear X-ray binaries have spectra that cut-off above similar to 10 keV. Such soft spectra are characteristic of ultraluminous X-ray sources observed to date by NuSTAR. C1 [Ptak, A.; Hornschemeier, A.; Lehmer, B.; Yukita, M.; Wik, D.; Tatum, M.; Venters, T.; Zhang, W. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Ptak, A.; Hornschemeier, A.; Lehmer, B.; Yukita, M.; Wik, D.] Johns Hopkins Univ, Baltimore, MD 21218 USA. [Zezas, A.] Univ Crete, Dept Phys, Iraklion, Greece. [Zezas, A.] FORTH, IESL, Iraklion, Crete, Greece. [Zezas, A.; Antoniou, V.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Argo, M. K.] Univ Manchester, Jodrell Bank, Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Ballo, L.; Della Ceca, R.] Osservatorio Astron Brera INAF, I-20121 Milan, Italy. [Bechtol, K.] Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Boggs, S.; Craig, W. W.; Krivonos, R.] UC Berkeley Space Sci Lab, Berkeley, CA USA. [Christensen, F. E.] Tech Univ Denmark, Natl Space Inst, DK-2100 Copenhagen, Denmark. [Craig, W. W.] Lawrence Livermore Natl Lab, Livermore, CA USA. [Hailey, C. J.] Columbia Univ, New York, NY USA. [Harrison, F. A.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. [Maccarone, T. J.] Texas Tech Univ, Dept Phys, Lubbock, TX 79409 USA. [Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Ptak, A (reprint author), NASA, Goddard Space Flight Ctr, Code 662, Greenbelt, MD 20771 USA. RI Boggs, Steven/E-4170-2015; Zezas, Andreas/C-7543-2011; Antoniou, Vallia/E-3837-2013; OI Boggs, Steven/0000-0001-9567-4224; Zezas, Andreas/0000-0001-8952-676X; Ballo, Lucia/0000-0002-5036-3497; Antoniou, Vallia/0000-0001-7539-1593; Della Ceca, Roberto/0000-0001-7551-2252; Argo, Megan/0000-0003-3594-0214 FU NuSTAR Data Analysis Software (NUSTARDAS); ASI Science Data Center (ASDC, Italy); Caltech (USA); NASA [NNX12AN05G]; Chandra grant [GO3-14124X]; [267251] FX This research has made use of data obtained with the NuSTAR mission, a project led by the California Institute of Technology (Caltech), managed by the Jet Propulsion Laboratory (JPL) and funded by NASA. The scientific results reported in this article are based in part on observations made by the Chandra X-ray Observatory. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NUSTARDAS), jointly developed by the ASI Science Data Center (ASDC, Italy) and Caltech (USA). We also made use of the NASA/IPAC Extragalactic Database (NED) and NASA's Astrophysics Data System. L. B. received financial supports from the European Commission Seventh Framework Programme (FP7/2007-2013) under grant agreement No. 267251 "Astronomy Fellowships in Italy" (AstroFIt). A.Z. acknowledges partial support by NASA grant NNX12AN05G and Chandra grant GO3-14124X. We thank the anonymous referee for suggestions that improved this paper. NR 37 TC 6 Z9 6 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2015 VL 800 IS 2 AR 104 DI 10.1088/0004-637X/800/2/104 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CB7CA UT WOS:000349782500027 ER PT J AU Scoville, N Faisst, A Capak, P Kakazu, Y Li, GJ Steinhardt, C AF Scoville, Nick Faisst, Andreas Capak, Peter Kakazu, Yuko Li, Gongjie Steinhardt, Charles TI DUST ATTENUATION IN HIGH REDSHIFT GALAXIES: "DIAMONDS IN THE SKY" SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; dust, extinction; Galaxy: evolution; galaxies: high-redshift; ISM: clouds ID INTERSTELLAR EXTINCTION; STARBURST GALAXIES; MAGELLANIC-CLOUD; STAR-FORMATION; QUASARS; LAW; SPECTROSCOPY; COSMOS AB We use observed optical to near-infrared spectral energy distributions (SEDs) of 266 galaxies in the COSMOS survey to derive the wavelength dependence of the dust attenuation at high redshift. All of the galaxies have spectroscopic redshifts in the range z = 2-6.5. The presence of the Civ absorption feature, indicating that the rest-frame UV-optical SED is dominated by OB stars, is used to select objects for which the intrinsic, unattenuated spectrum has a well-established shape. Comparison of this intrinsic spectrum with the observed broadband photometric SED then permits derivation of the wavelength dependence of the dust attenuation. The derived dust attenuation curve is similar in overall shape to the Calzetti curve for local starburst galaxies. We also see the 2175 angstrom bump feature which is present in the Milky Way and Large Magellanic Cloud extinction curves but not seen in the Calzetti curve. The bump feature is commonly attributed to graphite or polycyclic aromatic hydrocarbons. No significant dependence is seen with redshift between sub-samples at z = 2-4 and z = 4-6.5. The "extinction" curve obtained here provides a firm basis for color and extinction corrections of high redshift galaxy photometry. C1 [Scoville, Nick; Capak, Peter; Steinhardt, Charles] CALTECH, Pasadena, CA 91125 USA. [Faisst, Andreas] ETH, Swiss Fed Inst Technol, Inst Astron, CH-8093 Zurich, Switzerland. [Capak, Peter; Steinhardt, Charles] Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Kakazu, Yuko] Subaru Telescope, Hilo, HI 96720 USA. [Li, Gongjie] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. RP Scoville, N (reprint author), CALTECH, MC 249-17,1200 East Calif Blvd, Pasadena, CA 91125 USA. OI Faisst, Andreas/0000-0002-9382-9832 FU Swiss National Science Foundation FX We thank the referee for suggestions and Martin Elvis for comments on an early draft. We also thank Zara Scoville for proofreading the manuscript. A.F. acknowledges support from the Swiss National Science Foundation and thanks Caltech for hospitality while working on this article. NR 22 TC 15 Z9 15 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2015 VL 800 IS 2 AR 108 DI 10.1088/0004-637X/800/2/108 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CB7CA UT WOS:000349782500031 ER PT J AU Shan, YT McDonald, M Courteau, S AF Shan, Yutong McDonald, Michael Courteau, Stephane TI REVISED MASS-TO-LIGHT RATIOS FOR NEARBY GALAXY GROUPS AND CLUSTERS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: general; galaxies: groups: general; galaxies: photometry; galaxies: statistics galaxies: stellar content ID DIGITAL SKY SURVEY; X-RAY; STELLAR POPULATION; ELLIPTIC GALAXIES; STAR-FORMATION; BARYON FRACTIONS; DATA RELEASE; EVOLUTIONARY SYNTHESIS; PHOTOMETRIC REDSHIFTS; VELOCITY DISPERSION AB We present a detailed investigation of the cluster stellar mass-to-light (M*/L) ratio and cumulative stellar masses, derived on a galaxy-by-galaxy basis, for 12 massive (M-500 similar to 10(14)-10(15) M-circle dot), nearby clusters with available optical imaging data from the Sloan Digital Sky Survey Data Release 10 and X-ray data from the Chandra X-ray Observatory. Our method involves a statistical cluster membership using both photometric and spectroscopic redshifts when available to maximize completeness while minimizing contamination effects. We show that different methods of estimating the stellar mass-to-light ratio from observed photometry result in systematic discrepancies in the total stellar masses and average mass-to-light ratios of cluster galaxies. Nonetheless, all conversion methodologies point to a lack of correlation between M*/L-i and total cluster mass, even though low-mass groups contain relatively more blue galaxies. We also find no statistically significant correlation between M*/L-i and the fraction of blue galaxies (g - i < 0.85). For the mass range covered by our sample, the assumption of a Chabrier initial mass function (IMF) yields an integrated M*/L-i similar or equal to 1.7 +/- 0.2 M-circle dot/L-i,L-circle dot, a lower value than used in most similar studies, though consistent with the study of low-mass galaxy groups by Leauthaud et al. A light (diet) Salpeter IMF would imply a similar to 60% increase in M*/L-i. C1 [Shan, Yutong; Courteau, Stephane] Queens Univ, Dept Phys Engn Phys & Astron, Kingston, ON, Canada. [McDonald, Michael] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. RP Shan, YT (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. EM yshan@cfa.harvard.edu FU Natural Science and Engineering Research Council of Canada; NASA through a Hubble Fellowship grant from STScI; Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy Office of Science; University of Arizona; Brazilian Participation Group; Brookhaven National Laboratory; Carnegie Mellon University; University of Florida; French Participation Group; German Participation Group; Harvard University; Instituto de Astrofisica de Canarias; Michigan State/Notre Dame/JINA Participation Group; Johns Hopkins University; Lawrence Berkeley National Laboratory; Max Planck Institute for Astrophysics; Max Planck Institute for Extraterrestrial Physics; New Mexico State University; New York University; Ohio State University; Pennsylvania State University; University of Portsmouth; Princeton University; Spanish Participation Group; University of Tokyo; University of Utah; Vanderbilt University; University of Virginia; University of Washington; Yale University FX We are grateful to the anonymous referee for the thoughtful suggestions, which improved the content and clarity of this paper. Y.S. and S.C. are grateful to the Natural Science and Engineering Research Council of Canada for funding via an Undergraduate Summer Research Award and Research Discovery Grant, respectively, which made this study possible. M.M. acknowledges support provided by NASA through a Hubble Fellowship grant from STScI. Comments from Anthony Gonzalez on an earlier draft were most helpful. We also thank Larry Widrow, Joel Roediger, Carlos Cunha, and John Moustakas for constructive suggestions at various stages of this project.; Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. The SDSS-III Web site is http://www.sdss3.org/.; SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University. NR 89 TC 2 Z9 2 U1 1 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2015 VL 800 IS 2 AR 122 DI 10.1088/0004-637X/800/2/122 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CB7CA UT WOS:000349782500045 ER PT J AU Sironi, L Narayan, R AF Sironi, Lorenzo Narayan, Ramesh TI ELECTRON HEATING BY THE ION CYCLOTRON INSTABILITY IN COLLISIONLESS ACCRETION FLOWS. I. COMPRESSION-DRIVEN INSTABILITIES AND THE ELECTRON HEATING MECHANISM SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; galaxies: clusters: general; instabilities; plasmas; radiation mechanisms: general; solar wind ID ADVECTION-DOMINATED ACCRETION; TEMPERATURE-ANISOTROPY INSTABILITIES; EXPANDING SOLAR-WIND; PARTICLE SCATTERING RATE; SAGITTARIUS-A-ASTERISK; X-RAY BINARIES; BLACK-HOLE; MIRROR INSTABILITY; MAGNETOROTATIONAL INSTABILITY; HYBRID SIMULATIONS AB In systems accreting well below the Eddington rate, such as the central black hole in the Milky Way (Sgr A*), the plasma in the innermost regions of the disk is believed to be collisionless and have two temperatures, with the ions substantially hotter than the electrons. However, whether a collisionless faster-than-Coulomb energy transfer mechanism exists in two-temperature accretion flows is still an open question. We study the physics of electron heating during the growth of ion velocity-space instabilities by means of multidimensional, fully kinetic, particle-in-cell (PIC) simulations. A background large-scale compression-embedded in a novel form of the PIC equations-continuously amplifies the field. This constantly drives a pressure anisotropy P-perpendicular to > P-parallel to because of the adiabatic invariance of the particle magnetic moments. We find that, for ion plasma beta values beta(0i) similar to 5-30 appropriate for the midplane of low-luminosity accretion flows (here, beta(0i) is the ratio of ion thermal pressure to magnetic pressure), mirror modes dominate if the electron-to-proton temperature ratio is T-0e/T-0i greater than or similar to 0.2, whereas for T-0e/T-0i less than or similar to 0.2 the ion cyclotron instability triggers the growth of strong Alfven-like waves, which pitch-angle scatter the ions to maintain marginal stability. We develop an analytical model of electron heating during the growth of the ion cyclotron instability, which we validate with PIC simulations. We find that for cold electrons (beta(0e) less than or similar to 2m(e)/m(i), where beta(0e) is the ratio of electron thermal pressure to magnetic pressure), the electron energy gain is controlled by the magnitude of the E-cross-B velocity induced by the ion cyclotron waves. This term is independent of the initial electron temperature, so it provides a solid energy floor even for electrons starting with extremely low temperatures. On the other hand, the electron energy gain for beta(0e) less than or similar to 2m(e)/m(i)-governed by the conservation of the particle magnetic moment in the growing fields of the instability-is proportional to the initial electron temperature, and it scales with the magnetic energy of ion cyclotron waves. Our results have implications for two-temperature accretion flows as well as for solar wind and intracluster plasmas. C1 [Sironi, Lorenzo; Narayan, Ramesh] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Sironi, L (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM lsironi@cfa.harvard.edu; rnarayan@cfa.harvard.edu OI Narayan, Ramesh/0000-0002-1919-2730 FU NASA - Chandra X-ray Center [PF1-120090]; NASA [NAS8-03060]; NASA via the TCAN award grant [NNX14AB47G]; [TG-AST120010] FX We thank J. Drake, M. Kunz, L. Matteini, S. Naoz, and especially R. Penna for useful discussions. L.S. is supported by NASA through Einstein Postdoctoral Fellowship grant number PF1-120090 awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. This work is supported in part by NASA via the TCAN award grant NNX14AB47G. L.S. gratefully acknowledges access to the PICSciE-OIT High Performance Computing Center and Visualization Laboratory at Princeton University. The simulations were also performed on XSEDE resources under contract No. TG-AST120010 and on NASA High-End Computing (HEC) resources through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center. NR 113 TC 15 Z9 15 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2015 VL 800 IS 2 AR 88 DI 10.1088/0004-637X/800/2/88 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CB7CA UT WOS:000349782500011 ER PT J AU Sironi, L AF Sironi, Lorenzo TI ELECTRON HEATING BY THE ION CYCLOTRON INSTABILITY IN COLLISIONLESS ACCRETION FLOWS. II. ELECTRON HEATING EFFICIENCY AS A FUNCTION OF FLOW CONDITIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; galaxies: clusters: general; instabilities; plasmas radiation mechanisms: general; solar wind ID ADVECTION-DOMINATED ACCRETION; PROTON TEMPERATURE ANISOTROPY; SAGITTARIUS-A-ASTERISK; FAST SOLAR-WIND; BLACK-HOLE; PARTICLE-ACCELERATION; MIRROR INSTABILITY; GALACTIC-CENTER; LINEAR-THEORY; MAGNETOHYDRODYNAMIC TURBULENCE AB In the innermost regions of low-luminosity accretion flows, including Sgr A* at the center of our Galaxy, the frequency of Coulomb collisions is so low that the plasma has two temperatures, with the ions substantially hotter than the electrons. This paradigm assumes that Coulomb collisions are the only channel for transferring the ion energy to the electrons. In this work, the second of a series, we assess the efficiency of electron heating by ion velocity-space instabilities in collisionless accretion flows. The instabilities are seeded by the pressure anisotropy induced by magnetic field amplification, coupled to the adiabatic invariance of the particle magnetic moments. Using two-dimensional particle-in-cell (PIC) simulations, we showed in Paper I that if the electron-to-ion temperature ratio is T-0e/T-0i less than or similar to 0.2, the ion cyclotron instability is the dominant mode for ion betas beta(0i) similar to 5-30 (here, beta(0i) is the ratio of ion thermal pressure to magnetic pressure), as appropriate for the midplane of low-luminosity accretion flows. In this work, we employ analytical theory and one-dimensional PIC simulations (with the box aligned with the fastest-growing wave vector of the ion cyclotron mode) to fully characterize how the electron heating efficiency during the growth of the ion cyclotron instability depends on the electron-to-proton temperature ratio, the plasma beta, the Alfven speed, the amplification rate of the mean field (in units of the ion Larmor frequency), and the proton-to-electron mass ratio. Our findings can be incorporated as a physically grounded subgrid model into global fluid simulations of low-luminosity accretion flows, thus helping to assess the validity of the two-temperature assumption. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Sironi, L (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM lsironi@cfa.harvard.edu FU NASA - Chandra X-ray Center [PF1-120090]; NASA [NAS8-03060]; NASA via the TCAN award [NNX14AB47G]; [TG-AST120010] FX We thank M. Kunz and R. Narayan for useful discussions. L.S. is supported by NASA through Einstein Postdoctoral Fellowship grant number PF1-120090 awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. This work is supported in part by NASA via the TCAN award grant number NNX14AB47G. L.S. gratefully acknowledges access to the PICSciE-OIT High Performance Computing Center and Visualization Laboratory at Princeton University. The simulations were also performed on XSEDE resources under contract No. TG-AST120010, and on NASA High-End Computing (HEC) resources through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center. NR 87 TC 8 Z9 8 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 20 PY 2015 VL 800 IS 2 AR 89 DI 10.1088/0004-637X/800/2/89 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CB7CA UT WOS:000349782500012 ER PT J AU Torres, G Kipping, DM Fressin, F Caldwell, DA Twicken, JD Ballard, S Batalha, NM Bryson, ST Ciardi, DR Henze, CE Howell, SB Isaacson, HT Jenkins, J Muirhead, PS Newton, ER Petigura, EA Barclay, T Borucki, WJ Crepp, JR Everett, ME Horch, EP Howard, AW Kolbl, R Marcy, GW McCauliff, S Quintana, EV AF Torres, Guillermo Kipping, David M. Fressin, Francois Caldwell, Douglas A. Twicken, Joseph D. Ballard, Sarah Batalha, Natalie M. Bryson, Stephen T. Ciardi, David R. Henze, Christopher E. Howell, Steve B. Isaacson, Howard T. Jenkins, Jonm. Muirhead, Philip S. Newton, Elisabeth R. Petigura, Erik A. Barclay, Thomas Borucki, William J. Crepp, Justin R. Everett, Mark E. Horch, Elliott P. Howard, Andrew W. Kolbl, Rea Marcy, Geoffrey W. McCauliff, Sean Quintana, Elisa V. TI VALIDATION OF 12 SMALL KEPLER TRANSITING PLANETS IN THE HABITABLE ZONE SO ASTROPHYSICAL JOURNAL LA English DT Article DE methods: statistical; planetary systems; stars: individual (KOI-3284 (Kepler-438), KOI-4742 (Kepler-442)); techniques: photometric ID K-BAND SPECTRA; MAIN-SEQUENCE STARS; M DWARFS; FALSE POSITIVES; BINARY STARS; LIGHT CURVES; STELLAR EVOLUTION; CANDIDATE PLANETS; BLEND SCENARIOS; HIPPARCOS STARS AB We present an investigation of 12 candidate transiting planets from Kepler with orbital periods ranging from 34 to 207 days, selected from initial indications that they are small and potentially in the habitable zone (HZ) of their parent stars. Few of these objects are known. The expected Doppler signals are too small to confirm them by demonstrating that their masses are in the planetary regime. Here we verify their planetary nature by validating them statistically using the BLENDER technique, which simulates large numbers of false positives and compares the resulting light curves with the Kepler photometry. This analysis was supplemented with new follow-up observations (high-resolution optical and near-infrared spectroscopy, adaptive optics imaging, and speckle interferometry), as well as an analysis of the flux centroids. For 11 of them (KOI-0571.05, 1422.04, 1422.05, 2529.02, 3255.01, 3284.01, 4005.01, 4087.01, 4622.01, 4742.01, and 4745.01) we show that the likelihood they are true planets is far greater than that of a false positive, to a confidence level of 99.73% (3 sigma) or higher. For KOI-4427.01 the confidence level is about 99.2% (2.6 sigma). With our accurate characterization of the GKM host stars, the derived planetary radii range from 1.1 to 2.7R(circle plus). All 12 objects are confirmed to be in the HZ, and nine are small enough to be rocky. Excluding three of them that have been previously validated by others, our study doubles the number of known rocky planets in the HZ. KOI-3284.01 (Kepler-438b) and KOI-4742.01 (Kepler-442b) are the planets most similar to the Earth discovered to date when considering their size and incident flux jointly. C1 [Torres, Guillermo; Kipping, David M.; Fressin, Francois; Newton, Elisabeth R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Caldwell, Douglas A.; Twicken, Joseph D.] NASA, SETI Inst, Ames Res Ctr, Moffett Field, CA 94035 USA. [Ballard, Sarah] Univ Washington, Seattle, WA 98195 USA. [Batalha, Natalie M.; Bryson, Stephen T.; Henze, Christopher E.; Howell, Steve B.; Jenkins, Jonm.; Barclay, Thomas; Borucki, William J.; Quintana, Elisa V.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Ciardi, David R.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Isaacson, Howard T.; Petigura, Erik A.; Kolbl, Rea; Marcy, Geoffrey W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Muirhead, Philip S.] Boston Univ, Dept Astron, Boston, MA 02215 USA. [Crepp, Justin R.] Univ Notre Dame, Notre Dame, IN 46556 USA. [Everett, Mark E.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Horch, Elliott P.] So Connecticut State Univ, Dept Phys, New Haven, CT 06515 USA. [Howard, Andrew W.] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. [McCauliff, Sean] NASA, Ames Res Ctr, Orbital Sci Corp, Moffett Field, CA 94035 USA. RP Torres, G (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM gtorres@cfa.harvard.edu RI Howard, Andrew/D-4148-2015; Muirhead, Philip/H-2273-2014; OI Howard, Andrew/0000-0001-8638-0320; Muirhead, Philip/0000-0002-0638-8822; Ciardi, David/0000-0002-5741-3047; Newton, Elisabeth/0000-0003-4150-841X FU NASA's Science Mission Directorate; NASA [NNX14AB83G]; Harvard College Observatory Menzel Fellowship FX We thank the referee for helpful comments on the original manuscript. This paper includes data collected by the Kepler spacecraft. Funding for the Kepler Mission is provided by NASA's Science Mission Directorate. The research has also made use of the Michael Dodds Computing Facility, of NASA's Astrophysics Data System (ADS), and of data products from the Mikulski Archive for Space Telescopes (MAST). 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. We extend special thanks to those of Hawaiian ancestry on whose sacred mountain of Mauna Kea we are privileged to be guests. G.T. acknowledges partial support for this work from NASA grant NNX14AB83G (Kepler Participating Scientist Program). D.M.K. is supported by the Harvard College Observatory Menzel Fellowship. NR 116 TC 29 Z9 29 U1 7 U2 39 PU IOP PUBLISHING LTD 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 2015 VL 800 IS 2 AR 99 DI 10.1088/0004-637X/800/2/99 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CB7CA UT WOS:000349782500022 ER PT J AU Guzman, VV Pety, J Goicoechea, JR Gerin, M Roueff, E Gratier, P Oberg, KI AF Guzman, V. V. Pety, J. Goicoechea, J. R. Gerin, M. Roueff, E. Gratier, P. Oeberg, K. I. TI SPATIALLY RESOLVED l-C3H+ EMISSION IN THE HORSEHEAD PHOTODISSOCIATION REGION: FURTHER EVIDENCE FOR A TOP-DOWN HYDROCARBON CHEMISTRY SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE astrochemistry; ISM: abundances; ISM: molecules; molecular data; molecular processes; photon-dominated region (PDR) ID INTERSTELLAR GAS; DIFFUSE CLOUDS; DARK CLOUDS; C2H; TEMPERATURE; NEBULA; RATES; EDGE; PAHS; C3H2 AB Small hydrocarbons, such as C2H, C3H, and C3H2 are more abundant in photo-dissociation regions (PDRs) than expected based on gas-phase chemical models. To explore the hydrocarbon chemistry further, we observed a key intermediate species, the hydrocarbon ion l-C3H+, in the Horsehead PDR with the Plateau de Bure Interferometer at high-angular resolution (6 ''). We compare with previous observations of C2H and c-C3H2 at similar angular resolution and new gas-phase chemical model predictions to constrain the dominant formation mechanisms of small hydrocarbons in low-UV flux PDRs. We find that at the peak of the HCO emission (PDR position), the measured l-C3H+, C2H, and c-C3H2 abundances are consistent with current gas-phase model predictions. However, in the first PDR layers, at the 7.7 mu m polycyclic aromatic hydrocarbon band emission peak, which are more exposed to the radiation field and where the density is lower, the C2H and c-C3H2 abundances are underestimated by an order of magnitude. At this position, the l-C3H+ abundance is also underpredicted by the model but only by a factor of a few. In addition, contrary to the model predictions, l-C3H+ peaks further out in the PDR than the other hydrocarbons, C2H and c-C3H2. This cannot be explained by an excitation effect. Current gas-phase photochemical models thus cannot explain the observed abundances of hydrocarbons, in particular, in the first PDR layers. Our observations are consistent with a top-down hydrocarbon chemistry, in which large polyatomic molecules or small carbonaceous grains are photo-destroyed into smaller hydrocarbon molecules/precursors. C1 [Guzman, V. V.; Oeberg, K. I.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Pety, J.] Inst Radioastron Millimetr IRAM, F-38406 St Martin Dheres, France. [Pety, J.; Gerin, M.] PSL Res Univ, Ecole Normale Super, Observ Paris, LERMA,CNRS,UMR8112, F-75014 Paris, France. [Goicoechea, J. R.] CSIC, Inst Ciencia Mat Madrid, E-28049 Madrid, Spain. [Gerin, M.; Roueff, E.] Univ Paris 06, Sorbonne Univ, UMR8112, LERMA, F-75005 Paris, France. [Roueff, E.] PSL Res Univ, CNRS, UMR8112, LERMA,Observ Paris, F-92190 Meudon, France. [Gratier, P.] Univ Bordeaux, LAB, UMR 5804, F-33270 Floirac, France. [Gratier, P.] CNRS, UMR 5804, LAB, F-33270 Floirac, France. RP Guzman, VV (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM vguzman@cfa.harvard.edu OI PETY, Jerome/0000-0003-3061-6546; Gratier, Pierre/0000-0002-6636-4304 FU CNRS Programme Nationale de Physique et Chimie du Milieu Interstellaire (PCMI); Spanish MINECO [CSD2009-00038, AYA2009-07304, AYA2012-32032]; ERC Starting grant [3DICE (336474)] FX We thank the referee for useful comments that improved the manuscript. We thank the IRAM PdBI and 30 m staff for their support during the observations. This work was partially funded by the CNRS Programme Nationale de Physique et Chimie du Milieu Interstellaire (PCMI). J.R.G. thanks the Spanish MINECO for funding support from grants CSD2009-00038, AYA2009-07304, and AYA2012-32032. P.G. acknowledges funding from the ERC Starting grant 3DICE (336474). NR 30 TC 9 Z9 9 U1 1 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD FEB 20 PY 2015 VL 800 IS 2 AR L33 DI 10.1088/2041-8205/800/2/L33 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CB5UK UT WOS:000349692900014 ER PT J AU Nardini, E Reeves, JN Gofford, J Harrison, FA Risaliti, G Braito, V Costa, MT Matzeu, GA Walton, DJ Behar, E Boggs, SE Christensen, FE Craig, WW Hailey, CJ Matt, G Miller, JM O'Brien, PT Stern, D Turner, TJ Ward, MJ AF Nardini, E. Reeves, J. N. Gofford, J. Harrison, F. A. Risaliti, G. Braito, V. Costa, M. T. Matzeu, G. A. Walton, D. J. Behar, E. Boggs, S. E. Christensen, F. E. Craig, W. W. Hailey, C. J. Matt, G. Miller, J. M. O'Brien, P. T. Stern, D. Turner, T. J. Ward, M. J. TI Black hole feedback in the luminous quasar PDS 456 SO SCIENCE LA English DT Article ID RADIO-QUIET AGNS; HOST GALAXIES; SIGMA RELATION; OUTFLOWS; WIND; ABSORBER; LOCATION AB The evolution of galaxies is connected to the growth of supermassive black holes in their centers. During the quasar phase, a huge luminosity is released as matter falls onto the black hole, and radiation-driven winds can transfer most of this energy back to the host galaxy. Over five different epochs, we detected the signatures of a nearly spherical stream of highly ionized gas in the broadband x-ray spectra of the luminous quasar PDS 456. This persistent wind is expelled at relativistic speeds from the inner accretion disk, and its wide aperture suggests an effective coupling with the ambient gas. The outflow's kinetic power larger than 1046 ergs per second is enough to provide the feedback required by models of black hole and host galaxy coevolution. C1 [Nardini, E.; Reeves, J. N.; Gofford, J.; Costa, M. T.; Matzeu, G. A.] Keele Univ, Astrophys Grp, Sch Phys & Geog Sci, Keele ST5 5BG, Staffs, England. [Reeves, J. N.; Gofford, J.] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA. [Harrison, F. A.; Walton, D. J.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Risaliti, G.] Osserv Astrofis Arcetri, Ist Nazl Astrofis, I-50125 Florence, Italy. [Risaliti, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Braito, V.] Osserv Astron Brera, INAF, I-23807 Merate, LC, Italy. [Walton, D. J.; Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Behar, E.] Technion Israel Inst Technol, Dept Phys, IL-32000 Haifa, Israel. [Boggs, S. E.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Christensen, F. E.] Tech Univ Denmark, Space Natl Space Inst, DK-2800 Lyngby, Denmark. [Craig, W. W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Matt, G.] Univ Rome Tre, Dipartimento Matemat & Fis, I-00146 Rome, Italy. [Miller, J. M.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [O'Brien, P. T.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Turner, T. J.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA. [Turner, T. J.] Eureka Sci Inc, Oakland, CA 94602 USA. [Ward, M. J.] Univ Durham, Dept Phys, Durham DH1 3LE, England. RP Nardini, E (reprint author), Keele Univ, Astrophys Grp, Sch Phys & Geog Sci, Keele ST5 5BG, Staffs, England. EM e.nardini@keele.ac.uk RI Boggs, Steven/E-4170-2015; OI Boggs, Steven/0000-0001-9567-4224; Braito, Valentina/0000-0002-2629-4989; Risaliti, Guido/0000-0002-3556-977X FU U.K. Science and Technology Facilities Council [ST/J001384/1]; ESA member states; National Aeronautics and Space Administration; NASA [NNX11AJ57G, NNG08FD60C]; Italian Space Agency [ASI-INAF I/037/12/0]; Italian National Institute for Astrophysics [PRIN-INAF 2012]; I-CORE program of the Planning and Budgeting Committee; Israel Science Foundation [1937/12, 1163/10]; Israel's Ministry of Science and Technology FX This research was supported under the U.K. Science and Technology Facilities Council grant ST/J001384/1 and is based on x-ray observations obtained with the XMM-Newton and NuSTAR satellites. XMM-Newton is a European Space Agency (ESA) science mission with instruments and contributions directly funded by ESA member states and the National Aeronautics and Space Administration. The NuSTAR mission is a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by NASA. We thank the NuSTAR Operations, Software, and Calibration teams for support with execution and analysis of these observations. We also acknowledge financial support from the Italian Space Agency under grant ASI-INAF I/037/12/0 (G.R. and G.M.); the Italian National Institute for Astrophysics under grant PRIN-INAF 2012 (G.R.); the I-CORE program of the Planning and Budgeting Committee, the Israel Science Foundation under grants 1937/12 and 1163/10, Israel's Ministry of Science and Technology (E.B.); and NASA under grants NNX11AJ57G and NNG08FD60C (T.J.T.). The data are stored in the science archives of the two x-ray observatories involved and will become publicly available on 25 March 2015 (XMM-Newton) and with the upcoming DR6 data release (NuSTAR). NR 26 TC 30 Z9 30 U1 0 U2 14 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 EI 1095-9203 J9 SCIENCE JI Science PD FEB 20 PY 2015 VL 347 IS 6224 BP 860 EP 863 DI 10.1126/science.1259202 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CB6UB UT WOS:000349761100040 PM 25700515 ER PT J AU Kowalski, KP Bacon, C Bickford, W Braun, H Clay, K Leduc-Lapierre, M Lillard, E McCormick, MK Nelson, E Torres, M White, J Wilcox, DA AF Kowalski, Kurt P. Bacon, Charles Bickford, Wesley Braun, Heather Clay, Keith Leduc-Lapierre, Michele Lillard, Elizabeth McCormick, Melissa K. Nelson, Eric Torres, Monica White, James Wilcox, Douglas A. TI Advancing the science of microbial symbiosis to support invasive species management: a case study on Phragmites in the Great Lakes SO FRONTIERS IN MICROBIOLOGY LA English DT Review DE symbiosis; Phragmites; invasive species management; fungi; bacteria; collaborative; endophyte; Great Lakes Region ID COMMON REED; FUNGAL ENDOPHYTES; GUT MICROBIOTA; AUSTRALIS POPULATIONS; AMMOPHILA-ARENARIA; RHIZOSPHERE MICROBIOME; HYPERICUM-PERFORATUM; OOMYCETE COMMUNITIES; BACTERIAL DIVERSITY; BIOMASS PRODUCTION AB A growing body of literature supports microbial symbiosis as a foundational principle for the competitive success of invasive plant species. Further exploration of the relationships between invasive species and their associated microbiomes, as well as the interactions with the microbiomes of native species, can lead to key new insights into invasive success and potentially new and effective control approaches. In this manuscript, we review microbial relationships with plants, outline steps necessary to develop invasive species control strategies that are based on those relationships, and use the invasive plant species Phragmites australis (common reed) as an example of how development of microbial-based control strategies can be enhanced using a collective impact approach. The proposed science agenda, developed by the Collaborative for Microbial Symbiosis and Phragmites Management, contains a foundation of sequential steps and mutually-reinforcing tasks to guide the development of microbial-based control strategies for Phragmites and other invasive species. Just as the science of plant-microbial symbiosis can be transferred for use in other invasive species, so too can the model of collective impact be applied to other avenues of research and management. C1 [Kowalski, Kurt P.; Bickford, Wesley] US Geol Survey, Great Lakes Sci Ctr, Ann Arbor, MI 48105 USA. [Bacon, Charles] USDA ARS, Athens, GA 30613 USA. [Braun, Heather; Leduc-Lapierre, Michele; Lillard, Elizabeth] Great Lakes Commiss, Ann Arbor, MI USA. [Clay, Keith] Indiana Univ, Dept Biol, Bloomington, IN USA. [McCormick, Melissa K.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Nelson, Eric] Cornell Univ, Dept Plant Pathol & Plant Microbe Biol, Ithaca, NY USA. [Torres, Monica; White, James] Rutgers State Univ, Dept Plant Biol & Pathol, New Brunswick, NJ 08903 USA. [Wilcox, Douglas A.] SUNY Coll Brockport, Coll Brockport, Dept Environm Sci & Biol, Brockport, NY 14420 USA. RP Kowalski, KP (reprint author), US Geol Survey, Great Lakes Sci Ctr, 1451 Green Rd, Ann Arbor, MI 48105 USA. EM kkowalski@usgs.gov OI Kowalski, Kurt/0000-0002-8424-4701 FU U.S. Geological Survey; NOAA Maryland SeaGrant; Great Lakes Restoration Initiative allowed the research team FX Financial support from the U.S. Geological Survey, NOAA Maryland SeaGrant, and the Great Lakes Restoration Initiative allowed the research team to complete this project. We thank Katherine Hollins and other staff at the Great Lakes Commission for scientific and administrative contributions. We thank Aubrey Scott for background materials and formatting assistance. We thank Ellen Crocker for her early contributions to the process. Finally, we thank the known and anonymous reviewers for their constructive comments. Any use of trade, product, or firm names is for descriptive purposes only and does not imply endorsement by the U.S. Government. This article is Contribution 1912 of the USGS Great Lakes Science Center. NR 159 TC 8 Z9 8 U1 8 U2 53 PU FRONTIERS RESEARCH FOUNDATION PI LAUSANNE PA PO BOX 110, LAUSANNE, 1015, SWITZERLAND SN 1664-302X J9 FRONT MICROBIOL JI Front. Microbiol. PD FEB 19 PY 2015 VL 6 DI 10.3389/fmicb.2015.00095 PG 14 WC Microbiology SC Microbiology GA CC4GC UT WOS:000350309100001 ER PT J AU Bales, EK Hyman, OJ Loudon, AH Harris, RN Lipps, G Chapman, E Roblee, K Kleopfer, JD Terrell, KA AF Bales, Emma K. Hyman, Oliver J. Loudon, Andrew H. Harris, Reid N. Lipps, Gregory Chapman, Eric Roblee, Kenneth Kleopfer, John D. Terrell, Kimberly A. TI Pathogenic Chytrid Fungus Batrachochytrium dendrobatidis, but Not B. salamandrivorans, Detected on Eastern Hellbenders SO PLOS ONE LA English DT Article ID CRYPTOBRANCHUS-ALLEGANIENSIS-ALLEGANIENSIS; EMERGING DISEASE; CHYTRIDIOMYCOSIS; AMPHIBIANS; POPULATIONS; INFECTION; USA AB Recent worldwide declines and extinctions of amphibian populations have been attributed to chytridiomycosis, a disease caused by the pathogenic fungus Batrachochytrium dendrobatidis (Bd). Until recently, Bd was thought to be the only Batrachochytrium species that infects amphibians; however a newly described species, Batrachochytrium salamandrivorans (Bs), is linked to die-offs in European fire salamanders (Salamandra salamandra). Little is known about the distribution, host range, or origin of Bs. In this study, we surveyed populations of an aquatic salamander that is declining in the United States, the eastern hellbender (Cryptobranchus alleganiensis alleganiensis), for the presence of Bs and Bd. Skin swabs were collected from a total of 91 individuals in New York, Pennsylvania, Ohio, and Virginia, and tested for both pathogens using duplex qPCR. Bs was not detected in any samples, suggesting it was not present in these hellbender populations (0% prevalence, 95% confidence intervals of 0.0-0.04). Bd was found on 22 hellbenders (24% prevalence, 95% confidence intervals of 0.16 <= 0.24 <= 0.34), representing all four states. All positive samples had low loads of Bd zoospores (12.7 +/- 4.9 S.E.M. genome equivalents) compared to other Bd susceptible species. More research is needed to determine the impact of Batrachochytrium infection on hellbender fitness and population viability. In particular, understanding how hellbenders limit Bd infection intensity in an aquatic environment may yield important insights for amphibian conservation. This study is among the first to evaluate the distribution of Bs in the United States, and is consistent with another, which failed to detect Bs in the U.S. Knowledge about the distribution, host-range, and origin of Bs may help control the spread of this pathogen, especially to regions of high salamander diversity, such as the eastern United States. C1 [Bales, Emma K.; Hyman, Oliver J.; Loudon, Andrew H.; Harris, Reid N.] James Madison Univ, Dept Biol, Harrisonburg, VA 22807 USA. [Lipps, Gregory] Gregory Lipps LLC, Toledo, OH USA. [Chapman, Eric] Western Penn Conservancy, Pittsburgh, PA USA. [Roblee, Kenneth] New York Dept Environm Conservat, Albany, NY USA. [Kleopfer, John D.] Virginia Dept Game & Inland Fisheries, Richmond, VA USA. [Terrell, Kimberly A.] Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA. RP Terrell, KA (reprint author), Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA. EM terrellk@si.edu FU Columbus Zoo; Aquarium Conservation fund; National Science Foundation [1136602] FX Funding was provided by the Columbus Zoo and Aquarium Conservation fund (Grant awarded to RNH and AHL) https://globalimpact. columbuszoo.org/about/columbus-zoo-fund-forconservation and National Science Foundation grant 1136602 (awarded to RNH) http://www.nsf.gov/funding/. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. Author GL is the owner and sole employee of Gregory Lipps, LLC. Gregory Lipps, LLC provided support in the form of salary for author GL, but did not have any additional role in the study design, data collection and analysis, decision to publish, or preparation of the manuscript. The specific role of this author is articulated in the author contributions' section. NR 35 TC 5 Z9 5 U1 7 U2 50 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD FEB 19 PY 2015 VL 10 IS 2 AR e0116405 PG 9 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CC0XE UT WOS:000350062300013 PM 25695636 ER PT J AU Forest, F Crandall, KA Chase, MW Faith, DP AF Forest, Felix Crandall, Keith A. Chase, Mark W. Faith, Daniel P. TI Phylogeny, extinction and conservation: embracing uncertainties in a time of urgency SO PHILOSOPHICAL TRANSACTIONS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Editorial Material DE evolutionary biology; extinction risks; feature diversity; phylogenetic diversity; uncertainty ID BIODIVERSITY CONSERVATION; ECOLOGICAL COMMUNITIES; EVOLUTIONARY HISTORY; FEATURE DIVERSITY; BETA DIVERSITY; HOTSPOTS; MAMMALS; PRIORITIZATION; PROBABILITIES; SYSTEMATICS AB Evolutionary studies have played a fundamental role in our understanding of life, but until recently, they had only a relatively modest involvement in addressing conservation issues. The main goal of the present discussion meeting issue is to offer a platform to present the available methods allowing the integration of phylogenetic and extinction risk data in conservation planning. Here, we identify the main knowledge gaps in biodiversity science, which include incomplete sampling, reconstruction biases in phylogenetic analyses, partly known species distribution ranges, and the difficulty in producing conservation assessments for all known species, not to mention that much of the effective biological diversity remains to be discovered. Given the impact that human activities have on biodiversity and the urgency with which we need to address these issues, imperfect assumptions need to be sanctioned and surrogates used in the race to salvage as much as possible of our natural and evolutionary heritage. We discuss some aspects of the uncertainties found in biodiversity science, such as the ideal surrogates for biodiversity, the gaps in our knowledge and the numerous available phylogenetic diversity-based methods. We also introduce a series of cases studies that demonstrate how evolutionary biology can effectively contribute to biodiversity conservation science. C1 [Forest, Felix; Chase, Mark W.] Royal Bot Gardens, Jodrell Lab, Richmond TW9 3DS, Surrey, England. [Crandall, Keith A.] George Washington Univ, Computat Biol Inst, Ashburn, VA 20147 USA. [Crandall, Keith A.] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20013 USA. [Chase, Mark W.] Univ Western Australia, Sch Plant Biol, Crawley, WA, Australia. [Faith, Daniel P.] Australian Museum, Sydney, NSW 2010, Australia. RP Forest, F (reprint author), Royal Bot Gardens, Jodrell Lab, Richmond TW9 3DS, Surrey, England. EM f.forest@kew.org RI Chase, Mark /A-6642-2011 NR 64 TC 8 Z9 8 U1 9 U2 87 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8436 EI 1471-2970 J9 PHILOS T R SOC B JI Philos. Trans. R. Soc. B-Biol. Sci. PD FEB 19 PY 2015 VL 370 IS 1662 AR 20140002 DI 10.1098/rstb.2014.0002 PG 8 WC Biology SC Life Sciences & Biomedicine - Other Topics GA AY0UM UT WOS:000347312400001 PM 25561663 ER PT J AU Owen, CL Bracken-Grissom, H Stern, D Crandall, KA AF Owen, Christopher L. Bracken-Grissom, Heather Stern, David Crandall, Keith A. TI A synthetic phylogeny of freshwater crayfish: insights for conservation SO PHILOSOPHICAL TRANSACTIONS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE crayfish; conservation; EDGE; phylogenetic diversity ID MITOCHONDRIAL-DNA SEQUENCES; EXTINCTION RATES; SUBGENUS AVITICAMBARUS; GENUS AUSTROPOTAMOBIUS; DECAPODA CAMBARIDAE; MOLECULAR EVOLUTION; TAXONOMIC REVISION; BURROWING CRAYFISH; DIVERGENCE TIMES; ABSOLUTE RATES AB Phylogenetic systematics is heading for a renaissance where we shift from considering our phylogenetic estimates as a static image in a published paper and taxonomies as a hardcopy checklist to treating both the phylogenetic estimate and dynamic taxonomies as metadata for further analyses. The Open Tree of Life project (opentreeoflife.org) is developing synthesis tools for harnessing the power of phylogenetic inference and robust taxonomy to develop a synthetic tree of life. We capitalize on this approach to estimate a synthesis tree for the freshwater crayfish. The crayfish make an exceptional group to demonstrate the utility of the synthesis approach, as there recently have been a number of phylogenetic studies on the crayfishes along with a robust underlying taxonomic framework. Importantly, the crayfish have also been extensively assessed by an IUCN Red List team and therefore have accurate and up-to-date area and conservation status data available for analysis within a phylogenetic context. Here, we develop a synthesis phylogeny for the world's freshwater crayfish and examine the phylogenetic distribution of threat. We also estimate a molecular phylogeny based on all available GenBank crayfish sequences and use this tree to estimate divergence times and test for divergence rate variation. Finally, we conduct EDGE and HEDGE analyses and identify a number of species of freshwater crayfish of highest priority in conservation efforts. C1 [Owen, Christopher L.; Stern, David; Crandall, Keith A.] George Washington Univ, Computat Biol Inst, Ashburn, VA 20147 USA. [Bracken-Grissom, Heather] Florida Int Univ, Dept Biol Sci, North Miami, FL 33181 USA. [Crandall, Keith A.] Smithsonian Inst, Dept Invertebrate Zool, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Crandall, KA (reprint author), George Washington Univ, Computat Biol Inst, Ashburn, VA 20147 USA. EM kcrandall@gwu.edu OI Crandall, Keith/0000-0002-0836-3389 FU US NSF [DEB 13-01820] FX This work was supported by the US NSF grant no. DEB 13-01820. NR 91 TC 5 Z9 5 U1 2 U2 40 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8436 EI 1471-2970 J9 PHILOS T R SOC B JI Philos. Trans. R. Soc. B-Biol. Sci. PD FEB 19 PY 2015 VL 370 IS 1662 AR 20140009 DI 10.1098/rstb.2014.0009 PG 10 WC Biology SC Life Sciences & Biomedicine - Other Topics GA AY0UM UT WOS:000347312400008 PM 25561670 ER PT J AU Richman, NI Boehm, M Adams, SB Alvarez, F Bergey, EA Bunn, JJS Burnham, Q Cordeiro, J Coughran, J Crandall, KA Dawkins, KL DiStefano, RJ Doran, NE Edsman, L Eversole, AG Fureder, L Furse, JM Gherardi, F Hamr, P Holdich, DM Horwitz, P Johnston, K Jones, CM Jones, JPG Jones, RL Jones, TG Kawai, T Lawler, S Lopez-Mejia, M Miller, RM Pedraza-Lara, C Reynolds, JD Richardson, AMM Schultz, MB Schuster, GA Sibley, PJ Souty-Grosset, C Taylor, CA Thoma, RF Walls, J Walsh, TS Collen, B AF Richman, Nadia I. Boehm, Monika Adams, Susan B. Alvarez, Fernando Bergey, Elizabeth A. Bunn, John J. S. Burnham, Quinton Cordeiro, Jay Coughran, Jason Crandall, Keith A. Dawkins, Kathryn L. DiStefano, Robert J. Doran, Niall E. Edsman, Lennart Eversole, Arnold G. Fuereder, Leopold Furse, James M. Gherardi, Francesca Hamr, Premek Holdich, David M. Horwitz, Pierre Johnston, Kerrylyn Jones, Clive M. Jones, Julia P. G. Jones, Robert L. Jones, Thomas G. Kawai, Tadashi Lawler, Susan Lopez-Mejia, Marilu Miller, Rebecca M. Pedraza-Lara, Carlos Reynolds, Julian D. Richardson, Alastair M. M. Schultz, Mark B. Schuster, Guenter A. Sibley, Peter J. Souty-Grosset, Catherine Taylor, Christopher A. Thoma, Roger F. Walls, Jerry Walsh, Todd S. Collen, Ben TI Multiple drivers of decline in the global status of freshwater crayfish (Decapoda: Astacidea) SO PHILOSOPHICAL TRANSACTIONS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE extinction risk; crayfish; IUCN Red List; threatened; freshwater biodiversity ID EXTINCTION RISK; CLIMATE-CHANGE; BIODIVERSITY CONSERVATION; EASTERN AUSTRALIA; SIGNAL CRAYFISH; UNITED-STATES; PARASTACIDAE; MANAGEMENT; PRIORITIES; BIOLOGY AB Rates of biodiversity loss are higher in freshwater ecosystems than in most terrestrial or marine ecosystems, making freshwater conservation a priority. However, prioritization methods are impeded by insufficient knowledge on the distribution and conservation status of freshwater taxa, particularly invertebrates. We evaluated the extinction risk of the world's 590 freshwater crayfish species using the IUCN Categories and Criteria and found 32% of all species are threatened with extinction. The level of extinction risk differed between families, with proportionally more threatened species in the Parastacidae and Astacidae than in the Cambaridae. Four described species were Extinct and 21% were assessed as Data Deficient. There was geographical variation in the dominant threats affecting the main centres of crayfish diversity. The majority of threatened US and Mexican species face threats associated with urban development, pollution, damming and water management. Conversely, the majority of Australian threatened species are affected by climate change, harvesting, agriculture and invasive species. Only a small proportion of crayfish are found within the boundaries of protected areas, suggesting that alternative means of long-term protection will be required. Our study highlights many of the significant challenges yet to come for freshwater biodiversity unless conservation planning shifts from a reactive to proactive approach. C1 [Richman, Nadia I.; Boehm, Monika] Zool Soc London, Inst Zool, London NW1 4RY, England. [Richman, Nadia I.; Jones, Julia P. G.] Bangor Univ, Sch Environm Nat Resources & Geog, Bangor LL57 2UW, Gwynedd, Wales. [Adams, Susan B.] US Forest Serv, USDA, Southern Res Stn, Ctr Bottomland Hardwoods Res, Oxford, MS 38655 USA. [Alvarez, Fernando] Univ Nacl Autonoma Mexico, Inst Biol, Colecc Nacl Crustaceos, Mexico City 04510, DF, Mexico. [Bergey, Elizabeth A.] Univ Oklahoma, Oklahoma Biol Survey, Norman, OK 73019 USA. [Bergey, Elizabeth A.] Univ Oklahoma, Dept Biol, Norman, OK 73019 USA. [Bunn, John J. S.; Burnham, Quinton; Coughran, Jason; Horwitz, Pierre] Edith Cowan Univ, Sch Nat Sci, Joondalup, WA, Australia. [Cordeiro, Jay] Northeast Nat Hist & Supply, Middleboro, MA 02346 USA. [Coughran, Jason] Jagabar Environm, Duncraig, WA 6023, Australia. [Crandall, Keith A.] George Washington Univ, Computat Biol Inst, Ashburn, VA 20147 USA. [Crandall, Keith A.] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20013 USA. [Dawkins, Kathryn L.] Griffith Univ, Griffith Sch Environm, Australian Rivers Inst, Gold Coast Campus, Qld 4222, Australia. [DiStefano, Robert J.] Missouri Dept Conservat, Columbia, MO 65201 USA. [Doran, Niall E.] Univ Tasmania, Bookend Trust, Sandy Bay, Tas 7006, Australia. [Doran, Niall E.] Univ Tasmania, Sch Biol Sci, Sandy Bay, Tas 7006, Australia. [Edsman, Lennart] Swedish Univ Agr Sci, Dept Aquat Resources, Inst Freshwater Res, S-17893 Drottningholm, Sweden. [Eversole, Arnold G.] Clemson Univ, Sch Agr Forestry & Environm Sci, Clemson, SC 29634 USA. [Fuereder, Leopold] Univ Innsbruck, Inst Ecol, A-6020 Innsbruck, Austria. [Furse, James M.] Griffith Univ, Griffith Sch Environm, Gold Coast Campus, Qld 4222, Australia. [Furse, James M.] Griffith Univ, Environm Futures Res Inst, Gold Coast Campus, Qld 4222, Australia. [Gherardi, Francesca] Univ Florence, Dipartimento Biol, I-50125 Florence, Italy. [Hamr, Premek] Upper Canada Coll, Toronto, ON M4V 1W6, Canada. [Miller, Rebecca M.] Peak Ecol Ltd, Crayfish Survey, Bakewell DE45 1GT, Derby, England. [Holdich, David M.] Peak Ecol Ltd, Res, Bakewell DE45 1GT, Derby, England. [Johnston, Kerrylyn] Murdoch Univ, Murdoch, WA 6150, Australia. [Johnston, Kerrylyn] Murdoch Univ, Marine & Freshwater Res Lab, Murdoch, WA 6150, Australia. [Jones, Clive M.] James Cook Univ, Sch Marine & Trop Biol, Cairns, Qld 4870, Australia. [Jones, Robert L.] Museum Nat Sci, Mississippi Dept Wildlife Fisheries & Pk, Jackson, MS 39202 USA. [Jones, Thomas G.] Marshall Univ, Dept Integrated Sci & Technol, Huntington, WV 25755 USA. [Kawai, Tadashi] Wakkanai Fisheries Inst, Wakkanai, Hokkaido 0970001, Japan. [Lawler, Susan] La Trobe Univ, Dept Environm Management & Ecol, Wodonga, Vic 3690, Australia. [Lopez-Mejia, Marilu] Univ Quintana Roo, Evolutionary Biol & Populat Genet Lab, Unidad Acad Cozumel, Cozumel 77600, Q Roo, Mexico. [Miller, Rebecca M.] Global Ecosyst Management Programme, Int Union Conservat Nat, Cambridge CB3 0DL, England. [Pedraza-Lara, Carlos] Univ Nacl Autonoma Mexico, Fac Med, Mexico City 04510, DF, Mexico. [Pedraza-Lara, Carlos] Univ Nacl Autonoma Mexico, Inst Biol, Mexico City 04510, DF, Mexico. [Reynolds, Julian D.] Trinity Coll Dublin, Stillorgan, Dublin, Ireland. [Richardson, Alastair M. M.] Univ Tasmania, Sch Biol, Hobart, Tas 7001, Australia. [Schultz, Mark B.] Univ Melbourne, Dept Biochem & Mol Biol, Melbourne, Vic 3010, Australia. [Sibley, Peter J.] Environm Agcy, Wessex Area, East Quay TA6 4YS, Bridgwater, England. [Souty-Grosset, Catherine] Univ Poitiers, UMR CNRS 7267, Lab Ecol & Biol Interact, Equipe Ecol Evolut Symbiose, Poitiers, France. [Taylor, Christopher A.] Illinois Nat Hist Survey, Prairie Res Inst, Champaign, IL 61820 USA. [Thoma, Roger F.] Midwest Biodivers Inst, Hilliard, OH 43026 USA. [Walls, Jerry] Louisiana State Univ, Dept Biol Sci, Alexandria, LA 71302 USA. [Collen, Ben] UCL, Ctr Biodivers & Environm Res, London WC1E 6BT, England. RP Richman, NI (reprint author), Zool Soc London, Inst Zool, Regents Pk, London NW1 4RY, England. EM nadia.richman@ioz.ac.uk RI Jones, Clive/D-2991-2009; CSTFA, ResearcherID/P-1067-2014; Jones, Julia/A-3031-2011; Collen, Ben/F-2543-2016; OI Jones, Clive/0000-0002-6319-2068; Jones, Julia/0000-0002-5199-3335; Collen, Ben/0000-0003-2564-4243; Schultz, Mark/0000-0002-7689-6531; Crandall, Keith/0000-0002-0836-3389; Dawkins, Kathryn/0000-0001-5092-2378 FU Esmee Fairbairn Foundation; Rufford Foundation; Biodiversity Synthesis Center in Chicago FX The authors acknowledge the Esmee Fairbairn Foundation (N.I.R. and M.B.), the Rufford Foundation (B.C. and M.B.) and the Biodiversity Synthesis Center in Chicago who funded and hosted the workshop in which all North American species were assessed. For data compilation, we thank Alison Batchelor, Georgia Cryer, Ranmali De Silva, Ellie Dyer, Blythe Jopling, Gita Kasthala, Fiona Livingston, Maiko Lutz, Shane McGuinness, Harriet Milligan, Mala Ram, Jeremy Smith, Anne-Marie Soulsby, Kathryn Sullivan and Felix Whitton. We also acknowledge the vast network of data contributors who have been kind enough to review reports; Christopher Austin, Miklos Puky, Eva Kozubikova, William R. Elliott, John Foster, Holga Schulz, Ivana Maguire, Japo Jussila, Stephanie Peay, Peter Manko, Emmanuil Manos, Marina Paolucci, Martin Pugh, Naomi Wilson, Paul Bradley, Ralf Schulz, Boris Sket, Soren Berg, Adrian Hutchings, Angel Zaikov, Margaret Palmer, Daniel Hefti, Yoann Allanic, Markku Pursiainen, Liviu Miron, Lucian Parvulescu, Peter Manko, Roger Cammaerts, Valery Fedotov, Olga Mandryka, Pedro Gutierrez and Przemyslaw Smietana. We thank our two anonymous referees for helpful comments on an earlier version of this paper. NR 90 TC 22 Z9 23 U1 5 U2 150 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8436 EI 1471-2970 J9 PHILOS T R SOC B JI Philos. Trans. R. Soc. B-Biol. Sci. PD FEB 19 PY 2015 VL 370 IS 1662 AR 20140060 DI 10.1098/rstb.2014.0060 PG 11 WC Biology SC Life Sciences & Biomedicine - Other Topics GA AY0UM UT WOS:000347312400017 PM 25561679 ER PT J AU Breedy, O Cairns, SD Haussermann, V AF Breedy, Odalisca Cairns, Stephen D. Haeussermann, Verena TI A new alcyonacean octocoral (Cnidaria, Anthozoa, Octocorallia) from Chilean fjords SO ZOOTAXA LA English DT Article DE Alcyonacea; Chile; Chilean fjord region; Cnidaria; new species; Octocorallia; Plexauridae; IUCN Red List of Threatened Species ID SOUTHERN CHILE; ECOSYSTEMS; RESPONSES AB A new species, Swiftia comauensis, is described from Chile. It occurs in shallow waters from 18 to 59 m in the Patagonian fjord region and seems to be endemic to the northern part of the region. The species is characterized by having straggly colonies with sparse branching and long drooping branches, prominent polyp mounds, and long, thin spindles; the colonies are bright orange with pale yellow polyp mounds. A sharp decline in colony abundance was observed between 2003 and 2013, and in January 2014 a proposal was submitted to the IUCN for the addition of this taxon to the Red List of Threatened Species. C1 [Breedy, Odalisca] Ctr Invest Ciencias Mar & Limnol, San Jose, Costa Rica. [Breedy, Odalisca] Univ Costa Rica, Ctr Invest Estruct Microscop, San Jose, Costa Rica. [Breedy, Odalisca] Smithsonian Trop Res Inst, Panama City, Panama. [Cairns, Stephen D.] Natl Museum Nat Hist, Smithsonian Inst, Dept Invertebrate Zool, Washington, DC 20560 USA. [Haeussermann, Verena] Pontificia Univ Catolica Valparaiso, Fac Recursos Nat, Escuela Ciencias Mar, Valparaiso, Chile. [Haeussermann, Verena] Huinay Sci Field Stn, Puerto Montt, Chile. RP Breedy, O (reprint author), Ctr Invest Ciencias Mar & Limnol, POB 11501-2060, San Jose, Costa Rica. EM odaliscab@gmail.com; cairnss@si.edu; v.haussermann@gmail.com FU PADI Foundation; Vicerrectoria de Investigacion; UCR; Fondecyt project [1131039] FX We thank Eric Pante, and the anonymous reviewers for their comments that have improved this paper. Many thanks to Gunter Forsterra who helped collect specimens of Swiftia comauensis in the Comau Fjord. Robert Ford is thanked for the production of figures 2 and 3, and Ulrich Porschmann for making the map. Part of the work was financed by a grant of the PADI Foundation (2006) for the project "Octocoral biodiversity in the Chilean-Patagonian fjord region and zoogeographic implications," Vicerrectoria de Investigacion, UCR, and the Fondecyt project nr 1131039 to VH. This is publication No. 105 of Huinay Scientific Field Station. NR 34 TC 1 Z9 1 U1 0 U2 9 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 17 PY 2015 VL 3919 IS 2 BP 327 EP 334 DI 10.11646/zootaxa.3919.2.5 PG 8 WC Zoology SC Zoology GA CB5VI UT WOS:000349695300005 PM 25781130 ER PT J AU Leray, M Knowlton, N AF Leray, Matthieu Knowlton, Nancy TI DNA barcoding and metabarcoding of standardized samples reveal patterns of marine benthic diversity SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE oyster reefs; operational taxonomic units; meiofauna; ARMS; cryptic species ID SPECIES-RICHNESS; BIODIVERSITY; MAGNITUDE; REGION; CORAL; TAXA AB Documenting the diversity of marine life is challenging because many species are cryptic, small, and rare, and belong to poorly known groups. New sequencing technologies, especially when combined with standardized sampling, promise to make comprehensive biodiversity assessments and monitoring feasible on a large scale. We used this approach to characterize patterns of diversity on oyster reefs across a range of geographic scales comprising a temperate location [Virginia (VA)] and a subtropical location [Florida (FL)]. Eukaryotic organisms that colonized multilayered settlement surfaces (autonomous reef monitoring structures) over a 6-mo period were identified by cytochrome c oxidase subunit I barcoding (>2-mm mobile organisms) and metabarcoding (sessile and smaller mobile organisms). In a total area of similar to 15.64 m(2) and volume of similar to 0.09 m(3), 2,179 operational taxonomic units (OTUs) were recorded from 983,056 sequences. However, only 10.9% could be matched to reference barcodes in public data-bases, with only 8.2% matching barcodes with both genus and species names. Taxonomic coverage was broad, particularly for animals (22 phyla recorded), but 35.6% of OTUs detected via meta-barcoding could not be confidently assigned to a taxonomic group. The smallest size fraction (500 to 106 pm) was the most diverse (more than two-thirds of OTUs). There was little taxonomic overlap between VA and FL, and samples separated by similar to 2 m were significantly more similar than samples separated by similar to 100 m. Ground-truthing with independent assessments of taxonomic composition indicated that both presence-absence information and relative abundance information are captured by metabarcoding data, suggesting considerable potential for ecological studies and environmental monitoring. C1 [Leray, Matthieu; Knowlton, Nancy] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Knowlton, N (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. EM knowlton@si.edu FU US Army Corps of Engineers in FL [SAJ-2012-02893]; Sant Chair and Smithsonian Tennenbaum Marine Observatories Network FX We thank Natalia Agudelo, Sherry Reed, Woody Lee, and Sean Fate for help in the field; the Smithsonian Laboratory of Analytical Biology staff for assistance; and Daryl Hurley II for allowing research to be conducted on his oyster reef in VA. Research Permit SAJ-2012-02893(NW-SLR) was provided by the US Army Corps of Engineers in FL. Financial support was provided by the Sant Chair and Smithsonian Tennenbaum Marine Observatories Network, for which this paper is Contribution 1. NR 30 TC 43 Z9 46 U1 21 U2 127 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 17 PY 2015 VL 112 IS 7 BP 2076 EP 2081 DI 10.1073/pnas.1424997112 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CB2GV UT WOS:000349446000063 PM 25646458 ER PT J AU Carn, SA Yang, K Prata, AJ Krotkov, NA AF Carn, S. A. Yang, K. Prata, A. J. Krotkov, N. A. TI Extending the long-term record of volcanic SO2 emissions with the Ozone Mapping and Profiler Suite nadir mapper SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE remote sensing; volcanology; sulfur dioxide; Paluweh volcano ID STRATOSPHERIC AEROSOL LAYER; SULFUR-DIOXIDE; SPECTROMETER; CLIMATE; INSTRUMENTS; SATELLITE; CLOUD AB Uninterrupted, global space-based monitoring of volcanic sulfur dioxide (SO2) emissions is critical for climate modeling and aviation hazard mitigation. We report the first volcanic SO2 measurements using ultraviolet (UV) Ozone Mapping and Profiler Suite (OMPS) nadir mapper data. OMPS was launched on the Suomi National Polar-orbiting Partnership satellite in October 2011. We demonstrate the sensitivity of OMPS SO2 measurements by quantifying SO2 emissions from the modest eruption of Paluweh volcano (Indonesia) in February 2013 and tracking the dispersion of the volcanic SO2 cloud. The OMPS SO2 retrievals are validated using Ozone Monitoring Instrument and Atmospheric Infrared Sounder measurements. The results confirm the ability of OMPS to extend the long-term record of volcanic SO2 emissions based on UV satellite observations. We also show that the Paluweh volcanic SO2 reached the lower stratosphere, further demonstrating the impact of small tropical volcanic eruptions on stratospheric aerosol optical depth and climate. C1 [Carn, S. A.] Michigan Technol Univ, Dept Geol & Mining Engn & Sci, Houghton, MI 49931 USA. [Carn, S. A.] Smithsonian Inst, Dept Mineral Sci, Natl Museum Nat Hist, Washington, DC 20560 USA. [Yang, K.] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA. [Prata, A. J.] Norwegian Inst Air Res, Atmosphere & Climate Dept, Kjeller, Norway. [Krotkov, N. A.] NASA, Goddard Space Flight Ctr, Armospher Chem & Dynam Lab, Greenbelt, MD 20771 USA. RP Carn, SA (reprint author), Michigan Technol Univ, Dept Geol & Mining Engn & Sci, Houghton, MI 49931 USA. EM scarn@mtu.edu RI Krotkov, Nickolay/E-1541-2012 OI Krotkov, Nickolay/0000-0001-6170-6750 FU NASA [NNX11AK95G, NNX13AF50G] FX We acknowledge NASA's support for this work through grants NNX11AK95G (Continuation of Long-Term Sulfur Dioxide EDR with the SNPP/OMPS NM) and NNX13AF50G (Multidecadal Sulfur Dioxide Climatology from Satellite Instruments). We thank the NASA-funded SNPP Ozone Product Evaluation and Algorithm Test Element for providing OMPS Level 1B data and gratefully acknowledge the NOAA Air Resources Laboratory for the provision of the HYSPLIT transport and dispersion model and/or READY website (http://www.ready.noaa.gov) used in this publication. Two anonymous reviewers provided thorough reviews that greatly improved the final paper. All satellite data used in this paper can either be accessed for free at the NASA data centers listed herein (AIRS, OMI, CALIOP, and MLS) or can be obtained from the corresponding author (OMPS-NM). NR 33 TC 9 Z9 9 U1 2 U2 17 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD FEB 16 PY 2015 VL 42 IS 3 BP 925 EP 932 DI 10.1002/2014GL062437 PG 8 WC Geosciences, Multidisciplinary SC Geology GA CD8OT UT WOS:000351355600032 ER PT J AU Fergus, JLB Johnsen, S Osborn, KJ AF Fergus, Jamie L. Baldwin Johnsen, Soenke Osborn, Karen J. TI A Unique Apposition Compound Eye in the Mesopelagic Hyperiid Amphipod Paraphronima gracilis SO CURRENT BIOLOGY LA English DT Article ID DEEP-SEA; VISUAL PIGMENTS; FINE-STRUCTURE; VISION; CRUSTACEANS; PHRONIMA; LIGHT AB The mesopelagic habitat is a vast space that lacks physical landmarks and is structured by depth, light penetration, and horizontal currents. Solar illumination is visible in the upper 1,000 m of the ocean, becoming dimmer and spectrally filtered with depth-generating a nearly monochromatic blue light field [1]. The struggle to perceive dim downwelling light and bioluminescent sources and the need to remain unseen generate contrasting selective pressures on the eyes of mesopelagic inhabitants [2]. Hyperiid amphipods are cosmopolitan members of the mesopelagic fauna with at least ten different eye configurations across the family-ranging from absent eyes in deep-living species to four enlarged eyes in mesopelagic individuals [3-7]. The hyperiid amphipod Paraphronima gracilis has a pair of bi-lobed apposition compound eyes, each with a large upward-looking portion and a small lateral-looking portion. The most unusual feature of the P. gracilis eye is that its upward-looking portion is resolved into a discontinuous retina with 12 distinct groups, each serving one transverse row of continuously spaced facets. On the basis of eye morphology, we estimated spatial acuity (2.5 degrees +/- 6 0.11 degrees, SEM; n = 25) and optical sensitivity (30 +/- 3.4 mu m(2).sr, SEM; n = 25). Microspectrophotometry showed that spectral sensitivity of the eye peaked at 516 nm (+/- 3.9 nm, SEM; n = 6), significantly offset from the peak of downwelling irradiance in the mesopelagic realm (480 nm). Modeling of spatial summation within the linear retinal groups showed that it boosts sensitivity with less cost to spatial acuity than more typical configurations. C1 [Fergus, Jamie L. Baldwin; Osborn, Karen J.] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20013 USA. [Johnsen, Soenke] Duke Univ, Dept Biol, Durham, NC 27708 USA. RP Fergus, JLB (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20013 USA. EM jamiebfergus@gmail.com OI Osborn, Karen/0000-0002-4226-9257 FU Peter Buck Postdoctoral Fellowship; Office of Naval Research [N00014-09-1-1053] FX We thank the crew of MBARI's R/V Western Flyer and Kyra Schlinning for assistance with video review and VARS searches. Drs. Barbara Carlsward and Paul Switzer provided laboratory and equipment space. Dr. Jon Norenburg provided histology training. Freya Goetz, Stephanie Bush, Kim Reisenbichler, Kris Walz, and Robert Sherlock provided assistance with specimen collection, and Drs. Bruce Robison and Steven Haddock provided invitations to participate in MBARI field expeditions. Thank you to Drs. William Browne and Daniel Speiser for commenting on early versions of the manuscript, as well as two anonymous reviewers. Rachel Goncalves drew the schematic of the MSP (Figure S3). J.B.F. was supported by a Peter Buck Postdoctoral Fellowship. S.J. was supported in part by a grant from the Office of Naval Research (N00014-09-1-1053). NR 31 TC 1 Z9 1 U1 1 U2 7 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 FEB 16 PY 2015 VL 25 IS 4 BP 473 EP 478 DI 10.1016/j.cub.2014.12.010 PG 6 WC Biochemistry & Molecular Biology; Cell Biology SC Biochemistry & Molecular Biology; Cell Biology GA CB1GT UT WOS:000349375900023 ER PT J AU Fisher, R O'Leary, RA Low-Choy, S Mengersen, K Knowlton, N Brainard, RE Caley, MJ AF Fisher, Rebecca O'Leary, Rebecca A. Low-Choy, Samantha Mengersen, Kerrie Knowlton, Nancy Brainard, Russell E. Caley, M. Julian TI Species Richness on Coral Reefs and the Pursuit of Convergent Global Estimates SO CURRENT BIOLOGY LA English DT Article ID EXPERT KNOWLEDGE; DIVERSITY; ELICITATION; MODELS; BIODIVERSITY; ECOSYSTEMS; MAGNITUDE; NUMBER; RATES AB Global species richness, whether estimated by taxon, habitat, or ecosystem, is a key biodiversity metric. Yet, despite the global importance of biodiversity and increasing threats to it (e.g., [1-4]), we are no better able to estimate global species richness now than we were six decades ago [5]. Estimates of global species richness remain highly uncertain and are often logically inconsistent [5]. They are also difficult to validate because estimation of global species richness requires extrapolation beyond the number of species known [6-13]. Given that somewhere between 3% and >96% of species on Earth may remain undiscovered [4], depending on the methods used and the taxa considered, such extrapolations, especially from small percentages of known species, are likely to be highly uncertain [13, 14]. An alternative approach is to estimate all species, the known and unknown, directly. Using expert taxonomic knowledge of the species already described and named, those already discovered but not yet described and named, and those still awaiting discovery, we estimate there to be 830,000 (95% credible limits: 550,0001,330,000) multi-cellular species on coral reefs worldwide, excluding fungi. Uncertainty surrounding this estimate and its components were often strongly skewed toward larger values, indicating that many more species on coral reefs is more plausible than many fewer. The uncertainties revealed here should guide future research toward achieving convergence in global species richness estimates for coral reefs and other ecosystems via adaptive learning protocols whereby such estimates can be tested and improved, and their uncertainties reduced, as new knowledge is acquired. C1 [Fisher, Rebecca; O'Leary, Rebecca A.] UWA Oceans Inst, Australian Inst Marine Sci, Crawley, WA 6009, Australia. [Low-Choy, Samantha; Mengersen, Kerrie] Queensland Univ Technol, Sch Math Sci, Brisbane, Qld 4001, Australia. [Knowlton, Nancy] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20013 USA. [Brainard, Russell E.] NOAA, Coral Reef Ecosyst Div, Pacific Isl Fisheries Sci Ctr, Honolulu, HI 96818 USA. [Caley, M. Julian] Australian Inst Marine Sci, Townsville, Qld 4810, Australia. RP Caley, MJ (reprint author), Australian Inst Marine Sci, PMB 3, Townsville, Qld 4810, Australia. EM j.caley@aims.gov.au OI Mengersen, Kerrie/0000-0001-8625-9168; Caley, Julian/0000-0001-5739-749X; Fisher, Rebecca/0000-0001-5148-6731 FU BHP Billiton through CReefs Australia (CReefs, Census of Marine Life); Cooperative Research Centre for National Plant Biosecurity FX This work was funded by BHP Billiton through CReefs Australia (CReefs, Census of Marine Life). We thank the Cooperative Research Centre for National Plant Biosecurity for supporting contribution by S.L.-C. We are very grateful to the many taxonomists who agreed to be elicited and donated their time so generously: R. Adlard, S. Ahyong, P. Alderslade, A. Anker, C. Arango, I. Beveridge, M. Blazewicz, P. Bock, P. Bouchet, A. Bruce, N. Bruce, C. Bryce, M. Bryce, L. Cannon, M. Capa, T. Cribb, P. Davie, M. Ekins, D. Fautin, J. Fromont, C. Glasby, F. Gurgel, S. de Grave, J. Healy, M. Hodda, A. Hoggett, D. Hoese, J. Hooper, A. Hosie, L. Hughes, J. Huisman, C. Aguilar Hurtado, P. Hutchings, V. Ivanenko, I. Karanovic, R. Lasley, J. Lowry, A. Maiorova, I. Marin, P. Mather, T. Miller, A. Miskelly, C. Meyer, P. Ng, M. Norman, T. O'Hara, J. Otto, G. Paulay, W. Ponder, G. Poore, J. Reimer, B. Richer de Forges, B. Russell, K. Sanders, P. Sutcliffe, J. Taylor, K. Tilbrook, C. Wallace, C. Watson, J. Watson, R. Willan, and R. Wilson. Thanks also to A. Hamilton, M. Costello, and N. Stork for helping us improve this manuscript. NR 40 TC 17 Z9 18 U1 9 U2 47 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 FEB 16 PY 2015 VL 25 IS 4 BP 500 EP 505 DI 10.1016/j.cub.2014.12.022 PG 6 WC Biochemistry & Molecular Biology; Cell Biology SC Biochemistry & Molecular Biology; Cell Biology GA CB1GT UT WOS:000349375900028 PM 25639239 ER PT J AU Schachat, SR Oliver, JC Monteiro, A AF Schachat, Sandra R. Oliver, Jeffrey C. Monteiro, Antonia TI Nymphalid eyespots are co-opted to novel wing locations following a similar pattern in independent lineages SO BMC EVOLUTIONARY BIOLOGY LA English DT Article DE Serial homology; Correlation analysis; Ancestral states; Phylogeny; Wing patterns ID SERIAL HOMOLOGY; BUTTERFLY WINGS; EVOLUTION; DROSOPHILA; ELEMENTS; MECHANISMS; DIPTERA; ORIGIN; THORAX AB Background: Variation in the number of repeated traits, or serial homologs, has contributed greatly to animal body plan diversity. Eyespot color patterns of nymphalid butterflies, like arthropod and vertebrate limbs, are an example of serial homologs. These eyespot color patterns originated in a small number of wing sectors on the ventral hindwing surface and later appeared in novel wing sectors, novel wings, and novel wing surfaces. However, the details of how eyespots were co-opted to these novel wing locations are currently unknown. Results: We used a large data matrix of eyespot/presence absence data, previously assembled from photographs of contemporary species, to perform a phylogenetic investigation of eyespot origins in nine independent nymphalid lineages. To determine how the eyespot gene regulatory network acquired novel positional information, we used phylogenetic correlation analyses to test for non-independence in the origination of eyespots. We found consistent patterns of eyespot gene network redeployment in the nine lineages, where eyespots first redeployed from the ventral hindwing to the ventral forewing, then to new sectors within the ventral wing surface, and finally to the dorsal wing surface. Eyespots that appeared in novel wing sectors modified the positional information of their serial homolog ancestors in one of two ways: by changing the wing or surface identity while retaining sector identity, or by changing the sector identity while retaining wing and surface identity. Conclusions: Eyespot redeployment to novel sectors, wings, and surfaces happened multiple times in different nymphalid subfamilies following a similar pattern. This indicates that parallel mutations altering expression of the eyespot gene regulatory network led to its co-option to novel wing locations over time. C1 [Schachat, Sandra R.] Mississippi State Univ, Dept Biochem Mol Biol Entomol & Plant Pathol, Mississippi State, MS 39762 USA. [Schachat, Sandra R.] Smithsonian Inst, Dept Paleobiol, Washington, DC 20013 USA. [Oliver, Jeffrey C.] Oregon State Univ, Dept Integrat Biol, Corvallis, OR 97331 USA. [Monteiro, Antonia] Yale Univ, Dept Ecol & Evolutionary Biol, New Haven, CT 06520 USA. [Monteiro, Antonia] Natl Univ Singapore, Dept Biol Sci, Singapore 117543, Singapore. [Monteiro, Antonia] Yale NUS Coll, Singapore 138614, Singapore. RP Schachat, SR (reprint author), Mississippi State Univ, Dept Biochem Mol Biol Entomol & Plant Pathol, Mississippi State, MS 39762 USA. EM schachatsr@si.edu; antonia.monteiro@nus.edu.sg RI Monteiro, Antonia/J-6452-2013; Schachat, Sandra/M-5399-2014 OI Monteiro, Antonia/0000-0001-9696-459X; Schachat, Sandra/0000-0003-3237-5619 FU NSF [IOS 0818731]; Ministry of Education of Singapore [R-154-000-602-112] FX We thank Donald J Harvey, Carla M Penz, and Jeffrey W Shultz for helpful suggestions and discussion, and Lawrence F Gall for assistance in the entomology collection of the Peabody Museum of Natural History. Numerous undergraduates assisted with photography and initial wing-scoring. NSF IOS 0818731 and Ministry of Education of Singapore R-154-000-602-112 grants supported this research. The authors declare no conflicts of interest. NR 34 TC 2 Z9 2 U1 0 U2 12 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 FEB 14 PY 2015 VL 15 AR 20 DI 10.1186/s12862-015-0300-x PG 9 WC Evolutionary Biology; Genetics & Heredity SC Evolutionary Biology; Genetics & Heredity GA CC0XB UT WOS:000350061900002 PM 25886182 ER PT J AU Pineda, JE Offner, SSR Parker, RJ Arce, HG Goodman, AA Caselli, P Fuller, GA Bourke, TL Corder, SA AF Pineda, Jaime E. Offner, Stella S. R. Parker, Richard J. Arce, Hector G. Goodman, Alyssa A. Caselli, Paola Fuller, Gary A. Bourke, Tyler L. Corder, Stuartt A. TI The formation of a quadruple star system with wide separation SO NATURE LA English DT Article ID STELLAR MULTIPLICITY; PROTOSTELLAR OUTFLOW; EMBEDDED PROTOSTARS; MOLECULAR CLOUDS; MASS FUNCTION; BINARY STARS; DENSE CORES; LARGE ARRAY; EVOLUTION; FRAGMENTATION AB The initial multiplicity of stellar systems is highly uncertain. A number of mechanisms have been proposed to explain the origin of binary and multiple star systems, including core fragmentation, disk fragmentation and stellar capture(1-3). Observations show that protostellar and pre-main-sequence multiplicity is higher than the multiplicity found in field stars(4-7), which suggests that dynamical interactions occur early, splitting up multiple systems and modifying the initial stellar separations(8,9). Without direct, high-resolution observations of forming systems, however, it is difficult to determine the true initial multiplicity and the dominant binary formation mechanism. Here we report observations of a wide-separation (greater than 1,000 astronomical units) quadruple system composed of a young protostar and three gravitationally bound dense gas condensations. These condensations are the result of fragmentation of dense gas filaments, and each condensation is expected to forma star on a time-scale of 40,000 years. We determine that the closest pair will form a bound binary, while the quadruple stellar system itself is bound but unstable on timescales of 500,000 years (comparable to the lifetime of the embedded protostellar phase(10)). These observations suggest that filament fragmentation on length scales of about 5,000 astronomical units offers a viable pathway to the formation of multiple systems. C1 [Pineda, Jaime E.] ETH, Inst Astron, CH-8093 Zurich, Switzerland. [Offner, Stella S. R.; Arce, Hector G.] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Offner, Stella S. R.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Parker, Richard J.] Liverpool John Moores Univ, Astrophys Res Inst, Liverpool L3 5RF, Merseyside, England. [Goodman, Alyssa A.; Bourke, Tyler L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Caselli, Paola] Max Planck Inst Extraterr Phys MPE, D-85741 Garching, Germany. [Fuller, Gary A.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, UK ARC Node, Manchester M13 9PL, Lancs, England. [Bourke, Tyler L.] Jodrell Bank Observ, SKA Org, Macclesfield SK11 9DL, Cheshire, England. [Corder, Stuartt A.] Joint ALMA Observ, Santiago, Chile. [Corder, Stuartt A.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. RP Pineda, JE (reprint author), ETH, Inst Astron, Wolfgang Pauli Str 27, CH-8093 Zurich, Switzerland. EM jpineda@mpe.mpg.de RI Goodman, Alyssa/A-6007-2010; OI Goodman, Alyssa/0000-0003-1312-0477; Pineda, Jaime/0000-0002-3972-1978 FU Swiss National Science Foundation [CRSII2_141880]; NSF CAREER award [AST-0845619]; NSF [AST-0908159]; ERC [PALs 320620]; NASA [NNX09AB89G, 51311.01, NAS 5-26555]; Space Telescope Science Institute; Royal Astronomical Society; Canada Foundation for Innovation FX We thank K. Todorov for discussions and comments that improved the paper. We acknowledge support from the Swiss National Science Foundation project CRSII2_141880 (J.E.P.), NSF CAREER award AST-0845619 (H.G.A.), NSF grant AST-0908159 (A.A.G.), ERC project PALs 320620 (P.C.) and NASA grant NNX09AB89G (T.L.B.). S.S.R.O. acknowledges support from NASA through Hubble Fellowship grant 51311.01 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. R.J.P. acknowledges support from the Royal Astronomical Society through a research fellowship. This research made use of astrodendro (http://www.dendrograms.org), Astropy, and APLpy (http://aplpy.github.com). The James Clerk Maxwell Telescope is operated by the Joint Astronomy Centre on behalf of the Science and Technology Facilities Council of the UK, the National Research Council of Canada, and (up to 31 March 2013) the Netherlands Organisation for Scientific Research. Additional funds for the construction of SCUBA-2 were provided by the Canada Foundation for Innovation. The National Radio Astronomy Observatory is a facility of the NSF operated under cooperative agreement by Associated Universities, Inc. NR 30 TC 15 Z9 15 U1 0 U2 4 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 EI 1476-4687 J9 NATURE JI Nature PD FEB 12 PY 2015 VL 518 IS 7538 BP 213 EP U447 DI 10.1038/nature14166 PG 8 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CA8SD UT WOS:000349190300033 PM 25673415 ER PT J AU Sales, LV Vogelsberger, M Genel, S Torrey, P Nelson, D Rodriguez-Gomez, V Wang, WT Pillepich, A Sijacki, D Springel, V Hernquist, L AF Sales, Laura V. Vogelsberger, Mark Genel, Shy Torrey, Paul Nelson, Dylan Rodriguez-Gomez, Vicente Wang, Wenting Pillepich, Annalisa Sijacki, Debora Springel, Volker Hernquist, Lars TI The colours of satellite galaxies in the Illustris simulation SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: evolution; galaxies: haloes; galaxies: structure ID RADIAL-DISTRIBUTION; MASSIVE GALAXIES; LEGACY SURVEY; EVOLUTION; FRACTION; STELLAR; MATTER; DARK; GAS; POPULATION AB Observationally, the fraction of blue satellite galaxies decreases steeply with host halo mass, and their radial distribution around central galaxies is significantly shallower in massive (M-* >= 10(11) M-circle dot) than in Milky Way-like systems. Theoretical models, based primarily on semi-analytical techniques, have had a long-standing problem with reproducing these trends, instead predicting too few blue satellites in general but also estimating a radial distribution that is too shallow, regardless of primary mass. In this Letter, we use the Illustris cosmological simulation to study the properties of satellite galaxies around isolated primaries. For the first time, we find good agreement between theory and observations. We identify the main source of this success relative to earlier work to be a consequence of the large gas contents of satellites at infall, a factor similar to 5-10 times larger than in semi-analytical models. Because of their relatively large gas reservoirs, satellites can continue to form stars long after infall, with a typical time-scale for star-formation to be quenched similar to 2 Gyr in groups but more than similar to 5 Gyr for satellites around Milky Way-like primaries. The gas contents we infer are consistent with z = 0 observations of HI gas in galaxies, although we find large discrepancies among reported values in the literature. A testable prediction of our model is that the gas-to-stellar mass ratio of satellite progenitors should vary only weakly with cosmic time. C1 [Sales, Laura V.; Genel, Shy; Torrey, Paul; Nelson, Dylan; Rodriguez-Gomez, Vicente; Pillepich, Annalisa; Hernquist, Lars] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Vogelsberger, Mark; Torrey, Paul] MIT, Dept Phys, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Wang, Wenting] Univ Durham, Inst Computat Cosmol, Durham DH1 3LE, England. [Sijacki, Debora] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Sijacki, Debora] Univ Cambridge, Kavli Inst Cosmol, Cambridge CB3 0HA, England. [Springel, Volker] Heidelberg Inst Theoret Studies, D-69118 Heidelberg, Germany. [Springel, Volker] Heidelberg Univ, ARI, Zentrum Fuer Astron, D-69120 Heidelberg, Germany. RP Sales, LV (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM lsales@cfa.harvard.edu OI Torrey, Paul/0000-0002-5653-0786; Rodriguez-Gomez, Vicente/0000-0002-9495-0079 FU CEA/France as part of PRACE project [RA0844]; Leibniz Computing Centre, Germany [pr85je]; NASA [NNX12AC67G]; NSF [AST-1312095]; European Research Council [EXAGAL-308037] FX LVS wishes to thank Simon White and Guinnevere Kauffmann for stimulating discussions and Manolis Papastergis for facilitating ALFALFA tables. Simulations were run on the Harvard Odyssey and CfA/ITC clusters, the Ranger and Stampede supercomputers at the Texas Advanced Computing Center as part of XSEDE, the Kraken supercomputer at Oak Ridge National Laboratory as part of XSEDE, the CURIE supercomputer at CEA/France as part of PRACE project RA0844, and the SuperMUC computer at the Leibniz Computing Centre, Germany, as part of project pr85je. LH acknowledges support from NASA grant NNX12AC67G and NSF grant AST-1312095. VS acknowledges support from the European Research Council through ERC-StG grant EXAGAL-308037. NR 31 TC 14 Z9 14 U1 0 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB 11 PY 2015 VL 447 IS 1 BP L6 EP L10 DI 10.1093/mnrasl/slu173 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CQ4CR UT WOS:000360552300002 ER PT J AU Mortlock, A Conselice, CJ Hartley, WG Duncan, K Lani, C Ownsworth, JR Almaini, O van der Wel, A Huang, KH Ashby, MLN Willner, SP Fontana, A Dekel, A Koekemoer, AM Ferguson, HC Faber, SM Grogin, NA Kocevski, DD AF Mortlock, Alice Conselice, Christopher. J. Hartley, William G. Duncan, Ken Lani, Caterina Ownsworth, Jamie R. Almaini, Omar van der Wel, Arjen Huang, Kuang-Han Ashby, Matthew L. N. Willner, S. P. Fontana, Adriano Dekel, Avishai Koekemoer, Anton M. Ferguson, Harry C. Faber, Sandra M. Grogin, Norman A. Kocevski, Dale D. TI Deconstructing the galaxy stellar mass function with UKIDSS and CANDELS: the impact of colour, structure and environment SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: evolution; galaxies: formation; galaxies: luminosity function, mass function; galaxies: structure ID SIMILAR-TO 2; MORPHOLOGY-DENSITY RELATION; STAR-FORMATION RATES; EXTRAGALACTIC LEGACY SURVEY; GOODS NICMOS SURVEY; ULTRA-DEEP SURVEY; COSMIC EVOLUTION SURVEY; HUBBLE-SPACE-TELESCOPE; HIGH-REDSHIFT GALAXIES; LY-ALPHA EMITTERS AB We combine photometry from the Ultra Deep Survey (UDS), Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey (CANDELS) UDS and CANDELS the Great Observatories Origins Deep Survey-South (GOODS-S) surveys to construct the galaxy stellar mass function probing both the low-and high-mass end accurately in the redshift range 0.3 < z < 3. The advantages of using a homogeneous concatenation of these data sets include meaningful measures of environment in the UDS, due to its large area (0.88 deg(2)), and the high-resolution deep imaging in CANDELS (H-160 > 26.0), affording us robust measures of structural parameters. We construct stellar mass functions for the entire sample as parametrized by the Schechter function, and find that there is a decline in the values of phi and of alpha with higher redshifts, and a nearly constant M* up to z similar to 3. We divide the galaxy stellar mass function by colour, structure, and environment and explore the links between environmental overdensity, morphology, and the quenching of star formation. We find that a double Schechter function describes galaxies with high Sersic index (n > 2.5), similar to galaxies which are red or passive. The low-mass end of the n > 2.5 stellar mass function is dominated by blue galaxies, whereas the high-mass end is dominated by red galaxies. This shows that there is a possible link between morphological evolution and star formation quenching in high mass galaxies, which is not seen in lower mass systems. This in turn suggests that there are strong mass-dependent quenching mechanisms. In addition, we find that the number density of high-mass systems is elevated in dense environments, suggesting that an environmental process is building up massive galaxies quicker in over densities than in lower densities. C1 [Mortlock, Alice; Conselice, Christopher. J.; Hartley, William G.; Duncan, Ken; Lani, Caterina; Ownsworth, Jamie R.; Almaini, Omar] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. [Mortlock, Alice] Univ Edinburgh, Inst Astron, SUPA, Edinburgh EH9 3HJ, Midlothian, Scotland. [Hartley, William G.] ETH, Inst Astron, CH-8093 Zurich, Switzerland. [van der Wel, Arjen] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Huang, Kuang-Han] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Ashby, Matthew L. N.; Willner, S. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Fontana, Adriano] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy. [Dekel, Avishai] Hebrew Univ Jerusalem, Racah Inst Phys, IL-91904 Jerusalem, Israel. [Koekemoer, Anton M.; Ferguson, Harry C.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Faber, Sandra M.; Grogin, Norman A.] Univ Calif Santa Cruz, Dept Astron & Astrophys, UCO Lick Observ, Santa Cruz, CA 95064 USA. [Kocevski, Dale D.] Univ Kentucky, Dept Phys & Astron, Lexington, KY 40506 USA. RP Mortlock, A (reprint author), Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. EM alicem@roe.ac.uk OI Duncan, Kenneth/0000-0001-6889-8388; Almaini, Omar/0000-0001-9328-3991; Koekemoer, Anton/0000-0002-6610-2048; fontana, adriano/0000-0003-3820-2823 FU STFC; European Research Council; Leverhulme trust FX AM acknowledges funding from the STFC and a European Research Council Consolidator Grant (PI: McLure). We also acknowledge funding from the Leverhulme trust. NR 119 TC 33 Z9 33 U1 0 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB 11 PY 2015 VL 447 IS 1 BP 2 EP 24 DI 10.1093/mnras/stu2403 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CC3TK UT WOS:000350272700001 ER PT J AU Sadowski, A Narayan, R Tchekhovskoy, A Abarca, D Zhu, YC McKinney, JC AF Sadowski, Aleksander Narayan, Ramesh Tchekhovskoy, Alexander Abarca, David Zhu, Yucong McKinney, Jonathan C. TI Global simulations of axisymmetric radiative black hole accretion discs in general relativity with a mean-field magnetic dynamo SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; black hole physics; relativistic processes; methods: numerical; galaxies: jets ID MAGNETOHYDRODYNAMIC SIMULATIONS; DOMINATED ACCRETION; NUMERICAL SIMULATIONS; COMPARABLE RADIATION; TRANSFER EQUATION; THICK ACCRETION; GODUNOV METHOD; GAS-PRESSURE; M1 CLOSURE; DISKS AB We present a mean-field model that emulates the magnetic dynamo operating in magnetized accretion discs. We have implemented this model in the general relativisic radiation magnetohydrodynamic (GRRMHD) code KORAL, using results from local shearing sheet simulations of the magnetorotational instability to fix the parameters of the dynamo. With the inclusion of this dynamo, we are able to run 2D axisymmetric GRRMHD simulations of accretion discs for arbitrarily long times. The simulated discs exhibit sustained turbulence, with the poloidal and toroidal magnetic field components driven towards a state similar to that seen in 3D studies. Using this dynamo code, we present a set of long-duration global simulations of super-Eddington, optically thick discs around non-spinning and spinning black holes. Super-Eddington discs around non-rotating black holes exhibit a surprisingly large efficiency, eta approximate to 0.04, independent of the accretion rate, where we measure efficiency in terms of the total energy output, both radiation and mechanical, flowing out to infinity. This value significantly exceeds the efficiency predicted by slim disc models for these accretion rates. Super-Eddington discs around spinning black holes are even more efficient, and appear to extract black hole rotational energy through a process similar to the Blandford-Znajek mechanism. All the simulated models are characterized by highly super-Eddington radiative fluxes collimated along the rotation axis. We also present a set of simulations that were designed to have Eddington or slightly sub-Eddington accretion rates ((M) over dot less than or similar to 2 (M) over dot(Edd)). None of these models reached a steady state. Instead, the discs collapsed as a result of runaway cooling, presumably because of a thermal instability. C1 [Sadowski, Aleksander; Narayan, Ramesh; Abarca, David; Zhu, Yucong] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02134 USA. [Tchekhovskoy, Alexander] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [McKinney, Jonathan C.] Univ Maryland, Dept Phys, Joint Space Sci Inst, College Pk, MD 20742 USA. RP Sadowski, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02134 USA. EM asadowski@cfa.harvard.edu OI Narayan, Ramesh/0000-0002-1919-2730 FU NSF [AST1312651]; NASA [TCAN NNX14AB47G, NAS8-03060]; NASA by the Chandra X-ray Center [PF3-140115]; NSF via XSEDE resources [TG-AST080026N, TG-AST100040] FX AS and RN were supported in part by NSF grant AST1312651 and NASA grant TCAN NNX14AB47G. AT was supported by NASA through Einstein Postdoctoral Fellowship grant number PF3-140115 awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. We also acknowledge computational support from NSF via XSEDE resources (grant TG-AST080026N to RN and AS, and grant TG-AST100040 to AT), and from NASA (to RN and AS) via the High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center. The authors thank Dimitrios Psaltis and the anonymous referee for valuable comments on the manuscript. NR 67 TC 34 Z9 34 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 11 PY 2015 VL 447 IS 1 BP 49 EP 71 DI 10.1093/mnras/stu2387 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CC3TK UT WOS:000350272700004 ER PT J AU Parker, ML Fabian, AC Matt, G Koljonen, KII Kara, E Alston, W Walton, DJ Marinucci, A Brenneman, L Risaliti, G AF Parker, M. L. Fabian, A. C. Matt, G. Koljonen, K. I. I. Kara, E. Alston, W. Walton, D. J. Marinucci, A. Brenneman, L. Risaliti, G. TI Revealing the X-ray variability of AGN with principal component analysis SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: active; galaxies: nuclei; galaxies: Seyfert ID ACTIVE GALACTIC NUCLEI; XMM-NEWTON OBSERVATIONS; GALAXY NGC 3516; SPECTRAL VARIABILITY; BLACK-HOLE; ACCRETION DISK; PDS 456; REVERBERATION LAGS; WARM ABSORBER; EVENT HORIZON AB We analyse a sample of 26 active galactic nuclei (AGN) with deep XMM-Newton observations, using principal component analysis (PCA) to find model-independent spectra of the different variable components. In total, we identify at least 12 qualitatively different patterns of spectral variability, involving several different mechanisms, including five sources which show evidence of variable relativistic reflection (MCG-6-30-15, NGC 4051, 1H 0707-495, NGC 3516 and Mrk 766) and three which show evidence of varying partial covering neutral absorption (NGC 4395, NGC 1365 and NGC 4151). In over half of the sources studied, the variability is dominated by changes in a power-law continuum, both in terms of changes in flux and power-law index, which could be produced by propagating fluctuations within the corona. Simulations are used to find unique predictions for different physical models, and we then attempt to qualitatively match the results from the simulations to the behaviour observed in the real data. We are able to explain a large proportion of the variability in these sources using simple models of spectral variability, but more complex models may be needed for the remainder. We have begun the process of building up a library of different principal components, so that spectral variability in AGN can quickly be matched to physical processes. We show that PCA can be an extremely powerful tool for distinguishing different patterns of variability in AGN, and that it can be used effectively on the large amounts of high-quality archival data available from the current generation of X-ray telescopes. We will make our PCA code available upon request to the lead author. C1 [Parker, M. L.; Fabian, A. C.; Kara, E.; Alston, W.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Matt, G.; Marinucci, A.] Univ Rome Tre, Dipartimento Matemat & Fis, I-00146 Rome, Italy. [Koljonen, K. I. I.] Aalto Univ, Metsahovi Radio Observ, FIN-02540 Kylmala, Finland. [Koljonen, K. I. I.] New York Univ Abu Dhabi, Abu Dhabi, U Arab Emirates. [Walton, D. J.] CALTECH, Pasadena, CA 91125 USA. [Brenneman, L.; Risaliti, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Risaliti, G.] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. RP Parker, ML (reprint author), Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. EM mlparker@ast.cam.ac.uk OI Risaliti, Guido/0000-0002-3556-977X FU Science and Technology Facilities Council (STFC) FX MLP acknowledges financial support from the Science and Technology Facilities Council (STFC). NR 89 TC 9 Z9 9 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 11 PY 2015 VL 447 IS 1 BP 72 EP 96 DI 10.1093/mnras/stu2424 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CC3TK UT WOS:000350272700005 ER PT J AU White, M Reid, B Chuang, CH Tinker, JL McBride, CK Prada, F Samushia, L AF White, Martin Reid, Beth Chuang, Chia-Hsun Tinker, Jeremy L. McBride, Cameron K. Prada, Francisco Samushia, Lado TI Tests of redshift-space distortions models in configuration space for the analysis of the BOSS final data release SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE gravitation; galaxies: haloes; galaxies: statistics; cosmological parameters; large-scale structure of Universe ID OSCILLATION SPECTROSCOPIC SURVEY; HALO OCCUPATION DISTRIBUTION; COSMOLOGICAL MASS DENSITY; DIGITAL SKY SURVEY; SDSS-III; POWER SPECTRUM; GROWTH-RATE; LINEAR REGIME; LUMINOSITY DEPENDENCE; SYSTEMATIC-ERRORS AB Observations of redshift-space distortions in spectroscopic galaxy surveys offer an attractive method for observing the build-up of cosmological structure, which depends both on the expansion rate of the Universe and our theory of gravity. In preparation for analysis of redshift-space distortions from the Baryon Oscillation Spectroscopic Survey (BOSS) final data release, we compare a number of analytic and phenomenological models, specified in configuration space, to mock catalogues derived in different ways from several N-body simulations. The galaxies in each mock catalogue have properties similar to those of the higher redshift galaxies measured by BOSS but differ in the details of how small-scale velocities and halo occupancy are determined. We find that all of the analytic models fit the simulations over a limited range of scales while failing at small scales. We discuss which models are most robust and on which scales they return reliable estimates of the rate of growth of structure: we find that models based on some form of resummation can fit our N-body data for BOSS-like galaxies above 30 h(-1) Mpc well enough to return unbiased parameter estimates. C1 [White, Martin] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [White, Martin] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [White, Martin; Reid, Beth] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Chuang, Chia-Hsun; Prada, Francisco] Univ Autonoma Madrid, CSIC, Inst Fis Teor, E-28049 Madrid, Spain. [Tinker, Jeremy L.] NYU, Ctr Cosmol & Particle Phys, New York, NY 10003 USA. [McBride, Cameron K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Prada, Francisco] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain. [Samushia, Lado] Kansas State Univ, Dept Phys, Manhattan, KS 66506 USA. [Samushia, Lado] Ilia State Univ, Natl Abastumani Astrophys Observ, GE-1060 Tbilisi, Rep of Georgia. RP White, M (reprint author), Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. EM mwhite@berkeley.edu RI White, Martin/I-3880-2015 OI White, Martin/0000-0001-9912-5070 FU NASA; Leibniz-Institute for Astrophysics Potsdam (AIP) [CSD2009-00064]; Spanish MultiDark Consolider Project [CSD2009-00064] FX MW would like to thank Chris Blake for helpful comments on an early draft of the manuscript. MW is supported by NASA. This work made extensive use of the NASA Astrophysics Data System and of the astro-ph preprint archive at arXiv.org. The analysis made use of the computing resources of the National Energy Research Scientific Computing Center. The MultiDark Database used in this paper and the web application providing online access to it were constructed as part of the activities of the German Astrophysical Virtual Observatory as result of a collaboration between the Leibniz-Institute for Astrophysics Potsdam (AIP) and the Spanish MultiDark Consolider Project CSD2009-00064. The BigMD simulation suite was performed in the supercomputer at LRZ. NR 90 TC 18 Z9 18 U1 0 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB 11 PY 2015 VL 447 IS 1 BP 234 EP 245 DI 10.1093/mnras/stu2460 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CC3TK UT WOS:000350272700017 ER PT J AU Petroff, E Bailes, M Barr, ED Barsdell, BR Bhat, NDR Bian, F Burke-Spolaor, S Caleb, M Champion, D Chandra, P Da Costa, G Delvaux, C Flynn, C Gehrels, N Greiner, J Jameson, A Johnston, S Kasliwal, MM Keane, EF Keller, S Kocz, J Kramer, M Leloudas, G Malesani, D Mulchaey, JS Ng, C Ofek, EO Perley, DA Possenti, A Schmidt, BP Shen, Y Stappers, B Tisserand, P van Straten, W Wolf, C AF Petroff, E. Bailes, M. Barr, E. D. Barsdell, B. R. Bhat, N. D. R. Bian, F. Burke-Spolaor, S. Caleb, M. Champion, D. Chandra, P. Da Costa, G. Delvaux, C. Flynn, C. Gehrels, N. Greiner, J. Jameson, A. Johnston, S. Kasliwal, M. M. Keane, E. F. Keller, S. Kocz, J. Kramer, M. Leloudas, G. Malesani, D. Mulchaey, J. S. Ng, C. Ofek, E. O. Perley, D. A. Possenti, A. Schmidt, B. P. Shen, Yue Stappers, B. Tisserand, P. van Straten, W. Wolf, C. TI A real-time fast radio burst: polarization detection and multiwavelength follow-up SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE polarization; radiation mechanisms: general; intergalactic medium; radio continuum: general ID GAMMA-RAY BURST; 25 APRIL 1998; CIRCULAR-POLARIZATION; UNUSUAL SUPERNOVA; MAGNETIC-FIELD; PULSAR SURVEY; CRAB PULSAR; AD LEONIS; EMISSION; DISCOVERY AB Fast radio bursts (FRBs) are one of the most tantalizing mysteries of the radio sky; their progenitors and origins remain unknown and until now no rapid multiwavelength follow-up of an FRB has been possible. New instrumentation has decreased the time between observation and discovery from years to seconds, and enables polarimetry to be performed on FRBs for the first time. We have discovered an FRB (FRB 140514) in real-time on 2014 May 14 at 17:14:11.06 UTC at the Parkes radio telescope and triggered follow-up at other wavelengths within hours of the event. FRB 140514 was found with a dispersion measure (DM) of 562.7(6) cm(-3) pc, giving an upper limit on source redshift of z less than or similar to 0.5. FRB 140514 was found to be 21 +/- 7 per cent (3 sigma) circularly polarized on the leading edge with a 1 sigma upper limit on linear polarization <10 per cent. We conclude that this polarization is intrinsic to the FRB. If there was any intrinsic linear polarization, as might be expected from coherent emission, then it may have been depolarized by Faraday rotation caused by passing through strong magnetic fields and/or high-density environments. FRB 140514 was discovered during a campaign to re-observe known FRB fields, and lies close to a previous discovery, FRB 110220; based on the difference in DMs of these bursts and time-on-sky arguments, we attribute the proximity to sampling bias and conclude that they are distinct objects. Follow-up conducted by 12 telescopes observing from X-ray to radio wavelengths was unable to identify a variable multiwavelength counterpart, allowing us to rule out models in which FRBs originate from nearby (z < 0.3) supernovae and long duration gamma-ray bursts. C1 [Petroff, E.; Bailes, M.; Barr, E. D.; Caleb, M.; Flynn, C.; Jameson, A.; Keane, E. F.; van Straten, W.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Petroff, E.; Johnston, S.] Australia Telescope Natl Facil, CSIRO Astron & Space Sci, Epping, NSW 1710, Australia. [Barsdell, B. R.; Kocz, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bhat, N. D. R.] Curtin Univ, Int Ctr Radio Astron Res, Bentley, WA 6102, Australia. [Bian, F.; Caleb, M.; Da Costa, G.; Keller, S.; Schmidt, B. P.; Tisserand, P.; Wolf, C.] Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. [Burke-Spolaor, S.; Perley, D. A.] CALTECH, Cahill Ctr Astrophys, Pasadena, CA 91125 USA. [Champion, D.; Kramer, M.; Ng, C.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Chandra, P.] Tata Inst Fundamental Res, Natl Ctr Radio Astrophys, Pune 411007, Maharashtra, India. [Delvaux, C.; Greiner, J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Gehrels, N.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Kasliwal, M. M.; Mulchaey, J. S.] Observ Carnegie Inst Sci, Pasadena, CA 91101 USA. [Kocz, J.; Shen, Yue] CALTECH, Jet Prop Lab, Pasadena, CA 91104 USA. [Kramer, M.; Stappers, B.] Univ Manchester, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Leloudas, G.; Malesani, D.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr DARK, DK-2100 Copenhagen O, Denmark. [Leloudas, G.; Ofek, E. O.] Weizmann Inst Sci, Dept Particle Phys & Astrophys, IL-76100 Rehovot, Israel. [Possenti, A.] INAF Osservatorio Astron Cagliari, I-09047 Selargius, CA, Italy. [Shen, Yue] Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China. [Tisserand, P.] Univ Paris 06, Inst Astrophys Paris, Sorbonne Univ, F-75005 Paris, France. [Tisserand, P.] CNRS, UMR 7095, Inst Astrophys, F-75014 Paris, France. RP Petroff, E (reprint author), Swinburne Univ Technol, Ctr Astrophys & Supercomp, POB 218, Hawthorn, Vic 3122, Australia. EM epetroff@astro.swin.edu.au OI Champion, David/0000-0003-1361-7723; Schmidt, Brian/0000-0001-6589-1287; van Straten, Willem/0000-0003-2519-7375 FU Commonwealth of Australia; Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO) [CE110001020]; ARC [DP120101237]; Leibniz-Prize; DFG [HA 1850/28-1]; Danish National Research council; Curtin Research Fellowship; EXTraS - European Union [607452]; Hubble Fellowship; Carnegie-Princeton Fellowship; Instrument Center for Danish Astrophysics (IDA); Willner Family Leadership Institute Ilan Gluzman (Secaucus NJ); Israeli Ministry of Science; Israel Science Foundation; Minerva; Weizmann-UK; I-CORE Program of the Planning and Budgeting Committee; NASA by the Space Telescope Science Institute [HST-HF-51296.01-A]; NASA [NAS 5-26555]; ARC via CAASTRO; [LF0992131] FX The Parkes radio telescope and the ATCA are part of the Australia Telescope National Facility which is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. Parts of this research were conducted by the Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO), through project number CE110001020. We thank the staff of the GMRT that made these observations possible. GMRT is run by the National Centre for Radio Astrophysics of the Tata Institute of Fundamental Research. Research with the ANU SkyMapper telescope is supported in part through ARC Discovery Grant DP120101237. We thank the Carnegie Supernova Project team (PI M. Phillips) and intermediate Palomar Transient Factory team (PI S. Kulkarni) for promptly taking follow-up data. Part of the funding for GROND (both hardware as well as personnel) was generously granted from the Leibniz-Prize to Professor G. Hasinger (DFG grand HA 1850/28-1). The Dark Cosmology Centre is supported by the Danish National Research council. We thank A. Krauss for prompt observations with the Effelsberg Radio Telescope. Partly based on observations made with the NOT, operated by the Nordic Optical Telescope Scientific Association at the Observatorio del Roque de los Muchachos, La Palma, Spain, of the Instituto de Astrofisica de Canarias.; We thank the anonymous referee for valuable input which improved the clarity of this paper. EP would like to thank M. Murphy, J. Cooke, and C. Vale for useful discussion and valuable comments. NDRB is supported by a Curtin Research Fellowship. CD acknowledges support through EXTraS, funded from the European Union's Seventh Framework Programme for research, technological development and demonstration under grant agreement no 607452. MMK acknowledges generous support from the Hubble Fellowship and Carnegie-Princeton Fellowship. DM acknowledged the Instrument Center for Danish Astrophysics (IDA) for support. EOO is incumbent of the Arye Dissentshik career development chair and is grateful to support by grants from the Willner Family Leadership Institute Ilan Gluzman (Secaucus NJ), Israeli Ministry of Science, Israel Science Foundation, Minerva, Weizmann-UK and the I-CORE Program of the Planning and Budgeting Committee and The Israel Science Foundation. Support for DAP was provided by NASA through Hubble Fellowship grant HST-HF-51296.01-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. BPS, CW, and PT acknowledge funding from the ARC via CAASTRO and grand LF0992131. NR 55 TC 76 Z9 76 U1 2 U2 6 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB 11 PY 2015 VL 447 IS 1 BP 246 EP 255 DI 10.1093/mnras/stu2419 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CC3TK UT WOS:000350272700018 ER PT J AU Fox, OD Silverman, JM Filippenko, AV Mauerhan, J Becker, J Borish, HJ Cenko, SB Clubb, KI Graham, M Hsiao, E Kelly, PL Lee, WH Marion, GH Milisavljevic, D Parrent, J Shivvers, I Skrutskie, M Smith, N Wilson, J Zheng, WK AF Fox, Ori D. Silverman, Jeffrey M. Filippenko, Alexei V. Mauerhan, Jon Becker, Juliette Borish, H. Jacob Cenko, S. Bradley Clubb, Kelsey I. Graham, Melissa Hsiao, Eric Kelly, Patrick L. Lee, William H. Marion, G. H. Milisavljevic, Dan Parrent, Jerod Shivvers, Isaac Skrutskie, Michael Smith, Nathan Wilson, John Zheng, Weikang TI On the nature of Type IIn/Ia-CSM supernovae: optical and near-infrared spectra of SN 2012ca and SN 2013dn SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE circumstellar matter; supernovae: general; supernovae: individual: SN2005ip; supernovae: individual: SN 2009dc; supernovae: individual: SN 2012ca; supernovae: individual: SN 2013dn ID CORE-COLLAPSE SUPERNOVAE; IA SUPERNOVAE; CIRCUMSTELLAR MEDIUM; DUST FORMATION; MASSIVE STAR; STRIPPED-ENVELOPE; I. OBSERVATIONS; II SUPERNOVAE; SKY SURVEY; SPECTROSCOPY AB A growing subset of Type Ia supernovae (SNe Ia) shows evidence via narrow emission lines for unexpected interaction with a dense circumstellar medium (SNe IIn/Ia-CSM). The precise nature of the progenitor, however, remains debated owing to spectral ambiguities arising from a strong contribution from the CSM interaction. Late-time spectra offer potential insight if the post-shock cold, dense shell becomes sufficiently thin and/or the ejecta begin to cross the reverse shock. To date, only a few high-quality spectra of this kind exist. Here we report on the late-time optical and infrared spectra of the SNe Ia-CSM 2012ca and 2013dn. These SNe Ia-CSM spectra exhibit low [Fe III]/[Fe II] ratios and strong [Ca II] at late epochs. Such characteristics are reminiscent of the super-Chandrasekhar-mass candidate SN 2009dc, for which these features suggested a low-ionization state due to high densities, although the broad Fe features admittedly show similarities to the blue 'quasi-continuum' observed in some core collapse SNe Ibn and IIn. Neither SN 2012ca nor any of the other SNe Ia-CSM in this paper show evidence for broad oxygen, carbon, or magnesium in their spectra. Similar to the interacting Type IIn SN 2005ip, a number of high-ionization lines are identified in SN 2012ca, including [S III], [Ar III], [Ar X], [Fe VIII], [Fe X], and possibly [Fe XI]. The total bolometric energy output does not exceed 10(51) erg, but does require a large kinetic-to-radiative conversion efficiency. All of these observations taken together suggest that SNe Ia-CSM are more consistent with a thermonuclear explosion than a core collapse event, although detailed radiative transfer models are certainly necessary to confirm these results. C1 [Fox, Ori D.; Filippenko, Alexei V.; Mauerhan, Jon; Clubb, Kelsey I.; Graham, Melissa; Kelly, Patrick L.; Shivvers, Isaac; Zheng, Weikang] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Silverman, Jeffrey M.; Marion, G. H.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Becker, Juliette] CALTECH, Cahill Ctr Astrophys, Pasadena, CA 91125 USA. [Borish, H. Jacob; Skrutskie, Michael; Wilson, John] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Cenko, S. Bradley] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Cenko, S. Bradley] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA. [Hsiao, Eric] Carnegie Inst Sci, Las Campanas Observ, Casilla 601, Chile. [Hsiao, Eric] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark. [Lee, William H.] Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico. [Milisavljevic, Dan; Parrent, Jerod] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Smith, Nathan] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. RP Fox, OD (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. EM ofox@berkeley.edu OI Shivvers, Isaac/0000-0003-3373-8047; Becker, Juliette/0000-0002-7733-4522 FU NSF [PHYS-1066293, AST-1211916]; W. M. Keck Foundation; NASA [NNX09AH71G, NNX09AT02G, NNX10AI27G, NNX12AE66G]; CONACyT [INFR-2009-01-122785]; UNAM PAPIIT [IN113810]; UC MEXUS-CONACyT; NSF Astronomy and Astrophysics Postdoctoral Fellowship [AST-1302771]; TABASGO Foundation; Richard and Rhoda Goldman Fund; Christopher R. Redlich Fund FX We thank the referee, Stefano Benetti, for useful comments that strengthened this paper. Insightful discussions were shared with many at the Aspen Center for Physics, including Ryan Foley, Ryan Chornock, and Craig Wheeler. This work was supported in part by NSF Grant No. PHYS-1066293 and the hospitality of the Aspen Center for Physics. 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 are grateful to the staffs of the Lick and Keck Observatory for their assistance with the observations, and thank the RATIR instrument team and the staff of the Observatorio Astronomico Nacional on Sierra San Pedro Martir. RATIR is a collaboration between the University of California, the Universidad Nacional Autonoma de Mexxico, NASA Goddard Space Flight Center, and Arizona State University, benefiting from the loan of an H2RG detector from Teledyne Scientific and Imaging. RATIR, the automation of the Harold L. Johnson Telescope of the Observatorio Astronomico Nacional on Sierra, San Pedro, Martir, and the operation of both is funded by the partner institutions and through NASA grants NNX09AH71G, NNX09AT02G, NNX10AI27G, and NNX12AE66G, CONACyT grant INFR-2009-01-122785, UNAM PAPIIT grant IN113810, and a UC MEXUS-CONACyT grant. JMS is supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-1302771. AVF's supernova group at UC Berkeley received support through NSF grant AST-1211916, the TABASGO Foundation, Gary and Cynthia Bengier, the Richard and Rhoda Goldman Fund, and the Christopher R. Redlich Fund. NR 102 TC 11 Z9 11 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 11 PY 2015 VL 447 IS 1 BP 772 EP 785 DI 10.1093/mnras/stu2435 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CC3TK UT WOS:000350272700061 ER PT J AU Boyajian, T von Braun, K Feiden, GA Huber, D Basu, S Demarque, P Fischer, DA Schaefer, G Mann, AW White, TR Maestro, V Brewer, J Lamell, CB Spada, F Lopez-Morales, M Ireland, M Farrington, C van Belle, GT Kane, SR Jones, J ten Brummelaar, TA Ciardi, DR McAlister, HA Ridgway, S Goldfinger, PJ Turner, NH Sturmann, L AF Boyajian, Tabetha von Braun, Kaspar Feiden, Gregory A. Huber, Daniel Basu, Sarbani Demarque, Pierre Fischer, Debra A. Schaefer, Gail Mann, Andrew W. White, Timothy R. Maestro, Vicente Brewer, John Lamell, C. Brooke Spada, Federico Lopez-Morales, Mercedes Ireland, Michael Farrington, Chris van Belle, Gerard T. Kane, Stephen R. Jones, Jeremy ten Brummelaar, Theo A. Ciardi, David R. McAlister, Harold A. Ridgway, Stephen Goldfinger, P. J. Turner, Nils H. Sturmann, Laszlo TI Stellar diameters and temperatures - VI. High angular resolution measurements of the transiting exoplanet host stars HD 189733 and HD 209458 and implications for models of cool dwarfs SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE techniques: interferometric; stars: fundamental parameters; stars: individual: HD 189733; stars: individual: HD 209458; stars: late-type; infrared: stars ID INFRARED FLUX METHOD; INTEGRAL-FIELD SPECTROGRAPH; BASE-LINE INTERFEROMETRY; VIRTUAL OBSERVATORY TOOL; LOW-MASS STARS; CHARA ARRAY; ASTROPHYSICAL PARAMETERS; FUNDAMENTAL PROPERTIES; EXTRASOLAR PLANETS; MAIN-SEQUENCE AB We present direct radii measurements of the well-known transiting exoplanet host stars HD 189733 and HD 209458 using the CHARA Array interferometer. We find the limb-darkened angular diameters to be theta(LD) = 0.3848 +/- 0.0055 and 0.2254 +/- 0.0072 mas for HD 189733 and HD 209458, respectively. HD 189733 and HD 209458 are currently the only two transiting exoplanet systems where detection of the respective planetary companion's orbital motion from high-resolution spectroscopy has revealed absolute masses for both star and planet. We use our new measurements together with the orbital information from radial velocity and photometric time series data, Hipparcos distances, and newly measured bolometric fluxes to determine the stellar effective temperatures (T-eff = 4875 +/- 43, 6092 +/- 103 K), stellar linear radii (R-* = 0.805 +/- 0.016, 1.203 +/- 0.061 R-circle dot), mean stellar densities (rho(*) = 1.62 +/- 0.11, 0.58 +/- 0.14 rho(circle dot)), planetary radii (R-p = 1.216 +/- 0.024, 1.451 +/- 0.074 R-Jup), and mean planetary densities (rho(p) = 0.605 +/- 0.029, 0.196 +/- 0.033 rho(Jup)) for HD 189733b and HD 209458b, respectively. The stellar parameters for HD 209458, an F9 dwarf, are consistent with indirect estimates derived from spectroscopic and evolutionary modelling. However, we find that models are unable to reproduce the observational results for the K2 dwarf, HD 189733. We show that, for stellar evolutionary models to match the observed stellar properties of HD 189733, adjustments lowering the solar-calibrated mixing-length parameter to alpha(MLT) = 1.34 need to be employed. C1 [Boyajian, Tabetha; Basu, Sarbani; Demarque, Pierre; Fischer, Debra A.; Brewer, John; Lamell, C. Brooke] Yale Univ, New Haven, CT 06520 USA. [von Braun, Kaspar] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [von Braun, Kaspar] Mirasol Inst, D-81679 Munich, Germany. [von Braun, Kaspar; van Belle, Gerard T.] Lowell Observ, Flagstaff, AZ 86001 USA. [Feiden, Gregory A.] Uppsala Univ, Dept Phys & Astron, SE-75120 Uppsala, Sweden. [Huber, Daniel] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Huber, Daniel] SETI Inst, Mountain View, CA 94043 USA. [Schaefer, Gail; Farrington, Chris; ten Brummelaar, Theo A.; Goldfinger, P. J.; Turner, Nils H.; Sturmann, Laszlo] Mt Wilson Observ, CHARA Array, Mount Wilson, CA 91023 USA. [Mann, Andrew W.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [White, Timothy R.] Univ Gottingen, Inst Astrophys, D-37077 Gottingen, Germany. [Maestro, Vicente] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia. [Spada, Federico] Leibniz Inst f ur Astrophys Potsdam AIP, D-14482 Potsdam, Germany. [Lopez-Morales, Mercedes] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ireland, Michael] Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. [Kane, Stephen R.] San Francisco State Univ, Dept Phys & Astron, San Francisco, CA 94132 USA. [Jones, Jeremy; McAlister, Harold A.] Georgia State Univ, Ctr High Angular Resolut Astron, Atlanta, GA 30303 USA. [Jones, Jeremy; McAlister, Harold A.] Georgia State Univ, Dept Phys & Astron, Atlanta, GA 30303 USA. [Ciardi, David R.] CALTECH, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Ridgway, Stephen] Natl Opt Astron Observ, Tucson, AZ 85719 USA. RP Boyajian, T (reprint author), Yale Univ, New Haven, CT 06520 USA. EM tabetha.boyajian@yale.edu RI Feiden, Gregory/F-1505-2015; OI Feiden, Gregory/0000-0002-2012-7215; Spada, Federico/0000-0001-6948-4259; Brewer, John/0000-0002-9873-1471; Ciardi, David/0000-0002-5741-3047 FU NASA [ADAP12-0172, 14-XRP14_2-0147, NNX14AB92G]; NSF [AST-1105930]; National Science Foundation through NSF [AST-0606958, AST-0908253]; Georgia State University through the College of Arts and Sciences; W. M. Keck Foundation FX TSB acknowledges support provided through NASA grants ADAP12-0172 and 14-XRP14_2-0147. DH acknowledges support by NASA Grant NNX14AB92G issued through the Kepler Participating Scientist Program. SB acknowledges partial support of NSF grant AST-1105930. Judit Sturmann keeps some tight beams in place - hats off to you girl! The CHARA Array is funded by the National Science Foundation through NSF grants AST-0606958 and AST-0908253 and by Georgia State University through the College of Arts and Sciences, as well as the W. M. Keck Foundation. This research made use of the SIMBAD and VIZIER Astronomical Databases, operated at CDS, Strasbourg, France (http://cdsweb.u-strasbg.fr/), and of NASA's Astrophysics Data System, of the Jean-Marie Mariotti Center SearchCal service (http://www.jmmc.fr/searchcal), co-developed by FIZEAU and LAOG/IPAG. NR 120 TC 17 Z9 17 U1 1 U2 2 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB 11 PY 2015 VL 447 IS 1 BP 846 EP 857 DI 10.1093/mnras/stu2502 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CC3TK UT WOS:000350272700066 ER PT J AU Breitburg, DL Hondorp, D Audemard, C Carnegie, RB Burrell, RB Trice, M Clark, V AF Breitburg, Denise L. Hondorp, Darryl Audemard, Corinne Carnegie, Ryan B. Burrell, Rebecca B. Trice, Mark Clark, Virginia TI Landscape-Level Variation in Disease Susceptibility Related to Shallow-Water Hypoxia SO PLOS ONE LA English DT Article ID REAL-TIME PCR; PARASITE PERKINSUS-MARINUS; CHESAPEAKE BAY; HYPERCAPNIC HYPOXIA; VIBRIO-PARAHAEMOLYTICUS; CRASSOSTREA-VIRGINICA; OYSTER POPULATIONS; DISSOLVED-OXYGEN; IMMUNE-RESPONSE; DYNAMICS AB Diel-cycling hypoxia is widespread in shallow portions of estuaries and lagoons, especially in systems with high nutrient loads resulting from human activities. Far less is known about the effects of this form of hypoxia than deeper-water seasonal or persistent low dissolved oxygen. We examined field patterns of diel-cycling hypoxia and used field and laboratory experiments to test its effects on acquisition and progression of Perkinsus marinus infections in the eastern oyster, Crassostrea virginica, as well as on oyster growth and filtration. P. marinus infections cause the disease known as Dermo, have been responsible for declines in oyster populations, and have limited success of oyster restoration efforts. The severity of diel-cycling hypoxia varied among shallow monitored sites in Chesapeake Bay, and average daily minimum dissolved oxygen was positively correlated with average daily minimum pH. In both field and laboratory experiments, diel-cycling hypoxia increased acquisition and progression of infections, with stronger results found for younger (1-year-old) than older (2-3-year-old) oysters, and more pronounced effects on both infections and growth found in the field than in the laboratory. Filtration by oysters was reduced during brief periods of exposure to severe hypoxia. This should have reduced exposure to waterborne P. marinus, and contributed to the negative relationship found between hypoxia frequency and oyster growth. Negative effects of hypoxia on the host immune response is, therefore, the likely mechanism leading to elevated infections in oysters exposed to hypoxia relative to control treatments. Because there is considerable spatial variation in the frequency and severity of hypoxia, diel-cycling hypoxia may contribute to landscape-level spatial variation in disease dynamics within and among estuarine systems. C1 [Breitburg, Denise L.; Hondorp, Darryl; Burrell, Rebecca B.; Clark, Virginia] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Hondorp, Darryl] USGS Great Lakes Sci Ctr, Ann Arbor, MI 48105 USA. [Audemard, Corinne; Carnegie, Ryan B.] Coll William & Mary, Virginia Inst Marine Sci, Gloucester Point, VA 23062 USA. [Trice, Mark] Maryland Dept Nat Resources, Annapolis, MD 21401 USA. RP Breitburg, DL (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM breitburgd@si.edu FU MD Sea Grant [SA7528085-CC]; Smithsonian Institution Johnson Fund; Smithsonian Women's Committee FX Research was funded by Award # SA7528085-CC from MD Sea Grant to DLB and CA, Smithsonian Institution Johnson Fund to DH, and Smithsonian Women's Committee funding to VC. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 62 TC 5 Z9 5 U1 1 U2 22 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD FEB 11 PY 2015 VL 10 IS 2 AR e0116223 DI 10.1371/journal.pone.0116223 PG 27 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CB3RF UT WOS:000349545300018 PM 25671595 ER PT J AU Stapley, J Garcia, M Andrews, RM AF Stapley, Jessica Garcia, Milton Andrews, Robin M. TI Long-Term Data Reveal a Population Decline of the Tropical Lizard Anolis apletophallus, and a Negative Affect of El Nino Years on Population Growth Rate SO PLOS ONE LA English DT Article ID CLIMATE-CHANGE; FOREST CHRONOSEQUENCE; LIMIFRONS; DYNAMICS; ECTOTHERMS; RESPONSES; SURVIVAL; IMPACTS; EGGS AB Climate change threatens biodiversity worldwide, however predicting how particular species will respond is difficult because climate varies spatially, complex factors regulate population abundance, and species vary in their susceptibility to climate change. Studies need to incorporate these factors with long-term data in order to link climate change to population abundance. We used 40 years of lizard abundance data and local climate data from Barro Colorado Island to ask how climate, total lizard abundance and cohort-specific abundance have changed over time, and how total and cohort-specific abundance relate to climate variables including those predicted to make the species vulnerable to climate change (i.e. temperatures exceeding preferred body temperature). We documented a decrease in lizard abundance over the last 40 years, and changes in the local climate. Population growth rate was related to the previous years' southern oscillation index; increasing following cooler-wetter, la nina years, decreasing following warmer-drier, el nino years. Within-year recruitment was negatively related to rainfall and minimum temperature. This study simultaneously identified climatic factors driving long-termpopulation fluctuations and climate variables influencing short-term annual recruitment, both of which may be contributing to the population decline and influence the population's future persistence. C1 [Stapley, Jessica; Garcia, Milton] Smithsonian Trop Res Inst, Panama City, Panama. [Andrews, Robin M.] Virginia Tech, Dept Biol Sci, Blacksburg, VA 24061 USA. RP Stapley, J (reprint author), Smithsonian Trop Res Inst, Apartado Postal 0843-03092, Panama City, Panama. EM j.stapley@sheffield.ac.uk RI Stapley, Jessica/B-3858-2010; OI Stapley, Jessica/0000-0002-9138-5684 FU Smithsonian Tropical Research Institute; Smithsonian Tropical Research Institute Postdoctoral Fellowship FX Smithsonian Tropical Research Institute (http://www.stri.si.edu/) has funded the long-term data collection. JS was supported by a Smithsonian Tropical Research Institute Postdoctoral Fellowship. NR 33 TC 0 Z9 0 U1 2 U2 14 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD FEB 11 PY 2015 VL 10 IS 2 AR e0115450 DI 10.1371/journal.pone.0115450 PG 14 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CB3RF UT WOS:000349545300007 PM 25671423 ER PT J AU Aliu, E Archambault, S Archer, A Aune, T Barnacka, A Beilicke, M Benbow, W Bird, R Buckley, JH Bugaev, V Byrum, K Cardenzana, JV Cerruti, M Chen, X Ciupik, L Connolly, MP Cui, W Dickinson, HJ Dumm, J Eisch, JD Errando, M Falcone, A Feng, Q Finley, JP Fleischhack, H Fortin, P Fortson, L Furniss, A Gillanders, GH Griffin, S Griffiths, ST Grube, J Gyuk, G Kansson, NH Hanna, D Holder, J Humensky, TB Johnson, CA Kaaret, P Kar, P Kertzman, M Kieda, D Krennrich, F Kumar, S Lang, MJ Lyutikov, M Madhavan, AS Maier, G McArthur, S McCann, A Meagher, K Millis, J Moriarty, P Mukherjee, R Nieto, D de Bhroithe, AO Ong, RA Otte, AN Park, N Pohl, M Popkow, A Prokoph, H Pueschel, E Quinn, J Ragan, K Reyes, LC Reynolds, PT Richards, GT Roache, E Santander, M Sembroski, GH Shahinyan, K Smith, AW Staszak, D Telezhinsky, I Tucci, JV Tyler, J Varlotta, A Vincent, S Wakely, SP Weinstein, A Williams, DA Zajczyk, A Zitzer, B AF Aliu, E. Archambault, S. Archer, A. Aune, T. Barnacka, A. Beilicke, M. Benbow, W. Bird, R. Buckley, J. H. Bugaev, V. Byrum, K. Cardenzana, J. V. Cerruti, M. Chen, X. Ciupik, L. Connolly, M. P. Cui, W. Dickinson, H. J. Dumm, J. Eisch, J. D. Errando, M. Falcone, A. Feng, Q. Finley, J. P. Fleischhack, H. Fortin, P. Fortson, L. Furniss, A. Gillanders, G. H. Griffin, S. Griffiths, S. T. Grube, J. Gyuk, G. Kansson, N. H. A. Hanna, D. Holder, J. Humensky, T. B. Johnson, C. A. Kaaret, P. Kar, P. Kertzman, M. Kieda, D. Krennrich, F. Kumar, S. Lang, M. J. Lyutikov, M. Madhavan, A. S. Maier, G. McArthur, S. McCann, A. Meagher, K. Millis, J. Moriarty, P. Mukherjee, R. Nieto, D. de Bhroithe, A. O'Faolain Ong, R. A. Otte, A. N. Park, N. Pohl, M. Popkow, A. Prokoph, H. Pueschel, E. Quinn, J. Ragan, K. Reyes, L. C. Reynolds, P. T. Richards, G. T. Roache, E. Santander, M. Sembroski, G. H. Shahinyan, K. Smith, A. W. Staszak, D. Telezhinsky, I. Tucci, J. V. Tyler, J. Varlotta, A. Vincent, S. Wakely, S. P. Weinstein, A. Williams, D. A. Zajczyk, A. Zitzer, B. TI A SEARCH FOR PULSATIONS FROM GEMINGA ABOVE 100 GeV WITH VERITAS SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma rays: stars; pulsars: general; pulsars: individual (PSR J0633+1746, Geminga) ID TEV GAMMA-RAYS; LARGE-AREA TELESCOPE; HIGH-ENERGY EMISSION; FERMI-LAT OBSERVATIONS; CRAB PULSAR; GALACTIC SOURCES; VELA PULSAR; PG 1553+113; X-RAY; CATALOG AB We present the results of 71.6 hr of observations of the Geminga pulsar (PSR J0633+1746) with the VERITAS very-high-energy gamma-ray telescope array. Data taken with VERITAS between 2007 November and 2013 February were phase-folded using a Geminga pulsar timing solution derived from data recorded by the XMM-Newton and Fermi-LAT space telescopes. No significant pulsed emission above 100 GeV is observed, and we report upper limits at the 95% confidence level on the integral flux above 135 GeV (spectral analysis threshold) of 4.0x10(-13) s(-1) cm(-2) and 1.7 x 10(-13) s(-1) cm(-2) for the two principal peaks in the emission profile. These upper limits, placed in context with phase-resolved spectral energy distributions determined from 5 yr of data from the Fermi-Large Area Telescope (LAT), constrain possible hardening of the Geminga pulsar emission spectra above similar to 50 GeV. C1 [Aliu, E.; Errando, M.; Mukherjee, R.; Santander, M.] Columbia Univ, Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA. [Aliu, E.] Univ Barcelona, IEEC UB, Inst Ciencies Cosmos, Dept Astron & Meteorol, E-08028 Barcelona, Spain. [Archambault, S.; Griffin, S.; Hanna, D.; Ragan, K.; Staszak, D.; Tyler, J.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Archer, A.; Beilicke, M.; Buckley, J. H.; Bugaev, V.; Zajczyk, A.] Washington Univ, Dept Phys, St Louis, MO 63130 USA. [Aune, T.; Ong, R. A.; Popkow, A.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Barnacka, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Benbow, W.; Cerruti, M.; Fortin, P.; Roache, E.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. [Bird, R.; Pueschel, E.; Quinn, J.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland. [Byrum, K.; Zitzer, B.] Argonne Natl Lab, Argonne, IL 60439 USA. [Cardenzana, J. V.; Dickinson, H. J.; Eisch, J. D.; Krennrich, F.; Madhavan, A. S.; Weinstein, A.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Chen, X.; Kansson, N. H. A.; Pohl, M.; Telezhinsky, I.] Univ Potsdam, Inst Phys & Astron, D-14476 Golm, Germany. [Chen, X.; Fleischhack, H.; Maier, G.; de Bhroithe, A. O'Faolain; Pohl, M.; Prokoph, H.; Telezhinsky, I.; Vincent, S.] DESY, D-15738 Zeuthen, Germany. [Ciupik, L.; Grube, J.; Gyuk, G.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA. [Connolly, M. P.; Gillanders, G. H.; Lang, M. J.; Moriarty, P.] Natl Univ Ireland Galway, Sch Phys, Galway, Ireland. [Cui, W.; Feng, Q.; Finley, J. P.; Lyutikov, M.; Sembroski, G. H.; Tucci, J. V.; Varlotta, A.] Purdue Univ, Dept Phys & Astron, W Lafayette, IN 47907 USA. [Fortson, L.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. [Falcone, A.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Furniss, A.; Johnson, C. A.; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Furniss, A.; Johnson, C. A.; Williams, D. A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA. [Griffiths, S. T.; Kaaret, P.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Holder, J.; Kumar, S.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Holder, J.; Kumar, S.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Humensky, T. B.; Nieto, D.] Columbia Univ, Dept Phys, New York, NY 10027 USA. [Kar, P.; Kieda, D.; Smith, A. W.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Kertzman, M.] Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA. [McArthur, S.; Wakely, S. P.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [McCann, A.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Meagher, K.; Otte, A. N.; Richards, G. T.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA. [Meagher, K.; Otte, A. N.; Richards, G. T.] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Millis, J.] Anderson Univ, Dept Phys, Anderson, IN 46012 USA. [Reyes, L. C.] Calif Polytech State Univ San Luis Obispo, Dept Phys, San Luis Obispo, CA 94307 USA. [Reynolds, P. T.] Cork Inst Technol, Dept Appl Phys & Instrumentat, Cork, Ireland. RP Aliu, E (reprint author), Columbia Univ, Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA. EM mccann@kicp.uchicago.edu; gtrichards@gatech.edu RI Nieto, Daniel/J-7250-2015; OI Nieto, Daniel/0000-0003-3343-0755; Pueschel, Elisa/0000-0002-0529-1973; Cui, Wei/0000-0002-6324-5772; Bird, Ralph/0000-0002-4596-8563 FU U.S. Department of Energy Office of Science; U.S. National Science Foundation; Smithsonian Institution; NSERC in Canada; Science Foundation Ireland [SFI 10/RFP/AST2748]; STFC in the U.K; Kavli Institute for Cosmological Physics at the University of Chicago [NSF PHY-1125897] FX This research is supported by grants from the U.S. Department of Energy Office of Science, the U.S. National Science Foundation, and the Smithsonian Institution, by NSERC in Canada, by Science Foundation Ireland (SFI 10/RFP/AST2748), and by STFC in the U.K. We acknowledge the excellent work of the technical support staff at the Fred Lawrence Whipple Observatory and at the collaborating institutions in the construction and operation of the instrument. The VERITAS Collaboration is grateful to Trevor Weekes for his seminal contributions and leadership in the field of VHE gamma-ray astrophysics, which made this study possible. A. Mc. is supported in part by the Kavli Institute for Cosmological Physics at the University of Chicago through grant NSF PHY-1125897 and an endowment from the Kavli Foundation and its founder Fred Kavli. NR 61 TC 6 Z9 6 U1 2 U2 12 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2015 VL 800 IS 1 AR 61 DI 10.1088/0004-637X/800/1/61 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CA9IQ UT WOS:000349236900061 ER PT J AU Cordero, MJ Pilachowski, CA Johnson, CI Vesperini, E AF Cordero, M. J. Pilachowski, C. A. Johnson, C. I. Vesperini, E. TI LIGHT-ELEMENT ABUNDANCES OF GIANT STARS IN THE GLOBULAR CLUSTER M71 (NGC 6838) SO ASTROPHYSICAL JOURNAL LA English DT Article DE globular clusters: individual (M71); stars: abundances; stars: Population II ID SELF-ENRICHMENT SCENARIO; MAIN-SEQUENCE TURNOFF; DYNAMICAL EVOLUTION; MULTIPLE POPULATIONS; ALUMINUM ABUNDANCES; CHEMICAL-COMPOSITION; STELLAR POPULATIONS; LARGE-SAMPLE; RED GIANTS; M13 GIANTS AB Aluminum is the heaviest light element displaying large star-to-star variations in Galactic globular clusters (GCs). This element may provide additional insight into the origin of the multiple populations, now known to be common place in GCs, and also the nature of the first-generation stars responsible for a cluster's chemical inhomogeneities. In a previous analysis, we found that unlike more metal-poor GCs, 47 Tuc did not exhibit a strong Na-Al correlation, which motivates a careful study of the similar metallicity but less massive GCM71. We present chemical abundances of O, Na, Al, and Fe for 33 giants in M71 using spectra obtained with the WIYN-Hydra spectrograph. Our spectroscopic analysis finds that similar to 47 Tuc and in contrast with more metal-poor GCs, M71 stars do not exhibit a strong Na-Al correlation and span a relatively narrow range in [Al/Fe], which are characteristics that GC formation models must reproduce. C1 [Cordero, M. J.] Heidelberg Univ, Zentrum Astron, Heidelberg, Germany. [Cordero, M. J.; Pilachowski, C. A.; Vesperini, E.] Indiana Univ, Dept Astron, Bloomington, IN 47405 USA. [Johnson, C. I.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Cordero, MJ (reprint author), Heidelberg Univ, Zentrum Astron, Konigstuhl 12, Heidelberg, Germany. EM mjcorde@lsw.uni-heidelberg.de; catyp@astro.indiana.edu; cjohnson@cfa.harvard.edu; evesperi@indiana.edu FU National Aeronautics and Space Administration; National Science Foundation; Sonderforschungsbereich [SFB 881]; German Research Foundation (DFG); Clay Fellowship; [NASA-NNX13AF45G] FX We thank Karen Butler, Jena Christensen, Charles Corson, Dianne Harmer, Jennifer Power, Heidi Schweiker, David Summers, and Daryl Willmarth for their assistance in the data acquisition. This research has made use of the NASA Astrophysics Data System Bibliographic Services. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. This work was supported by Sonderforschungsbereich SFB 881 "The Milky Way System" (subprojects A4 and A5) of the German Research Foundation (DFG). C.A.P. acknowledges the generosity of the Kirkwood Research Fund at Indiana University. C.I.J. gratefully acknowledges support from the Clay Fellowship, administered by the Smithsonian Astrophysical Observatory. E.V. acknowledges support from grant NASA-NNX13AF45G. We thank the anonymous referee for suggestions for improving this paper. NR 68 TC 11 Z9 11 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2015 VL 800 IS 1 AR 3 DI 10.1088/0004-637X/800/1/3 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CA9IQ UT WOS:000349236900003 ER PT J AU Fragos, T McClintock, JE AF Fragos, T. McClintock, J. E. TI THE ORIGIN OF BLACK HOLE SPIN IN GALACTIC LOW-MASS X-RAY BINARIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: close; black hole physics; Galaxy: stellar content; stars: black holes; stars: evolution X-rays: binaries ID COMPACT OBJECT FORMATION; QUASI-PERIODIC OSCILLATIONS; MICROQUASAR XTE J1550-564; COMMON ENVELOPE EVOLUTION; STELLAR ASTROPHYSICS MESA; CONTINUUM-FITTING METHOD; NOVA OPHIUCHI 1977; CYGNUS X-1; DYNAMICAL EVIDENCE; RADIO PULSARS AB Galactic field black hole (BH) low-mass X-ray binaries (LMXBs) are believed to form in situ via the evolution of isolated binaries. In the standard formation channel, these systems survived a common envelope phase, after which the remaining helium core of the primary star and the subsequently formed BH are not expected to be highly spinning. However, the measured spins of BHs in LMXBs cover the whole range of spin parameters. We propose here that the BH spin in LMXBs is acquired through accretion onto the BH after its formation. In order to test this hypothesis, we calculated extensive grids of detailed binary mass-transfer sequences. For each sequence, we examined whether, at any point in time, the calculated binary properties are in agreement with their observationally inferred counterparts of 16 Galactic LMXBs. The "successful" sequences give estimates of the mass that the BH has accreted since the onset of Roche-Lobe overflow. We find that in all Galactic LMXBs with measured BH spin, the origin of the spin can be accounted for by the accreted matter, and we make predictions about the maximum BH spin in LMXBs where no measurement is yet available. Furthermore, we derive limits on the maximum spin that any BH can have depending on current properties of the binary it resides in. Finally we discuss the implication that our findings have on the BH birth-mass distribution, which is shifted by similar to 1.5M(circle dot) toward lower masses, compared to the currently observed one. C1 [Fragos, T.] Univ Geneva, Observ Geneva, CH-1290 Sauverny, Switzerland. [McClintock, J. E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Fragos, T (reprint author), Univ Geneva, Observ Geneva, Chemin Maillettes 51, CH-1290 Sauverny, Switzerland. EM anastasios.fragkos@unige.ch RI Fragos, Tassos/A-3581-2016 OI Fragos, Tassos/0000-0003-1474-1523 FU Ambizione Fellowship of the Swiss National Science Foundation [PZ00P2_148123]; ITC prize fellowship program of the Institute of Theory and Computation at the Harvard-Smithsonian Center for Astrophysics; NASA [NNX11AD08G]; FAS Division of Science, Research Computing Group at Harvard University FX We thank R. Narayan for useful discussions and the anonymous referee whose insightful comments improved this paper. T.F. acknowledges support from the Ambizione Fellowship of the Swiss National Science Foundation (grant PZ00P2_148123) and the ITC prize fellowship program of the Institute of Theory and Computation at the Harvard-Smithsonian Center for Astrophysics, where part of this work was carried out. J.E.M. acknowledges the support of NASA grant NNX11AD08G. The computations in this paper were run on the Odyssey cluster supported by the FAS Division of Science, Research Computing Group at Harvard University. NR 139 TC 25 Z9 25 U1 0 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2015 VL 800 IS 1 AR 17 DI 10.1088/0004-637X/800/1/17 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CA9IQ UT WOS:000349236900017 ER PT J AU Gatuzz, E Garcia, J Kallman, TR Mendoza, C Gorczyca, TW AF Gatuzz, E. Garcia, J. Kallman, T. R. Mendoza, C. Gorczyca, T. W. TI ISMabs: A COMPREHENSIVE X-RAY ABSORPTION MODEL FOR THE INTERSTELLAR MEDIUM SO ASTROPHYSICAL JOURNAL LA English DT Article ID XMM-NEWTON OBSERVATION; K-SHELL PHOTOIONIZATION; CROSS-SECTIONS; NEUTRON-STAR; LOW/HARD STATE; ATOMIC OXYGEN; SCORPIUS X-1; CYG X-2; SPECTROSCOPY; BINARIES AB We present an X-ray absorption model for the interstellar medium, to be referred to as ISMabs, that takes into account both neutral and ionized species of cosmically abundant elements, and includes the most accurate atomic data available. Using high-resolution spectra from eight X-ray binaries obtained with the Chandra High Energy Transmission Grating Spectrometer, we proceed to benchmark the atomic data in the model particularly in the neon K-edge region. Compared with previous photoabsorption models, which solely rely on neutral species, the inclusion of ions leads to improved spectral fits. Fit parameters comprise the column densities of abundant contributors that allow direct estimates of the ionization states. ISMabs is provided in the appropriate format to be implemented in widely used X-ray spectral fitting packages such as XSPEC, ISIS, and SHERPA. C1 [Gatuzz, E.; Mendoza, C.] IVIC, Ctr Fis, Caracas 1020A, Venezuela. [Garcia, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kallman, T. R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Gorczyca, T. W.] Western Michigan Univ, Dept Phys, Kalamazoo, MI 49008 USA. RP Gatuzz, E (reprint author), IVIC, Ctr Fis, POB 20632, Caracas 1020A, Venezuela. EM egatuzz@ivic.gob.ve; javier@head.cfa.harvard.edu; timothy.r.kallman@nasa.gov; claudio@ivic.gob.ve; thomas.gorczyca@wmich.edu OI Mendoza, Claudio/0000-0002-2854-4806 FU Chandra Theory Program [15400673] FX This work was supported by grant 15400673 of the Chandra Theory Program. NR 53 TC 9 Z9 9 U1 1 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2015 VL 800 IS 1 AR 29 DI 10.1088/0004-637X/800/1/29 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CA9IQ UT WOS:000349236900029 ER PT J AU Gonzalez-Alfonso, E Fischer, J Sturm, E Gracia-Carpio, J Veilleux, S Melendez, M Lutz, D Poglitsch, A Aalto, S Falstad, N Spoon, HWW Farrah, D Blasco, A Henkel, C Contursi, A Verma, A Spaans, M Smith, HA Ashby, MLN Hailey-Dunsheath, S Garcia-Burillo, S Martin-Pintado, J Van Der Werf, P Meijerink, R Genzel, R AF Gonzalez-Alfonso, E. Fischer, J. Sturm, E. Gracia-Carpio, J. Veilleux, S. Melendez, M. Lutz, D. Poglitsch, A. Aalto, S. Falstad, N. Spoon, H. W. W. Farrah, D. Blasco, A. Henkel, C. Contursi, A. Verma, A. Spaans, M. Smith, H. A. Ashby, M. L. N. Hailey-Dunsheath, S. Garcia-Burillo, S. Martin-Pintado, J. Van Der Werf, P. Meijerink, R. Genzel, R. TI HIGH-LYING OH ABSORPTION, [C II] DEFICITS, AND EXTREME L-FIR/M-H2 RATIOS IN GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: ISM; infrared: galaxies; line: formation ID ULTRALUMINOUS INFRARED GALAXIES; MICRON LINE DEFICIT; STAR-FORMATION LAWS; MOLECULAR GAS; NGC 4418; PHOTODISSOCIATION REGIONS; OPTICAL SPECTROSCOPY; HERSCHEL-PACS; DENSE GAS; ARP 220 AB Herschel/PACS observations of 29 local (ultra) luminous infrared galaxies, including both starburst and active galactic nucleus (AGN) dominated sources as diagnosed in the mid-infrared/optical, show that the equivalent width of the absorbing OH 65 mu m.3/2 J = 9/2-7/2 line (Weq(OH65)) with lower level energy Elow 300 K, is anticorrelated with the [Cii] 158 mu m line to far-infrared luminosity ratio, and correlated with the far-infrared luminosity per unit gas mass and with the 60-to-100 mu m far-infrared color. While all sources are in the active LIR/MH2 > 50L /M mode as derived from previous CO line studies, the OH65 absorption shows a bimodal distribution with a discontinuity at LFIR/MH2 100L /M . In the most buried sources, OH65 probes material partially responsible for the silicate 9.7 mu m absorption. Combined with observations of the OH 71 mu m.1/2 J = 7/2-5/2 doublet (Elow 415 K), radiative transfer models characterized by the equivalent dust temperature, Tdust, and the continuum optical depth at 100 mu m, t100, indicate that strong [C ii] 158 mu m deficits are associated with far-IR thick (t100 0.7, NH 1024 cm-2), warm (Tdust 60 K) structures where the OH 65 mu m absorption is produced, most likely in circumnuclear disks/tori/cocoons. With their high LFIR/MH2 ratios and columns, the presence of these structures is expected to give rise to strong [C ii] deficits. Weq(OH65) probes the fraction of infrared luminosity arising from these compact/warm environments, which is 30%-50% in sources with high Weq(OH65). Sources with high Weq(OH65) have surface densities of both LIR and MH2 higher than inferred from the half-light (CO or UV/optical) radius, tracing coherent structures that represent the most buried/active stage of (circum) nuclear starburst-AGN co-evolution. C1 [Gonzalez-Alfonso, E.; Blasco, A.] Univ Alcala de Henares, Dept Fis & Matemat, E-28871 Madrid, Spain. [Fischer, J.] Naval Res Lab, Remote Sensing Div, Washington, DC 20375 USA. [Sturm, E.; Gracia-Carpio, J.; Lutz, D.; Poglitsch, A.; Contursi, A.; Genzel, R.] Max Planck Inst Extraterr Phys MPE, D-85748 Garching, Germany. [Veilleux, S.; Melendez, M.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Aalto, S.; Falstad, N.] Chalmers, Onsala Space Observ, Dept Earth & Space Sci, SE-43992 Onsala, Sweden. [Spoon, H. W. W.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Farrah, D.] Virginia Tech, Dept Phys, Blacksburg, VA 24061 USA. [Henkel, C.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Henkel, C.] Kind Abdulaziz Univ, Dept Astron, Jeddah 21589, Saudi Arabia. [Verma, A.] Univ Oxford, Oxford Astrophys, Oxford OX1 3RH, England. [Spaans, M.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AB Groningen, Netherlands. [Smith, H. A.; Ashby, M. L. N.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hailey-Dunsheath, S.] CALTECH, Pasadena, CA 91125 USA. [Garcia-Burillo, S.] Observ Madrid, OAN, E-28014 Madrid, Spain. [Martin-Pintado, J.] CSIC INTA, E-28850 Madrid, Spain. [Van Der Werf, P.; Meijerink, R.] Leiden Univ, Sterrewacht Leiden, NL-2300 RA Leiden, Netherlands. RP Gonzalez-Alfonso, E (reprint author), Univ Alcala de Henares, Dept Fis & Matemat, Campus Univ, E-28871 Madrid, Spain. RI Martin-Pintado, Jesus/H-6107-2015; OI Martin-Pintado, Jesus/0000-0003-4561-3508; Poglitsch, Albrecht/0000-0002-6414-9408; Gonzalez-Alfonso, Eduardo/0000-0001-5285-8517; Fischer, Jacqueline/0000-0001-6697-7808; Veilleux, Sylvain/0000-0002-3158-6820 FU BMVIT (Austria); ESA-PRODEX (Belgium); CEA/CNES (France); DLR (Germany); ASI/INAF (Italy); CICYT/MCYT (Spain); Spanish Ministerio de Economia y Competitividad [AYA2010-21697-C05-0, FIS2012-39162-C06-01]; NHSC/JPL RSA [1455432]; NASA grant [NNX14AJ61G]; US-ONR; NHSC/JPL [139807, 1456609, 1427277, 1454738] FX PACS has been developed by a consortium of institutes led by MPE (Germany) and including UVIE (Austria); KU Leuven, CSL, IMEC (Belgium); CEA, LAM (France); MPIA (Germany); INAFIFSI/OAA/OAP/OAT, LENS, SISSA (Italy); IAC (Spain). This development has been supported by the funding agencies BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI/INAF (Italy), and CICYT/MCYT (Spain). E.G.-A. is a Research Associate at the Harvard-Smithsonian CfA, and thanks the Spanish Ministerio de Economia y Competitividad for support under projects AYA2010-21697-C05-0 and FIS2012-39162-C06-01. E. G.-A. and H. A. S. acknowledge partial support from NHSC/JPL RSA 1455432; H. A. S acknowledges NASA grant NNX14AJ61G. Basic research in IR astronomy at NRL is funded by the US-ONR; J. F. acknowledges support from NHSC/JPL subcontracts 139807 and 1456609. S. V. and M. M. acknowledge partial support from NHSC/JPL RSA 1427277 and 1454738. This research has made use of NASA's Astrophysics Data System and of GILDAS (http://www. iram. fr/IRAMFR/GILDAS). NR 70 TC 11 Z9 11 U1 1 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2015 VL 800 IS 1 AR 69 DI 10.1088/0004-637X/800/1/69 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CA9IQ UT WOS:000349236900069 ER PT J AU Hachisuka, K Choi, YK Reid, MJ Brunthaler, A Menten, KM Sanna, A Dame, TM AF Hachisuka, K. Choi, Y. K. Reid, M. J. Brunthaler, A. Menten, K. M. Sanna, A. Dame, T. M. TI PARALLAXES OF STAR-FORMING REGIONS IN THE OUTER SPIRAL ARM OF THE MILKY WAY SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrometry; Galaxy: kinematics and dynamics; Galaxy: structure; masers; stars: distances ID TRIGONOMETRIC PARALLAXES; IRAS SOURCES; FUNDAMENTAL PARAMETERS; METHANOL MASERS; VLBI ASTROMETRY; WATER MASERS; SOLAR CIRCLE; GALAXY; DISTANCE; DISK AB We report parallaxes and proper motions of three water maser sources in high-mass star-forming regions in the Outer Spiral Arm of the Milky Way. The observations were conducted with the Very Long Baseline Array as part of Bar and Spiral Structure Legacy Survey and double the number of such measurements in the literature. The Outer Arm has a pitch angle of 14 degrees.9 +/- 2 degrees.7 and a Galactocentric distance of 14.1 +/- 0.6 kpc toward the Galactic anticenter. The average motion of these sources toward the Galactic center is 10.7 +/- 2.1 kms(-1) and we see no sign of a significant fall in the rotation curve out to 15 kpc from the Galactic center. The three-dimensional locations of these star-forming regions are consistent with a Galactic warp of several hundred parsecs from the plane. C1 [Hachisuka, K.] Yamaguchi Univ, Res Inst Time Studies, Yamaguchi 7538511, Japan. [Hachisuka, K.] Chinese Acad Sci, Shanghai Astron Observ, Shanghai 200030, Peoples R China. [Hachisuka, K.] Ibaraki Univ, Ctr Astron, Mito, Ibaraki 2108512, Japan. [Choi, Y. K.] Korea Astron & Space Inst, Taejon 305348, South Korea. [Choi, Y. K.; Brunthaler, A.; Menten, K. M.; Sanna, A.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Reid, M. J.; Dame, T. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Hachisuka, K (reprint author), Yamaguchi Univ, Res Inst Time Studies, Yoshida 1677-1, Yamaguchi 7538511, Japan. FU China Ministry of Science and Technology [2012CB821800]; National Natural Science Foundation of China [10625314, 11121062]; European Research Council [247078] FX This work is partly supported by the China Ministry of Science and Technology under State Key Development Program for Basic Research (2012CB821800), the National Natural Science Foundation of China (grants 10625314, 11121062). The authors acknowledge the financial support by the European Research Council for the ERC Advanced Grant GLOSTAR under contract no. 247078. NR 39 TC 13 Z9 13 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2015 VL 800 IS 1 AR 2 DI 10.1088/0004-637X/800/1/2 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CA9IQ UT WOS:000349236900002 ER PT J AU Honig, ZN Reid, MJ AF Honig, Z. N. Reid, M. J. TI CHARACTERISTICS OF SPIRAL ARMS IN LATE-TYPE GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: individual (M51, M74, NGC 1232, NGC 3184); galaxies: spiral ID STAR-FORMING REGIONS; TRIGONOMETRIC PARALLAXES; PITCH-ANGLE; MILKY-WAY; SEGMENTS AB We have measured the positions of large numbers of H II regions in four nearly face-on, late-type, spiral galaxies: NGC 628 (M74), NGC 1232, NGC 3184, and NGC 5194 (M51). Fitting log-periodic spiral models to segments of each arm yields local estimates of spiral pitch angle and arm width. While pitch angles vary considerably along individual arms, among arms within a galaxy, and among galaxies, we find no systematic trend with galactocentric distance. We estimate the widths of the arm segments from the scatter in the distances of the H II regions from the spiral model. All major arms in these galaxies show spiral arm width increasing with distance from the galactic center, similar to the trend seen in the Milky Way. However, in the outermost parts of the galaxies, where massive star formation declines, some arms reverse this trend and narrow. We find that spiral arms often appear to be composed of segments of similar to 5 kpc length, which join to form kinks and abrupt changes in pitch angle and arm width; these characteristics are consistent with properties seen in the large N-body simulations of D'Onghia et al. and others. C1 [Honig, Z. N.; Reid, M. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Honig, ZN (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mreid@cfa.harvard.edu NR 24 TC 10 Z9 10 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 2015 VL 800 IS 1 AR 53 DI 10.1088/0004-637X/800/1/53 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CA9IQ UT WOS:000349236900053 ER PT J AU Kuo, CY Braatz, JA Lo, KY Reid, MJ Suyu, SH Pesce, DW Condon, JJ Henkel, C Impellizzeri, CMV AF Kuo, C. Y. Braatz, J. A. Lo, K. Y. Reid, M. J. Suyu, S. H. Pesce, D. W. Condon, J. J. Henkel, C. Impellizzeri, C. M. V. TI THE MEGAMASER COSMOLOGY PROJECT. VI. OBSERVATIONS OF NGC 6323 SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; galaxies: active; galaxies: ISM; galaxies: nuclei; galaxies: Seyfert; masers ID ANGULAR-DIAMETER DISTANCE; UGC 3789 AB We present observations of the H2O megamasers in the accretion disk of NGC 6323. By combining interferometric and spectral monitoring data, we estimate H-0 = 73(-22)(+26) km s(-1) Mpc(-1), where the low strength of the systemic masers (<15 mJy) limits the accuracy of this estimate. The methods developed here for dealing with weak maser emission provide guidance for observations of similar sources, until significant increases in radio telescope sensitivity, such as anticipated from the next generation Very Large Array, are realized. C1 [Kuo, C. Y.; Suyu, S. H.] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Braatz, J. A.; Lo, K. Y.; Condon, J. J.; Impellizzeri, C. M. V.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Reid, M. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Pesce, D. W.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Henkel, C.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Henkel, C.] King Abdulaziz Univ, Fac Sci, Dept Astron, Jeddah, Saudi Arabia. RP Kuo, CY (reprint author), Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 10617, Taiwan. RI Faculty of, Sciences, KAU/E-7305-2017 FU National Science Foundation (NSF) FX The VLBA is a facility of the National Radio Astronomy Observatory, which is operated by the Associated Universities, Inc. under a cooperative agreement with the National Science Foundation (NSF). NR 8 TC 6 Z9 6 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2015 VL 800 IS 1 AR 26 DI 10.1088/0004-637X/800/1/26 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CA9IQ UT WOS:000349236900026 ER PT J AU Liao, K Treu, T Marshall, P Fassnacht, CD Rumbaugh, N Dobler, G Aghamousa, A Bonvin, V Courbin, F Hojjati, A Jackson, N Kashyap, V Kumar, SR Linder, E Mandel, K Meng, XL Meylan, G Moustakas, LA Prabhu, TP Romero-Wolf, A Shafieloo, A Siemiginowska, A Stalin, CS Tak, H Tewes, M van Dyk, D AF Liao, Kai Treu, Tommaso Marshall, Phil Fassnacht, Christopher D. Rumbaugh, Nick Dobler, Gregory Aghamousa, Amir Bonvin, Vivien Courbin, Frederic Hojjati, Alireza Jackson, Neal Kashyap, Vinay Kumar, S. Rathna Linder, Eric Mandel, Kaisey Meng, Xiao-Li Meylan, Georges Moustakas, Leonidas A. Prabhu, Tushar P. Romero-Wolf, Andrew Shafieloo, Arman Siemiginowska, Aneta Stalin, Chelliah S. Tak, Hyungsuk Tewes, Malte van Dyk, David TI STRONG LENS TIME DELAY CHALLENGE. II. RESULTS OF TDC1 SO ASTROPHYSICAL JOURNAL LA English DT Article DE gravitational lensing: strong; methods: data analysis ID HUBBLE CONSTANT; COSMOLOGICAL PARAMETERS; EXPANSION HISTORY; DARK ENERGY; QUASARS; VARIABILITY; COSMOGRAIL; DISTANCES; GALAXIES; UNIVERSE AB We present the results of the first strong lens time delay challenge. The motivation, experimental design, and entry level challenge are described in a companion paper. This paper presents the main challenge, TDC1, which consisted of analyzing thousands of simulated light curves blindly. The observational properties of the light curves cover the range in quality obtained for current targeted efforts (e.g., COSMOGRAIL) and expected from future synoptic surveys (e.g., LSST), and include simulated systematic errors. Seven teams participated in TDC1, submitting results from 78 different method variants. After describing each method, we compute and analyze basic statisticsmeasuring accuracy (or bias) A, goodness of fit chi(2), precision P, and success rate f. For some methods we identify outliers as an important issue. Other methods show that outliers can be controlled via visual inspection or conservative quality control. Several methods are competitive, i.e., give vertical bar A vertical bar < 0.03, P < 0.03, and chi(2) < 1.5, with some of the methods already reaching sub-percent accuracy. The fraction of light curves yielding a time delay measurement is typically in the range f = 20%-40%. It depends strongly on the quality of the data: COSMOGRAIL-quality cadence and light curve lengths yield significantly higher f than does sparser sampling. Taking the results of TDC1 at face value, we estimate that LSST should provide around 400 robust time-delay measurements, each with P < 0.03 and vertical bar A vertical bar < 0.01, comparable to current lens modeling uncertainties. In terms of observing strategies, we find that A and f depend mostly on season length, while P depends mostly on cadence and campaign duration. C1 [Liao, Kai] Beijing Normal Univ, Dept Astron, Beijing 100875, Peoples R China. [Liao, Kai; Treu, Tommaso] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Marshall, Phil] Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94309 USA. [Fassnacht, Christopher D.; Rumbaugh, Nick] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Dobler, Gregory] Univ Calif Santa Barbara, Kavli Inst Theoret Phys, Santa Barbara, CA 93106 USA. [Aghamousa, Amir; Shafieloo, Arman] Asia Pacific Ctr Theoret Phys, Pohang 790784, Gyeongbuk, South Korea. [Bonvin, Vivien; Courbin, Frederic; Meylan, Georges] Ecole Polytech Fed Lausanne, CH-1015 Lausanne, Switzerland. [Hojjati, Alireza] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Hojjati, Alireza] Simon Fraser Univ, Dept Phys, Burnaby, BC V5A 1S6, Canada. [Jackson, Neal] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Kashyap, Vinay; Mandel, Kaisey; Siemiginowska, Aneta] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kumar, S. Rathna; Prabhu, Tushar P.; Stalin, Chelliah S.] Indian Inst Astrophys, Bangalore 560034, Karnataka, India. [Linder, Eric] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Linder, Eric] Univ Calif Berkeley, Berkeley, CA 94720 USA. [Linder, Eric] Korea Astron & Space Sci Inst, Taejon 305248, South Korea. [Meng, Xiao-Li; Tak, Hyungsuk] Harvard Univ, Dept Stat, Cambridge, MA 02138 USA. [Moustakas, Leonidas A.; Romero-Wolf, Andrew] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Shafieloo, Arman] POSTECH, Dept Phys, Pohang 790784, Gyeongbuk, South Korea. [Tewes, Malte] Argelander Inst Astron, D-53121 Bonn, Germany. [van Dyk, David] Univ London Imperial Coll Sci Technol & Med, Dept Math, London SW7 2AZ, England. [Liao, Kai; Treu, Tommaso] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Dobler, Gregory] NYU, Ctr Urban Sci Progress, Brooklyn, NY 11201 USA. RP Liao, K (reprint author), Beijing Normal Univ, Dept Astron, Beijing 100875, Peoples R China. OI Prabhu, Tushar/0000-0003-0797-5057; Moustakas, Leonidas/0000-0003-3030-2360 FU National Science Foundation collaborative grant "Collaborative Research: Accurate cosmology with strong gravitational lens time delays" [AST-1312329, AST-1450141]; Packard Foundation through a Packard Research Fellowship; China Scholarship Council; U.S. Department of Energy [DE-AC02-76SF00515]; Swiss National Science Foundation (SNSF); DFG [Hi 1495/2-1]; Korea Ministry of Education, Science and Technology, Gyeongsangbuk-Do; Pohang City for Independent Junior Research Groups at the Asia Pacific Center for Theoretical Physics; National Research Foundation of Korea [NRF-2013R1A1A2013795]; DOE [DE-SC-0007867, DE-AC02-05CH11231]; NSERC grant; NSF [AST-1211196] FX We acknowledge the LSST Dark Energy Science Collaboration for hosting several meetings of the "Evil" Team, and the private code repository used in this work. We thank the referee for constructive criticism which helped improved this paper. T.T., C.D.F., and K.L. acknowledge support from the National Science Foundation collaborative grant "Collaborative Research: Accurate cosmology with strong gravitational lens time delays" (AST-1312329 and AST-1450141). T.T. gratefully acknowledges support by the Packard Foundation through a Packard Research Fellowship. K.L. is supported by China Scholarship Council. The work of P.J.M. was supported by the U.S. Department of Energy under contract number DE-AC02-76SF00515. V.B. and F.C. are supported by the Swiss National Science Foundation (SNSF). M.T. acknowledges support by the DFG grant Hi 1495/2-1. A.A and A.S. wish to acknowledge support from the Korea Ministry of Education, Science and Technology, Gyeongsangbuk-Do and Pohang City for Independent Junior Research Groups at the Asia Pacific Center for Theoretical Physics. A.S. would like to acknowledge the support of the National Research Foundation of Korea (NRF-2013R1A1A2013795). E.L. is supported by DOE grant DE-SC-0007867 and contract No. DE-AC02-05CH11231. A.H. is supported by an NSERC grant and thanks the Institute for the Early Universe, Korea, for computational resources. A.A., A.S., A.H., and E.L. thank IBS Korea for hospitality. The work of L.A.M. and A.R.W. was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. K.M. is supported at Harvard by NSF grant AST-1211196. NR 46 TC 20 Z9 20 U1 1 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2015 VL 800 IS 1 AR 11 DI 10.1088/0004-637X/800/1/11 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CA9IQ UT WOS:000349236900011 ER PT J AU Munoz-Jaramillo, A Senkpeil, RR Windmueller, JC Amouzou, EC Longcope, DW Tlatov, AG Nagovitsyn, YA Pevtsov, AA Chapman, GA Cookson, AM Yeates, AR Watson, FT Balmaceda, LA DeLuca, EE Martens, PCH AF Munoz-Jaramillo, Andres Senkpeil, Ryan R. Windmueller, John C. Amouzou, Ernest C. Longcope, Dana W. Tlatov, Andrey G. Nagovitsyn, Yury A. Pevtsov, Alexei A. Chapman, Gary A. Cookson, Angela M. Yeates, Anthony R. Watson, Fraser T. Balmaceda, Laura A. DeLuca, Edward E. Martens, Petrus C. H. TI SMALL-SCALE AND GLOBAL DYNAMOS AND THE AREA AND FLUX DISTRIBUTIONS OF ACTIVE REGIONS, SUNSPOT GROUPS, AND SUNSPOTS: A MULTI-DATABASE STUDY SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: activity; Sun: magnetic fields; Sun: photosphere; sunspots ID STATISTICAL PROPERTIES; SIZE DISTRIBUTION; MAGNETIC-FIELDS; SOLAR-CYCLE; SIMULATIONS; EMERGENCE AB In this work, we take advantage of 11 different sunspot group, sunspot, and active region databases to characterize the area and flux distributions of photospheric magnetic structures. We find that, when taken separately, different databases are better fitted by different distributions (as has been reported previously in the literature). However, we find that all our databases can be reconciled by the simple application of a proportionality constant, and that, in reality, different databases are sampling different parts of a composite distribution. This composite distribution is made up by linear combination of Weibull and log-normal distributions-where a pure Weibull (log-normal) characterizes the distribution of structures with fluxes below (above) 10(21)Mx (10(22)Mx). Additionally, we demonstrate that the Weibull distribution shows the expected linear behavior of a power-law distribution (when extended to smaller fluxes), making our results compatible with the results of Parnell et al. We propose that this is evidence of two separate mechanisms giving rise to visible structures on the photosphere: one directly connected to the global component of the dynamo (and the generation of bipolar active regions), and the other with the small-scale component of the dynamo (and the fragmentation of magnetic structures due to their interaction with turbulent convection). C1 [Munoz-Jaramillo, Andres; Windmueller, John C.; Amouzou, Ernest C.; Longcope, Dana W.] Montana State Univ, Dept Phys, Bozeman, MT 59717 USA. [Munoz-Jaramillo, Andres] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Munoz-Jaramillo, Andres] Stanford Univ, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. [Senkpeil, Ryan R.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Tlatov, Andrey G.] Pulkovo Observ, Kislovodsk Mt Astron Stn, Kislovodsk 357700, Russia. [Nagovitsyn, Yury A.] Russian Acad Sci, Pulkovo Astron Observ, St Petersburg 196140, Russia. [Pevtsov, Alexei A.] Natl Solar Observ, Sunspot, NM 88349 USA. [Chapman, Gary A.; Cookson, Angela M.] Calif State Univ Northridge, Dept Phys & Astron, San Fernando Observ, Northridge, CA 91330 USA. [Yeates, Anthony R.] Univ Durham, Dept Math Sci, Durham DH1 3LE, England. [Watson, Fraser T.] Natl Solar Observ, Tucson, AZ 85719 USA. [Balmaceda, Laura A.] Inst Astron Terr & Space Sci ICATE CONICET, San Juan, Argentina. [Balmaceda, Laura A.] Natl Inst Space Res INPE, Sao Jose Dos Campos, Brazil. [DeLuca, Edward E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Martens, Petrus C. H.] Georgia State Univ, Dept Phys & Astron, Atlanta, GA 30303 USA. RP Munoz-Jaramillo, A (reprint author), Montana State Univ, Dept Phys, Bozeman, MT 59717 USA. EM munoz@solar.physics.montana.edu RI DeLuca, Edward/L-7534-2013; OI DeLuca, Edward/0000-0001-7416-2895; Munoz-Jaramillo, Andres/0000-0002-4716-0840; Balmaceda, Laura/0000-0003-1162-5498; Pevtsov, Alexei/0000-0003-0489-0920 FU NASA Living; Star Jack Eddy Postdoctoral Fellowship Program; Lockheed-Martin [SP02H1701R]; CfA Solar Physics REU program, NSF [AGS-1263241] FX We thank our anonymous referee for a very detailed and conscientious report, which significantly improved the quality of this paper. Additionally, we thank Giuliana de Toma, Neil Sheeley, Jack Harvey, Craig DeForest, Willian Dean Pesnell, Steve Cranmer, and Maria Navas Moreno for useful discussions and suggestions. We are very grateful to Neil R. Sheeley Jr. for sharing his KPVT BMR database with us. This research was supported by the NASA Living With a Star Jack Eddy Postdoctoral Fellowship Program, administered by the UCAR Visiting Scientist Programs, contract SP02H1701R from Lockheed-Martin to the Smithsonian Astrophysical Observatory, and the CfA Solar Physics REU program, NSF grant number AGS-1263241. Andres Munoz-Jaramillo is very grateful to George Fisher and Stuart Bale for their support at the University of California - Berkeley, and Phil Scherrer for his support at Stanford University. The National Solar Observatory (NSO) is operated by the Association of Universities for Research in Astronomy, AURA Inc under cooperative agreement with the National Science Foundation (NSF). NR 38 TC 5 Z9 5 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2015 VL 800 IS 1 AR 48 DI 10.1088/0004-637X/800/1/48 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CA9IQ UT WOS:000349236900048 ER PT J AU Sanders, NE Betancourt, M Soderberg, AM AF Sanders, N. E. Betancourt, M. Soderberg, A. M. TI UNSUPERVISED TRANSIENT LIGHT CURVE ANALYSIS VIA HIERARCHICAL BAYESIAN INFERENCE SO ASTROPHYSICAL JOURNAL LA English DT Article DE methods: numerical; methods: statistical; supernovae: general; surveys ID CORE-COLLAPSE SUPERNOVAE; HAMILTONIAN MONTE-CARLO; PAN-STARRS; HOST GALAXIES; MODELS; NUCLEOSYNTHESIS; PROGENITORS; REGRESSION; TELESCOPE; EVOLUTION AB Historically, light curve studies of supernovae (SNe) and other transient classes have focused on individual objects with copious and high signal-to-noise observations. In the nascent era of wide field transient searches, objects with detailed observations are decreasing as a fraction of the overall known SN population, and this strategy sacrifices the majority of the information contained in the data about the underlying population of transients. A population level modeling approach, simultaneously fitting all available observations of objects in a transient sub-class of interest, fully mines the data to infer the properties of the population and avoids certain systematic biases. We present a novel hierarchical Bayesian statistical model for population level modeling of transient light curves, and discuss its implementation using an efficient Hamiltonian Monte Carlo technique. As a test case, we apply this model to the Type IIP SN sample from the Pan-STARRS1 Medium Deep Survey, consisting of 18,837 photometric observations of 76 SNe, corresponding to a joint posterior distribution with 9176 parameters under our model. Our hierarchical model fits provide improved constraints on light curve parameters relevant to the physical properties of their progenitor stars relative to modeling individual light curves alone. Moreover, we directly evaluate the probability for occurrence rates of unseen light curve characteristics from the model hyperparameters, addressing observational biases in survey methodology. We view this modeling framework as an unsupervised machine learning technique with the ability to maximize scientific returns from data to be collected by future wide field transient searches like LSST. C1 [Sanders, N. E.; Soderberg, A. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Betancourt, M.] Univ Warwick, Dept Stat, Coventry CV4 7AL, W Midlands, England. RP Sanders, NE (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM nsanders@cfa.harvard.edu FU National Aeronautics and Space Administration [NNX08AR22G]; National Science Foundation [AST-1238877]; David and Lucile Packard Foundation; EPSRC [EP/J016934/1]; FAS Science Division Research Computing Group at Harvard University FX The PS1 surveys have been made possible through contributions of the Institute for Astronomy, the University of Hawaii, the Pan-STARRS Project Office, the Max-Planck Society and its participating institutes, the Max Planck Institute for Astronomy, Heidelberg and the Max Planck Institute for Extraterrestrial Physics, Garching, The Johns Hopkins University, Durham University, the University of Edinburgh, Queen's University Belfast, the Harvard-Smithsonian Center for Astrophysics, the Las Cumbres Observatory Global Telescope Network Incorporated, the National Central University of Taiwan, the Space Telescope Science Institute, the National Aeronautics and Space Administration under grant No. NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate, the National Science Foundation under grant No. AST-1238877, the University of Maryland, and Eotvos Lorand University (ELTE). Support for this work was provided by the David and Lucile Packard Foundation Fellowship for Science and Engineering awarded to A. M. S. M. B. is supported under EPSRC grant EP/J016934/1. Computations presented in this paper were performed using the Odyssey supercomputing cluster supported by the FAS Science Division Research Computing Group at Harvard University. NR 45 TC 0 Z9 0 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2015 VL 800 IS 1 AR 36 DI 10.1088/0004-637X/800/1/36 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CA9IQ UT WOS:000349236900036 ER PT J AU Schimoia, JS Storchi-Bergmann, T Grupe, D Eracleous, M Peterson, BM Baldwin, JA Nemmen, RS Winge, C AF Schimoia, Jaderson S. Storchi-Bergmann, Thaisa Grupe, Dirk Eracleous, Michael Peterson, Bradley M. Baldwin, Jack A. Nemmen, Rodrigo S. Winge, Claudia TI SHORT-TIMESCALE MONITORING OF THE X-RAY, UV, AND BROAD DOUBLE-PEAK EMISSION LINE OF THE NUCLEUS OF NGC 1097 SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; galaxies: individual (NGC 1097); galaxies: nuclei; galaxies: Seyfert; line: profiles ID ACTIVE GALACTIC NUCLEI; SWIFT ULTRAVIOLET/OPTICAL TELESCOPE; TERM PROFILE VARIABILITY; GALAXY 3C 390.3; ACCRETION DISK; BLACK-HOLE; BALMER LINES; REGION SIZES; ARP 102B; NGC-1097 AB Recent studies have suggested that the short-timescale (less than or similar to 7 days) variability of the broad (similar to 10,000 km s(-1)) double-peaked H alpha profile of the LINER nucleus of NGC 1097 could be driven by a variable X-ray emission from a central radiatively inefficient accretion flow. To test this scenario, we have monitored the NGC 1097 nucleus in X-ray and UV continuum with Swift and the H alpha flux and profile in the optical spectrum using SOAR and Gemini-South from 2012 August to 2013 February. During the monitoring campaign, the H alpha flux remained at a very low level-three times lower than the maximum flux observed in previous campaigns and showing only limited (similar to 20%) variability. The X-ray variations were small, only similar to 13% throughout the campaign, while the UV did not show significant variations. We concluded that the timescale of the H alpha profile variation is close to the sampling interval of the optical observations, which results in only a marginal correlation between the X-ray and H alpha fluxes. We have caught the active galaxy nucleus in NGC 1097 in a very low activity state, in which the ionizing source was very weak and capable of ionizing just the innermost part of the gas in the disk. Nonetheless, the data presented here still support the picture in which the gas that emits the broad double-peaked Balmer lines is illuminated/ionized by a source of high-energy photons which is located interior to the inner radius of the line-emitting part of the disk. C1 [Schimoia, Jaderson S.; Storchi-Bergmann, Thaisa] Univ Fed Rio Grande do Sul, Inst Fis, Porto Alegre, RS, Brazil. [Storchi-Bergmann, Thaisa; Peterson, Bradley M.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Storchi-Bergmann, Thaisa] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Grupe, Dirk] Morehead State Univ, Ctr Space Sci, Morehead, KY 40351 USA. [Eracleous, Michael] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Eracleous, Michael] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. [Peterson, Bradley M.] Ohio State Univ, Ctr Cosmol & AstroParticle Phys, Columbus, OH 43210 USA. [Baldwin, Jack A.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48864 USA. [Nemmen, Rodrigo S.] Univ Sao Paulo, Inst Astron Geofis & Ciencias Atmosfericas, BR-05508090 Sao Paulo, Brazil. [Winge, Claudia] Gemini South Observ, La Serena, Chile. [Grupe, Dirk] Swift Miss Operat Ctr, State Coll, PA 16801 USA. [Eracleous, Michael] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Eracleous, Michael] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Nemmen, Rodrigo S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Nemmen, Rodrigo S.] Univ Maryland, Dept Phys, Baltimore, MD 21250 USA. RP Schimoia, JS (reprint author), Univ Fed Rio Grande do Sul, Inst Fis, Campus Vale, Porto Alegre, RS, Brazil. EM silva.schimoia@ufrgs.br RI Nemmen, Rodrigo/O-6841-2014; OI Grupe, Dirk/0000-0002-9961-3661 FU CNPq; National Council for Scientific and Technological Development-Brazil; NASA Swift program [NAS5-00136]; NSF [AST-1008882]; NSF; National Science Foundation (United States); National Research Council (Canada); CONICYT (Chile); Australian Research Council (Australia); Ministerio da Ciencia, Tecnologia e Inovacao (Brazil); Ministerio de Ciencia, Tecnologia e Innovacion Productiva (Argentina) FX J.S.S. acknowledges CNPq, the National Council for Scientific and Technological Development-Brazil, for support and The Ohio State University for their hospitality. At Penn State, D.G. and M.E. acknowledge support from the NASA Swift program through contract NAS5-00136. Additionally, M.E. acknowledges the warm hospitality of the Center for Relativistic Astrophysics at Georgia Tech and the Department of Astronomy at the University of Washington. B.M.P. is grateful for support by the NSF through grant AST-1008882 to The Ohio State University.; This research has made use of the XRT Data Analysis Software (XRTDAS) developed under the responsibility of the ASI Science Data Center (ASDC), Italy. This research has made use of data obtained through the High Energy Astrophysics Science Archive Research Center Online Service, provided by the NASA/Goddard Space Flight Center. This research is based on observations obtained at the Southern Astrophysical Research (SOAR) telescope, which is a joint project of the Ministerio da Ciencia, Tecnologia, e Inovacao (MCTI) da Republica Federativa do Brasil, the U.S. National Optical Astronomy Observatory (NOAO), the University of North Carolina at Chapel Hill (UNC), and Michigan State University (MSU). This research is also based 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 National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), Ministerio da Ciencia, Tecnologia e Inovacao (Brazil) and Ministerio de Ciencia, Tecnologia e Innovacion Productiva (Argentina). NR 45 TC 1 Z9 1 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2015 VL 800 IS 1 AR 63 DI 10.1088/0004-637X/800/1/63 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CA9IQ UT WOS:000349236900063 ER PT J AU Scoville, N Sheth, K Walter, F Manohar, S Zschaechner, L Yun, M Koda, J Sanders, D Murchikova, L Thompson, T Robertson, B Genzel, R Hernquist, L Tacconi, L Brown, R Narayanan, D Hayward, CC Barnes, J Kartaltepe, J Davies, R Van Der Werf, P Fomalont, E AF Scoville, Nick Sheth, Kartik Walter, Fabian Manohar, Swarnima Zschaechner, Laura Yun, Min Koda, Jin Sanders, David Murchikova, Lena Thompson, Todd Robertson, Brant Genzel, Reinhard Hernquist, Lars Tacconi, Linda Brown, Robert Narayanan, Desika Hayward, Christopher C. Barnes, Joshua Kartaltepe, Jeyhan Davies, Richard Van Der Werf, Paul Fomalont, Edward TI ALMA IMAGING OF HCN, CS, AND DUST IN ARP 220 AND NGC 6240 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: individual (Arp 220, NGC 6240); galaxies: starburst ID LUMINOUS INFRARED GALAXIES; RESOLUTION CO OBSERVATIONS; ACTIVE GALACTIC NUCLEUS; INDUCED STAR-FORMATION; GIANT MOLECULAR CLOUD; ROTATIONAL-EXCITATION; INTERSTELLAR-MEDIUM; BLACK-HOLES; HIGH-MASS; GAS AB We report ALMA Band 7 (350 GHz) imaging at 0".4-0".6 resolution and Band 9 (696 GHz) at similar to 0".25 resolution of the luminous IR galaxies Arp 220 and NGC 6240. The long wavelength dust continuum is used to estimate interstellar medium masses for Arp 220 east and west and NGC 6240 of 1.9, 4.2, and 1.6 x 10(9) M-circle dot within radii of 69, 65, and 190 pc. The HCN emission was modeled to derive the emissivity distribution as a function of radius and the kinematics of each nuclear disk, yielding dynamical masses consistent with the masses and sizes derived from the dust emission. In Arp 220, the major dust and gas concentrations are at radii less than 50 pc in both counter-rotating nuclear disks. The thickness of the disks in Arp 220 estimated from the velocity dispersion and rotation velocities are 10-20 pc and the mean gas densities are n(H2) similar to 10(5) cm(-3) at R < 50 pc. We develop an analytic treatment for the molecular excitation (including photon trapping), yielding volume densities for both the HCN and CS emission with n(H2) similar to 2 x 10(5) cm(-3). The agreement of the mean density from the total mass and size with that required for excitation suggests that the volume is essentially filled with dense gas, i.e., it is not cloudy or like swiss cheese. C1 [Scoville, Nick; Manohar, Swarnima; Murchikova, Lena] CALTECH, Pasadena, CA 91125 USA. [Sheth, Kartik; Fomalont, Edward] Natl Radio Astron Observ, North Amer ALMA Sci Ctr, Charlottesville, VA 22901 USA. [Walter, Fabian; Zschaechner, Laura] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Yun, Min] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Koda, Jin] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA. [Sanders, David; Barnes, Joshua] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Thompson, Todd] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Thompson, Todd] Ohio State Univ, Ctr Cosmol & AstroParticle Phys, Columbus, OH 43210 USA. [Robertson, Brant; Tacconi, Linda; Narayanan, Desika] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA. [Robertson, Brant; Tacconi, Linda; Narayanan, Desika] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Genzel, Reinhard; Davies, Richard] Max Planck Inst Extraterr Phys MPE, D-85748 Garching, Germany. [Hernquist, Lars] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Brown, Robert; Fomalont, Edward] Natl Radio Astron Observ, Charlottesville, VA 22901 USA. [Hayward, Christopher C.] CALTECH, TAPIR 350 17, Pasadena, CA 91125 USA. [Kartaltepe, Jeyhan] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Van Der Werf, Paul] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. RP Scoville, N (reprint author), CALTECH, MC 249-17,1200 East Calif Blvd, Pasadena, CA 91125 USA. RI Hayward, Christopher/I-4756-2012; OI Hayward, Christopher/0000-0003-4073-3236; Koda, Jin/0000-0002-8762-7863 FU National Radio Astronomy Observatory; National Science Foundation FX We thank the referee for a very thorough reading of the manuscript. We thank Zara Scoville for proofreading the manuscript. K.S. is supported by the National Radio Astronomy Observatory, which is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This paper makes use of the following ALMA data: ADS/JAO.ALMA2011.0.00175. S. ALMA is a partnership of ESO (representing its member states), NSF (USA), and NINS (Japan); together with NRC (Canada) and NSC and ASIAA (Taiwan), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. NR 69 TC 30 Z9 30 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 2015 VL 800 IS 1 AR 70 DI 10.1088/0004-637X/800/1/70 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CA9IQ UT WOS:000349236900070 ER PT J AU Vanderburg, A Montet, BT Johnson, JA Buchhave, LA Zeng, L Pepe, F Cameron, AC Latham, DW Molinari, E Udry, S Lovis, C Matthews, JM Cameron, C Law, N Bowler, BP Angus, R Baranec, C Bieryla, A Boschin, W Charbonneau, D Cosentino, R Dumusque, X Figueira, P Guenther, DB Harutyunyan, A Hellier, C Kuschnig, R Lopez-Morales, M Mayor, M Micela, G Moffat, AFJ Pedani, M Phillip, DF Piotto, G Pollacco, D Queloz, D Rice, K Riddle, R Rowe, JF Rucinski, SM Sasselov, D Segransan, D Sozzetti, A Szentgyorgyi, A Watson, C Weiss, WW AF Vanderburg, Andrew Montet, Benjamin T. Johnson, John Asher Buchhave, Lars A. Zeng, Li Pepe, Francesco Cameron, Andrew Collier Latham, David W. Molinari, Emilio Udry, Stephane Lovis, Christophe Matthews, Jaymie M. Cameron, Chris Law, Nicholas Bowler, Brendan P. Angus, Ruth Baranec, Christoph Bieryla, Allyson Boschin, Walter Charbonneau, David Cosentino, Rosario Dumusque, Xavier Figueira, Pedro Guenther, David B. Harutyunyan, Avet Hellier, Coel Kuschnig, Rainer Lopez-Morales, Mercedes Mayor, Michel Micela, Giusi Moffat, Anthony F. J. Pedani, Marco Phillip, David F. Piotto, Giampaolo Pollacco, Don Queloz, Didier Rice, Ken Riddle, Reed Rowe, Jason F. Rucinski, Slavek M. Sasselov, Dimitar Segransan, Damien Sozzetti, Alessandro Szentgyorgyi, Andrew Watson, Chris Weiss, Werner W. TI CHARACTERIZING K2 PLANET DISCOVERIES: A SUPER-EARTH TRANSITING THE BRIGHT K DWARF HIP 116454 SO ASTROPHYSICAL JOURNAL LA English DT Article DE planets and satellites: detection; techniques: photometric ID LASER ADAPTIVE OPTICS; NEPTUNE-MASS PLANET; SKY SURVEY; PROPER-MOTION; SHORT-PERIOD; HD 97658B; EXOPLANET; KEPLER; STARS; MISSION AB We report the first planet discovery from the two-wheeled Kepler (K2) mission: HIP 116454 b. The host star HIP 116454 is a bright (V = 10.1, K = 8.0) K1 dwarf with high proper motion and a parallax-based distance of 55.2 +/- 5.4 pc. Based on high-resolution optical spectroscopy, we find that the host star is metal-poor with [Fe/H]= -0.16 +/- 0.08 and has a radius R-star = 0.716 +/- 0.024 R-circle dot and mass M-star = 0.775 +/- 0.027M(circle dot). The star was observed by the Kepler spacecraft during its Two-Wheeled Concept Engineering Test in 2014 February. During the 9 days of observations, K2 observed a single transit event. Using a new K2 photometric analysis technique, we are able to correct small telescope drifts and recover the observed transit at high confidence, corresponding to a planetary radius of R-p = 2.53 +/- 0.18 R-circle plus. Radial velocity observations with the HARPS-N spectrograph reveal a 11.82 +/- 1.33 M-circle plus planet in a 9.1 day orbit, consistent with the transit depth, duration, and ephemeris. Follow-up photometric measurements from the MOST satellite confirm the transit observed in the K2 photometry and provide a refined ephemeris, making HIP 116454 b amenable for future follow-up observations of this latest addition to the growing population of transiting super-Earths around nearby, bright stars. C1 [Vanderburg, Andrew; Montet, Benjamin T.; Johnson, John Asher; Buchhave, Lars A.; Zeng, Li; Latham, David W.; Angus, Ruth; Bieryla, Allyson; Charbonneau, David; Dumusque, Xavier; Lopez-Morales, Mercedes; Phillip, David F.; Sasselov, Dimitar; Szentgyorgyi, Andrew] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Montet, Benjamin T.; Bowler, Brendan P.; Riddle, Reed] CALTECH, Pasadena, CA 91125 USA. [Pepe, Francesco; Udry, Stephane; Lovis, Christophe; Mayor, Michel; Segransan, Damien] Univ Geneva, Astron Observ, CH-1290 Versoix, Switzerland. [Cameron, Andrew Collier] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland. [Molinari, Emilio; Boschin, Walter; Cosentino, Rosario; Harutyunyan, Avet; Pedani, Marco; Piotto, Giampaolo] INAF Fdn Galileo Galilei, E-38712 Brena Baja, Spain. [Molinari, Emilio; Piotto, Giampaolo] INAF IASF Milano, I-20133 Milan, Italy. [Matthews, Jaymie M.] Univ British Columbia, Vancouver, BC V6T 1Z1, Canada. [Cameron, Chris] Cape Breton Univ, Sydney, NS B1P 6L2, Canada. [Law, Nicholas] Univ N Carolina, Chapel Hill, NC 27599 USA. [Angus, Ruth] Univ Oxford, Oxford, England. [Baranec, Christoph] Univ Hawaii Manoa, Hilo, HI 96720 USA. [Figueira, Pedro] Univ Porto, Ctr Astrofis, P-4150762 Oporto, Portugal. [Figueira, Pedro] Univ Porto, CAUP, Inst Astrofis & Ciencias Espaco, P-4150762 Oporto, Portugal. [Guenther, David B.] St Marys Univ, Halifax, NS B3H 3C3, Canada. [Hellier, Coel] Keele Univ, Astrophys Grp, Keele ST5 5BG, Staffs, England. [Kuschnig, Rainer; Weiss, Werner W.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria. [Micela, Giusi] INAF Osservatorio Astron Palermo, I-90124 Palermo, Italy. [Moffat, Anthony F. J.] Univ Montreal, Montreal, PQ H3C 3J7, Canada. [Moffat, Anthony F. J.] Obs Mont Megant, Notre Dame Des Bois, PQ J0B 2E0, Canada. [Pollacco, Don] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Queloz, Didier] Univ Cambridge, Cavendish Lab, Cambridge CB3 0HE, England. [Rice, Ken] Univ Edinburgh, Inst Astron, Royal Observ, SUPA, Edinburgh EH9 3HJ, Midlothian, Scotland. [Rowe, Jason F.] SETI Inst, Mountain View, CA 94043 USA. [Rowe, Jason F.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Rucinski, Slavek M.] Univ Toronto, Toronto, ON M5S 3H4, Canada. [Sozzetti, Alessandro] INAF Osservatorio Astron Torino, I-10025 Pino Torinese, Italy. [Watson, Chris] Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland. RP Vanderburg, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM avanderburg@cfa.harvard.edu RI Rice, Ken/H-5084-2011; Figueira, Pedro/J-4916-2013; OI Rice, Ken/0000-0002-6379-9185; Figueira, Pedro/0000-0001-8504-283X; Sozzetti, Alessandro/0000-0002-7504-365X; Montet, Benjamin/0000-0001-7516-8308; Zeng, Li/0000-0003-1957-6635; Molinari, Emilio/0000-0002-1742-7735; Cameron, Andrew/0000-0002-8863-7828; Buchhave, Lars A./0000-0003-1605-5666 FU NASA [NAS5-26555]; NASA Office of Space Science [NNX13AC07G]; NASA Science Mission directorate; National Aeronautics and Space Administration under the Exoplanet Exploration Program; National Science Foundation Graduate Research Fellowship [DGE 1144152, DGE 1144469]; David and Lucile Packard Foundation; Alfred P. Sloan Foundation; Fundacao para a Ciencia e a Tecnologia (FCT) through Investigador FCT [IF/01037/2013]; POPH/FSE (EC) by FEDER through the program "Programa Operacional de Factores de Competitividade-COMPETE; Austrian Science Fund [FWF P22691-N16]; European Union Seventh Framework Programme (FP7) [313014 (ETAEARTH)]; John Templeton Foundation; Prodex program of the Swiss Space Office (SSO); Harvard University Origin of Life Initiative (HUOLI); Scottish Universities Physics Alliance (SUPA); University of Geneva; Smithsonian Astrophysical Observatory (SAO); Italian National Astrophysical Institute (INAF); University of St. Andrews; Queens University Belfast; University of Edinburgh; California Institute of Technology; Inter-University Centre for Astronomy and Astrophysics; National Science Foundation [AST-0906060, AST-0960343, AST-1207891]; Mount Cuba Astronomical Foundation; W.M. Keck Foundation; UK's Science and Technology Facilities Council (STFC); U.S. Government [NAG W-2166]; National Geographic Society; National Science Foundation; Sloan Foundation; Samuel Oschin Foundation; Eastman Kodak Corporation; U.S. Department of Energy Office of Science; University of Arizona; Brazilian Participation Group; Brookhaven National Laboratory; Carnegie Mellon University; University of Florida; French Participation Group; German Participation Group; Harvard University; Instituto de Astrofisica de Canarias; Michigan State/NotreDame/JINA Participation Group; Johns Hopkins University; Lawrence Berkeley National Laboratory; Max Planck Institute for Astrophysics; Max Planck Institute for Extraterrestrial Physics; New Mexico State University; New York University; Ohio State University; Pennsylvania State University; University of Portsmouth; Princeton University; Spanish Participation Group; University of Tokyo; University of Utah; Vanderbilt University; University of Virginia; University of Washington; Yale University FX Some of the data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant NNX13AC07G and by other grants and contracts. This paper includes data collected by the Kepler mission. Funding for the Kepler mission is provided by the NASA Science Mission directorate.; This research has made use of NASA's Astrophysics Data System; the SIMBAD database and VizieR catalog access tool, operated at CDS, Strasbourg, France; the Exoplanet Orbit Database and the Exoplanet Data Explorer at http://www.exoplanets.org; PyAstronomy, the repository and documentation for which can be found at https://github.com/sczesla/PyAstronomy; and the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program.; A.V. and B.T.M. are supported by the National Science Foundation Graduate Research Fellowship, grants No. DGE 1144152 and DGE 1144469, respectively. J.A.J. is supported by generous grants from the David and Lucile Packard and Alfred P. Sloan Foundations. C.B. acknowledges support from the Alfred P. Sloan Foundation. P.F. acknowledges support by Fundacao para a Ciencia e a Tecnologia (FCT) through Investigador FCT contracts of reference IF/01037/2013 and POPH/FSE (EC) by FEDER funding through the program "Programa Operacional de Factores de Competitividade-COMPETE." W.W.W. was supported by the Austrian Science Fund (FWF P22691-N16). The research leading to these results has received funding from the European Union Seventh Framework Programme (FP7/2007-2013) under grant Agreement No. 313014 (ETAEARTH). This publication was made possible through the support of a grant from the John Templeton Foundation. The opinions expressed in this publication are those of the authors and do not necessarily reflect the views of the John Templeton Foundation.; This work is based on observations made with the Italian Telescopio Nazionale Galileo (TNG) operated on the island of La Palma by the Fundacin Galileo Galilei of the INAF (Istituto Nazionale di Astrofisica) at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. The HARPS-N project was funded by the Prodex program of the Swiss Space Office (SSO), the Harvard University Origin of Life Initiative (HUOLI), the Scottish Universities Physics Alliance (SUPA), the University of Geneva, the Smithsonian Astrophysical Observatory (SAO), and the Italian National Astrophysical Institute (INAF), University of St. Andrews, Queens University Belfast, and University of Edinburgh.; The Robo-AO system is supported by collaborating partner institutions, the California Institute of Technology and the Inter-University Centre for Astronomy and Astrophysics, and by the National Science Foundation under grant Nos. AST-0906060, AST-0960343, and AST-1207891, by the Mount Cuba Astronomical Foundation, by a gift from Samuel Oschin.; Some of the data presented herein were obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The observatory was made possible by the generous financial support of the W.M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain.; WASP-South is hosted by the SAAO and SuperWASP by the Isaac Newton Group and the Instituto de Astrofisica deCanarias; we gratefully acknowledge their ongoing support and assistance. Funding for WASP comes from consortium universities and from the UK's Science and Technology Facilities Council (STFC).; The Digitized Sky Surveys were produced at the Space Telescope Science Institute under U.S. Government grant NAG W-2166. The images of these surveys are based on photographic data obtained using the Oschin Schmidt Telescope on Palomar Mountain and the U.K. Schmidt Telescope. The plates were processed into the present compressed digital form with the permission of these institutions.; The National Geographic Society-Palomar Observatory Sky Atlas (POSS-I) was made by the California Institute of Technology with grants from the National Geographic Society. The Second Palomar Observatory Sky Survey (POSS-II) was made by the California Institute of Technology with funds from the National Science Foundation, the National Geographic Society, the Sloan Foundation, the Samuel Oschin Foundation, and the Eastman Kodak Corporation. The Oschin Schmidt Telescope is operated by the California Institute of Technology and Palomar Observatory.; Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the participating institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. The SDSS-III web site is http://www.sdss3.org/.; SDSS-III is managed by the Astrophysical Research Consortium for the participating institutions of the SDSS-III Collaboration, including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/NotreDame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University. NR 73 TC 31 Z9 31 U1 2 U2 32 PU IOP PUBLISHING LTD 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 2015 VL 800 IS 1 AR 59 DI 10.1088/0004-637X/800/1/59 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CA9IQ UT WOS:000349236900059 ER PT J AU Wittenmyer, RA Wang, L Liu, F Horner, J Endl, M Johnson, JA Tinney, CG Carter, BD AF Wittenmyer, Robert A. Wang, Liang Liu, Fan Horner, Jonathan Endl, Michael Johnson, John Asher Tinney, C. G. Carter, B. D. TI THE PAN-PACIFIC PLANET SEARCH. II. CONFIRMATION OF A TWO-PLANET SYSTEM AROUND HD 121056 SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; stars: individual (HD 121056); techniques: radial velocities ID ANGLO-AUSTRALIAN PLANET; RADIAL-VELOCITY MEASUREMENTS; GIANT PLANET; STELLAR EVOLUTION; JUPITER ANALOGS; SPACED DATA; BD+20 2457; K-GIANT; STARS; SUBGIANTS AB Precise radial velocities from the Anglo-Australian Telescope (AAT) confirm the presence of a rare short-period planet around the K0 giant HD 121056. An independent two-planet solution using the AAT data shows that the inner planet has P = 89.1 +/- 0.1 days, and m sin i = 1.35 +/- 0.17 M-Jup. These data also confirm the planetary nature of the outer companion, with m sin i = 3.9 +/- 0.6 M-Jup and a = 2.96 +/- 0.16 AU. HD 121056 is the most-evolved star to host a confirmed multiple-planet system, and is a valuable example of a giant star hosting both a short-period and a long-period planet. C1 [Wittenmyer, Robert A.; Tinney, C. G.] Univ New S Wales, Sch Phys, Sydney, NSW 2052, Australia. [Wittenmyer, Robert A.; Horner, Jonathan; Tinney, C. G.] Univ New S Wales, Australian Ctr Astrobiol, Sydney, NSW 2052, Australia. [Wang, Liang] Chinese Acad Sci, Key Lab Opt Astron, Natl Astron Observ, Beijing 100012, Peoples R China. [Liu, Fan] Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. [Horner, Jonathan; Carter, B. D.] Univ So Queensland, Computat Engn & Sci Res Ctr, Toowoomba, Qld 4350, Australia. [Endl, Michael] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA. [Johnson, John Asher] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Wittenmyer, RA (reprint author), Univ New S Wales, Sch Phys, Sydney, NSW 2052, Australia. EM rob@unsw.edu.au OI Tinney, Christopher/0000-0002-7595-0970; Wang, Liang/0000-0003-3603-1901; Horner, Jonti/0000-0002-1160-7970 FU Australian Research Council [DP0774000, DP130102695]; USQ's Strategic Research Fund; National Science Foundation [AST-1313075] FX C.G.T. is supported by Australian Research Council grants DP0774000 and DP130102695. J.H. and B.D.C. are supported by USQ's Strategic Research Fund. We gratefully acknowledge the efforts of PPPS guest observers Hugh Jones and Simon O'Toole. This research has made use of NASA's Astrophysics Data System (ADS), and the SIMBAD database, operated at CDS, Strasbourg, France. This research has also made use of the Exoplanet Orbit Database and the Exoplanet Data Explorer at exoplanets. org (Wright et al. 2011). M.E. is supported by the National Science Foundation through grant AST-1313075. NR 96 TC 4 Z9 4 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2015 VL 800 IS 1 AR 74 DI 10.1088/0004-637X/800/1/74 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CA9IQ UT WOS:000349236900074 ER PT J AU Zhu, QR Hernquist, L Li, YX AF Zhu, Qirong Hernquist, Lars Li, Yuexing TI NUMERICAL CONVERGENCE IN SMOOTHED PARTICLE HYDRODYNAMICS SO ASTROPHYSICAL JOURNAL LA English DT Article DE hydrodynamics; methods: numerical ID MOVING-MESH; SUBSONIC TURBULENCE; GALAXY FORMATION; SIMULATION CODE; SPH; PROJECT; ENVIRONMENTS; DISSIPATION; FEEDBACK; DENSITY AB We study the convergence properties of smoothed particle hydrodynamics (SPH) using numerical tests and simple analytic considerations. Our analysis shows that formal numerical convergence is possible in SPH only in the joint limit N -> infinity, h -> 0, and N-nb -> infinity, where N is the total number of particles, h is the smoothing length, and N-nb is the number of neighbor particles within the smoothing volume used to compute smoothed estimates. Previous work has generally assumed that the conditions N -> infinity and h -> 0 are sufficient to achieve convergence, while holding N-nb fixed. We demonstrate that if Nnb is held fixed as the resolution is increased, there will be a residual source of error that does not vanish as N -> infinity and h -> 0. Formal numerical convergence in SPH is possible only if N-nb is increased systematically as the resolution is improved. Using analytic arguments, we derive an optimal compromise scaling for N-nb by requiring that this source of error balance that present in the smoothing procedure. For typical choices of the smoothing kernel, we find N-nb proportional to N-0.5. This means that if SPH is to be used as a numerically convergent method, the required computational cost does not scale with particle number as O(N), but rather as O(N1+delta), where delta approximate to 0.5, with a weak dependence on the form of the smoothing kernel. C1 [Zhu, Qirong; Li, Yuexing] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Zhu, Qirong; Li, Yuexing] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. [Hernquist, Lars] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Zhu, QR (reprint author), Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA. FU NASA [NNX12AC67G]; NSF [AST-1312095, AST-0965694, AST-1009867, AST-1412719]; Eberly College of Science; Office of the Senior Vice President for Research at the Pennsylvania State University FX We thank Volker Springel, Phil Hopkins, Mark Vogelsberger, Jim Stone, Andreas Bauer, and Daniel Price for valuable discussions on this work. We further thank Paul Torrey for his contributions to the experimental setups in the early stage and suggestions throughout the project. L.H. acknowledges support from NASA grant NNX12AC67G and NSF grant AST-1312095. Y.L. acknowledges support from NSF grants AST-0965694, AST-1009867, and AST-1412719. We acknowledge the Institute For CyberScience at the Pennsylvania State University for providing computational resources and services that have contributed to the research results reported in this paper. The Institute for Gravitation and the Cosmos is supported by the Eberly College of Science and the Office of the Senior Vice President for Research at the Pennsylvania State University. NR 50 TC 11 Z9 11 U1 0 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2015 VL 800 IS 1 AR 6 DI 10.1088/0004-637X/800/1/6 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CA9IQ UT WOS:000349236900006 ER PT J AU Van Loo, S Tan, JC Falle, SAEG AF Van Loo, Sven Tan, Jonathan C. Falle, Sam A. E. G. TI MAGNETIC FIELDS AND GALACTIC STAR FORMATION RATES SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: ISM; galaxies: star clusters: general; ISM: clouds; ISM: structure; methods: numerical; stars: formation ID GIANT MOLECULAR CLOUDS; INTERSTELLAR CLOUDS; NEARBY GALAXIES; MILKY-WAY; SIMULATIONS; GAS; COLLISIONS; EVOLUTION AB The regulation of galactic-scale star formation rates (SFRs) is a basic problem for theories of galaxy formation and evolution: which processes are responsible for making observed star formation rates so inefficient compared to maximal rates of gas content divided by dynamical timescale? Here we study the effect of magnetic fields of different strengths on the evolution of giant molecular clouds (GMCs) within a kiloparsec patch of a disk galaxy and resolving scales down to. similar or equal to 0.5 pc. Including an empirically motivated prescription for star formation from dense gas (n(H) > 10(5) cm(-3)) at an efficiency of 2% per local free-fall time, we derive the amount of suppression of star formation by magnetic fields compared to the nonmagnetized case. We find GMC fragmentation, dense clump formation, and SFR can be significantly affected by the inclusion of magnetic fields, especially in our strongest investigated B-field case of 80 mu G. However, our chosen kiloparsec-scale region, extracted from a global galaxy simulation, happens to contain a starbursting cloud complex that is only modestly affected by these magnetic fields and likely requires internal star formation feedback to regulate its SFR. C1 [Van Loo, Sven] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Van Loo, Sven] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Tan, Jonathan C.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Tan, Jonathan C.] Univ Florida, Dept Phys, Gainesville, FL 32611 USA. [Falle, Sam A. E. G.] Univ Leeds, Dept Appl Math, Leeds LS2 9JT, W Yorkshire, England. RP Van Loo, S (reprint author), Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. EM S.VanLoo@leeds.ac.uk OI Van Loo, Sven/0000-0003-4746-8500 FU SMA Postdoctoral Fellowship (SAO); NASA [ATP 09-0094] FX S.V.L. acknowledges support from the SMA Postdoctoral Fellowship (SAO). J.C.T. acknowledges support from NASA grant ATP 09-0094. Resources supporting this work were provided by NASA High-End Computing Program, the Smithsonian Institution High Performance Cluster and the High Performance Computing facilities at the University of Leeds. NR 36 TC 6 Z9 6 U1 4 U2 12 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD FEB 10 PY 2015 VL 800 IS 1 AR L11 DI 10.1088/2041-8205/800/1/L11 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CB0KY UT WOS:000349316000011 ER PT J AU Frandsen, PB Calcott, B Mayer, C Lanfear, R AF Frandsen, Paul B. Calcott, Brett Mayer, Christoph Lanfear, Robert TI Automatic selection of partitioning schemes for phylogenetic analyses using iterative k-means clustering of site rates SO BMC EVOLUTIONARY BIOLOGY LA English DT Article DE Model selection; Partitioning; Partitionfinder; Phylogenetics; Phylogenomics; K-means; Clustering; Ultra-conserved elements; UCE's ID MAXIMUM-LIKELIHOOD; ULTRACONSERVED ELEMENTS; SUBSTITUTION MODELS; NUCLEOTIDE SUBSTITUTION; MOLECULAR PHYLOGENETICS; BAYESIAN PHYLOGENETICS; MITOCHONDRIAL GENOMES; SEQUENCE EVOLUTION; SYSTEMATIC BIASES; MIXTURE-MODELS AB Background: Model selection is a vital part of most phylogenetic analyses, and accounting for the heterogeneity in evolutionary patterns across sites is particularly important. Mixture models and partitioning are commonly used to account for this variation, and partitioning is the most popular approach. Most current partitioning methods require some a priori partitioning scheme to be defined, typically guided by known structural features of the sequences, such as gene boundaries or codon positions. Recent evidence suggests that these a priori boundaries often fail to adequately account for variation in rates and patterns of evolution among sites. Furthermore, new phylogenomic datasets such as those assembled from ultra-conserved elements lack obvious structural features on which to define a priori partitioning schemes. The upshot is that, for many phylogenetic datasets, partitioned models of molecular evolution may be inadequate, thus limiting the accuracy of downstream phylogenetic analyses. Results: We present a new algorithm that automatically selects a partitioning scheme via the iterative division of the alignment into subsets of similar sites based on their rates of evolution. We compare this method to existing approaches using a wide range of empirical datasets, and show that it consistently leads to large increases in the fit of partitioned models of molecular evolution when measured using AICc and BIC scores. In doing so, we demonstrate that some related approaches to solving this problem may have been associated with a small but important bias. Conclusions: Our method provides an alternative to traditional approaches to partitioning, such as dividing alignments by gene and codon position. Because our method is data-driven, it can be used to estimate partitioned models for all types of alignments, including those that are not amenable to traditional approaches to partitioning. C1 [Frandsen, Paul B.] Smithsonian Inst, Off CIO, Off Res Informat Serv, Washington, DC 20560 USA. [Frandsen, Paul B.] Rutgers State Univ, Dept Entomol, New Brunswick, NJ USA. [Calcott, Brett] Arizona State Univ, Sch Life Sci, Tempe, AZ USA. [Mayer, Christoph] Zentrum Mol Biodiversitatsforsch, Zool Forsch Museum Alexander Koenig ZFMK, Bonn, Germany. [Lanfear, Robert] Australian Natl Univ, Res Sch Biol, Canberra, ACT, Australia. [Lanfear, Robert] Natl Evolutionary Synth Ctr, Durham, NC USA. [Lanfear, Robert] Macquarie Univ, Dept Biol Sci, Sydney, NSW 2109, Australia. RP Frandsen, PB (reprint author), Smithsonian Inst, Off CIO, Off Res Informat Serv, Washington, DC 20560 USA. EM paulbfrandsen@gmail.com OI Frandsen, Paul/0000-0002-4801-7579 FU Google; National Evolutionary Synthesis Center (NESCent) through the Google Summer of Code/NESCent Phyloinformatics Summer of Code; Department of Entomology at Rutgers University; DAAD; NSF [DEB 0816865]; Australian Research Council FX PF is supported by (i) Google and the National Evolutionary Synthesis Center (NESCent) through the Google Summer of Code/NESCent Phyloinformatics Summer of Code, (ii) the Department of Entomology at Rutgers University through the Thomas J. Headlee fellowship, (iii) the DAAD (Germany academic exchange service) and (iv) NSF DEB 0816865. PF would like to thank Karl Kjer for many useful conversations concerning the development of the method and construction of the manuscript and Christine Frandsen for assistance with the figures. RL is supported by the Australian Research Council, and a short-term visitor grant to the National Evolutionary Synthesis Center (NESCent) provided by the NSF. NR 95 TC 15 Z9 16 U1 6 U2 24 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 FEB 10 PY 2015 VL 15 AR 13 DI 10.1186/s12862-015-0283-7 PG 17 WC Evolutionary Biology; Genetics & Heredity SC Evolutionary Biology; Genetics & Heredity GA CB0TJ UT WOS:000349339900001 PM 25887041 ER PT J AU Craine, JM Elmore, AJ Wang, LX Augusto, L Baisden, WT Brookshire, ENJ Cramer, MD Hasselquist, NJ Hobbie, EA Kahmen, A Koba, K Kranabetter, JM Mack, MC Marin-Spiotta, E Mayor, JR McLauchlan, KK Michelsen, A Nardoto, GB Oliveira, RS Perakis, SS Peri, PL Quesada, CA Richter, A Schipper, LA Stevenson, BA Tumer, BL Viani, RAG Wanek, W Zeller, B AF Craine, Joseph M. Elmore, Andrew J. Wang, Lixin Augusto, Laurent Baisden, W. Troy Brookshire, E. N. J. Cramer, Michael D. Hasselquist, Niles J. Hobbie, Erik A. Kahmen, Ansgar Koba, Keisuke Kranabetter, J. Marty Mack, Michelle C. Marin-Spiotta, Erika Mayor, Jordan R. McLauchlan, Kendra K. Michelsen, Anders Nardoto, Gabriela B. Oliveira, Rafael S. Perakis, Steven S. Peri, Pablo L. Quesada, Carlos A. Richter, Andreas Schipper, Louis A. Stevenson, Bryan A. Tumer, Benjamin L. Viani, Ricardo A. G. Wanek, Wolfgang Zeller, Bernd TI Convergence of soil nitrogen isotopes across global climate gradients SO SCIENTIFIC REPORTS LA English DT Article ID N-15 NATURAL-ABUNDANCE; ORGANIC-MATTER; LITTER DECOMPOSITION; INORGANIC NITROGEN; TROPICAL FORESTS; CARBON; PATTERNS; MODEL; FRACTIONATION; AVAILABILITY AB Quantifying global patterns of terrestrial nitrogen (N) cycling is central to predicting future patterns of primary productivity, carbon sequestration, nutrient fluxes to aquatic systems, and climate forcing. With limited direct measures of soil N cycling at the global scale, syntheses of the N-15 : N-14 ratio of soil organic matter across climate gradients provide key insights into understanding global patterns of N cycling. In synthesizing data from over 6000 soil samples, we show strong global relationships among soil N isotopes, mean annual temperature (MAT), mean annual precipitation (MAP), and the concentrations of organic carbon and clay in soil. In both hot ecosystems and dry ecosystems, soil organic matter was more enriched in N-15 than in corresponding cold ecosystems or wet ecosystems. Below a MAT of 9.8 degrees C, soil delta N-15 was invariant with MAT. At the global scale, soil organic C concentrations also declined with increasing MAT and decreasing MAP. After standardizing for variation among mineral soils in soil C and clay concentrations, soil delta N-15 showed no consistent trends across global climate and latitudinal gradients. Our analyses could place new constraints on interpretations of patterns of ecosystem N cycling and global budgets of gaseous N loss. C1 [Craine, Joseph M.] Kansas State Univ, Div Biol, Manhattan, KS 66506 USA. [Elmore, Andrew J.] Univ Maryland, Ctr Environm Sci, Appalachian Lab, Frostburg, MD 21532 USA. [Wang, Lixin] Indiana Univ Purdue Univ, Dept Earth Sci, Indianapolis, IN 46202 USA. [Augusto, Laurent] Bordeaux Sci Agro, INRA, UMR TCEM 1220, F-33883 Villenave Dornon, France. [Baisden, W. Troy] GNS Sci, Natl Isotope Ctr, Lower Hutt 5040, New Zealand. [Brookshire, E. N. J.] Montana State Univ, Dept Land Resources & Environm Sci, Bozeman, MT 59717 USA. [Cramer, Michael D.] Univ Cape Town, Dept Biol Sci, Rondebosch, South Africa. [Hasselquist, Niles J.] Swedish Univ Agr Sci SLU, Forest Ecol & Management, S-90183 Umea, Sweden. [Hobbie, Erik A.] Univ New Hampshire, Earth Syst Res Ctr, Durham, NH 03824 USA. [Kahmen, Ansgar] Dept Environm Sci Bot, CH-4056 Basel, Switzerland. [Koba, Keisuke] Tokyo Univ Agr & Technol, Inst Agr, Fuchu, Tokyo 1838509, Japan. [Kranabetter, J. Marty] British Columbia Minist Forests, Lands & Nat Resource Operat, Victoria, BC V8Z 5J3, Canada. [Mack, Michelle C.] Univ Florida, Dept Biol, Gainesville, FL 32607 USA. [Marin-Spiotta, Erika] Univ Wisconsin, Dept Geog, Madison, WI 53706 USA. [Mayor, Jordan R.] Swedish Univ Agr Sci, Dept Forest Ecol & Management, S-90183 Umea, Sweden. [McLauchlan, Kendra K.] Kansas State Univ, Dept Geog, Manhattan, KS 66506 USA. [Michelsen, Anders] Univ Copenhagen, Dept Biol, DK-2100 Copenhagen O, Denmark. [Nardoto, Gabriela B.] Univ Brasilia, Fac UnB Planaltina, BR-73345010 Brasilia, DF, Brazil. [Oliveira, Rafael S.] Univ Estadual Campinas, Inst Biol, Dept Biol Vegetal, BR-13083862 Campinas, Brazil. [Perakis, Steven S.] US Geol Survey, Forest & Rangeland Ecosyst Sci Ctr, Corvallis, OR 97331 USA. [Peri, Pablo L.] Univ Nacl Patagonia, Austral INTA CONICET, RA-9400 Santa Cruz, CA, Argentina. [Quesada, Carlos A.] Inst Nacl de Pesquisas da Amazonia, BR-69011 Manaus, Amazonas, Brazil. [Richter, Andreas] Univ Vienna, Dept Terr Ecosyst Res, A-1090 Vienna, Austria. [Schipper, Louis A.] Univ Waikato, Environm Res Inst, Hamilton 3240, New Zealand. [Stevenson, Bryan A.] Landcare Res Hamilton, Hamilton 3240, New Zealand. [Tumer, Benjamin L.] Smithsonian Trop Res Inst, Balboa, Panama. [Viani, Ricardo A. G.] Univ Fed Sao Carlos, DBPVA, Ctr Ciencias Agr, BR-13600970 Araras, SP, Brazil. [Zeller, Bernd] INRA Nancy, Biogeochim Ecosyst Forestiers, F-54280 Champenoux, France. RP Craine, JM (reprint author), Kansas State Univ, Div Biol, Manhattan, KS 66506 USA. EM josephmcraine@gmail.com RI Schipper, Louis/F-1605-2010; Craine, Joseph/D-4569-2009; Oliveira, Rafael/B-3422-2013; Wang, Lixin/A-2572-2008; Koba, Keisuke/A-3699-2012; Richter, Andreas/D-8483-2012; Elmore, Andrew/D-4341-2012; Wanek, Wolfgang/E-7001-2012; Michelsen, Anders/L-5279-2014; Nardoto, Gabriela/J-7459-2012; OI Schipper, Louis/0000-0001-9899-1276; Craine, Joseph/0000-0001-6561-3244; Oliveira, Rafael/0000-0002-6392-2526; Wang, Lixin/0000-0003-0968-1247; Koba, Keisuke/0000-0003-1942-9811; Richter, Andreas/0000-0003-3282-4808; Elmore, Andrew/0000-0002-9697-9457; Wanek, Wolfgang/0000-0003-2178-8258; Michelsen, Anders/0000-0002-9541-8658; Nardoto, Gabriela/0000-0001-8062-7417; Marin-Spiotta, Erika/0000-0001-7343-9354 NR 43 TC 13 Z9 13 U1 11 U2 101 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 2045-2322 J9 SCI REP-UK JI Sci Rep PD FEB 6 PY 2015 VL 5 AR 8280 DI 10.1038/srep08280 PG 8 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CA4VJ UT WOS:000348903800001 PM 25655192 ER PT J AU Johnson, KR AF Johnson, Kirk R. TI Life on Display Revolutionizing US Museums of Science and Natural History in the Twentieth Century SO SCIENCE LA English DT Book Review C1 [Johnson, Kirk R.] Smithsonian Natl Museum Nat Hist, Washington, DC 20560 USA. RP Johnson, KR (reprint author), Smithsonian Natl Museum Nat Hist, Washington, DC 20560 USA. EM johnsonkr@si.edu NR 1 TC 1 Z9 1 U1 0 U2 3 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 EI 1095-9203 J9 SCIENCE JI Science PD FEB 6 PY 2015 VL 347 IS 6222 BP 618 EP 618 DI 10.1126/science.aaa0840 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CA8CX UT WOS:000349145200027 ER PT J AU Ayon-Parente, M Hendrickx, ME Lemaitre, R AF Ayon-Parente, Manuel Hendrickx, Michel E. Lemaitre, Rafael TI Redescription and taxonomic status of Paguristes praedator Glassell, 1937 and P. oxyophthalmus Holthuis, 1959 (Anomura: Paguroidea: Diogenidae), with an emendation to the diagnosis of the genus Areopaguristes Rahayu & McLaughlin, 2010 SO ZOOTAXA LA English DT Article DE Crustacea; Diogenidae; hermit crabs; Areopaguristes; new combination; eastern Pacific; western Atlantic ID EASTERN TROPICAL PACIFIC; DECAPOD CRUSTACEANS; COSTA-RICA; CHECKLIST; CRABS AB The taxonomic status of Paguristes praedator Glassell, 1937, and Paguristes oxyophthalmus Holthuis, 1959, is reevaluated, and the two species redescribed and illustrated in detail. Both species are transferred to the genus Areopaguristes Rahayu & McLaughlin, 2010, a genus previously defined to accommodate species of Paguristes sensu lato with 12 pairs of gills instead of 13. Two important characters in both species were found to differ or have not been mentioned in the current definition of Areopaguristes, i.e., the first maxilliped lacking epipod, and dactyls of second and third pereopods unarmed on the ventral margins. The presence of other diagnostically significant characters (e. g., lack of first pleopods in females) previously noted in other species of Areopaguristes, requires the generic emendation of this genus presented herein. With the transfer of A. praedator nov. comb. and A. oxyophthalmus nov. comb. to Areopaguristes, this genus now contains 27 species, of which nine occur in the Americas (four in the eastern tropical Pacific, and five in the western Atlantic). C1 [Ayon-Parente, Manuel] CUCBA Univ Guadalajara, Dept Ecol, Zapopan 45110, Jalisco, Mexico. [Hendrickx, Michel E.] Univ Nacl Autonoma Mexico, Lab Invertebrados Benton, Unidad Acad Mazatlan, Inst Ciencias Mar & Limnol, Mazatlan 82000, Sinaloa, Mexico. [Lemaitre, Rafael] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Suitland, MD 20746 USA. RP Ayon-Parente, M (reprint author), CUCBA Univ Guadalajara, Dept Ecol, Carretera Nogales Km 15-5, Zapopan 45110, Jalisco, Mexico. EM manuel_aparente@hotmail.com; michel@ola.icmyl.unam.mx; lemaitrr@si.edu FU CONACyt [125847]; CONACyT, Mexico [PCCBNA-021996]; [FONCICYT 94482] FX The authors acknowledge with deep gratitude the cooperation and assistance provided by Joel W. Martin and George E. Davis (LACM CR), Harim Cha (SIO-C), Mary W. Wicksten (TCWC) and Victor Landa (CEC) during the stay by one of us (MAP) in their respective museum, and for loan of material. Thank to Rosa Maria Prol for providing material (project FONCICYT 94482). Thanks also to R. Gulledge (USNM) for helping with some illustrations. One of us (MAP) was supported by a CONACyt grant (125847). Molluscs identifications were performed by Arturo Toledano-Granados. Ship time aboard the R/V "El Puma" (SIPCO, CORTES, GUAYTEC and BIOCAPESS cruises) was provided by the Instituto de Ciencias del Mar y Limnologia, UNAM. The CORTES project was partly supported by CONACyT (PCCBNA-021996), Mexico. NR 44 TC 2 Z9 2 U1 0 U2 4 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD FEB 5 PY 2015 VL 3915 IS 4 BP 491 EP 509 PG 19 WC Zoology SC Zoology GA CB5PT UT WOS:000349680700002 PM 25662139 ER PT J AU Sohn, JC Labandeira, CC Davis, DR AF Sohn, Jae-Cheon Labandeira, Conrad C. Davis, Donald R. TI The fossil record and taphonomy of butterflies and moths (Insecta, Lepidoptera): implications for evolutionary diversity and divergence-time estimates SO BMC EVOLUTIONARY BIOLOGY LA English DT Review DE Lepidoptera; Fossil record; Taphonomy; Diversity; Divergence-time estimation ID SPECIES RICHNESS; DIVERSIFICATION; GENE; AGE; ANGIOSPERMS; PHYLOGENY; PATTERNS; LINEAGE; CLOCK; AMBER AB Background: It is conventionally accepted that the lepidopteran fossil record is significantly incomplete when compared to the fossil records of other, very diverse, extant insect orders. Such an assumption, however, has been based on cumulative diversity data rather than using alternative statistical approaches from actual specimen counts. Results: We reviewed documented specimens of the lepidopteran fossil record, currently consisting of 4,593 known specimens that are comprised of 4,262 body fossils and 331 trace fossils. The temporal distribution of the lepidopteran fossil record shows significant bias towards the late Paleocene to middle Eocene time interval. Lepidopteran fossils also record major shifts in preservational style and number of represented localities at the Mesozoic stage and Cenozoic epoch level of temporal resolution. Only 985 of the total known fossil specimens (21.4%) were assigned to 23 of the 40 extant lepidopteran superfamilies. Absolute numbers and proportions of preservation types for identified fossils varied significantly across superfamilies. The secular increase of lepidopteran family-level diversity through geologic time significantly deviates from the general pattern of other hyperdiverse, ordinal-level lineages. Conclusion: Our statistical analyses of the lepidopteran fossil record show extreme biases in preservation type, age, and taxonomic composition. We highlight the scarcity of identified lepidopteran fossils and provide a correspondence between the latest lepidopteran divergence-time estimates and relevant fossil occurrences at the superfamily level. These findings provide caution in interpreting the lepidopteran fossil record through the modeling of evolutionary diversification and in determination of divergence time estimates. C1 [Sohn, Jae-Cheon; Davis, Donald R.] Natl Museum Nat Hist, Smithsonian Inst, Dept Entomol, Washington, DC 20560 USA. [Sohn, Jae-Cheon; Labandeira, Conrad C.] Natl Museum Nat Hist, Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA. [Sohn, Jae-Cheon; Labandeira, Conrad C.] Univ Maryland, Dept Entomol, College Pk, MD 20742 USA. [Labandeira, Conrad C.] Capital Normal Univ, Coll Life Sci, Beijing, Peoples R China. RP Sohn, JC (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Dept Entomol, Washington, DC 20560 USA. EM jsohn@umd.edu FU U. S. National Science Foundation [0531769]; Peter Buck Postdoctoral Fellowship (Smithsonian Institution) FX We are very grateful to Charles Mitter, Jerome Regier (Department of Entomology, University of Maryland), Michael Cummings (Laboratory of Molecular Evolution, University of Maryland), Andreas Zwick (State Museum of Natural History, Stuttgart) and other colleagues in the Lepidoptera Assembling the Tree of Life project ("LepTree") for their contributions to an improved lepidopteran phylogeny that forms the basis of our work. The first author is especially indebted to many museum curators acknowledged in Sohn et al. (2012) that provided assistance with the institutional collections. Financial support was provided by the U. S. National Science Foundation's Assembling the Tree of Life program (award 0531769) and the Peter Buck Postdoctoral Fellowship (Smithsonian Institution). Finnegan Marsh adeptly rendered Figures 1, 2, 3 and 4. This is contribution 267 of the Evolution of Terrestrial Ecosystems consortium of the National Museum of Natural History, in Washington, D. C. NR 78 TC 9 Z9 9 U1 4 U2 37 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 FEB 4 PY 2015 VL 15 AR 12 DI 10.1186/s12862-015-0290-8 PG 15 WC Evolutionary Biology; Genetics & Heredity SC Evolutionary Biology; Genetics & Heredity GA CB0TG UT WOS:000349339600001 PM 25649001 ER PT J AU Agarwal, V Li, J Rahman, I Borgen, M Aluwihare, LI Biggs, JS Paul, VJ Moore, BS AF Agarwal, Vinayak Li, Jie Rahman, Imran Borgen, Miles Aluwihare, Lihini I. Biggs, Jason S. Paul, Valerie J. Moore, Bradley S. TI Complexity of Naturally Produced Polybrominated Diphenyl Ethers Revealed via Mass Spectrometry SO ENVIRONMENTAL SCIENCE & TECHNOLOGY LA English DT Article ID MARINE SPONGE; VANADIUM BROMOPEROXIDASE; OH-PBDES; BIOSYNTHESIS; HALOGENATION; INHIBITORS; ANALOGS; QUANTIFICATION; IDENTIFICATION; METABOLITES AB Polybrominated diphenyl ethers (PBDEs) are persistent and bioaccumulative anthropogenic and natural chemicals that are broadly distributed in the marine environment. PBDEs are potentially toxic due to inhibition of various mammalian signaling pathways and enzymatic reactions. PBDE isoforms vary in toxicity in accordance with structural differences, primarily in the number and pattern of hydroxyl moieties afforded upon a conserved core structure. Over four decades of isolation and discovery-based efforts have established an impressive repertoire of natural PBDEs. Based on our recent reports describing the bacterial biosyntheses of PBDEs, we predicted the presence of additional classes of PBDEs to those previously identified from marine sources. Using mass spectrometry and NMR spectroscopy, we now establish the existence of new structural classes of PBDEs in marine sponges. Our findings expand the chemical space explored by naturally produced PBDEs, which may inform future environmental toxicology studies. Furthermore, we provide evidence for iodinated PBDEs and direct attention toward the contribution of promiscuous halogenating enzymes in further expanding the diversity of these polyhalogenated marine natural products. C1 [Agarwal, Vinayak; Rahman, Imran; Borgen, Miles; Aluwihare, Lihini I.; Moore, Bradley S.] Univ Calif San Diego, Scripps Ctr Oceans & Human Hlth, San Diego, CA 92037 USA. [Li, Jie; Moore, Bradley S.] Univ Calif San Diego, Ctr Marine Biotechnol & Biomed, San Diego, CA 92037 USA. [Aluwihare, Lihini I.] Univ Calif San Diego, Scripps Inst Oceanog, Geosci Res Div, San Diego, CA 92037 USA. [Moore, Bradley S.] Univ Calif San Diego, Skaggs Sch Pharm & Pharmaceut Sci, San Diego, CA 92037 USA. [Biggs, Jason S.] Univ Guam, Marine Lab, UoG Stn, Mangilao, GU 96923 USA. [Paul, Valerie J.] Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL 34949 USA. RP Moore, BS (reprint author), Univ Calif San Diego, Scripps Ctr Oceans & Human Hlth, San Diego, CA 92037 USA. EM bsmoore@ucsd.edu FU NIH [P01-ES021921, S10-RR031562, R01-CA172310]; NSF [OCE-1313747]; Helen Hay Whitney Foundation FX We thank our UCSD colleague B. M. Duggan for assistance with NMR data acquisition and analysis, and SMS intern Lindsay Spiers for assistance with collecting sponge samples. Funding was generously provided by the NIH (P01-ES021921) and NSF (OCE-1313747) through the Oceans and Human Health program, NIH instrumentation grant S10-RR031562, and the Helen Hay Whitney Foundation via a postdoctoral fellowship to V.A. V.J.P. acknowledges partial support from the NIH (R01-CA172310) for sample collection. NR 45 TC 7 Z9 7 U1 4 U2 49 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0013-936X EI 1520-5851 J9 ENVIRON SCI TECHNOL JI Environ. Sci. Technol. PD FEB 3 PY 2015 VL 49 IS 3 BP 1339 EP 1346 DI 10.1021/es505440j PG 8 WC Engineering, Environmental; Environmental Sciences SC Engineering; Environmental Sciences & Ecology GA CA6XH UT WOS:000349060300014 PM 25559102 ER PT J AU Martinez, O Crabtree, KN Gottlieb, CA Stanton, JF McCarthy, MC AF Martinez, Oscar, Jr. Crabtree, Kyle N. Gottlieb, Carl A. Stanton, John F. McCarthy, Michael C. TI An Accurate Molecular Structure of Phenyl, the Simplest Aryl Radical SO ANGEWANDTE CHEMIE-INTERNATIONAL EDITION LA English DT Article DE abinitio calculations; molecular structure; rotational spectroscopy ID ELECTRON SPIN RESONANCE; ACETYL BENZOYL PEROXIDE; ABSORPTION-SPECTRUM; LOW-TEMPERATURE; ARGON MATRIX; INFRARED-SPECTROSCOPY; EQUILIBRIUM STRUCTURE; CHEMICAL REACTION; GAS-PHASE; DEGREES K AB The phenyl radical (C6H5.) is the prototypical sigma-type aryl radical and one of the most common aromatic building blocks for larger ring molecules. Using a combination of rotational spectroscopy of singly substituted isotopic species and vibrational corrections calculated theoretically, an extremely accurate molecular structure has been determined. Relative to benzene, the phenyl radical has a substantially larger C-C-ipso-C bond angle [125.8(3)degrees vs. 120 degrees], and a shorter distance [2.713(3)angstrom vs. 2.783(2)angstrom] between the ipso and para carbon atoms. C1 [Martinez, Oscar, Jr.; Crabtree, Kyle N.; Gottlieb, Carl A.; McCarthy, Michael C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Stanton, John F.] Univ Texas Austin, Inst Theoret Chem, Dept Chem, Austin, TX 78712 USA. RP McCarthy, MC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. FU NSF [CHE-1058063]; Robert A. Welch Foundation of Houston, Texas [F-1283]; US Department of Energy, Office of Basic Energy Sciences [DE-FG02-07ER15884]; CfA Postdoctoral Fellowship from Smithsonian Astrophysical Observatory FX The experimental work in Cambridge was supported by the NSF, grant number CHE-1058063. The theoretical studies were supported by the Robert A. Welch Foundation (grant F-1283) of Houston, Texas, and the US Department of Energy, Office of Basic Energy Sciences (contract DE-FG02-07ER15884). K.N.C. was supported by a CfA Postdoctoral Fellowship from the Smithsonian Astrophysical Observatory. We thank E. S. Palmer for technical assistance, and G. B. Ellison, D. J. Nesbitt, and C. Puzzarini for helpful discussions. NR 51 TC 4 Z9 4 U1 3 U2 26 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA POSTFACH 101161, 69451 WEINHEIM, GERMANY SN 1433-7851 EI 1521-3773 J9 ANGEW CHEM INT EDIT JI Angew. Chem.-Int. Edit. PD FEB 2 PY 2015 VL 54 IS 6 BP 1808 EP 1811 DI 10.1002/anie.201409896 PG 4 WC Chemistry, Multidisciplinary SC Chemistry GA CA8ZH UT WOS:000349209200021 PM 25521111 ER PT J AU Rodgers, TW Giacalone, J Heske, EJ Janecka, JE Jansen, PA Phillips, CA Schooley, RL AF Rodgers, Torrey W. Giacalone, Jacalyn Heske, Edward J. Janecka, Jan E. Jansen, Patrick A. Phillips, Christopher A. Schooley, Robert L. TI Socio-spatial organization and kin structure in ocelots from integration of camera trapping and noninvasive genetics SO JOURNAL OF MAMMALOGY LA English DT Article DE Barro Colorado Island; genetic relatedness; Leopardus pardalis; ocelot; space-use overlap; spatial organization ID INBREEDING AVOIDANCE; RESOURCE DISPERSION; LEOPARDUS-PARDALIS; SPATIAL STRUCTURE; RADIATION HYBRID; HOME-RANGE; MAMMALS; CAT; RELATEDNESS; POPULATION AB Kin selection theory predicts that under certain conditions animals will tolerate related individuals in their home ranges. We examined the relationship between spatiotemporal overlap and genetic relatedness in ocelots (Leopardus pardalis) to determine if kin selection plays a role in structuring ocelot populations. We used 3 years of camera trapping to examine the spatial organization of an ocelot population on Barro Colorado Island in Panama. We also placed camera traps on ocelot latrines to match photographs of individual ocelots with microsatellite genotypes from feces. Strengths of spatiotemporal overlap between individual ocelots were calculated using a half-weight association index based on how often individuals were photographed at the same camera within 30 days of one another. We calculated relatedness between individuals based on 11 variable microsatellite loci. Male ocelots overlapped with <= 11 females, and females overlapped with <= 7 males. We detected no clear evidence of strict intersexual territoriality in either sex. Mean overlap among males was more than 5 times greater than overlap among females; however, spatiotemporal overlap was strong between some female pairs. Overall, overlapping individuals were more related to one another than was the sample population as a whole, consistent with the hypothesis that kin selection influences ocelot spatial organization. This finding was driven by relatedness among overlapping females, and by relatedness among overlapping individuals of opposite sex, but not by overlapping males. C1 [Rodgers, Torrey W.; Heske, Edward J.] Univ Illinois, Dept Anim Biol, Urbana, IL 61801 USA. [Rodgers, Torrey W.; Giacalone, Jacalyn; Jansen, Patrick A.] Smithsonian Trop Res Inst, Balboa 084303092, Ancon, Panama. [Giacalone, Jacalyn] Montclair State Univ, Montclair, NJ 07043 USA. [Schooley, Robert L.] Univ Illinois, Dept Nat Resources & Environm Sci, Urbana, IL 61801 USA. [Janecka, Jan E.] Duquesne Univ, Dept Biol Sci, Pittsburgh, PA 15282 USA. [Jansen, Patrick A.] Univ Wageningen & Res Ctr, Dept Environm Sci, NL-6700 AA Wageningen, Netherlands. [Heske, Edward J.; Phillips, Christopher A.] Univ Illinois, Prairie Res Inst, Illinois Nat Hist Survey, Champaign, IL 61820 USA. RP Rodgers, TW (reprint author), Univ Illinois, Dept Anim Biol, 505 S Goodwin Ave, Urbana, IL 61801 USA. EM torrey.w.rodgers@gmail.com RI Jansen, Patrick/G-2545-2015 OI Jansen, Patrick/0000-0002-4660-0314 FU Smithsonian Tropical Research Institute; American Society of Mammalogists; University of Illinois Graduate College FX We thank R. Kays and R. Moreno for sharing their knowledge of the Barro Colorado Island ocelot population. We also thank G. Smallwood for field assistance, N. Pawlikowski and J. Lyko for help with photo identification, and Y. Liefting for administration of the Smithsonian Tropical Research Institute (STRI) camera trap database. C. Kontos, Jr. helped to establish the ocelot photo identification procedure, and G. Willis provided financial support and years of mammal census fieldwork. K. Paige provided helpful comments on an earlier version of this manuscript. This work was funded by the Smithsonian Tropical Research Institute, American Society of Mammalogists, and University of Illinois Graduate College. NR 57 TC 3 Z9 3 U1 6 U2 39 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 0022-2372 EI 1545-1542 J9 J MAMMAL JI J. Mammal. PD FEB PY 2015 VL 96 IS 1 BP 120 EP 128 DI 10.1093/jmammal/gyu012 PG 9 WC Zoology SC Zoology GA CG5LV UT WOS:000353334300015 ER PT J AU Woodman, N Stabile, FA AF Woodman, Neal Stabile, Frank A. TI Variation in the myosoricine hand skeleton and its implications for locomotory behavior (Eulipotyphla: Soricidae) SO JOURNAL OF MAMMALOGY LA English DT Article DE anatomy; Insectivora; manus; Myosoricinae; postcranial; ray; semifossorial; Soricomorpha ID NEW-SPECIES MAMMALIA; SMALL-EARED SHREWS; GENUS CRYPTOTIS; MYOSOREX MAMMALIA; DIVERSITY; PROPORTIONS; MORPHOLOGY; GUATEMALA; HIGHLANDS; ADAPTATIONS AB Substrate use and locomotory behavior of mammals are typically reflected in external characteristics of the forefeet, such as the relative proportions of the digits and claws. Although skeletal anatomy of the forefeet can be more informative than external characters, skeletons remain rare in systematic collections. This is particularly true for the Myosoricinae (Eulipotyphla: Soricidae), a small clade of African shrews that includes both ambulatory forest shrews (Myosorex) and semifossorial mole shrews (Surdisorex). Most species in this subfamily have restricted distributions, and their behavior and ecology are mostly unstudied. To better understand the potential range of locomotory behavior among myosoricines, we used digital x-rays to image and facilitate measuring the forefoot skeletons of 9 species. As a gauge of potential variation, we compared them with the ambulatory talpid Uropsilus (Talpidae) and the semifossorial talpid Neurotrichus. The hand morphologies of myosoricines show a graded range of potential substrate use between ambulatory and semifossorial. Some of these shrews exhibit adaptations for increased burrowing efficiency that are similar to those seen in talpids and other mammals, such as longer, broader distal phalanges and claws and shorter, wider metacarpals and proximal and middle phalanges. They also, however, have characteristics that are distinct from talpids, such as maintenance of forefoot asymmetry and an increased emphasis of ray III. C1 [Woodman, Neal] Smithsonian Inst, USGS Patuxent Wildlife Res Ctr, Natl Museum Nat Hist, Washington, DC 20013 USA. [Stabile, Frank A.] Coll New Jersey, Dept Biol, Ewing, NJ 08628 USA. RP Woodman, N (reprint author), Smithsonian Inst, USGS Patuxent Wildlife Res Ctr, Natl Museum Nat Hist, MRC 111,POB 37012, Washington, DC 20013 USA. EM woodmann@si.edu OI Woodman, Neal/0000-0003-2689-7373 FU National Science Foundation through the Natural History Research Experiences program of the National Museum of Natural History, Washington, D.C FX We thank the following curators and collections managers for access to specimens under their care: N. B. Simmons, R. S. Voss, and E. Westwig (American Museum of Natural History, New York); and L. R. Heaney, B. D. Patterson, and W. T. Stanley (Field Museum of Natural History, Chicago). We are particularly grateful to W. T. Stanley and J. Kerbis Peterhans for graciously permitting us to examine recently collected series of specimens of poorly documented species that resulted from their field work. FAS was supported by funds from the National Science Foundation through the Natural History Research Experiences program of the National Museum of Natural History, Washington, D.C. A. L. Gardner, J. Kerbis Peterhans, and an anonymous reviewer provided valuable comments on a previous version of this manuscript. Any use of trade, product, or firm names is for descriptive purposes only and does not imply endorsement by the United States government. NR 39 TC 2 Z9 2 U1 0 U2 5 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 0022-2372 EI 1545-1542 J9 J MAMMAL JI J. Mammal. PD FEB PY 2015 VL 96 IS 1 BP 159 EP 171 DI 10.1093/jmammal/gyu017 PG 13 WC Zoology SC Zoology GA CG5LV UT WOS:000353334300020 ER PT J AU Gingerich, O AF Gingerich, Owen TI Studies on the 'Sphere' of Johannes de Sacrobosco SO JOURNAL FOR THE HISTORY OF ASTRONOMY LA English DT Book Review C1 [Gingerich, Owen] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Gingerich, O (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. EM ogingerich@cfa.harvard.edu NR 1 TC 0 Z9 0 U1 1 U2 1 PU SAGE PUBLICATIONS LTD PI LONDON PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND SN 0021-8286 EI 1753-8556 J9 J HIST ASTRON JI J. Hist. Astron. PD FEB PY 2015 VL 46 BP 101 EP 102 DI 10.1177/0021828614552236 PN 1 PG 2 WC History & Philosophy Of Science SC History & Philosophy of Science GA CF6EH UT WOS:000352649000008 ER PT J AU Launius, RD AF Launius, Roger D. TI The Wright Company: From Invention to Industry SO AMERICAN HISTORICAL REVIEW LA English DT Book Review C1 [Launius, Roger D.] Natl Air & Space Museum, Smithsonian Inst, Washington, DC 20560 USA. RP Launius, RD (reprint author), Natl Air & Space Museum, Smithsonian Inst, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0002-8762 EI 1937-5239 J9 AM HIST REV JI Am. Hist. Rev. PD FEB PY 2015 VL 120 IS 1 BP 264 EP 265 PG 3 WC History SC History GA CE8GM UT WOS:000352079900095 ER PT J AU Bilby, K AF Bilby, Kenneth TI Suriname in the Long Twentieth Century: Domination, Contestation, Globalization SO AMERICAN HISTORICAL REVIEW LA English DT Book Review C1 [Bilby, Kenneth] Smithsonian Inst, Washington, DC 20560 USA. RP Bilby, K (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 1 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0002-8762 EI 1937-5239 J9 AM HIST REV JI Am. Hist. Rev. PD FEB PY 2015 VL 120 IS 1 BP 304 EP 305 PG 3 WC History SC History GA CE8GM UT WOS:000352079900137 ER PT J AU van Donkelaar, A Martin, RV Brauer, M Boys, BL AF van Donkelaar, Aaron Martin, Randall V. Brauer, Michael Boys, Brian L. TI Use of Satellite Observations for Long-Term Exposure Assessment of Global Concentrations of Fine Particulate Matter SO ENVIRONMENTAL HEALTH PERSPECTIVES LA English DT Article ID OUTDOOR AIR-POLLUTION; UNITED-STATES; AEROSOL MEASUREMENTS; TIME-SERIES; MORTALITY; PM2.5; ASSOCIATION; PRODUCTS; DISEASE; REGIONS AB BACKGROUND: More than a decade of satellite observations offers global information about the trend and magnitude of human exposure to fine particulate matter (PM2.5). OBJECTIVE: In this study, we developed improved global exposure estimates of ambient PM2.5 mass and trend using PM2.5 concentrations inferred from multiple satellite instruments. METHODS: We combined three satellite-derived PM2.5 sources to produce global PM2.5 estimates at about 10 km x 10 km from 1998 through 2012. For each source, we related total column retrievals of aerosol optical depth to near-ground PM2.5 using the GEOS-Chem chemical transport model to represent local aerosol optical properties and vertical profiles. We collected 210 global ground-based PM2.5 observations from the literature to evaluate our satellite-based estimates with values measured in areas other than North America and Europe. RESULTS: We estimated that global population-weighted ambient PM2.5 concentrations increased 0.55 mu g/m(3)/year (95% CI: 0.43, 0.67) (2.1%/year; 95% CI: 1.6, 2.6) from 1998 through 2012. Increasing PM2.5 in some developing regions drove this global change, despite decreasing PM2.5 in some developed regions. The estimated proportion of the population of East Asia living above the World Health Organization (WHO) Interim Target-1 of 35 mu g/m(3) increased from 51% in 1998-2000 to 70% in 2010-2012. In contrast, the North American proportion above the WHO Air Quality Guideline of 10 mu g/m(3) fell from 62% in 1998-2000 to 19% in 2010-2012. We found significant agreement between satellite-derived estimates and ground-based measurements outside North America and Europe (r = 0.81; n = 210; slope = 0.68). The low bias in satellite-derived estimates suggests that true global concentrations could be even greater. CONCLUSIONS: Satellite observations provide insight into global long-term changes in ambient PM2.5 concentrations. Satellite-derived estimates and ground-based PM2.5 observations from this study are available for public use. C1 [van Donkelaar, Aaron; Martin, Randall V.; Boys, Brian L.] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 4R2, Canada. [Martin, Randall V.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Brauer, Michael] Univ British Columbia, Sch Environm Hlth, Vancouver, BC V5Z 1M9, Canada. RP van Donkelaar, A (reprint author), Dalhousie Univ, Dept Phys & Atmospher Sci, 6300 Coburg Rd, Halifax, NS B3H 4R2, Canada. EM Aaron.van.Donkelaar@dal.ca RI Chem, GEOS/C-5595-2014; Martin, Randall/C-1205-2014; OI Martin, Randall/0000-0003-2632-8402; Brauer, Michael/0000-0002-9103-9343 FU Health Canada; Natural Sciences and Engineering Research Council of Canada; U.S. National Institutes of Health FX This work was supported by Health Canada, the Natural Sciences and Engineering Research Council of Canada, and the U.S. National Institutes of Health. Some of the computing facilities used here were provided by the Atlantic Computational Excellence Network. NR 40 TC 72 Z9 72 U1 19 U2 96 PU US DEPT HEALTH HUMAN SCIENCES PUBLIC HEALTH SCIENCE PI RES TRIANGLE PK PA NATL INST HEALTH, NATL INST ENVIRONMENTAL HEALTH SCIENCES, PO BOX 12233, RES TRIANGLE PK, NC 27709-2233 USA SN 0091-6765 EI 1552-9924 J9 ENVIRON HEALTH PERSP JI Environ. Health Perspect. PD FEB PY 2015 VL 123 IS 2 BP 135 EP 143 DI 10.1289/ehp.1408646 PG 9 WC Environmental Sciences; Public, Environmental & Occupational Health; Toxicology SC Environmental Sciences & Ecology; Public, Environmental & Occupational Health; Toxicology GA CE8GI UT WOS:000352079400013 PM 25343779 ER PT J AU Detto, M Asner, GP Muller-Landau, HC Sonnentag, O AF Detto, Matteo Asner, Gregory P. Muller-Landau, Helene C. Sonnentag, Oliver TI Spatial variability in tropical forest leaf area density from multireturn lidar and modeling SO JOURNAL OF GEOPHYSICAL RESEARCH-BIOGEOSCIENCES LA English DT Article DE waveform lidar; tropical forest; leaf area density; leaf area index; complex forest; multireturn lidar ID INCLINATION ANGLE DISTRIBUTION; GROUND-BASED LIDAR; CANOPY STRUCTURE; CARBON STOCKS; WAVE-FORMS; INDEX; RADIATION; AMAZON; TEMPERATE; LANDSCAPE AB Leaf area index and leaf area density profiles are key variables for upscaling from leaves to ecosystems yet are difficult to measure well in dense and tall forest canopies. We present a new model to estimate leaf area density profiles from discrete multireturn data derived by airborne waveform light detection and ranging (lidar), a model based on stochastic radiative transfer theory. We tested the method on simulated ray tracing data for highly clumped forest canopies, both vertically homogenous and vertically inhomogeneous. Our method was able to reproduce simulated vertical foliage profiles with small errors and predictable biases in dense canopies (leaf area index=6) including layers below densely foliated upper canopies. As a case study, we then applied the method to real multireturn airborne lidar data for a 50ha plot of moist tropical forest on Barro Colorado Island, Panama. The method is suitable for estimating foliage profiles in a complex tropical forest, which opens new avenues for analyses of spatial and temporal variations in foliage distributions. C1 [Detto, Matteo; Muller-Landau, Helene C.] Smithsonian Trop Res Inst, Panama City, Panama. [Asner, Gregory P.] Carnegie Inst Sci, Palo Alto, CA USA. [Sonnentag, Oliver] Univ Montreal, Dept Geog, Montreal, PQ H3C 3J7, Canada. RP Detto, M (reprint author), Smithsonian Trop Res Inst, Panama City, Panama. EM dettom@si.edu FU Smithsonian Institution Global Earth Observatory (SIGEO); Carnegie Airborne Observatory (CAO) FX This work was supported by Smithsonian Institution Global Earth Observatory (SIGEO) and Carnegie Airborne Observatory (CAO). CAO is made possible by the Gordon and Betty Moore Foundation, the John D. and Catherine T. MacArthur Foundation, W.M. Keck Foundation, the Margaret A. Cargill Foundation, Grantham Foundation for the Protection of the Environment, Mary Anne Nyburg Baker and G. Leonard Baker Jr., and William R. Hearst III. Anyone wishing collaborate on use of the lidar data analyzed here should contact Gregory Asner (gpa@stanford.edu) with the request. NR 49 TC 5 Z9 5 U1 3 U2 30 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-8953 EI 2169-8961 J9 J GEOPHYS RES-BIOGEO JI J. Geophys. Res.-Biogeosci. PD FEB PY 2015 VL 120 IS 2 BP 294 EP 309 DI 10.1002/2014JG002774 PG 16 WC Environmental Sciences; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Geology GA CD9FI UT WOS:000351402800008 ER PT J AU Bleem, LE Stalder, B de Haan, T Aird, KA Allen, SW Applegate, DE Ashby, MLN Bautz, M Bayliss, M Benson, BA Bocquet, S Brodwin, M Carlstrom, JE Chang, CL Chiu, I Cho, HM Clocchiatti, A Crawford, TM Crites, AT Desai, S Dietrich, JP Dobbs, MA Foley, RJ Forman, WR George, EM Gladders, MD Gonzalez, AH Halverson, NW Hennig, C Hoekstra, H Holder, GP Holzapfel, WL Hrubes, JD Jones, C Keisler, R Knox, L Lee, AT Leitch, EM Liu, J Lueker, M Luong-Van, D Mantz, A Marrone, DP McDonald, M McMahon, JJ Meyer, SS Mocanu, L Mohr, JJ Murray, SS Padin, S Pryke, C Reichardt, CL Rest, A Ruel, J Ruhl, JE Saliwanchik, BR Saro, A Sayre, JT Schaffer, KK Schrabback, T Shirokoff, E Song, J Spieler, HG Stanford, SA Staniszewski, Z Stark, AA Story, KT Stubbs, CW Vanderlinde, K Vieira, JD Vikhlinin, A Williamson, R Zahn, O Zenteno, A AF Bleem, L. E. Stalder, B. de Haan, T. Aird, K. A. Allen, S. W. Applegate, D. E. Ashby, M. L. N. Bautz, M. Bayliss, M. Benson, B. A. Bocquet, S. Brodwin, M. Carlstrom, J. E. Chang, C. L. Chiu, I. Cho, H. M. Clocchiatti, A. Crawford, T. M. Crites, A. T. Desai, S. Dietrich, J. P. Dobbs, M. A. Foley, R. J. Forman, W. R. George, E. M. Gladders, M. D. Gonzalez, A. H. Halverson, N. W. Hennig, C. Hoekstra, H. Holder, G. P. Holzapfel, W. L. Hrubes, J. D. Jones, C. Keisler, R. Knox, L. Lee, A. T. Leitch, E. M. Liu, J. Lueker, M. Luong-Van, D. Mantz, A. Marrone, D. P. McDonald, M. McMahon, J. J. Meyer, S. S. Mocanu, L. Mohr, J. J. Murray, S. S. Padin, S. Pryke, C. Reichardt, C. L. Rest, A. Ruel, J. Ruhl, J. E. Saliwanchik, B. R. Saro, A. Sayre, J. T. Schaffer, K. K. Schrabback, T. Shirokoff, E. Song, J. Spieler, H. G. Stanford, S. A. Staniszewski, Z. Stark, A. A. Story, K. T. Stubbs, C. W. Vanderlinde, K. Vieira, J. D. Vikhlinin, A. Williamson, R. Zahn, O. Zenteno, A. TI GALAXY CLUSTERS DISCOVERED VIA THE SUNYAEV-ZEL'DOVICH EFFECT IN THE 2500-SQUARE-DEGREE SPT-SZ SURVEY SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE cosmology: observations; galaxies: clusters: individual; large-scale structure of universe ID SOUTH-POLE TELESCOPE; ALL-SKY SURVEY; SIMILAR-TO 1; BLANCO COSMOLOGY SURVEY; MICROWAVE BACKGROUND ANISOTROPIES; SHEAR-SELECTED CLUSTERS; STAR-FORMING GALAXIES; FLUX-LIMITED SAMPLE; X-RAY OBSERVATIONS; 720 SQUARE DEGREES AB We present a catalog of galaxy clusters selected via their Sunyaev-Zel'dovich (SZ) effect signature from 2500 deg(2) of South Pole Telescope (SPT) data. This work represents the complete sample of clusters detected at high significance in the 2500 deg(2) SPT-SZ survey, which was completed in 2011. A total of 677 (409) cluster candidates are identified above a signal-to-noise threshold of xi = 4.5 (5.0). Ground-and space-based optical and near-infrared (NIR) imaging confirms overdensities of similarly colored galaxies in the direction of 516 (or 76%) of the xi > 4.5 candidates and 387 (or 95%) of the xi > 5 candidates; the measured purity is consistent with expectations from simulations. Of these confirmed clusters, 415 were first identified in SPT data, including 251 new discoveries reported in this work. We estimate photometric redshifts for all candidates with identified optical and/or NIR counterparts; we additionally report redshifts derived from spectroscopic observations for 141 of these systems. The mass threshold of the catalog is roughly independent of redshift above z similar to 0.25 leading to a sample of massive clusters that extends to high redshift. The median mass of the sample is M-500c(rho(crit)) similar to 3.5 x 10(14) M-circle dot h(70)(-1) 70, the median redshift is z(med) = 0.55, and the highest-redshift systems are at z > 1.4. The combination of large redshift extent, clean selection, and high typical mass makes this cluster sample of particular interest for cosmological analyses and studies of cluster formation and evolution. C1 [Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.] Argonne Natl Lab, Div High Energy Phys, Argonne, IL 60439 USA. [Bleem, L. E.; Benson, B. A.; Carlstrom, J. E.; Chang, C. L.; Crawford, T. M.; Crites, A. T.; Gladders, M. D.; Keisler, R.; Leitch, E. M.; Mantz, A.; Meyer, S. S.; Mocanu, L.; Padin, S.; Schaffer, K. K.; Story, K. T.; Williamson, R.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Bleem, L. E.; Carlstrom, J. E.; Keisler, R.; Meyer, S. S.; Story, K. T.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA. [Stalder, B.; Ashby, M. L. N.; Bayliss, M.; Foley, R. J.; Forman, W. R.; Jones, C.; Murray, S. S.; Stark, A. A.; Stubbs, C. W.; Vikhlinin, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [de Haan, T.; Dobbs, M. A.; Holder, G. P.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Aird, K. A.; Hrubes, J. D.; Luong-Van, D.] Univ Chicago, Chicago, IL 60637 USA. [Allen, S. W.; Keisler, R.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Allen, S. W.; Keisler, R.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Allen, S. W.] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA. [Applegate, D. E.; Schrabback, T.] Argelander Inst Astron, D-53121 Bonn, Germany. [Bautz, M.; McDonald, M.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Bayliss, M.; Ruel, J.; Stubbs, C. W.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Benson, B. A.] Fermilab Natl Accelerator Lab, Batavia, IL 60510 USA. [Benson, B. A.; Carlstrom, J. E.; Crawford, T. M.; Crites, A. T.; Gladders, M. D.; Leitch, E. M.; Meyer, S. S.; Mocanu, L.; Padin, S.; Williamson, R.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Bocquet, S.; Chiu, I.; Desai, S.; Dietrich, J. P.; Hennig, C.; Liu, J.; Mohr, J. J.; Saro, A.; Zenteno, A.] Univ Munich, Dept Phys, D-81679 Munich, Germany. [Bocquet, S.; Chiu, I.; Desai, S.; Dietrich, J. P.; Hennig, C.; Liu, J.; Mohr, J. J.] Excellence Cluster Universe, D-85748 Garching, Germany. [Brodwin, M.] Univ Missouri, Dept Phys & Astron, Kansas City, MO 64110 USA. [Carlstrom, J. E.; Chang, C. L.; Meyer, S. S.; Schaffer, K. K.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Cho, H. M.] NIST, Quantum Devices Grp, Boulder, CO 80305 USA. [Clocchiatti, A.] Pontificia Univ Catolica Chile, Dept Astron & Astrosif, Santiago, Chile. [Crites, A. T.; Lueker, M.; Padin, S.; Shirokoff, E.; Staniszewski, Z.; Williamson, R.] CALTECH, Pasadena, CA 91125 USA. [Dobbs, M. A.] Canadian Inst Adv Res, CIFAR Program Cosmol & Grav, Toronto, ON M5G 1Z8, Canada. [Foley, R. J.; Vieira, J. D.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA. [Foley, R. J.; Vieira, J. D.] Univ Illinois, Dept Phys, Urbana, IL 61801 USA. [George, E. M.; Holzapfel, W. L.; Lee, A. T.; Lueker, M.; Reichardt, C. L.; Shirokoff, E.; Zahn, O.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [George, E. M.; Mohr, J. J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Gonzalez, A. H.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Halverson, N. W.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. [Halverson, N. W.] Univ Colorado, Dept Phys, Boulder, CO 80309 USA. [Hoekstra, H.] Leiden Univ, Leiden Observ, NL-2333 CA Leiden, Netherlands. [Knox, L.; Stanford, S. A.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Lee, A. T.; Spieler, H. G.] Lawrence Berkeley Natl Lab, Div Phys, Berkeley, CA 94720 USA. [Marrone, D. P.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [McMahon, J. J.; Song, J.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Pryke, C.] Univ Minnesota, Dept Phys, Minneapolis, MN 55455 USA. [Reichardt, C. L.] Univ Melbourne, Sch Phys, Parkville, Vic 3010, Australia. [Rest, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Ruhl, J. E.; Saliwanchik, B. R.; Sayre, J. T.; Staniszewski, Z.] Case Western Reserve Univ, Dept Phys, Ctr Educ & Res Cosmol & Astrophys, Cleveland, OH 44106 USA. [Schaffer, K. K.] Sch Art Inst Chicago, Liberal Arts Dept, Chicago, IL 60603 USA. [Song, J.] Korea Astron & Space Sci Inst, Taejon 305348, South Korea. [Stanford, S. A.] Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94551 USA. [Vanderlinde, K.] Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Vanderlinde, K.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Zahn, O.] Univ Calif Berkeley, Berkeley Ctr Cosmol Phys, Dept Phys, Berkeley, CA 94720 USA. [Zahn, O.] Lawrence Berkeley Natl Labs, Lawrence, CA 94720 USA. [Zenteno, A.] Natl Opt Astron Observ, Cerro Tololo Inter Amer Observ, La Serena, Chile. RP Bleem, LE (reprint author), Argonne Natl Lab, Div High Energy Phys, 9700 South Cass Ave, Argonne, IL 60439 USA. RI Williamson, Ross/H-1734-2015; Holzapfel, William/I-4836-2015; Stubbs, Christopher/C-2829-2012; OI Williamson, Ross/0000-0002-6945-2975; Stubbs, Christopher/0000-0003-0347-1724; Marrone, Daniel/0000-0002-2367-1080; CRAWFORD, THOMAS/0000-0001-9000-5013; Dietrich, Jorg/0000-0002-8134-9591; Aird, Kenneth/0000-0003-1441-9518; Forman, William/0000-0002-9478-1682; Stark, Antony/0000-0002-2718-9996; Reichardt, Christian/0000-0003-2226-9169 FU National Science Foundation [PLR-1248097]; NSF Physics Frontier Center [PHY-1125897]; Kavli Foundation; Gordon and Betty Moore Foundation [GBMF 947]; NSF [AST-1009012, AST-1009649, MRI-0723073]; National Sciences and Engineering Research Council of Canada; Canada Research Chairs program; Canadian Institute for Advanced Research; U.S. Department of Energy [DE-AC02-06CH11357]; United States Department of Energy [De-AC02-07CH11359]; DFG Cluster of Excellence "Origin and Structure of the Universe"; Transregio program "The Dark Universe" [TR33]; NASA through a Hubble Fellowship - Space Telescope Science Institute [HST-HF51308.01-A]; German Federal Ministry of Economics and Technology (BMWi) through DLR [50 OR 1210]; Cerro Tololo Interamerican Observatories [2005B- 0043, 2009B-0400, 2010A-0441, 2010B-0598]; VLT programs [086.A-0741, 087.A-0843, 088.A-0796(A), 088.A- 0889(A,B,C), 286.A-5021]; Gemini programs [GS-2009B-Q-16, GS-2011A-C-3, GS-2011B-C-6, GS-2012A-Q-4, GS-2012A-Q-37, GS-2012B-Q-29, GS-2012B-Q-59, GS-2013A-Q-5, GS-2013A-Q-45, GS-2013B-Q-25, GS-2013B-Q-72]; NASA [NAS 5-26555]; NASA through JPL/Caltech; Space Telescope Science Institute under U.S. Government [NAG W-2166]; [12246]; [12477]; [13412] FX The South Pole Telescope is supported by the National Science Foundation through grant PLR-1248097. Partial support is also provided by the NSF Physics Frontier Center grant PHY-1125897 to the Kavli Institute of Cosmological Physics at the University of Chicago, the Kavli Foundation, and the Gordon and Betty Moore Foundation grant GBMF 947. Galaxy cluster research at Harvard is supported by NSF grant AST-1009012 and at SAO in part by NSF grants AST-1009649 and MRI-0723073. The McGill group acknowledges funding from the National Sciences and Engineering Research Council of Canada, Canada Research Chairs program, and the Canadian Institute for Advanced Research. Argonne National Laboratory's work was supported under U.S. Department of Energy contract DE-AC02-06CH11357. This work was partially completed at Fermilab, operated by Fermi Research Alliance, LLC under contract no. De-AC02-07CH11359 with the United States Department of Energy. The Munich group acknowledges support from the DFG Cluster of Excellence "Origin and Structure of the Universe" and the Transregio program TR33 "The Dark Universe." M.M. acknowledges support by NASA through a Hubble Fellowship grant HST-HF51308.01-A awarded by the Space Telescope Science Institute. T.S. and D.A. acknowledge support from the German Federal Ministry of Economics and Technology (BMWi) provided through DLR under project 50 OR 1210.; Optical imaging data from the Blanco 4 m at Cerro Tololo Interamerican Observatories (programs 2005B- 0043, 2009B-0400, 2010A-0441, 2010B-0598) and spectroscopic observations from VLT programs 086.A-0741, 087.A-0843, 088.A-0796(A), 088.A- 0889(A,B,C), and 286.A-5021 and Gemini programs GS-2009B-Q-16, GS-2011A-C-3, GS-2011B-C-6, GS-2012A-Q-4, GS-2012A-Q-37, GS-2012B-Q-29, GS-2012B-Q-59, GS-2013A-Q-5, GS-2013A-Q-45, GS-2013B-Q-25 and GS-2013B-Q-72 were included in this work. Additional data were obtained with the 6.5 m Magellan Telescopes and the Swope Telescope, which are located at the Las Campanas Observatory in Chile and the MPG/ESO 2.2 m and ESO NTT located at La Silla Facility in Chile. This work is based in part on observations made with the Spitzer Space Telescope (PIDs 60099, 70053, 80012 and 10101), which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. This work is also partly based on observations made with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555; these observations are associated with programs 12246, 12477, and 13412. The Digitized Sky Surveys were produced at the Space Telescope Science Institute under U.S. Government grant NAG W-2166. The images of these surveys are based on photographic data obtained using the Oschin Schmidt Telescope on Palomar Mountain and the UK Schmidt Telescope. The plates were processed into the present compressed digital form with the permission of these institutions. NR 158 TC 87 Z9 87 U1 2 U2 14 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 FEB PY 2015 VL 216 IS 2 AR 27 DI 10.1088/0067-0049/216/2/27 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CD2ID UT WOS:000350899000006 ER PT J AU Cooksy, AL Gottlieb, CA Killian, TC Thaddeus, P Patel, NA Young, KH McCarthy, MC AF Cooksy, Andrew L. Gottlieb, C. A. Killian, T. C. Thaddeus, P. Patel, Nimesh A. Young, Ken H. McCarthy, M. C. TI VIBRATIONALLY EXCITED C4H SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE circumstellar matter; line: identification; molecular processes; stars: AGB and post-AGB; stars: individual (IRC+10216) ID DUST FORMATION; IRC+10216; ENVELOPE; STATES; GHZ; SPECTROSCOPY; MOLECULES; CHEMISTRY; SPECTRA; WINDS AB Rotational spectra in four new excited vibrational levels of the linear carbon chain radical C4H were observed in the millimeter band between 69 and 364 GHz in a low pressure glow discharge, and two of these were observed in a supersonic molecular beam between 19 and 38 GHz. All have rotational constants within 0.4% of the X-2 Sigma(+) ground vibrational state of C4H and were assigned to new bending vibrational levels, two each with (2)Sigma and (2)Pi vibrational symmetry. The new levels are tentatively assigned to the 1 nu(6) and 1 nu(5) bending vibrational modes (both with (2)Pi symmetry), and the1 nu(6) + 1 nu(7) and 1 nu(5) + 1 nu(6) combination levels ((2)Sigma symmetry) on the basis of the derived spectroscopic constants, relative intensities in our discharge source, and published laser spectroscopic and quantum calculations. Prior spectroscopic constants in the 1 nu(7) and 2 nu(7) levels were refined. Also presented are interferometric maps of the ground state and the 1 nu(7) level obtained with the Submillimeter Array (SMA) near 257 GHz which show that C4H is present near the central star in IRC+10216. We found no evidence with the SMA for the new vibrationally excited levels of C4H at a peak flux density averaged over a 3 '' synthesized beam of >= 0.15 Jy/beam in the 294-296 and 304-306 GHz range, but it is anticipated that rotational lines in the new levels might be observed in IRC+10216 when ALMA attains its full design capability. C1 [Cooksy, Andrew L.] San Diego State Univ, Dept Chem & Biochem, San Diego, CA 92182 USA. [Gottlieb, C. A.; Thaddeus, P.; Patel, Nimesh A.; Young, Ken H.; McCarthy, M. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Killian, T. C.] Rice Univ, Dept Phys & Astron, Houston, TX 77005 USA. [Killian, T. C.] Rice Univ, Rice Quantum Inst, Houston, TX 77005 USA. [Thaddeus, P.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA. RP Cooksy, AL (reprint author), San Diego State Univ, Dept Chem & Biochem, 5500 Campanile Dr, San Diego, CA 92182 USA. FU National Aeronautics and Space Administration [NNX13AE59G]; Army Research Office [57989-CH]; Robert A. Welch Foundation [C-1844] FX This work is supported by the National Aeronautics and Space Administration grant NNX13AE59G. Additional support is provided by the Army Research Office through grant 57989-CH to A. L. C. at San Diego State University, and the Robert A. Welch Foundation through grant C-1844 to T. C. K. at Rice University. NR 32 TC 1 Z9 1 U1 3 U2 7 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 FEB PY 2015 VL 216 IS 2 AR 30 DI 10.1088/0067-0049/216/2/30 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CD2ID UT WOS:000350899000009 ER PT J AU Protopapas, P Huijse, P Estevez, PA Zegers, P Principe, JC Marquette, JB AF Protopapas, Pavlos Huijse, Pablo Estevez, Pablo A. Zegers, Pablo Principe, Jose C. Marquette, Jean-Baptiste TI A NOVEL, FULLY AUTOMATED PIPELINE FOR PERIOD ESTIMATION IN THE EROS 2 DATA SET SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE methods: data analysis; stars: variables: general ID GRAVITATIONAL LENSING EXPERIMENT.; OGLE-III CATALOG; LARGE-MAGELLANIC-CLOUD; CLASSICAL CEPHEIDS; LIGHT CURVES; TIME-SERIES; STARS; VARIABILITY; VARIABLES; PROJECT AB We present a new method to discriminate periodic from nonperiodic irregularly sampled light curves. We introduce a periodic kernel and maximize a similarity measure derived from information theory to estimate the periods and a discriminator factor. We tested the method on a data set containing 100,000 synthetic periodic and nonperiodic light curves with various periods, amplitudes, and shapes generated using a multivariate generative model. We correctly identified periodic and nonperiodic light curves with a completeness of similar to 90% and a precision of similar to 95%, for light curves with a signal-to-noise ratio (S/N) larger than 0.5. We characterize the efficiency and reliability of the model using these synthetic light curves and apply the method on the EROS-2 data set. A crucial consideration is the speed at which the method can be executed. Using a hierarchical search and some simplification on the parameter search, we were able to analyze 32.8 million light curves in similar to 18 hr on a cluster of GPGPUs. Using the sensitivity analysis on the synthetic data set, we infer that 0.42% of the sources in the LMC and 0.61% of the sources in the SMC show periodic behavior. The training set, catalogs, and source code are all available at http://timemachine.iic.harvard.edu. C1 [Protopapas, Pavlos] Harvard Univ, Inst Appl Computat Sci, Cambridge, MA 02138 USA. [Protopapas, Pavlos] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Huijse, Pablo; Estevez, Pablo A.] Millennium Inst Astrophys, Santiago, Chile. [Huijse, Pablo; Estevez, Pablo A.] Univ Chile, Dept Elect Engn, Santiago, Chile. [Huijse, Pablo; Estevez, Pablo A.] Univ Chile, Adv Min Technol Ctr, Santiago, Chile. [Zegers, Pablo] Univ Los Andes, Fac Ingn & Ciencias Aplicadas, Santiago, Chile. [Principe, Jose C.] Univ Florida, Computat Neuroengn Lab, Gainesville, FL 32611 USA. [Marquette, Jean-Baptiste] UPMC CNRS, Inst Astrophys Paris, UMR7095, F-75014 Paris, France. RP Protopapas, P (reprint author), Harvard Univ, Inst Appl Computat Sci, Cambridge, MA 02138 USA. EM pavlos@seas.harvard.edu RI Huijse, Pablo/J-4700-2015; Estevez, Pablo/A-9377-2008 OI Huijse, Pablo/0000-0003-3541-1697; Estevez, Pablo/0000-0001-9164-4722 FU CONICYT-CHILE under grant FONDECYT [1110701, 1140816]; Doctorate Scholarship program; Ministry of Economy, Development, and Tourism's Millennium Science Initiative [IC12009]; National Science Foundation [OCI-1053575]; CEA; CNRS through the IN2P3 institute; CNRS through INSU institute; "Programme National de Physique Stellaire" (PNPS) of CNRS/INSU, France FX This work was funded by CONICYT-CHILE under grant FONDECYT 1110701 and 1140816 and its Doctorate Scholarship program. P.E. acknowledges support from the Ministry of Economy, Development, and Tourism's Millennium Science Initiative through grant IC12009, awarded to the Millennium Institute of Astrophysics, MAS.; This work used the Extreme Science and Engineering Discovery Environment (XSEDE), which is supported by National Science Foundation grant number OCI-1053575.; The EROS-2 project was funded by the CEA and the CNRS through the IN2P3 and INSU institutes. J.-B.M. acknowledges financial support from "Programme National de Physique Stellaire" (PNPS) of CNRS/INSU, France. NR 41 TC 1 Z9 1 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 EI 1538-4365 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD FEB PY 2015 VL 216 IS 2 AR 25 DI 10.1088/0067-0049/216/2/25 PG 30 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CD2ID UT WOS:000350899000004 ER PT J AU Routti, H Krafft, BA Herzke, D Eisert, R Oftedal, O AF Routti, Heli Krafft, Bjorn A. Herzke, Dorte Eisert, Regina Oftedal, Olav TI Perfluoroalkyl substances detected in the world's southernmost marine mammal, the Weddell seal (Leptonychotes weddellii) SO ENVIRONMENTAL POLLUTION LA English DT Article DE Weddell seal; Perfluoroalkyl substances; Long-range transport; Local pollution; McMurdo ID PERFLUORINATED COMPOUNDS; MCMURDO-SOUND; PERFLUOROOCTANE SULFONATE; FOOD-WEB; POLYFLUOROALKYL SUBSTANCES; ROSS SEA; POLYFLUORINATED COMPOUNDS; GLOBAL DISTRIBUTION; SPATIAL VARIATION; 1ST REPRODUCTION AB This study investigates concentrations of 18 perfluoroalkyl substances (PFAS) in blood plasma of adult lactating Weddell seals (Leptonychotes weddellii) (n = 10) from McMurdo Sound, Antarctica. Perfluoroundecanoic acid (PFUnDA) was detected in all samples at concentrations ranging from 0.08 to 0.23 ng/ml. Perfluorooctane sulfonate (PFOS), perfluorohexanoate (PFHxA) and perfluorotridecanoate (PFTriDA) were sporadically detected, while the remaining compounds were below the limit of detection. This is the first report of detectible concentrations of PFASs in an endemic Antarctic marine mammal species. We suggest that the pollutants have been subjected to long range atmospheric transportation and/or derive from a local source. A review of these and published data indicate that perfluoroalkyl carboxylates (PFCAs) dominate in biotic PFAS patterns in species feeding south of the Antarctic Circumpolar Current (ACC), whereas PFOS was the major PFAS detected in species feeding predominantly north of the current. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Routti, Heli] Norwegian Polar Res Inst, Fram Ctr, N-9296 Tromso, Norway. [Krafft, Bjorn A.] Inst Marine Res, N-5817 Bergen, Norway. [Herzke, Dorte] Norwegian Inst Air Res, Fram Ctr, N-9296 Tromso, Norway. [Eisert, Regina] Univ Canterbury, Gateway Antarctica, Christchurch 8140, New Zealand. [Eisert, Regina; Oftedal, Olav] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Routti, H (reprint author), Norwegian Polar Res Inst, Fram Ctr, N-9296 Tromso, Norway. EM heli.routti@npolar.no FU United States Antarctic Program (USAP); National Science Foundation Office of Polar Programs [B-024, NSF/OPP 0538592]; Norwegian Polar Institute FX This field work was supported by the United States Antarctic Program (USAP) and funded by the National Science Foundation Office of Polar Programs (Project number B-024; NSF/OPP 0538592). The contaminant analyses were funded by the Norwegian Polar Institute. Thanks are also extended to Morten Wexels Riser, Dan Borritt, Mike Lara and Daryl Boness for their contributions to the field work, to Arntraut Gotsch for her help with the chemical analyses and to Robert Garrott for providing ages of our animals. NR 63 TC 4 Z9 4 U1 8 U2 34 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0269-7491 EI 1873-6424 J9 ENVIRON POLLUT JI Environ. Pollut. PD FEB PY 2015 VL 197 BP 62 EP 67 DI 10.1016/j.envpol.2014.11.026 PG 6 WC Environmental Sciences SC Environmental Sciences & Ecology GA CD2PM UT WOS:000350921500008 PM 25497307 ER PT J AU Lund, M Bjerke, JW Drake, BG Engelsen, O Hansen, GH Parmentier, FJW Powell, TL Silvennoinen, H Sottocornola, M Tommervik, H Weldon, S Rasse, DP AF Lund, Magnus Bjerke, J. W. Drake, B. G. Engelsen, O. Hansen, G. H. Parmentier, F. J. W. Powell, T. L. Silvennoinen, H. Sottocornola, M. Tommervik, H. Weldon, S. Rasse, D. P. TI Low impact of dry conditions on the CO2 exchange of a Northern-Norwegian blanket bog SO ENVIRONMENTAL RESEARCH LETTERS LA English DT Article DE peatland; carbon; blanket bog; eddy covariance; climate change; net ecosystem exchange ID NET ECOSYSTEM EXCHANGE; CARBON-DIOXIDE EXCHANGE; INTERANNUAL VARIABILITY; ARCTIC TUNDRA; PEATLAND; BALANCE; RESPIRATION; FLUXES; MIRE; PARAMETERIZATION AB Northern peatlands hold large amounts of organic carbon (C) in their soils and are as such important in a climate change context. Blanket bogs, i.e. nutrient-poor peatlands restricted to maritime climates, may be extra vulnerable to global warming since they require a positive water balance to sustain their moss dominated vegetation and C sink functioning. This study presents a 4.5 year record of land-atmosphere carbon dioxide (CO2) exchange from the Andoya blanket bog in northern Norway. Compared with other peatlands, the Andoya peatland exhibited low flux rates, related to the low productivity of the dominating moss and lichen communities and the maritime settings that attenuated seasonal temperature variations. It was observed that under periods of high vapour pressure deficit, net ecosystem exchange was reduced, which was mainly caused by a decrease in gross primary production. However, no persistent effects of dry conditions on the CO2 exchange dynamics were observed, indicating that under present conditions and within the range of observed meteorological conditions the Andoya blanket bog retained its C uptake function. Continued monitoring of these ecosystem types is essential in order to detect possible effects of a changing climate. C1 [Lund, Magnus; Parmentier, F. J. W.] Aarhus Univ, Arct Res Ctr, Dept Biosci, DK-8000 Aarhus C, Denmark. [Bjerke, J. W.; Tommervik, H.] Norwegian Inst Nat Res, Trondheim, Norway. [Drake, B. G.] Smithsonian Environm Res Ctr, Edgewater, MD USA. [Engelsen, O.; Hansen, G. H.] Norwegian Inst Air Res, Stjordal, Norway. [Lund, Magnus; Parmentier, F. J. W.] Lund Univ, Dept Phys Geog & Ecosyst Sci, S-22100 Lund, Sweden. [Powell, T. L.] Harvard Univ, Dept Organism & Evolutionary Biol, Cambridge, MA 02138 USA. [Parmentier, F. J. W.; Silvennoinen, H.; Weldon, S.; Rasse, D. P.] Norwegian Inst Agr & Environm Res, Bioforsk, Stjordal, Norway. [Sottocornola, M.] Waterford Inst Technol, Dept Sci, Waterford, Ireland. [Sottocornola, M.] Univ Coll Cork, Environm Res Inst, Cork, Ireland. RP Lund, M (reprint author), Aarhus Univ, Arct Res Ctr, Dept Biosci, DK-8000 Aarhus C, Denmark. EM ml@bios.au.dk RI Powell, Thomas/F-9877-2016; Parmentier, Frans-Jan/D-9022-2013; Sottocornola, Matteo/E-9092-2010; Lund, Magnus/J-4922-2013 OI Powell, Thomas/0000-0002-3516-7164; Parmentier, Frans-Jan/0000-0003-2952-7706; Daniel, Rasse/0000-0002-5977-3863; Lund, Magnus/0000-0003-1622-2305 FU Research Council of Norway; Stiftelsen Fondet for Jord-og Myrundersokelser; Bioforsk Strategic Research Funds; Norwegian Institute for Nature Research; Norwegian Institute for Air Research; FRAM-High North Centre for Climate; Environment Tromso FX Research at Andoya peatland was made possible through generous grants from the Research Council of Norway, Stiftelsen Fondet for Jord-og Myrundersokelser, Bioforsk Strategic Research Funds, Norwegian Institute for Nature Research, Norwegian Institute for Air Research and FRAM-High North Centre for Climate and the Environment Tromso. Instrumentation at the site as well as installation support was supplied by the Smithsonian Environmental Research Center. Logistic and technical support from the Andoya Rocket Range is gratefully acknowledged. NR 55 TC 7 Z9 7 U1 1 U2 35 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 1748-9326 J9 ENVIRON RES LETT JI Environ. Res. Lett. PD FEB PY 2015 VL 10 IS 2 AR 025004 DI 10.1088/1748-9326/10/2/025004 PG 13 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA CC7UI UT WOS:000350573500025 ER PT J AU Moratelli, R Calisher, CH AF Moratelli, Ricardo Calisher, Charles H. TI Bats and zoonotic viruses: can we confidently link bats with emerging deadly viruses? SO MEMORIAS DO INSTITUTO OSWALDO CRUZ LA English DT Article DE bat-borne viruses; biosafety; Chiroptera; bat immunology; emerging infectious diseases; zoonosis ID RESPIRATORY SYNDROME CORONAVIRUS; WHITE-NOSE SYNDROME; NIPAH VIRUS; EBOLA-VIRUS; FRUIT BATS; RESERVOIR HOSTS; FLYING-FOXES; RABIES VIRUS; BIODIVERSITY HOTSPOTS; IMMUNE-RESPONSES AB An increasingly asked question is 'can we confidently link bats with emerging viruses?'. No, or not yet, is the qualified answer based on the evidence available. Although more than 200 viruses-some of them deadly zoonotic viruses -have been isolated from or otherwise detected in bats, the supposed connections between bats, bat viruses and human diseases have been raised more on speculation than on evidence supporting their direct or indirect roles in the epidemiology of diseases (except for rabies). However, we are convinced that the evidence points in that direction and that at some point it will be proved that bats are competent hosts for at least a few zoonotic viruses. In this review, we cover aspects of bat biology, ecology and evolution that might be relevant in medical investigations and we provide a historical synthesis of some disease outbreaks causally linked to bats. We provide evolutionary-based hypotheses to tentatively explain the viral transmission route through mammalian intermediate hosts and to explain the geographic concentration of most outbreaks, but both are no more than speculations that still require formal assessment. C1 [Moratelli, Ricardo] Fiocruz Mata Atlantica, Rio De Janeiro, RJ, Brazil. [Calisher, Charles H.] Colorado State Univ, Coll Vet Med & Biomed Sci, Dept Microbiol Immunol & Pathol, Arthropod Borne & Infect Dis Lab, Ft Collins, CO 80523 USA. RP Moratelli, R (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Div Mammals, Washington, DC 20560 USA. EM rmoratelli@fiocruz.br RI Rocha, Ricardo/A-5735-2013 OI Rocha, Ricardo/0000-0003-0942-6633 FU PAPES; FIOCRUZ; CNPq [407623/2012-4]; CNPq/CsF [202612/2012]; FAPERJ [E-26/111.288/2014]; Smithsonian Institution (USA) FX PAPES, FIOCRUZ, CNPq (407623/2012-4), CNPq/CsF (202612/2012), FAPERJ (E-26/111.288/2014), Smithsonian Institution (USA) NR 134 TC 22 Z9 22 U1 17 U2 84 PU FUNDACO OSWALDO CRUZ PI RIO DE JANEIRO, RJ PA AV BRASIL 4365, 21045-900 RIO DE JANEIRO, RJ, BRAZIL SN 0074-0276 EI 1678-8060 J9 MEM I OSWALDO CRUZ JI Mem. Inst. Oswaldo Cruz PD FEB PY 2015 VL 110 IS 1 BP 1 EP 22 DI 10.1590/0074-02760150048 PG 22 WC Parasitology; Tropical Medicine SC Parasitology; Tropical Medicine GA CC9OB UT WOS:000350699000001 PM 25742261 ER PT J AU Keuskamp, JA Feller, IC Laanbroek, HJ Verhoeven, JTA Hefting, MM AF Keuskamp, Joost A. Feller, Ilka C. Laanbroek, Hendrikus J. Verhoeven, Jos T. A. Hefting, Mariet M. TI Short- and long-term effects of nutrient enrichment on microbial exoenzyme activity in mangrove peat SO SOIL BIOLOGY & BIOCHEMISTRY LA English DT Article DE Mangroves; Rhizophora; Peat; Microbial activity; SOC; Decomposition; Differential nutrient limitation; Microbial elemental stoichiometry ID EXTRACELLULAR ENZYME-ACTIVITY; RHIZOPHORA-MANGLE; ECOENZYMATIC STOICHIOMETRY; LITTER DECOMPOSITION; NITROGEN DEPOSITION; EXTRACTION METHOD; SOIL; CARBON; PHOSPHORUS; TANNINS AB Mangroves receive increasing quantities of nutrients as a result of coastal development, which could lead to significant changes in carbon sequestration and soil subsidence. We hypothesised that mangrove-produced tannins induce a nitrogen (N) limitation on microbial decomposition even when plant growth is limited by phosphorus (P). As a result, increased N influx would lead to a net loss of sequestered carbon negating the ability to compensate for sea level rise in P-limited mangroves. To examine this, we quantified the short- and long-term effects of N and P enrichment on microbial biomass and decomposition-related enzyme activities in a Rhizophora mangle-dominated mangrove, which had been subjected to fertilisation treatments for a period of fifteen years. We compared microbial biomass, elemental stoichiometry and potential enzyme activity in dwarf and fringe-type R. mangle-dominated sites, where primary production is limited by P or N depending on the proximity to open water. Even in P-limited mangroves, microbial activity was N-limited as indicated by stoichiometry and an increase in enzymic activity upon N amendment. Nevertheless, microbial biomass increased upon field additions of P, indicating that the carbon supply played even a larger role. Furthermore, we found that P amendment suppressed phenol oxidase activity, while N amendment did not. The possible differential nutrient limitations of microbial decomposers versus primary producers implies that the direction of the effect of eutrophication on carbon sequestration is nutrient-specific. In addition, this study shows that phenol oxidase activities in this system decrease through P, possibly strengthening the enzymic latch effect of mangrove tannins. Furthermore, it is argued that the often used division between N-harvesting, P-harvesting, and carbon-harvesting exoenzymes needs to be reconsidered. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Keuskamp, Joost A.; Laanbroek, Hendrikus J.; Verhoeven, Jos T. A.; Hefting, Mariet M.] Univ Utrecht, Dept Biol, Ecol & Biodivers, NL-3584 CH Utrecht, Netherlands. [Feller, Ilka C.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Laanbroek, Hendrikus J.] Netherlands Inst Ecol NIOO KNAW, Dept Microbial Wetland Ecol, Wageningen, Netherlands. RP Keuskamp, JA (reprint author), Univ Utrecht, Dept Biol, Ecol & Biodivers, Padualaan 8, NL-3584 CH Utrecht, Netherlands. EM j.a.keuskamp@uu.nl; feller@serc.si.edu; h.j.laanbroek@nioo.knaw.nl; j.t.a.verhoeven@uu.nl; m.m.hefting@uu.nl RI Laanbroek, Hendrikus J./C-3830-2008; Hefting, Mariet /L-9682-2016; OI Laanbroek, Hendrikus J./0000-0003-2400-3399; Hefting, Mariet /0000-0002-3852-7532; KNAW, NIOO-KNAW/0000-0002-3835-159X; Feller, Ilka/0000-0002-6391-1608 FU Schure-Beijerinck-Popping Fonds [SBP/JK/2010-30]; Smithsonian Marine Science Network; King Abdullah University of Science and Technology KAUST [KUK-C1-017-12] FX This study was supported by Schure-Beijerinck-Popping Fonds (SBP/JK/2010-30), the Smithsonian Marine Science Network and by the King Abdullah University of Science and Technology KAUST (KUK-C1-017-12). NR 51 TC 2 Z9 2 U1 8 U2 81 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 2015 VL 81 BP 38 EP 47 DI 10.1016/j.soilbio.2014.11.003 PG 10 WC Soil Science SC Agriculture GA CC7CG UT WOS:000350524700005 ER PT J AU Peterson, KM Heaney, PJ Post, JE Eng, PJ AF Peterson, Kristina M. Heaney, Peter J. Post, Jeffrey E. Eng, Peter J. TI A refined monoclinic structure for a variety of "hydrohematite" SO AMERICAN MINERALOGIST LA English DT Article DE Hydrohematite; protohematite; hematite; akaganeite; X-ray diffraction ID DEHYDRATION TRANSFORMATIONS; SYNTHETIC GOETHITE; POWDER DIFFRACTION; IRON-OXIDES; CRYSTAL-STRUCTURE; TWIN FORMATION; III OXIDE; IN-SITU; HEMATITE; PHASE AB In ferruginous soils, nano- to microscale hematite (alpha-Fe2O3) plays a central role in redox processes and contaminant cycling. Hematite is known to incorporate structural OH- and water, and the requisite charge balance is achieved by iron vacancies. Prior researchers have suggested that the defective hematite structures form unique phases called "protohematite" and "hydrohematite." Infrared and Raman spectroscopic studies have assigned a lower-symmetry space group to "hydrohematite" (R3c) relative to that of stoichiometric hematite (R (3) over barc). However, the existence and structure of these phases have been contentious, largely due to the lack of in situ X-ray diffraction data Here we present a new structure refinement for "hydrohematite" precipitated hydrothermally at 200 degrees C in a monoclinic space group (I2/a) using time-resolved synchrotron X-ray diffraction (TR-XRD) data collected during the in situ hydrothermal precipitation of akaganeite and its transformation to stoichiometric hematite. Distinct peak splitting was observed in the "hydrohematite" diffraction patterns, indicating a violation of the threefold rotational symmetry. A monoclinic unit cell with parameters of a = 7.3951(10), b = 5.0117(5), c = 5.4417(7) angstrom, beta = 95.666(5)degrees provided a good fit and significant reduction in chi(2) and R-wp to space group R (3) over barc. Rietveld analyses revealed that water concentrations in the first-formed crystals of "hydrohematite" were comparable to water contents of akaganeite and goethite. Thus, the hydrothermal transformation of akaganeite to "hydrohematite" is promoted not by dehydration but by reconstruction of the oxygen framework. C1 [Peterson, Kristina M.; Heaney, Peter J.] Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. [Post, Jeffrey E.] Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. [Eng, Peter J.] Univ Chicago, Consortium Adv Radiat Sources, Chicago, IL 60637 USA. RP Peterson, KM (reprint author), Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. EM kmp286682@gmail.com FU National Science Foundation [EAR07-45374, EAR11-47728]; DOE [CHE-0431328]; National Science Foundation, Earth Sciences [EAR-1128799]; Department of Energy, Geosciences [DE-FG02-94ER14466]; U.S. Department of Energy, Office of Science, Basic Energy Sciences [W-31-109-Eng-38] FX This work was made possible by the National Science Foundation Grants EAR07-45374 and EAR11-47728 and the Center for Environmental Kinetics Analysis (CEKA), an NSF- and DOE-sponsored Environmental Molecular Sciences Institute (CHE-0431328). GeoSoilEnviroCARS is supported by the National Science Foundation, Earth Sciences (EAR-1128799) and Department of Energy, Geosciences (DE-FG02-94ER14466). The Advanced Photon Source is supported by the U.S. Department of Energy, Office of Science, Basic Energy Sciences, under Contract No. W-31-109-Eng-38. We thank Joanne Stubbs and Nancy Lazarz at GSECARS BM-13, as well as Tim Fisher for their invaluable assistance in data collection at the beamline. NR 70 TC 4 Z9 4 U1 2 U2 27 PU MINERALOGICAL SOC AMER PI CHANTILLY PA 3635 CONCORDE PKWY STE 500, CHANTILLY, VA 20151-1125 USA SN 0003-004X EI 1945-3027 J9 AM MINERAL JI Am. Miner. PD FEB-MAR PY 2015 VL 100 IS 2-3 BP 570 EP 579 DI 10.2138/am-2015-4807 PG 10 WC Geochemistry & Geophysics; Mineralogy SC Geochemistry & Geophysics; Mineralogy GA CC1JI UT WOS:000350096600022 ER PT J AU Sollmann, R Gardner, B Chandler, RB Royle, JA Sillett, TS AF Sollmann, Rahel Gardner, Beth Chandler, Richard B. Royle, J. Andrew Sillett, T. Scott TI An open-population hierarchical distance sampling model SO ECOLOGY LA English DT Article DE Aphelocoma insularis; demography; distance sampling; Island Scrub-Jay; Markov model; population trend estimation; power analysis; Santa Cruz Island; California; USA; temporal autocorrelation ID ABUNDANCE; CONSERVATION; DYNAMICS; COUNTS; SIZE AB Modeling population dynamics while accounting for imperfect detection is essential to monitoring programs. Distance sampling allows estimating population size while accounting for imperfect detection, but existing methods do not allow for estimation of demographic parameters. We develop a model that uses temporal correlation in abundance arising from underlying population dynamics to estimate demographic parameters from repeated distance sampling surveys. Using a simulation study motivated by designing a monitoring program for Island Scrub-Jays (Aphelocoma insularis), we investigated the power of this model to detect population trends. We generated temporally autocorrelated abundance and distance sampling data over six surveys, using population rates of change of 0.95 and 0.90. We fit the data generating Markovian model and a mis-specified model with a log-linear time effect on abundance, and derived post hoc trend estimates from a model estimating abundance for each survey separately. We performed these analyses for varying numbers of survey points. Power to detect population changes was consistently greater under the Markov model than under the alternatives, particularly for reduced numbers of survey points. The model can readily be extended to more complex demographic processes than considered in our simulations. This novel framework can be widely adopted for wildlife population monitoring. C1 [Sollmann, Rahel; Gardner, Beth] N Carolina State Univ, Dept Forestry & Environm Resources, Raleigh, NC 27695 USA. [Chandler, Richard B.] Univ Georgia, Warnell Sch Forestry & Nat Resources, Athens, GA 30602 USA. [Royle, J. Andrew] USGS, Patuxent Wildlife Res Ctr, Laurel, MD 20708 USA. [Sillett, T. Scott] Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Washington, DC 20013 USA. RP Sollmann, R (reprint author), N Carolina State Univ, Dept Forestry & Environm Resources, Campus Box 8008, Raleigh, NC 27695 USA. EM rsollma@ncsu.edu RI Chandler, Richard/F-9702-2016; OI Royle, Jeffrey/0000-0003-3135-2167 FU U.S. National Park Service; U.S. Geological Survey Biological Resources Discipline FX The U.S. National Park Service and the U.S. Geological Survey Biological Resources Discipline jointly funded this study via the Park Oriented Biological Support program. This manuscript was improved by comments and advice from S. A. Morrison, Courtney Amundson, David L. Miller, Steve Buckland, and two anonymous reviewers. Any use of trade, firm, or product names is for descriptive purposes only and does not imply endorsement by the U.S. government. NR 26 TC 4 Z9 4 U1 5 U2 28 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA SN 0012-9658 EI 1939-9170 J9 ECOLOGY JI Ecology PD FEB PY 2015 VL 96 IS 2 BP 325 EP 331 DI 10.1890/14-1625.1 PG 7 WC Ecology SC Environmental Sciences & Ecology GA CC6OI UT WOS:000350484600003 PM 26240853 ER PT J AU Darroch, SAF Wagner, PJ AF Darroch, Simon A. F. Wagner, Peter J. TI Response of beta diversity to pulses of Ordovician-Silurian mass extinction SO ECOLOGY LA English DT Article DE beta diversity; brachiopods; climate change; glaciation; mass extinction; Ordovician; Silurian ID GEOGRAPHIC RANGE; CLIMATE-CHANGE; FOSSIL RECORD; PHANEROZOIC BIODIVERSITY; ECOLOGICAL COMMUNITIES; ENVIRONMENTAL-CHANGES; SPECIES-DIVERSITY; DISTANCE-DECAY; TURNOVER; GLACIATION AB Ecologists are increasingly using the fossil record of mass extinction to build predictive models for the ongoing biodiversity crisis. During mass extinctions, major depletions in global (i.e., gamma) diversity may reflect decrease in alpha diversity (i.e., local assemblages support fewer taxa), and/or decrease in beta diversity (such that similar pools of taxa are common to a greater number of local areas). Contrasting the effects of extinction on alpha and beta diversity is therefore central to understanding how global richness becomes depleted over these critical events. Here we investigate the spatial effects of mass extinction by examining changes in alpha, beta, and gamma diversity in brachiopod communities over both pulses of Ordovician-Silurian extinction (similar to 445.2 and similar to 438.8 million years ago), which had dramatically different causal mechanisms. We furthermore reconstruct geographic range sizes for brachiopod genera to test competing models for drivers of beta diversity change. We find that: (1) alpha and beta diversity respond differently to extinction; (2) these responses differ between pulses of extinction; (3) changes in beta diversity associated with extinction are accompanied by changes in geographic range size; and (4) changes in global beta diversity were driven by the extinction of taxa with statistically small and large ranges, rather than range expansion/contraction in taxa that survive into the aftermath. A symptom of ongoing biotic crisis may therefore be the extinction of specific narrow- or wide-ranging taxa, rather than the global proliferation of opportunistic and disaster forms. In addition, our results illustrate that changes in beta diversity on these longer timescales may largely be dictated by emplacement and removal of barriers to dispersal. Lastly, this study reinforces the utility of the fossil record in addressing questions surrounding the role of global-scale processes (such as mass extinctions) in sculpting and assembling regional biotas. C1 [Darroch, Simon A. F.] Yale Univ, Dept Geol & Geophys, New Haven, CT 06511 USA. [Darroch, Simon A. F.; Wagner, Peter J.] Smithsonian Inst NHB, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. RP Darroch, SAF (reprint author), Yale Univ, Dept Geol & Geophys, 210 Whitney Ave, New Haven, CT 06511 USA. EM simon.darroch@yale.edu RI Wagner, Peter/A-5514-2009 OI Wagner, Peter/0000-0002-9083-9787 FU Smithsonian Predoctoral fellowship; Paleontological Society; Yale Institute of Biospheric Sciences; Yale Peabody Museum of Natural History FX We acknowledge constructive comments from editors and two anonymous reviewers, which greatly improved an earlier version of the manuscript. S. A. F. Darroch acknowledges generous funding stemming from a Smithsonian Predoctoral fellowship, and by grants from the Paleontological Society, Yale Institute of Biospheric Sciences, and Yale Peabody Museum of Natural History. J. Belmaker gave substantial help with coding in R. For comments, we thank S. K. Lyons, R. Racicot, and all members of the Derek Briggs and Pincelli Hull research groups. This is Paleobiology Database publication No. 205. NR 109 TC 7 Z9 7 U1 3 U2 20 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0012-9658 EI 1939-9170 J9 ECOLOGY JI Ecology PD FEB PY 2015 VL 96 IS 2 BP 532 EP 549 DI 10.1890/14-1061.1 PG 18 WC Ecology SC Environmental Sciences & Ecology GA CC6OI UT WOS:000350484600024 PM 26240874 ER PT J AU McKinley, B Yang, R Lopez-Caniego, M Briggs, F Hurley-Walker, N Wayth, RB Offringa, AR Crocker, R Bernardi, G Procopio, P Gaensler, BM Tingay, SJ Johnston-Hollitt, M McDonald, M Bell, M Bhat, NDR Bowman, JD Cappallo, RJ Corey, BE Deshpande, AA Emrich, D Ewall-Wice, A Feng, L Goeke, R Greenhill, LJ Hazelton, BJ Hewitt, JN Hindson, L Jacobs, D Kaplan, DL Kasper, JC Kratzenberg, E Kudryavtseva, N Lenc, E Lonsdale, CJ Lynch, MJ McWhirter, SR Mitchell, DA Morales, MF Morgan, E Oberoi, D Ord, SM Pindor, B Prabu, T Riding, J Rogers, AEE Roshi, DA Shankar, NU Srivani, KS Subrahmanyan, R Waterson, M Webster, RL Whitney, AR Williams, A Williams, CL AF McKinley, B. Yang, R. Lopez-Caniego, M. Briggs, F. Hurley-Walker, N. Wayth, R. B. Offringa, A. R. Crocker, R. Bernardi, G. Procopio, P. Gaensler, B. M. Tingay, S. J. Johnston-Hollitt, M. McDonald, M. Bell, M. Bhat, N. D. R. Bowman, J. D. Cappallo, R. J. Corey, B. E. Deshpande, A. A. Emrich, D. Ewall-Wice, A. Feng, L. Goeke, R. Greenhill, L. J. Hazelton, B. J. Hewitt, J. N. Hindson, L. Jacobs, D. Kaplan, D. L. Kasper, J. C. Kratzenberg, E. Kudryavtseva, N. Lenc, E. Lonsdale, C. J. Lynch, M. J. McWhirter, S. R. Mitchell, D. A. Morales, M. F. Morgan, E. Oberoi, D. Ord, S. M. Pindor, B. Prabu, T. Riding, J. Rogers, A. E. E. Roshi, D. A. Shankar, N. Udaya Srivani, K. S. Subrahmanyan, R. Waterson, M. Webster, R. L. Whitney, A. R. Williams, A. Williams, C. L. TI Modelling of the spectral energy distribution of Fornax A: leptonic and hadronic production of high-energy emission from the radio lobes SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: active; galaxies: individual: NGC1316; radio continuum: galaxies ID LARGE-AREA TELESCOPE; MURCHISON WIDEFIELD ARRAY; PROBE WMAP OBSERVATIONS; MULTIFREQUENCY RADIO; SOURCE CATALOG; RAY-EMISSION; CYGNUS-A; 408 MHZ; X-RAY; GALAXY AB We present new low-frequency observations of the nearby radio galaxy Fornax A at 154 MHz with the Murchison Widefield Array, microwave flux-density measurements obtained from WMAP and Planck data, and gamma-ray flux densities obtained from Fermi data. We also compile a comprehensive list of previously published images and flux-density measurements at radio, microwave and X-ray energies. A detailed analysis of the spectrum of Fornax A between 154 and 1510 MHz reveals that both radio lobes have a similar spatially averaged spectral index, and that there exists a steep-spectrum bridge of diffuse emission between the lobes. Taking the spectral index of both lobes to be the same, we model the spectral energy distribution of Fornax A across an energy range spanning 18 orders of magnitude, to investigate the origin of the X-ray and gamma-ray emission. A standard leptonic model for the production of both the X-rays and gamma-rays by inverse-Compton scattering does not fit the multiwavelength observations. Our results best support a scenario where the X-rays are produced by inverse-Compton scattering and the gamma-rays are produced primarily by hadronic processes confined to the filamentary structures of the Fornax A lobes. C1 [McKinley, B.; Briggs, F.; Offringa, A. R.; Crocker, R.; Waterson, M.] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia. [McKinley, B.; Briggs, F.; Wayth, R. B.; Offringa, A. R.; Procopio, P.; Gaensler, B. M.; Tingay, S. J.; Bell, M.; Bhat, N. D. R.; Lenc, E.; Mitchell, D. A.; Ord, S. M.; Pindor, B.; Riding, J.; Subrahmanyan, R.; Webster, R. L.] Australian Natl Univ, ARC Ctr Excellence All Sky Astrophys CAASTRO, Canberra, ACT 2611, Australia. [Yang, R.] Max Planck Inst Kernphys, High Energy Astrophys Theory Grp, D-69029 Heidelberg, Germany. [Lopez-Caniego, M.] Inst Fis Cantabria CIC UC, E-39005 Santander, Spain. [Hurley-Walker, N.; Wayth, R. B.; Tingay, S. J.; Bhat, N. D. R.; Emrich, D.; Kudryavtseva, N.; Lynch, M. J.; Ord, S. M.; Waterson, M.; Williams, A.] Curtin Univ, Int Ctr Radio Astron Res, Bentley, WA 6102, Australia. [Bernardi, G.] SKA SA, ZA-7405 Pinelands, South Africa. [Bernardi, G.; Greenhill, L. J.; Kasper, J. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bernardi, G.] Rhodes Univ, Dept Phys & Elect, ZA-6140 Grahamstown, South Africa. [Procopio, P.; Mitchell, D. A.; Pindor, B.; Riding, J.; Webster, R. L.] Univ Melbourne, Sch Phys, Parkville, Vic 3010, Australia. [Gaensler, B. M.; Lenc, E.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia. [Johnston-Hollitt, M.; Hindson, L.] Victoria Univ Wellington, Sch Chem & Phys Sci, Wellington 6140, New Zealand. [McDonald, M.; Ewall-Wice, A.; Feng, L.; Goeke, R.; Hewitt, J. N.; Morgan, E.; Williams, C. L.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Bell, M.; Mitchell, D. A.] CSIRO Astron & Space Sci, Marsfield, NSW 2122, Australia. [Bowman, J. D.; Jacobs, D.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ USA. [Cappallo, R. J.; Corey, B. E.; Kratzenberg, E.; Lonsdale, C. J.; McWhirter, S. R.; Rogers, A. E. E.; Whitney, A. R.] MIT Haystack Observ, Westford, MA 01886 USA. [Deshpande, A. A.; Prabu, T.; Shankar, N. Udaya; Srivani, K. S.; Subrahmanyan, R.] Raman Res Inst, Bangalore 560080, Karnataka, India. [Hazelton, B. J.; Morales, M. F.] Univ Washington, Dept Phys, Seattle, WA 98195 USA. [Kaplan, D. L.] Univ Wisconsin, Dept Phys, Milwaukee, WI 53201 USA. [Kasper, J. C.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Oberoi, D.] Tata Inst Fundamental Res, Natl Ctr Radio Astrophys, Pune 411007, Maharashtra, India. [Roshi, D. A.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Roshi, D. A.] Natl Radio Astron Observ, Greenbank, VA 22903 USA. RP McKinley, B (reprint author), Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia. EM ben@mso.anu.edu.au RI Williams, Andrew/K-2931-2013; M, Manjunath/N-4000-2014; Deshpande, Avinash/D-4868-2012; Udayashankar , N/D-4901-2012; Wayth, Randall/B-2444-2013; Lopez-Caniego, Marcos/M-4695-2013; Emrich, David/B-7002-2013; Subrahmanyan, Ravi/D-4889-2012 OI Kudryavtseva, Nadia/0000-0002-1372-0942; Williams, Andrew/0000-0001-9080-0105; M, Manjunath/0000-0001-8710-0730; Lopez-Caniego, Marcos/0000-0003-1016-9283; /0000-0002-0086-7363; Lenc, Emil/0000-0002-9994-1593; Wayth, Randall/0000-0002-6995-4131; Emrich, David/0000-0002-4058-1837; FU U.S. National Science Foundation [AST-0457585, PHY-0835713, CAREER-0847753, AST-0908884]; Australian Research Council (LIEF) [LE0775621, LE0882938]; U.S. Air Force Office of Scientific Research [FA9550-0510247]; Centre for All-sky Astrophysics (an Australian Research Council Centre of Excellence) [CE110001020]; Smithsonian Astrophysical Observatory; MIT School of Science; Raman Research Institute; Australian National University; Victoria University of Wellington from the New Zealand Ministry of Economic Development [MED-E1799]; Victoria University of Wellington (IBM Shared University Research Grant); Commonwealth Scientific and Industrial Research Organisation (CSIRO); National Collaborative Research Infrastructure Strategy, Education Investment Fund; Australia India Strategic Research Fund; Astronomy Australia Limited; NVIDIA at Harvard University; International Centre for Radio Astronomy Research (ICRAR), a Joint Venture of Curtin University; University of Western Australia - Western Australian State government; Spanish MINECO [AYA2012-39475-C02-01, CSD2010-00064] FX This scientific work makes use of the Murchison Radio-astronomy Observatory, operated by CSIRO. We acknowledge the Wajarri Yamatji people as the traditional owners of the Observatory site. Support for the MWA comes from the U.S. National Science Foundation (grants AST-0457585, PHY-0835713, CAREER-0847753 and AST-0908884), the Australian Research Council (LIEF grants LE0775621 and LE0882938), the U.S. Air Force Office of Scientific Research (grant FA9550-0510247) and the Centre for All-sky Astrophysics (an Australian Research Council Centre of Excellence funded by grant CE110001020). Support is also provided by the Smithsonian Astrophysical Observatory, the MIT School of Science, the Raman Research Institute, the Australian National University and the Victoria University of Wellington (via grant MED-E1799 from the New Zealand Ministry of Economic Development and an IBM Shared University Research Grant). The Australian Federal government provides additional support via the Commonwealth Scientific and Industrial Research Organisation (CSIRO), National Collaborative Research Infrastructure Strategy, Education Investment Fund, and the Australia India Strategic Research Fund, and Astronomy Australia Limited, under contract to Curtin University. We acknowledge the iVEC Petabyte Data Store, the Initiative in Innovative Computing and the CUDA Center for Excellence sponsored by NVIDIA at Harvard University, and the International Centre for Radio Astronomy Research (ICRAR), a Joint Venture of Curtin University and The University of Western Australia, funded by the Western Australian State government. We acknowledge the support of the projects Spanish MINECO AYA2012-39475-C02-01 and CSD2010-00064. We would also like to thank the referee for their useful comments and suggestions. NR 73 TC 4 Z9 4 U1 1 U2 3 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB PY 2015 VL 446 IS 4 BP 3478 EP 3491 DI 10.1093/mnras/stu2310 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CC3TH UT WOS:000350272400018 ER PT J AU Keto, E Caselli, P Rawlings, J AF Keto, Eric Caselli, Paola Rawlings, Jonathan TI The dynamics of collapsing cores and star formation SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE ISM: abundances; ISM: clouds; ISM: evolution; ISM: individual objects: L1544; ISM: molecules ID MOLECULAR CLOUD CORES; PRE-STELLAR CORE; DENSE CORES; GRAVITATIONAL COLLAPSE; RADIATIVE-TRANSFER; ISOTHERMAL SPHERE; DARK CLOUDS; WATER-VAPOR; L1544; TURBULENCE AB Low-mass stars are understood to form by the gravitational collapse of the dense molecular clouds known as starless cores. However, it has proven impossible to use continuum observations to distinguish among the different hypotheses describing the collapse because the predicted density distributions for all spherical self-gravitating clouds are quite similar. However, the predicted velocities are quite different. We use two different molecular line transitions, H2O (1(10)-1(01)) and (CO)-O-18 (1-0), that are excited at different densities, 10(8) and 10(3) cm(-3), to measure the velocities at large and small radii in the contracting core L1544. We compare the observed spectra against those predicted for several different models of gravitational collapse including the Larson-Penston flow, the inside-out collapse of the singular isothermal sphere, the quasi-equilibrium contraction of an unstable Bonnor-Ebert sphere, and the non-equilibrium collapse of an overdense Bonnor-Ebert sphere. Only the model of the unstable quasi-equilibrium Bonnor-Ebert sphere is able to produce the observed shapes of both spectral lines. With this model, we interpret other molecular line observations of L1544 in the literature to find that the extended inward velocities seen in lines of CS(2-1) and N2H+ are located within the starless core itself, in particular in the region where the density profile follows an inverse square law. If these conclusions were to hold in the analysis of other starless cores, this would imply that the formation of hydrostatic clouds within the turbulent interstellar medium is not only possible but also not exceptional and may be an evolutionary phase in low-mass star formation. C1 [Keto, Eric] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02420 USA. [Caselli, Paola] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. [Rawlings, Jonathan] UCL, London WC1E 6BT, England. RP Keto, E (reprint author), Harvard Smithsonian Ctr Astrophys, 160 Garden St, Cambridge, MA 02420 USA. EM keto@cfa.harvard.edu FU European Research Council (ERC) [PALs 320620] FX PC acknowledges the financial support of the European Research Council (ERC; project PALs 320620) NR 56 TC 15 Z9 15 U1 0 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB PY 2015 VL 446 IS 4 BP 3731 EP 3740 DI 10.1093/mnras/stu2247 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CC3TH UT WOS:000350272400038 ER PT J AU Kepler, SO Pelisoli, I Koester, D Ourique, G Kleinman, SJ Romero, AD Nitta, A Eisenstein, DJ Costa, JES Kulebi, B Jordan, S Dufour, P Giommi, P Rebassa-Mansergas, A AF Kepler, S. O. Pelisoli, I. Koester, D. Ourique, G. Kleinman, S. J. Romero, A. D. Nitta, A. Eisenstein, D. J. Costa, J. E. S. Kuelebi, B. Jordan, S. Dufour, P. Giommi, Paolo Rebassa-Mansergas, Alberto TI New white dwarf stars in the Sloan Digital Sky Survey Data Release 10 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE catalogues; stars: magnetic field; subdwarfs; white dwarfs ID EXTREMELY LOW-MASS; OSCILLATION SPECTROSCOPIC SURVEY; MAIN-SEQUENCE BINARIES; 1ST DATA RELEASE; ATMOSPHERIC PARAMETERS; SDSS-III; SPECTRAL CLASSIFICATION; MERGER SYSTEMS; PROGENITORS; EVOLUTION AB We report the discovery of 9088 new spectroscopically confirmed white dwarfs and subdwarfs in the Sloan Digital Sky Survey Data Release 10. We obtain T-eff, log g and mass for hydrogen atmosphere white dwarf stars (DAs) and helium atmosphere white dwarf stars (DBs), and estimate the calcium/helium abundances for the white dwarf stars with metallic lines (DZs) and carbon/helium for carbon-dominated spectra DQs. We found 1 central star of a planetary nebula, 2 new oxygen spectra on helium atmosphere white dwarfs, 71 DQs, 42 hot DO/PG1159s, 171 white dwarf+main-sequence star binaries, 206 magnetic DAHs, 327 continuum-dominated DCs, 397 metal-polluted white dwarfs, 450 helium-dominated white dwarfs, 647 subdwarfs and 6887 new hydrogen-dominated white dwarf stars. C1 [Kepler, S. O.; Pelisoli, I.; Ourique, G.; Romero, A. D.; Costa, J. E. S.] Univ Fed Rio Grande do Sul, Inst Fis, BR-91501900 Porto Alegre, RS, Brazil. [Koester, D.] Univ Kiel, Inst Theoret Phys & Astrophys, D-24098 Kiel, Germany. [Kleinman, S. J.; Nitta, A.] Gemini Observ, Hilo, HI 96720 USA. [Eisenstein, D. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kuelebi, B.] Univ Autonoma Barcelona, Inst Ciencies Espai, E-08193 Barcelona, Spain. [Kuelebi, B.] Inst Space Studies Catalonia, E-08034 Barcelona, Spain. [Jordan, S.] Heidelberg Univ, Zentrum Astron, Astron Rechen Inst, D-69120 Heidelberg, Germany. [Dufour, P.] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada. [Giommi, Paolo] ASDC Agenzia Spaziale Italiana, I-00133 Rome, Italy. [Rebassa-Mansergas, Alberto] Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China. RP Kepler, SO (reprint author), Univ Fed Rio Grande do Sul, Inst Fis, BR-91501900 Porto Alegre, RS, Brazil. EM kepler@if.ufrgs.br RI Pelisoli, Ingrid/H-8619-2014; Romero, Alejandra/G-1644-2016; Kepler, S. O. /H-5901-2012 OI Kepler, S. O. /0000-0002-7470-5703 FU CNPq; FAPERGS-Pronex-Brazil; programme Science without Borders, MCIT/MEC-Brazil; MICINN [AYA08-1839/ESP]; ESF EUROCORES Program EuroGENESIS (MICINN) [EUI2009-04170]; Generalitat de Catalunya [2009SGR315]; EU-FEDER funds; Postdoctoral Science Foundation of China [2013M530470, 2014T70010]; Research Fund for International Young Scientists by the National Natural Science Foundation of China [11350110496]; Alfred P. Sloan Foundation; National Science Foundation; US Department of Energy Office of Science; University of Arizona; Brazilian Participation Group; Brookhaven National Laboratory; Carnegie Mellon University; University of Florida; French Participation Group; German Participation Group; Harvard University; Instituto de Astrofisica de Canarias; Michigan State/Notre Dame/JINA Participation Group; Johns Hopkins University; Lawrence Berkeley National Laboratory; Max Planck Institute for Astrophysics; Max Planck Institute for Extraterrestrial Physics; New Mexico State University; New York University; Ohio State University; Pennsylvania State University; University of Portsmouth; Princeton University; Spanish Participation Group; University of Tokyo; University of Utah; Vanderbilt University; University of Virginia; University of Washington; Yale University FX SOK, IP, GO, ADR and JESC are supported by CNPq and FAPERGS-Pronex-Brazil. DK received support from programme Science without Borders, MCIT/MEC-Brazil. BK is supported by the MICINN grant AYA08-1839/ESP, by the ESF EUROCORES Program EuroGENESIS (MICINN grant EUI2009-04170), by the 2009SGR315 of the Generalitat de Catalunya and EU-FEDER funds. ARM acknowledges financial support from the Postdoctoral Science Foundation of China (grants 2013M530470 and 2014T70010) and from the Research Fund for International Young Scientists by the National Natural Science Foundation of China (grant 11350110496).; Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation and the US Department of Energy Office of Science. The SDSS-III website is http://www.sdss3.org/.; SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington and Yale University. NR 74 TC 35 Z9 35 U1 1 U2 3 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB PY 2015 VL 446 IS 4 BP 4078 EP 4087 DI 10.1093/mnras/stu2388 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CC3TH UT WOS:000350272400063 ER PT J AU Plotkin, RM Gallo, E Markoff, S Homan, J Jonker, PG Miller-Jones, JCA Russell, DM Drappeau, S AF Plotkin, Richard M. Gallo, Elena Markoff, Sera Homan, Jeroen Jonker, Peter G. Miller-Jones, James C. A. Russell, David M. Drappeau, Samia TI Constraints on relativistic jets in quiescent black hole X-ray binaries from broad-band spectral modelling SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE acceleration of particles; accretion, accretion discs; stars: individual: XTE J1118+480; ISM: jets and outflows; X-rays: binaries ID ADVECTION-DOMINATED ACCRETION; DIFFUSIVE SHOCK ACCELERATION; SAGITTARIUS-A-ASTERISK; NOVA XTE J1118+480; SYNCHROTRON EMISSION; MULTIWAVELENGTH OBSERVATIONS; 2005 OUTBURST; HARD STATE; SGR-A; PARTICLE-ACCELERATION AB The nature of black hole jets at the lowest detectable luminosities remains an open question, largely due to a dearth of observational constraints. Here, we present a new, nearly simultaneous broad-band spectrum of the black hole X-ray binary (BHXB) XTE J1118+480 at an extremely low Eddington ratio (L-X similar to 10(-8.5)L(Edd)). Our new spectral energy distribution (SED) includes the radio, near-infrared, optical, ultraviolet, and X-ray wavebands. XTE J1118+480 is now the second BHXB at such a low Eddington ratio with a well-sampled SED, thereby providing new constraints on highly sub-Eddington accretion flows and jets, and opening the door to begin comparison studies between systems. We apply a multizone jet model to the new broad-band SED, and we compare our results to previous fits to the same source using the same model at 4-5 decades higher luminosity. We find that after a BHXB transitions to the so-called quiescent spectral state, the jet base becomes more compact (by up to an order of magnitude) and slightly cooler (by at least a factor of 2). Our preferred model fit indicates that jet particle acceleration is much weaker after the transition into quiescence. That is, accelerated non-thermal particles no longer reach high enough Lorentz factors to contribute significant amounts of synchrotron X-ray emission. Instead, the X-ray waveband is dominated by synchrotron self-Compton emission from a population of mildly relativistic electrons with a quasi-thermal velocity distribution that are associated with the jet base. The corresponding (thermal) synchrotron component from the jet base emits primarily in the infrared through ultraviolet wavebands. Our results on XTE J1118+480 are consistent with broad-band modelling for A0620-00 (the only other comparably low Eddington ratio BHXB with a well-sampled SED) and for Sgr A* (the quiescent supermassive black hole at the Galactic centre). The above could therefore represent a canonical baseline geometry for accreting black holes in quiescence. We conclude with suggestions for future studies to further investigate the above scenario. C1 [Plotkin, Richard M.; Gallo, Elena] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Markoff, Sera] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands. [Homan, Jeroen] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Jonker, Peter G.] SRON Netherlands Inst Space Res, SRON, NL-3584 CA Utrecht, Netherlands. [Jonker, Peter G.] Radboud Univ Nijmegen, IMAPP, Dept Astrophys, NL-6525 AJ Nijmegen, Netherlands. [Jonker, Peter G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Miller-Jones, James C. A.] Curtin Univ, Int Ctr Radio Astron Res, Perth, WA 6845, Australia. [Russell, David M.] New York Univ Abu Dhabi, Abu Dhabi, U Arab Emirates. [Drappeau, Samia] IRAP, F-31028 Toulouse, France. RP Plotkin, RM (reprint author), Univ Michigan, Dept Astron, 1085 South Univ Ave, Ann Arbor, MI 48109 USA. EM rplotkin@umich.edu RI Miller-Jones, James/B-2411-2013; Plotkin, Richard/I-3221-2016; OI Miller-Jones, James/0000-0003-3124-2814; Plotkin, Richard/0000-0002-7092-0326; Russell, David/0000-0002-3500-631X FU National Aeronautics and Space Administration through Chandra Award [GO3-14036X]; National Aeronautics Space Administration [NAS8-03060]; Australian Research Council (ARC) [FT140101082]; ARC [DP120102393]; french Research National Agency: CHAOS project [ANR-12-BS05-0009]; National Aeronautics and Space Administration FX We thank Marianne Heida for her help with the reduction of the NIR William Herschel Telescope (WHT) images, and we thank Neil Gehrels and the Swift team for approving and scheduling the Swift/UVOT observations. Support for this work was provided by the National Aeronautics and Space Administration through Chandra Award Number GO3-14036X 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. JMJ is supported by an Australian Research Council (ARC) Future Fellowship (FT140101082) and also acknowledges support from an ARC Discovery Grant (DP120102393). SD acknowledges funding support from the french Research National Agency: CHAOS project ANR-12-BS05-0009. This research has made use of software provided by the Chandra X-ray Center (CXC) in the application package CIAO. 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 Astrofsica de Canarias. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This publication makes use of data products from the WISE, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. This work is based in part on archival data obtained with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. NR 102 TC 12 Z9 12 U1 1 U2 2 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB PY 2015 VL 446 IS 4 BP 4098 EP 4111 DI 10.1093/mnras/stu2385 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CC3TH UT WOS:000350272400065 ER PT J AU Whitten, J Head, JW AF Whitten, Jennifer Head, James W. TI Lunar cryptomaria: Mineralogy and composition of ancient volcanic deposits SO PLANETARY AND SPACE SCIENCE LA English DT Article DE Moon; Volcanism; Cryptomaria; Moon Mineralogy Mapper; Visible to near infrared; Spectroscopy; Modified Gaussian Model (MGM) ID MODIFIED GAUSSIAN MODEL; PROSPECTOR GAMMA-RAY; MARE VOLCANISM; PYROXENE MIXTURES; IMPACT BASINS; MOON; SURFACE; SPECTRA; OLIVINE; SPECTROSCOPY AB Ancient lunar volcanic deposits, known as cryptomaria, have been detected by remote telescopic and orbital measurements since the 1970s. Cryptomaria are most easily identified by the presence of dark-halo impact craters and are associated with a mare basalt mineralogy, which is indicated by two pyroxene spectral absorption features near 1 mu m and 2 mu m in the visible to near-infrared (VNIR) wavelengths. However, there are many early igneous lithologies that have been identified in the Apollo sample collection that have a similar VNIR spectral signal, implying a pyroxene-dominant mineralogy. In this study we use high resolution Moon Mineralogy Mapper (M-3) VNIR spectral data and the Modified Gaussian Model (MGM) to determine cryptomare mineralogy as well as Lunar Prospector gamma-ray spectrometer (LP GRS) FeO and Th compositional measurements to evaluate which ancient igneous rocks (e.g., low-Ti mare basalt, high-Ti mare basalt, Mg-suite rocks, dunite, high-Al mare basalt, KREEP basalt) are consistent with our mineralogical observations. In addition, spectra from different M-3 optical periods were compared to determine how the MGM-derived absorption band centers vary between datasets. Band center differences between optical periods are on the order of similar to 6 +/- 4 nm and similar to 25 +/- 10 nm for the 1 mu m and 2 mu m features, respectively. Cryptomare mineralogies are dominated by clinopyroxene and are consistent with measurements from locally exposed mare basalts. LP GRS measurements support a mare basalt rock type when regolith mixing is taken into account. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Whitten, Jennifer] Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20013 USA. [Head, James W.] Brown Univ, Dept Earth Environm & Planetary Sci, Providence, RI 02912 USA. RP Whitten, J (reprint author), Smithsonian Inst, Ctr Earth & Planetary Studies, MRC 315,POB 37012, Washington, DC 20013 USA. EM WhittenJ@si.edu FU NASA Solar System Exploration Research Virtual Institute (SSERVI) grant [NNA14AB01A] FX We thank S. Besse and H. Clenet for their constructive reviews of this manuscript. This research was supported by the NASA Solar System Exploration Research Virtual Institute (SSERVI) grant for Evolution and Environment of Exploration Destinations under cooperative agreement number NNA14AB01A at Brown University. NR 93 TC 7 Z9 7 U1 1 U2 7 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0032-0633 J9 PLANET SPACE SCI JI Planet Space Sci. PD FEB PY 2015 VL 106 BP 67 EP 81 DI 10.1016/j.pss.2014.11.027 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CC7AD UT WOS:000350519200005 ER PT J AU Cruz, P Barrado, D Lillo-Box, J Diaz, M Birkby, J Lopez-Morales, M Hodgkin, S Fortney, JJ AF Cruz, Patricia Barrado, David Lillo-Box, Jorge Diaz, Marcos Birkby, Jayne Lopez-Morales, Mercedes Hodgkin, Simon Fortney, Jonathan J. TI Detection of the secondary eclipse of WASP-10b in the Ks-band SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE planetary systems; stars: individual: WASP 10; techniques: photometric ID INFRARED THERMAL EMISSION; GROUND-BASED DETECTION; EARTH-LIKE EXOPLANETS; EJECTION CME ACTIVITY; TRANSIT LIGHT CURVES; IN HABITABLE ZONES; LOW-MASS STARS; HOT JUPITERS; TERRESTRIAL EXOPLANETS; MAGNETIC ACTIVITY AB Context. WASP-10b, a non-inflated hot Jupiter, was discovered around a K-dwarf in a near circular orbit (similar to 0.06). Since its discovery in 2009, different published parameters for this system have led to a discussion about the size, density, and eccentricity of this exoplanet. Aims. In order to test the hypothesis of a circular orbit for WASP-10b, we observed its secondary eclipse in the Ks-band. where the contribution of planetary light is high enough to be detected from the ground. Methods, Observations were performed with the OMEGA2000 instrument at the 3.5 m telescope at Calar Alto (Almeria, Spain). in staring mode during 5.4 continuous hours. with the telescope defocused, monitoring the target during the expected secondary eclipse. A relative light curve was generated and corrected from systematic effects, using the principal component analysis (PCA) technique. The final light curve was fitted using a transit model to find the eclipse depth and a possible phase shift. Results. The best model obtained from the Markov chain Monte Carlo analysis resulted in an eclipse depth of Delta F of 0.137%(+0.013%)(-0.019%) and a phase offset of Delta phi of -0.00284(-0.0004)(+0.005). The eclipse phase offset derived from our modeling has systematic errors that were not taken into account and should not be considered as evidence of an eccentric orbit. The offset in phase obtained leads to a value for vertical bar e cos omega vertical bar of 0.0044, The derived eccentricity is too small to be of any significance. C1 [Cruz, Patricia; Barrado, David; Lillo-Box, Jorge] Ctr Astrobiol INTA CSIC, Dept Astrofis, Villanueva De La Canada 28691, Spain. [Diaz, Marcos] Univ Sao Paulo IAG USP, Inst Astron Geofis & Ciencias Atmosfer, Sao Paulo, Brazil. [Birkby, Jayne] Leiden Univ, Leiden Observ, NL-2333 CA Leiden, Netherlands. [Lopez-Morales, Mercedes] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hodgkin, Simon] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Fortney, Jonathan J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. RP Cruz, P (reprint author), Ctr Astrobiol INTA CSIC, Dept Astrofis, ESAC Campus,POB 78, Villanueva De La Canada 28691, Spain. EM pcruz@cab.inta-csic.es RI Lillo-Box, Jorge/I-2841-2015; Barrado Navascues, David/C-1439-2017 OI Lillo-Box, Jorge/0000-0003-3742-1987; Barrado Navascues, David/0000-0002-5971-9242 FU Spanish grants [AYA2010-21161-C02-02, AYA2012-38897-C02-01, PRICIT-S2009/ESP-1496]; RoPACS network; European Commissions Seventh Framework Programme FX P.C. would like to thank Dr. A. Gil de Paz, Dr, M. R. Zapatero Osorio and Dr. I. A G. Snellen for all fruitful discussions and suggestions. This research has been funded by Spanish grants AYA2010-21161-C02-02, AYA2012-38897-C02-01, and PRICIT-S2009/ESP-1496. P.C., D.B., J.B. and S.H. have received support from the RoPACS network during this research, a Marie Curie Initial Training Network funded by the European Commissions Seventh Framework Programme. This article is based on data collected under Service Time program at the Catty Alto Observatory. the German Spanish Astronomical Center, Calar Alto, jointly operated by the Max-Planck-Institut fur Astronomic Heidelberg and the Instituto de Astrofisica de Andalucia (CSIC). We are very grateful to the CADA staff for the super quality of the observations. This work has made use of the ALADIN interactive sky atlas and the SIMBAD database, operated at CDS, Strasbourg, France, and of NASA's Astrophysics Data System Bibliographic Services. NR 39 TC 7 Z9 7 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD FEB PY 2015 VL 574 AR A103 DI 10.1051/0004-6361/201423509 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CB2OJ UT WOS:000349467000103 ER PT J AU Decin, L Richards, AMS Neufeld, D Steffen, W Melnick, G Lombaert, R AF Decin, L. Richards, A. M. S. Neufeld, D. Steffen, W. Melnick, G. Lombaert, R. TI ALMA data suggest the presence of spiral structure in the inner wind of CW Leonis SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: AGB and post-AGB; stars: mass-loss; circumstellar matter; binaries: general; stars: individual: CW Leo ID CARBON STAR IRC+10216; ROTATIONAL LINE-PROFILES; RED SUPERGIANT STARS; DUST FORMATION ZONE; GIANT BRANCH STARS; MASS-LOSS HISTORY; CIRCUMSTELLAR ENVELOPE; AGB STARS; MULTIPLE SHELLS; BINARY-SYSTEMS AB Context. Evolved low-mass stars lose a significant fraction of their mass through stellar winds. While the overall morphology of the stellar wind structure during the asymptotic giant branch (AGB) phase is thought to be roughly spherically symmetric, the morphology changes dramatically during the post-AGB and planetary nebula phase, during which bipolar and multi-polar structures are often observed. Aims. We aim to study the inner wind structure of the closest well-known AGB star CW Leo. Different diagnostics probing different geometrical scales have implied a non-homogeneous mass-loss process for this star: dust clumps are observed at milli-arcsec scale, a bipolar structure is seen at arcsecond-scale, and multi-concentric shells are detected beyond 1 ''. Methods. We present the first ALMA Cycle 0 band 9 data around 650 GHz (450 mu m) tracing the inner wind of CW Leo. The full-resolution data have a spatial resolution of 0 ''.42 x 0 ''.24, allowing us to study the morpho-kinematical structure of CW Leo within similar to 6 ''. Results. We have detected 25 molecular emission lines in four spectral windows. The emission of all but one line is spatially resolved. The dust and molecular lines are centered around the continuum peak position, which is assumed to be dominated by stellar emission. The dust emission has an asymmetric distribution with a central peak flux density of similar to 2 Jy. The molecular emission lines trace different regions in the wind acceleration region and imply that the wind velocity increases rapidly from about 5 R-star, almost reaching the terminal velocity at similar to 11 R-star. The images prove that vibrational lines are excited close to the stellar surface and that SiO is a parent molecule. The channel maps for the brighter lines show a complex structure; specifically, for the (CO)-C-13 J = 6-5 line, different arcs are detected within the first few arcseconds. The curved structure in the position-velocity (PV) map of the (CO)-C-13 J = 6-5 line can be explained by a spiral structure in the inner wind of CW Leo, probably induced by a binary companion. From modelling the ALMA data, we deduce that the potential orbital axis for the binary system lies at a position angle of similar to 10-20 degrees to the north-east and that the spiral structure is seen almost edge-on. We infer an orbital period of 55 yr and a binary separation of 25 au (or similar to 8.2 R-star). We tentatively estimate that the companion is an unevolved low-mass main-sequence star. Conclusions. A scenario of a binary-induced spiral shell can explain the correlated structure seen in the ALMA PV images of CW Leo. Moreover, this scenario can also explain many other observational signatures seen at different spatial scales and in different wavelength regions, such as the bipolar structure and the almost concentric shells. ALMA data hence for the first time provide the crucial kinematical link between the dust clumps seen at milli-arcsecond scale and the almost concentric arcs seen at arcsecond scale. C1 [Decin, L.; Lombaert, R.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Leuven, Belgium. [Richards, A. M. S.] Univ Manchester, JBCA, Dept Phys & Astron, Manchester M13 9PL, Lancs, England. [Neufeld, D.] Johns Hopkins Univ, Baltimore, MD 21218 USA. [Steffen, W.] Univ Nacl Autonoma Mexico, Inst Astron, Ensenada 22800, Baja California, Mexico. [Melnick, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Decin, L (reprint author), Katholieke Univ Leuven, Inst Sterrenkunde, Celestijnenlaan 200D, B-3001 Leuven, Belgium. EM Leen.Decin@ster.kuleuven.be FU UNAM-PAPIIT [101014] FX This paper makes use of the following ALMA data: ADS/JAO.ALMA#2011.0.00277.S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. W.S. acknowledges support by grant UNAM-PAPIIT 101014. The authors thank Nicholas Koning and Miguel Santander-Garcia for technical support with SHAPE. NR 74 TC 15 Z9 15 U1 0 U2 2 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD FEB PY 2015 VL 574 AR A5 DI 10.1051/0004-6361/201424593 PG 26 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CB2OJ UT WOS:000349467000005 ER PT J AU Delubac, T Bautista, JE Busca, NG Rich, J Kirkby, D Bailey, S Font-Ribera, A Slosar, A Lee, KG Pieri, MM Hamilton, JC Aubourg, E Blomqvist, M Bovy, J Brinkmann, J Carithers, W Dawson, KS Eisenstein, DJ Gontcho, SGA Kneib, JP Le Goff, JM Margala, D Miralda-Escude, J Myers, AD Nichol, RC Noterdaeme, P O'Connell, R Olmstead, MD Palanque-Delabrouille, N Paris, I Petitjean, P Ross, NP Rossi, G Schlegel, DJ Schneider, DP Weinberg, DH Yeche, C York, DG AF Delubac, Timothee Bautista, Julian E. Busca, Nicola G. Rich, James Kirkby, David Bailey, Stephen Font-Ribera, Andreu Slosar, Anze Lee, Khee-Gan Pieri, Matthew M. Hamilton, Jean-Christophe Aubourg, Eric Blomqvist, Michael Bovy, Jo Brinkmann, Jon Carithers, William Dawson, Kyle S. Eisenstein, Daniel J. Gontcho, Satya Gontcho A. Kneib, Jean-Paul Le Goff, Jean Marc Margala, Daniel Miralda-Escude, Jordi Myers, Adam D. Nichol, Robert C. Noterdaeme, Pasquier O'Connell, Ross Olmstead, Matthew D. Palanque-Delabrouille, Nathalie Paris, Isabelle Petitjean, Patrick Ross, Nicholas P. Rossi, Graziano Schlegel, David J. Schneider, Donald P. Weinberg, David H. Yeche, Christophe York, Donald G. TI Baryon acoustic oscillations in the Lya forest of BOSS DR11 quasars SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE cosmology: observations; dark energy; large-scale structure of Universe; cosmological parameters ID DIGITAL SKY SURVEY; DATA RELEASE 9; SPECTROSCOPIC GALAXY SAMPLE; LUMINOUS RED GALAXIES; 10TH DATA RELEASE; 9TH DATA RELEASE; MEASURING D-A; ALPHA FOREST; SDSS-III; TARGET SELECTION AB We report a detection of the baryon acoustic oscillation (BAO) feature in the flux-correlation function of the Ly alpha forest of high-redshift quasars with a statistical significance of five standard deviations. The study uses 137 562 quasars in the redshift range 2.1 <= z <= 3.5 from the data release 11 (DR11) of the Baryon Oscillation Spectroscopic Survey (BOSS) of SDSS-III. This sample contains three times the number of quasars used in previous studies. The measured position of the BAO peak determines the angular distance, D-A(Z = 2.34) and expansion rate, H(z = 2.34), both on a scale set by the sound horizon at the drag epoch, r(d). We find D-A/r(d) = 11.28 +/- 0.65(1 sigma)(-1.2)(+2.8)(2 sigma) and D-H/r(d) = 9.18 +/- 0.28(1 sigma) +/- 0.6(2 sigma) where D-H = c/H. The optimal combination, similar to(DHDA0.3)-D-0.7/r(d) is determined with a precision of similar to 2%. For the value r(d) = 147.4 Mpc, consistent with the cosmic microwave background power spectrum measured by Planck, we find D-A(Z = 2.34) = 1662 +/- 96(1 sigma) Mpc and H(z = 2.34) = 222 +/- 7(1 sigma) km s(-1) Mpc(-1). Tests with mock catalogs and variations of our analysis procedure have revealed no systematic uncertainties comparable to our statistical errors. Our results agree with the previously reported BAO measurement at the same redshift using the quasar-Ly alpha forest cross-correlation. The autocorrelation and cross-correlation approaches are complementary because of the quite different impact of redshift-space distortion on the two measurements. The combined constraints from the two correlation functions imply values of D-A/r(d) that are 7% lower and 7% higher for D-H/r(d) than the predictions of a flat ACDM cosmological model with the best-fit Planck parameters. With our estimated statistical errors, the significance of this discrepancy is approximate to 2.5 sigma. C1 [Delubac, Timothee; Rich, James; Le Goff, Jean Marc; Palanque-Delabrouille, Nathalie; Rossi, Graziano; Yeche, Christophe] CEA, Ctr Saclay, IRFU, F-91191 Gif Sur Yvette, France. [Bautista, Julian E.; Busca, Nicola G.; Hamilton, Jean-Christophe; Aubourg, Eric] Univ Paris 07, APC, CNRS, IN2P3,CEA,Observ Paris, F-75205 Paris, France. [Kirkby, David; Blomqvist, Michael; Margala, Daniel] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Bailey, Stephen; Font-Ribera, Andreu; Carithers, William; Ross, Nicholas P.; Schlegel, David J.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Slosar, Anze] Brookhaven Natl Lab, Upton, NY 11973 USA. [Lee, Khee-Gan] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Pieri, Matthew M.; Nichol, Robert C.] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England. [Bovy, Jo] Inst Adv Study, Princeton, NJ 08540 USA. [Brinkmann, Jon] Apache Point Observ, Sunspot, NM 88349 USA. [Dawson, Kyle S.; Olmstead, Matthew D.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Eisenstein, Daniel J.] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Delubac, Timothee; Kneib, Jean-Paul] Ecole Polytech Fed Lausanne, Lab Astrophys, CH-1015 Lausanne, Switzerland. [Kneib, Jean-Paul] Aix Marseille Univ, CNRS, LAM, UMR 7326, F-13388 Marseille, France. [Miralda-Escude, Jordi] Inst Catalana Recerca & Estudis, Barcelona, Catalonia, Spain. [Gontcho, Satya Gontcho A.; Miralda-Escude, Jordi] Univ Barcelona, IEEC, Inst Ciencies Cosmos, E-08028 Barcelona, Catalonia, Spain. [Myers, Adam D.] Univ Wyoming, Dept Phys & Astron, Laramie, WY 82071 USA. [Noterdaeme, Pasquier; Paris, Isabelle; Petitjean, Patrick] Univ Paris 06, F-75014 Paris, France. [Noterdaeme, Pasquier; Paris, Isabelle; Petitjean, Patrick] CNRS, Inst Astrophys Paris, F-75014 Paris, France. [O'Connell, Ross] Carnegie Mellon Univ, Bruce & Astrid McWilliams Ctr Cosmol, Pittsburgh, PA 15213 USA. [Ross, Nicholas P.] Drexel Univ, Dept Phys, Philadelphia, PA 19104 USA. [Schneider, Donald P.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Schneider, Donald P.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. [Weinberg, David H.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [York, Donald G.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60615 USA. [York, Donald G.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60615 USA. [Busca, Nicola G.] Observ Nacl, BR-20921400 Rio De Janeiro, Brazil. [Busca, Nicola G.] Lab Interinst & Astron LIneA, BR-20921400 Rio De Janeiro, Brazil. [Rossi, Graziano] Sejong Univ, Dept Astron & Space Sci, Seoul 143747, South Korea. RP Delubac, T (reprint author), CEA, Ctr Saclay, IRFU, F-91191 Gif Sur Yvette, France. EM timothee.delubac@epfl.ch RI Kneib, Jean-Paul/A-7919-2015; EPFL, Physics/O-6514-2016; OI Kneib, Jean-Paul/0000-0002-4616-4989; Bovy, Jo/0000-0001-6855-442X FU Alfred P. Sloan Foundation; National Science Foundation; US Department of Energy Office of Science; Agence Nationale de la Recherche [ANR-12-BS05-0015-01, ANR-08-BLAN-0222]; ERC advanced grant LIDA; European Union [PHF-GA-2011-301665]; University of Arizona; Brazilian Participation Group; Brookhaven National Laboratory; Carnegie Mellon University; University of Florida; French Participation Group; German Participation Group; Harvard University; Instituto de Astrofisica de Canarias; Michigan State/Notre Dame/JINA Participation Group; Johns Hopkins University; Lawrence Berkeley National Laboratory; Max Planck Institute for Astrophysics; Max Planck Institute for Extraterrestrial Physics; New Mexico State University; New York University; Ohio State University; Pennsylvania State University; University of Portsmouth; Princeton University; Spanish Participation Group; University of Tokyo; University of Utah; Vanderbilt University; University of Virginia; University of Washington; Yale University; ERC; European Union Seventh Framework Programme [PHF-GA-2011-301665] FX Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the US Department of Energy Office of Science. The SDSS-III web site is http: //www.adss3.org/. SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona. the Brazilian Participation Group, Brookhaven National Laboratory, Carnegie Mellon University, University of Florida, the French Participation Group. the German Participation Group, Harvard University. the Instituto de Astrofisica de Canarias. the Michigan State/Notre Dame/JINA Participation Group. Johns Hopkins University. Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University. University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University. The French Participation Group of SDSS-III was supported by the Agence Nationale de la Recherche under contracts ANR-08-BLAN-0222 and ANR-12-BS05-0015-01. Timothee Delubac and Jean Paul Kneib acknowledge support from the ERC advanced grant LIDA. Matthew Pieri has received funding from the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement No. [PHF-GA-2011-301665]. The authors acknowledge the support of France Grilles for providing computing resources on the French National Grid Infrastructure. NR 62 TC 120 Z9 121 U1 2 U2 13 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 2015 VL 574 AR A59 DI 10.1051/0004-6361/201423969 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CB2OJ UT WOS:000349467000059 ER PT J AU Moldon, J Deller, AT Wucknitz, O Jackson, N Drabent, A Carozzi, T Conway, J Kapinska, AD McKean, JP Morabito, L Varenius, E Zarka, P Anderson, J Asgekar, A Avruch, IM Bell, ME Bentum, MJ Bernardi, G Best, P Birzan, L Bregman, J Breitling, F Broderick, JW Bruggen, M Butcher, HR Carbone, D Ciardi, B de Gasperin, F de Geus, E Duscha, S Eisloffel, J Engels, D Falcke, H Fallows, RA Fender, R Ferrari, C Frieswijk, W Garrett, MA Griessmeier, J Gunst, AW Hamaker, JP Hassall, TE Heald, G Hoeft, M Juette, B Karastergiou, A Kondratiev, VI Kramer, M Kuniyoshi, M Kuper, G Maat, P Mann, G Markoff, S McFadden, R McKay-Bukowski, D Morganti, R Munk, H Norden, MJ Offringa, AR Orru, E Paas, H Pandey-Pommier, M Pizzo, R Polatidis, AG Reich, W Rottgering, H Rowlinson, A Scaife, AMM Schwarz, D Sluman, J Smirnov, O Stappers, BW Steinmetz, M Tagger, M Tang, Y Tasse, C Thoudam, S Toribio, MC Vermeulen, R Vocks, C van Weeren, RJ White, S Wise, MW Yatawatta, S Zensus, A AF Moldon, J. Deller, A. T. Wucknitz, O. Jackson, N. Drabent, A. Carozzi, T. Conway, J. Kapinska, A. D. McKean, J. P. Morabito, L. Varenius, E. Zarka, P. Anderson, J. Asgekar, A. Avruch, I. M. Bell, M. E. Bentum, M. J. Bernardi, G. Best, P. Birzan, L. Bregman, J. Breitling, F. Broderick, J. W. Brueggen, M. Butcher, H. R. Carbone, D. Ciardi, B. de Gasperin, F. de Geus, E. Duscha, S. Eisloeffel, J. Engels, D. Falcke, H. Fallows, R. A. Fender, R. Ferrari, C. Frieswijk, W. Garrett, M. A. Griessmeier, J. Gunst, A. W. Hamaker, J. P. Hassall, T. E. Heald, G. Hoeft, M. Juette, B. Karastergiou, A. Kondratiev, V. I. Kramer, M. Kuniyoshi, M. Kuper, G. Maat, P. Mann, G. Markoff, S. McFadden, R. McKay-Bukowski, D. Morganti, R. Munk, H. Norden, M. J. Offringa, A. R. Orru, E. Paas, H. Pandey-Pommier, M. Pizzo, R. Polatidis, A. G. Reich, W. Roettgering, H. Rowlinson, A. Scaife, A. M. M. Schwarz, D. Sluman, J. Smirnov, O. Stappers, B. W. Steinmetz, M. Tagger, M. Tang, Y. Tasse, C. Thoudam, S. Toribio, M. C. Vermeulen, R. Vocks, C. van Weeren, R. J. White, S. Wise, M. W. Yatawatta, S. Zensus, A. TI The LOFAR long baseline snapshot calibrator survey SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE instrumentation: high angular resolution; instrumentation: interferometers; methods: observational; techniques: interferometric; techniques: high angular resolution; catalogs ID METER-WAVELENGTH VLBI; SKY SURVEY; RADIO-SOURCES; ARRAY AB Aims. An efficient means of locating calibrator sources for international LOw Frequency ARray (LOFAR) is developed and used to determine the average density of usable calibrator sources on the sky for subarcsecond observations at 140 MHz. Methods. We used the multi-beaming capability of LOFAR to conduct a fast and computationally inexpensive survey with the full international LOFAR array. Sources were preselected on the basis of 325 MHz arcminute-scale flux density using existing catalogues. By observing 30 different sources in each of the 12 sets of pointings per hour, we were able to inspect 630 sources in two hours to determine if they possess a sufficiently bright compact component to be usable as LOFAR delay calibrators. Results. More than 40% of the observed sources are detected on multiple baselines between international stations and 86 are classified as satisfactory calibrators. We show that a flat low-frequency spectrum (from 74 to 325 MHz) is the best predictor of compactness at 140 MHz. We extrapolate from our sample to show that the sky density of calibrators that are sufficiently bright to calibrate dispersive and non-dispersive delays for the international LOFAR using existing methods is 1.0 per square degree. Conclusions. The observed density of satisfactory delay calibrator sources means that observations with international LOFAR should be possible at virtually any point in the sky provided that a fast and efficient search, using the methodology described here, is conducted prior to the observation to identify the best calibrator. C1 [Moldon, J.; Deller, A. T.; McKean, J. P.; Asgekar, A.; Bentum, M. J.; Bregman, J.; de Geus, E.; Duscha, S.; Falcke, H.; Fallows, R. A.; Frieswijk, W.; Garrett, M. A.; Gunst, A. W.; Hamaker, J. P.; Heald, G.; Kondratiev, V. I.; Kuper, G.; Maat, P.; McFadden, R.; Morganti, R.; Munk, H.; Norden, M. J.; Orru, E.; Pizzo, R.; Polatidis, A. G.; Sluman, J.; Tang, Y.; Toribio, M. C.; Vermeulen, R.; Wise, M. W.; Yatawatta, S.] ASTRON, NL-7990 AA Dwingeloo, Netherlands. [Wucknitz, O.; Kramer, M.; Kuniyoshi, M.; Reich, W.; Zensus, A.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Jackson, N.; Kramer, M.; Stappers, B. W.] Univ Manchester, Jodrell Bank Ctr Astrophys, Sch Phys & Astron, Manchester M13 9PL, Lancs, England. [Drabent, A.; Hoeft, M.] Thuringer Landessternwarte, D-07778 Tautenburg, Germany. [Carozzi, T.; Conway, J.; Varenius, E.] Chalmers, Dept Earth & Space Sci, Onsala Space Observ, S-43992 Onsala, Sweden. [Kapinska, A. D.] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England. [Kapinska, A. D.] Univ Sydney, Sydney Inst Astron, ARC Ctr Excellence All Sky Astrophys CAASTRO, Sydney, NSW 2006, Australia. [Kapinska, A. D.] Curtin Univ, Int Ctr Radio Astron Res, Perth, WA 6845, Australia. [Morabito, L.; Birzan, L.; Garrett, M. A.; Roettgering, H.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Zarka, P.] Univ Paris 06, CNRS, LESIA, Observ Paris,Univ Paris Diderot, F-75252 Paris 05, France. [Anderson, J.] DeutschesGeoForschungsZentrum GFZ, Helmholtz Zentrum Potsdam, Dept Geodesy & Remote Sensing 1, D-14473 Potsdam, Germany. [Asgekar, A.] Shell Technol Ctr, Bangalore, Karnataka, India. [Avruch, I. M.] SRON Netherlands Insitute Space Res, NL-9700 AV Groningen, Netherlands. [Avruch, I. M.; Morganti, R.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Bell, M. E.; Rowlinson, A.] CSIRO Australia Telescope Natl Facil, Epping, NSW 1710, Australia. [Bentum, M. J.] Univ Twente, NL-7522 NB Enschede, Netherlands. [Bernardi, G.; van Weeren, R. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Best, P.] Univ Edinburgh, Royal Observ Edinburgh, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. [Breitling, F.; Mann, G.; Steinmetz, M.; Vocks, C.] Leibniz Inst Astrophys Potsdam AIP, D-14482 Potsdam, Germany. [Broderick, J. W.; Fender, R.; Karastergiou, A.] Univ Oxford, Oxford OX1 3RH, England. [Broderick, J. W.; Hassall, T. E.; Scaife, A. M. M.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Brueggen, M.; de Gasperin, F.] Univ Hamburg, D-21029 Hamburg, Germany. [Butcher, H. R.; Offringa, A. R.] Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. [Carbone, D.; Markoff, S.; Wise, M. W.] Univ Amsterdam, Anton Pannekoek Inst, NL-1090 GE Amsterdam, Netherlands. [Ciardi, B.; White, S.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [de Geus, E.] SmarterVision BV, NL-9401 JX Assen, Netherlands. [Engels, D.] Hamburger Sternwarte, D-21029 Hamburg, Germany. [Falcke, H.; Thoudam, S.] Radboud Univ Nijmegen, Dept Astrophys, IMAPP, NL-6500 GL Nijmegen, Netherlands. [Ferrari, C.] Univ Nice Sophia Antipolis, Lab Lagrange, UMR7293, CNRS,Observ Cote Azur, F-06300 Nice, France. [Griessmeier, J.; Tagger, M.] Univ Orleans, CNRS, LPC2E, F-45067 Orleans, France. [Griessmeier, J.] Univ Orleans, Stn Radioastron Nancay, Observ Paris, CNRS,INSU,USR 704,OSUC, F-18330 Nancay, France. [Juette, B.] Ruhr Univ Bochum, Astron Inst, D-44780 Bochum, Germany. [Kondratiev, V. I.] Ctr Astro Space, Lebedev Phys Inst, Moscow 117997, Russia. [McKay-Bukowski, D.] Univ Oulu, Sodankyla Geophys Observ, Sodankyla 99600, Finland. [McKay-Bukowski, D.] STFC Rutherford Appleton Lab, Didcot OX11 0QX, Oxon, England. [Paas, H.] Univ Groningen, CIT, NL-9700 AB Groningen, Netherlands. [Pandey-Pommier, M.] Observ Lyon, Ctr Rech Astrophys Lyon, F-69561 St Genis Laval, France. [Schwarz, D.] Univ Bielefeld, Fak Phys, D-33501 Bielefeld, Germany. [Smirnov, O.] Rhodes Univ, Dept Phys & Elect, ZA-6140 Grahamstown, South Africa. [Smirnov, O.] SKA South Africa, ZA-7405 Pinelands, South Africa. [Tasse, C.] Observ Paris, CNRS, UMR 8109, LESIA, F-92195 Meudon, France. RP Moldon, J (reprint author), ASTRON, Postbus 2, NL-7990 AA Dwingeloo, Netherlands. EM moldon@astron.nl RI Tagger, Michel/O-6615-2014; Kapinska, Anna/B-3999-2014; Ciardi, Benedetta/N-7625-2015; Kondratiev, Vladislav/N-1105-2015; OI Tagger, Michel/0000-0003-2962-3220; Kapinska, Anna/0000-0002-5289-5729; Kondratiev, Vladislav/0000-0001-8864-7471; Varenius, Eskil/0000-0002-3248-9467; van Weeren, Reinout/0000-0002-0587-1660 FU Veni Fellowship from NWO; Australian Research Council Centre of Excellence for All sky Astrophysics (CAASTRO) [CE110001020]; NWO Top LOFAR project [614.001.006]; Agence Nationale de la Recherche [ANR-09-JCJC-0001-01] FX LOFAR, the Love Frequency Array designed and constructed by ASTRON, has facilities in several countries that are owned by various parties (each with their own funding sources), and that are collectively operated by the international LOEAR Telescope (ILT) foundation under a joint scientific policy. A.D. is supported by a Veni Fellowship from NWO. A.D.K. acknowledges support from the Australian Research Council Centre of Excellence for All sky Astrophysics (CAASTRO), through project number CE110001020. LKM acknowledges financial support from NWO Top LOFAR project, project n. 614.001.006. CF acknowledges financial support by the Agence Nationale de la Recherche through grant ANR-09-JCJC-0001-01. NR 27 TC 6 Z9 6 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 PY 2015 VL 574 AR A73 DI 10.1051/0004-6361/201425042 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CB2OJ UT WOS:000349467000073 ER PT J AU Mottram, JC Kristensen, LE van Dishoeck, EF Bruderer, S Jose-Garcia, IS Karska, A Visser, R Santangelo, G Benz, AO Bergin, EA Caselli, P Herpin, F Hogerheijde, MR Johnstone, D van Kempen, TA Liseau, R Nisini, B Tafalla, M van der Tak, FFS Wyrowski, F AF Mottram, J. C. Kristensen, L. E. van Dishoeck, E. F. Bruderer, S. Jose-Garcia, I. San Karska, A. Visser, R. Santangelo, G. Benz, A. O. Bergin, E. A. Caselli, P. Herpin, F. Hogerheijde, M. R. Johnstone, D. van Kempen, T. A. Liseau, R. Nisini, B. Tafalla, M. van der Tak, F. F. S. Wyrowski, F. TI Water in star-forming regions with Herschel (WISH) V. The physical conditions in low-rnass protostellar outflows revealed by multi-transition water observations (vol 572, A21, 2014) SO ASTRONOMY & ASTROPHYSICS LA English DT Correction DE stars: formation; ISM: jets and outflows; ISM: molecules; soars: protostars; errata, addenda C1 [Mottram, J. C.; van Dishoeck, E. F.; Jose-Garcia, I. San; Hogerheijde, M. R.; van Kempen, T. A.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Kristensen, L. E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [van Dishoeck, E. F.; Bruderer, S.; Karska, A.; Caselli, P.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Visser, R.; Bergin, E. A.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Santangelo, G.] Osserv Astrofis Arcetri, I-50125 Florence, Italy. [Santangelo, G.; Nisini, B.] Osserv Astron Roma, I-00040 Monte Porzio Catone, Italy. [Benz, A. O.] Swiss Fed Inst Technol, Inst Astron, CH-8093 Zurich, Switzerland. [Caselli, P.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Herpin, F.] Univ Bordeaux, Observ Aquitain Sci Univers, F-33270 Floirac, France. [Herpin, F.] CNRS, LAB, UMR 5804, Lab Astrophys Bordeaux, F-33270 Floirac, France. [Johnstone, D.] Joint Astron Ctr, Hilo, HI 96720 USA. [Johnstone, D.] Univ Victoria, Dept Phys & Astron, Victoria, BC V8W 3P6, Canada. [Johnstone, D.] NRC Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Liseau, R.] Chalmers, Onsala Space Observ, Dept Earth & Space Sci, S-43992 Onsala, Sweden. [Tafalla, M.] Observ Astron Nacl IGN, Madrid 28014, Spain. [van der Tak, F. F. S.] SRON Netherlands Inst Space Res, NL-9700 AV Groningen, Netherlands. [van der Tak, F. F. S.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Wyrowski, F.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. RP Mottram, JC (reprint author), Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. EM mottram@strw.leidenuniv.nl RI Kristensen, Lars/F-4774-2011; Karska, Agata/O-5311-2016 OI Kristensen, Lars/0000-0003-1159-3721; Karska, Agata/0000-0001-8913-925X NR 1 TC 0 Z9 0 U1 1 U2 7 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD FEB PY 2015 VL 574 AR C3 DI 10.1051/0004-6361/201424267e PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CB2OJ UT WOS:000349467000147 ER PT J AU Neilson, HR Schneider, FRN Izzard, RG Evans, NR Langer, N AF Neilson, Hilding R. Schneider, Fabian R. N. Izzard, Robert G. Evans, Nancy R. Langer, Norbert TI The occurrence of classical Cepheids in binary systems SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE binaries: general; stars: variables: Cepheids ID STELLAR EVOLUTION MODELS; LARGE-MAGELLANIC-CLOUD; ENHANCED MASS-LOSS; SOLAR-TYPE STARS; GALACTIC CEPHEIDS; DYNAMICAL MASS; MULTIPLICITY; DISCREPANCY; POPULATION; COMPANION AB Classical Cepheids, like binary stars, are laboratories for stellar evolution and Cepheids in binary systems are especially powerful ones. About one-third of Galactic Cepheids are known to have companions and Cepheids in eclipsing binary systems have recently been discovered in the Large Magellanic Cloud (LMC). However, there are no known Galactic binary Cepheids with orbital periods less than one year. We compute population synthesis models of binary Cepheids to compare to the observed period and eccentricity distributions of Galactic Cepheids as well as to the number of observed eclipsing binary Cepheids in the LMC. We find that our population synthesis models are consistent with observed binary properties of Cepheids. Furthermore, we show that binary interaction on the red giant branch prevents some red giant stars from becoming classical Cepheids. Such interactions suggest that the binary fraction of Cepheids should be significantly less than that of their main-sequence progenitors, and that almost all binary Cepheids have orbital periods longer than one year. If the Galactic Cepheid spectroscopic binary fraction is about 35%, then the spectroscopic binary fraction of their intermediate mass main sequence progenitors is about 40-45%. C1 [Neilson, Hilding R.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Neilson, Hilding R.] E Tennessee State Univ, Dept Phys & Astron, Johnson City, TN 37614 USA. [Schneider, Fabian R. N.; Izzard, Robert G.; Langer, Norbert] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany. [Evans, Nancy R.] Smithsonian Astrophys Observat, Cambridge, MA 02138 USA. RP Neilson, HR (reprint author), Univ Toronto, Dept Astron & Astrophys, 50 St George St, Toronto, ON M5S 3H4, Canada. EM neilson@astro.utoronto.ca OI Izzard, Robert/0000-0003-0378-4843; Neilson, Hilding/0000-0002-7322-7236 FU Alexander von Humboldt Foundation; National Science Foundation [AST-0807664]; BCGS (DFG); Chandra X-ray Center NASA [NAS8-03060] FX H.R.N. and R.G.I. thank the Alexander von Humboldt Foundation and H.R.N. thanks the National Science Foundation (AST-0807664) for funding. F.R.N.S. acknowledges funding by BCGS (DFG). N.R.E. acknowledges funding from the Chandra X-ray Center NASA Contract NAS8-03060. We also thank the referee for helpful comments that have improved this work. NR 65 TC 5 Z9 5 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD FEB PY 2015 VL 574 AR A2 DI 10.1051/0004-6361/201424408 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CB2OJ UT WOS:000349467000002 ER PT J AU Rots, AH Bunclark, PS Calabretta, MR Allen, SL Manchester, RN Thompson, WT AF Rots, Arnold H. Bunclark, Peter S. Calabretta, Mark R. Allen, Steven L. Manchester, Richard N. Thompson, William T. TI Representations of time coordinates in FITS Time and relative dimension in space SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE time; standards; methods: data analysis; techniques: miscellaneous; astronomical databases: miscellaneous; reference systems ID SOLAR AB Context. In a series of three previous papers, formulation and specifics of the representation of world coordinate transformations in FITS data have been presented. This fourth paper deals with encoding time. Aims. Time on all scales and precisions known in astronomical datasets is to be described in an unambiguous, complete, and self-consistent manner. Methods. Employing the well-established World Coordinate System (WCS) framework, and maintaining compatibility with the FITS conventions that are currently in use to specify time, the standard is extended to describe rigorously the time coordinate. Results. World coordinate functions are defined for temporal axes sampled linearly and as specified by a lookup table. The resulting standard is consistent with the existing FITS WCS standards and specifies a metadata set that achieves the aims enunciated above. C1 [Rots, Arnold H.] Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Bunclark, Peter S.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Calabretta, Mark R.; Manchester, Richard N.] CSIRO, Astron & Space Sci, Epping, NSW 1710, Australia. [Allen, Steven L.] Univ Calif Santa Cruz, UCO Lick Observ, Santa Cruz, CA 95064 USA. [Thompson, William T.] NASA, Goddard Space Flight Ctr, Adnet Syst Inc, Greenbelt, MD 20771 USA. RP Rots, AH (reprint author), Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, 60 Garden St MS 67, Cambridge, MA 02138 USA. EM arots@cfa.harvard.edu OI Rots, Arnold/0000-0003-2377-2356 FU NASA [NAS 8-03060] FX The authors want to express their deep gratitude and appreciation for the dedication and tireless efforts of their colleague and friend Peter Bunclark in moving the work on this paper forward. We received his last email on 8 December 2008, just two days before his untimely death. We miss Pete dearly, not only as a great co-author who kept us on the straight and narrow, but especially as a very good friend. It was a privilege to have collaborated with him. We are also very much indebted to former IAU FITS Working Group chair Bill Pence, who provided valuable comments and kept exhorting us to finally finish this paper. A.H.R. gratefully acknowledges the many helpful discussions he had with Jonathan McDowell and the support by NASA under contract NAS 8-03060 to the Smithsonian Astrophysical Observatory for operation of the Chandra X-ray Center. We thank an anonymous referee for helpful comments that resulted in improved clarity. And we thank Patrick Wallace, Ken Seidelmann, and George Kaplan for their comments and suggestions. NR 46 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 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD FEB PY 2015 VL 574 AR A36 DI 10.1051/0004-6361/201424653 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CB2OJ UT WOS:000349467000036 ER PT J AU Schwartz, P Heinzel, P Kotrc, P Farnik, F Kupryakov, YA DeLuca, EE Golub, L AF Schwartz, P. Heinzel, P. Kotrc, P. Farnik, F. Kupryakov, Yu A. DeLuca, E. E. Golub, L. TI Total mass of six quiescent prominences estimated from their multi-spectral observations SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE Sun: filaments, prominences; Sun: corona; Sun: UV radiation; Sun: X-rays, gamma rays; techniques: spectroscopic ID H-ALPHA LINE; ABSORPTION FEATURES; EXTREME-ULTRAVIOLET; ATOMIC DATABASE; SOLAR; HINODE; MISSION; TRACE; SOHO; TELESCOPE AB Context. Total masses of six solar prominences were estimated using prominence multi-spectral observations (in EUV, X-rays, H alpha, and Ca II H). The observations were made during the observing campaign from April through June 2011. Aims. The aim of the work was to apply a complex method for the prominence mass estimations that can be used later for other prominences observed during the observing campaign. Methods. Our method is based on the fact that intensity of the EUV solar corona at wavelengths below 912 angstrom is reduced by the absorption in resonance continua of hydrogen and helium (photoionisation) and at the same time also by a deficit of the coronal emissivity in volume occupied by the cool prominence plasma. Both mechanisms contribute to intensity decrease simultaneously. The observations in X-rays allow us to separate these mechanisms from each other. Coronal emission behind a prominence is not estimated by any temporal or spatial interpolation, but by using a new method based on comparing the ratio of the optical thickness at 193 angstrom and 211 angstrom determined from the observations with the theoretical ratio. Results. Values of the total mass estimated for six prominences are between 2.9 x 10(11) and 1.7 x 10(12) kg. The column density of hydrogen is of the order of 10(18)-10(19) cm(-2). Our results agree with results of other authors. Conclusions. The method is now ready to be used for all 30 prominences observed during the campaign. Then in the near future it will be possible to obtain a statistics of the total mass of quiescent solar prominences. C1 [Schwartz, P.; Heinzel, P.; Kotrc, P.; Farnik, F.; Kupryakov, Yu A.] Acad Sci Czech Republic, Astron Inst, Ondrejov 25165, Czech Republic. [Schwartz, P.] Slovak Acad Sci, Astron Inst, Tatranska Lomnica 05960, Slovakia. [Kupryakov, Yu A.] Sternberg Astron Inst, Moscow 119899, Russia. [DeLuca, E. E.; Golub, L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Schwartz, P (reprint author), Acad Sci Czech Republic, Astron Inst, Ondrejov 25165, Czech Republic. EM schwartz@asu.cas.cz; pheinzel@asu.cas.cz; pkotrc@asu.cas.cz; ffarnik@asu.cas.cz; kupry@asu.cas.cz; edeluca@cfa.harvard.edu; lgolub@cfa.harvard.edu RI Schwartz, Pavol/G-9039-2014; Farnik, Frantisek/G-9010-2014; Kotrc, Pavel/G-9030-2014; Heinzel, Petr/G-9014-2014; DeLuca, Edward/L-7534-2013 OI Schwartz, Pavol/0000-0001-5986-9948; DeLuca, Edward/0000-0001-7416-2895 FU Grant Agency of the Czech Republic [P209/12/0906]; Science Grant Agency [VEGA 2/0108/12]; Slovak, Research and Development Agency [APVV-0816-11]; [RVO: 67985815] FX P.S. and RH, acknowledge the support from grant P209/12/0906 of the Grant Agency of the Czech Republic. Work of RS. and P.N. was supported by the project RVO: 67985815. Work of P.S. was also supported by the grant project VEGA 2/0108/12 of the Science Grant Agency. P.S. acknowledges support from the Slovak, Research and Development Agency under the contract No APVV-0816-11. The AIA data are courtesy of NASA/SDO and the AIA science team. CHIANTI is a collaborative project involving George Mason University, the University of Michigan (USA) and the University of Cambridge (UK). NR 38 TC 4 Z9 4 U1 0 U2 2 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD FEB PY 2015 VL 574 AR A62 DI 10.1051/0004-6361/201423513 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CB2OJ UT WOS:000349467000062 ER PT J AU Danner, RM Greenberg, RS Danner, JE Walters, JR AF Danner, Raymond M. Greenberg, Russell S. Danner, Julie E. Walters, Jeffrey R. TI Winter food limits timing of pre-alternate moult in a short-distance migratory bird SO FUNCTIONAL ECOLOGY LA English DT Article DE carry-over effects; feather moult; food limitation; moult sequence; moult timing ID WHITE-CROWNED SPARROWS; STARLINGS STURNUS-VULGARIS; MELOSPIZA-GEORGIANA-NIGRESCENS; FEATHER-DEGRADING BACILLI; LAGOPUS-LAGOPUS-LAGOPUS; LIFE-HISTORY STAGES; SUPERB FAIRY-WRENS; POSTNUPTIAL MOLT; SWAMP SPARROW; WILLOW PTARMIGAN AB Moult is critical for fitness for many organisms for several reasons: it allows growth and maintains the function of the integument for protection, thermoregulation and communication. Feather moult in birds is costly and therefore typically does not overlap with migration or reproduction. In spring, the rapid succession of pre-alternate moult, migration (if a migrant) and breeding suggests that timing of moult could constrain the initiation of breeding. A trade-off between time spent moulting and breeding might also limit moult quality. The proximate basis for the timing of pre-alternate moult initiation is not well known, although it typically occurs during a resource poor time of year. Food limitation combined with fitness consequences of moulting earlier suggests that plasticity in timing of pre-alternate moult in response to food abundance should be advantageous. We experimentally tested, for the first time, if food abundance influences the timing of moult in the wild. We conducted a controlled food supplementation experiment on free-living swamp sparrows (Melospiza georgiana) preceding and during the time of natural pre-alternate moult (January-March 2009, 2010). Supplemented birds began moulting the body, face and crown earlier than control birds (11, 14, and 8days earlier, respectively), indicating that food abundance limits the initiation of moult. Along with interannual variation, these results indicate that photoperiod is not the sole cue for initiation of moult. Both control and supplemented birds moulted in sequence, starting with the body, followed by the crown 9days later, and the face 11days after the body. The presence of a sequence further suggests energetic limitation of moult or possibly a strategy to moult-specific regions first to ensure completion or growth at an optimal time. This study provides novel experimental evidence that food abundance can: (i) limit pre-alternate moult timing and (ii) limit moult timing in the wild. Food limitation of moult timing could allow earlier breeding or production of higher quality feathers and thus cascade through other life-history stages and affect reproductive success. These results indicate that food availability is a cue for moult initiation, possibly acting secondarily to photostimulation. C1 [Danner, Raymond M.; Danner, Julie E.; Walters, Jeffrey R.] Virginia Tech, Dept Biol Sci, Blacksburg, VA 24061 USA. [Danner, Raymond M.; Greenberg, Russell S.] Natl Zool Pk, Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Washington, DC 20008 USA. [Danner, Julie E.] Natl Zool Pk, Smithsonian Conservat Biol Inst, Ctr Conservat & Evolutionary Genet, Washington, DC 20008 USA. RP Danner, RM (reprint author), Virginia Tech, Dept Biol Sci, Blacksburg, VA 24061 USA. EM danner.ray@gmail.com NR 88 TC 4 Z9 4 U1 7 U2 31 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0269-8463 EI 1365-2435 J9 FUNCT ECOL JI Funct. Ecol. PD FEB PY 2015 VL 29 IS 2 BP 259 EP 267 DI 10.1111/1365-2435.12322 PG 9 WC Ecology SC Environmental Sciences & Ecology GA CC0UF UT WOS:000350051900012 ER PT J AU Puillandre, N Duda, TF Meyer, C Olivera, BM Bouchet, P AF Puillandre, N. Duda, T. F. Meyer, C. Olivera, B. M. Bouchet, P. TI One, four or 100 genera? A new classification of the cone snails SO JOURNAL OF MOLLUSCAN STUDIES LA English DT Article ID INDO-WEST PACIFIC; MOLECULAR PHYLOGENY; EVOLUTIONARY HISTORY; CONOIDEA GASTROPODA; DISCOVERY; DIVERSIFICATION; TEREBRIDAE; SPECIATION; DIVERSITY; APPARATUS AB We present a new classification for the genus Conus sensu lato (family Conidae), based on molecular phylogenetic analyses of 329 species. This classification departs from both the traditional classification in only one genus and from a recently proposed shell-and radula-based classification scheme that separates members of this group into five families and 115 genera. Roughly 140 genus-group names are available for Recent cone snails. We propose to place all cone snails within a single family (Conidae) containing four genera-Conus, Conasprella, Profundiconus and Californiconus (with Conus alone encompassing about 85% of known species)-based on the clear separation of cone snails into four distinct and well-supported groups/ lineages in molecular phylogenetic analyses. Within Conus and Conasprella, we recognize 57 and 11 subgenera, respectively, that represent well-supported subgroupings within these genera, which we interpret as evidence of intrageneric distinctiveness. We allocate the 803 Recent species of Conidae listed as valid in the World Register of Marine Species into these four genera and 71 subgenera, with an estimate of the confidence for placement of species in these taxonomic categories based on whether molecular or radula and/or shell data were used in these determinations. Our proposed classification effectively departs from previous schemes by (1) limiting the number of accepted genera, (2) retaining the majority of species within the genus Conus and (3) assigning members of these genera to species groups/subgenera to enable the effective communication of these groups, all of which we hope will encourage acceptance of this scheme. C1 [Puillandre, N.; Bouchet, P.] Museum Natl Hist Nat, ISyEB Inst, Dept Systemat & Evolut, UPMC,EPHE,UMR CNRS 7205, F-75231 Paris, France. [Duda, T. F.] Univ Michigan, Dept Ecol & Evolutionary Biol, Ann Arbor, MI 48109 USA. [Duda, T. F.] Univ Michigan, Museum Zool, Ann Arbor, MI 48109 USA. [Meyer, C.] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20013 USA. [Olivera, B. M.] Univ Utah, Dept Biol, Salt Lake City, UT 84112 USA. RP Puillandre, N (reprint author), Museum Natl Hist Nat, ISyEB Inst, Dept Systemat & Evolut, UPMC,EPHE,UMR CNRS 7205, 43 Rue Cuvier, F-75231 Paris, France. EM puillandre@mnhn.fr FU National Institutes of Health [GM48677]; National Institutes of Health (ICBG) [1U01TW008163]; CONOTAX - French 'Agence Nationale de la Recherche' [ANR-13-JSV7-0013-01] FX The authors thank Manuel J. Tenorio for helpful comments. Some of the specimens analysed by BMO for this work were obtained using grant support provided by the National Institutes of Health (GM48677 and ICBG grant 1U01TW008163). This work was partly supported by the CONOTAX project, funded by the French 'Agence Nationale de la Recherche' (grant number ANR-13-JSV7-0013-01). NR 39 TC 19 Z9 23 U1 5 U2 16 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0260-1230 EI 1464-3766 J9 J MOLLUS STUD JI J. Molluscan Stud. PD FEB PY 2015 VL 81 BP 1 EP 23 DI 10.1093/mollus/eyu055 PN 1 PG 23 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA CC0VE UT WOS:000350054900001 PM 26300576 ER PT J AU Harasewych, MG AF Harasewych, M. G. TI Systematics and phylogeography of Cerion sensu stricto (Pulmonata: Cerionidae) from Aruba, Curacao and Bonaire SO JOURNAL OF MOLLUSCAN STUDIES LA English DT Article ID GASTROPODA PULMONATA; GENE GENEALOGIES; PLEISTOCENE; FLORIDA; DNA AB The systematic relationships of the Cerion uva complex and its constituent taxa are reviewed based on partial sequences of the cytochrome c oxidase I and 16S rDNA genes from 19 populations spanning the geographic range of the species complex and including the type localities of 8 of the 9 subspecies and forms. Molecular data support the conclusion of prior morphometric studies that all living Cerion inhabiting Aruba, Curacao and Bonaire are members of a single species, C. uva. Sequence variability among and within populations is not sufficiently discontinuous to segregate populations into discrete, species-level taxa. Three of four subspecies, proposed on the basis of geographic isolation during the Quaternary, C. uva uva (Linnaeus, 1758), the nominotypical subspecies from eastern Curac, ao, C. uva knipensis Baker, 1924, from western Curac, ao, and C. uva bonairensis Baker, 1924, from Bonaire, are all supported by distinctive haplotypes. Cerion uva arubanum Baker, 1924, a taxon based on living specimens from Aruba, is shown to be a synonym of C. uva uva, with which it shares a preponderance of haplotypes. It is conjectured that C. uva was widespread on Aruba during the Quaternary, but had become extinct on that island, and was reintroduced from a population near Willemstad in eastern Curac, ao by humans (either by Caquetio Indians or by European settlers) within the past 800 years. Further investigation is needed to determine if Quaternary Aruban Cerion warrant subspecific recognition. On the island of Curac, ao, molecular data lend support to the partition of the Cerion fauna into C. uva knipensis, which is confined to an isolated western region, as defined by Baker, and C. uva uva, which inhabits a broad, eastern region that is composed of Baker's central and eastern regions. A population at Ronde Klip in eastern Curac, ao has remained genetically isolated, and retains subspecific status as C. uva diablensis Baker, 1924. A neotype is designated for Turbo uva Linnaeus, 1758, as is necessary to provide an objective standard of reference for this species-group taxon, and for the genus-and family-level taxa based upon it. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20013 USA. RP Harasewych, MG (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, POB 37012,MRC 163, Washington, DC 20013 USA. EM harasewych@si.edu NR 52 TC 4 Z9 4 U1 1 U2 5 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0260-1230 EI 1464-3766 J9 J MOLLUS STUD JI J. Molluscan Stud. PD FEB PY 2015 VL 81 BP 66 EP 84 DI 10.1093/mollus/eyu062 PN 1 PG 19 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA CC0VE UT WOS:000350054900007 ER PT J AU Dominguez, J Aira, M Breinholt, JW Stojanovic, M James, SW Perez-Losada, M AF Dominguez, Jorge Aira, Manuel Breinholt, Jesse W. Stojanovic, Mirjana James, Samuel W. Perez-Losada, Marcos TI Underground evolution: New roots for the old tree of lumbricid earthworms SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article DE Earthworms; Lumbricidae; Bayesian divergence time analysis; Ancestral state reconstruction; Spermathecae; Endogeic ancestors ID SPECIES COMPLEX OLIGOCHAETA; NUCLEAR-DNA SEQUENCES; PHYLOGENETIC INFERENCE; SELECTION; MITOCHONDRIAL; CLITELLATA; DIVERSIFICATION; PARTHENOGENESIS; HORMOGASTRIDAE; BIOGEOGRAPHY AB Earthworms belonging to the family Lumbricidae are extremely abundant in terrestrial temperate regions. They affect soil properties and nutrient cycling, thus shaping plant community composition and aboveground food webs. Some lumbricids are also model organisms in ecology and toxicology. Despite the intense research efforts dedicated to lumbricids over the last 130 years, the evolutionary relationships and taxonomic classification of these organisms are still subject to great debate. Resolution of their systematics is hampered by the structural simplicity of the earthworm body plan and the existence of cryptic species. We sampled 160 earthworm specimens belonging to 84 lumbricid species (28 genera) and 22 Lumbricoidea outgroups, sequenced two nuclear genes, four mitochondrial genes and seven mitochondrial tRNAs and examined 22 morphological characters. We then applied a combination of phylogenetic methods to generate the first robust genus-level phylogeny of the Lumbricidae. Our results show that the current Lumbricidae classification and the underlying hypotheses of character evolution must be revised. Our chronogram suggests that lumbricids emerged in the Lower Cretaceous in the holarctic region and that their diversification has been driven by tectonic processes (e.g. Laurasia split) and geographical isolation. Our chronogram and character reconstruction analysis reveal that spermathecae number does not follow a gradual pattern of reduction and that parthenogenesis arose from sexual relatives multiple times in the group; the same analysis also indicates that both epigeic and anecic earthworms evolved from endogeic ancestors. These findings emphasize the strong and multiple changes to which morphological and ecological characters are subjected, challenging the hypothesis of character stasis in Lumbricidae. (C) 2014 Elsevier Inc. All rights reserved. C1 [Dominguez, Jorge; Aira, Manuel] Univ Vigo, Dept Ecol & Biol Anim, E-36310 Vigo, Spain. [Breinholt, Jesse W.] Univ Florida, Florida Museum Nat Hist, Gainesville, FL 32611 USA. [Stojanovic, Mirjana] Fac Sci, Inst Biol & Ecol, Kragujevac 34000, Serbia. [James, Samuel W.] Univ Iowa, Dept Biol, Iowa City, IA 52242 USA. [Perez-Losada, Marcos] Univ Porto, Ctr Invest Biodiversidade & Recursos Genet, CIBIO, P-4485661 Vairao, Portugal. [Perez-Losada, Marcos] George Washington Univ, Computat Biol Inst, Ashburn, VA 20147 USA. [Perez-Losada, Marcos] Smithsonian Inst, US Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20013 USA. RP Dominguez, J (reprint author), Univ Vigo, Dept Ecol & Biol Anim, E-36310 Vigo, Spain. EM jdguez@uvigo.es RI Dominguez, Jorge/M-2046-2014; Aira, Manuel/B-4506-2016; Perez-Losada, Marcos/I-4407-2013; OI Dominguez, Jorge/0000-0002-4313-8582; Aira, Manuel/0000-0002-2513-4609; Perez-Losada, Marcos/0000-0002-2585-4657; James, Samuel/0000-0001-6758-5726 FU Spanish Ministerio de Ciencia e Innovacion [CGL2006-11928, CTM2009-08477]; Xunta de Galicia [CN2012/305]; United States National Science Foundation [DEB-0516439]; FCT Investigator Program FX This research was funded by the Spanish Ministerio de Ciencia e Innovacion (projects CGL2006-11928 and CTM2009-08477), Xunta de Galicia (CN2012/305), the United States National Science Foundation Award DEB-0516439 (James) and a "Projeto de investigacao Exploratoria" from the FCT Investigator Program to MP-L. We gratefully acknowledge Grzegorz Gryziak, Konstantin Gongalsky, Jari Haimi, Martin Holmstrup, Mervi Niemen, Nicolas Bottinelli, Veikko Huhta, Pascal Jouquet, Sonja Migge-Kleian, Yvan Capowiez, Danuta Plisko, Marta Novo, Dario Diaz Cosin and Alexander Feijoo for generously providing earthworm samples. We also thank Maigualida Ricoy, Cristina Lazcano, Maria Gomez, Marta Lores, Cristobal Perez, Pablo Gonzalez and Fernando Monroy for collaborating in collecting earthworms to complete this study and Alberto Velando for critical discussions and helpful revisions of previous drafts of the manuscript. NR 82 TC 5 Z9 6 U1 5 U2 38 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 FEB PY 2015 VL 83 BP 7 EP 19 DI 10.1016/j.ympev.2014.10.024 PG 13 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA CC0EK UT WOS:000350008400002 PM 25463017 ER PT J AU Hailer, F James, HF Olson, SL Fleischer, RC AF Hailer, Frank James, Helen F. Olson, Storrs L. Fleischer, Robert C. TI Distinct and extinct: Genetic differentiation of the Hawaiian eagle SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article DE Ancient DNA; Bald eagle; Island endemic; Haliaeetus albicilla; Haliaeetus leucocephalus; mtDNA ID WHITE-TAILED EAGLE; MITOCHONDRIAL-DNA; GENUS HALIAEETUS; SEQUENCE DATA; SEA EAGLE; MTDNA; PHYLOGEOGRAPHY; PHYLOGENY; RADIATION; DIVERSITY AB Eagles currently occur in the Hawaiian Islands only as vagrants, but Quaternary bones of Haliaeetus eagles have been found on three of the major islands. A previous study of a similar to 3500-year-old skeleton from Maui found its mtDNA more similar to White-tailed (H. albicilla) than to Bald (H. leucocephalus) Eagles, but low intraspecific resolution of the markers and lack of comparative data from mainland populations precluded assessment of whether the individual was part of the diversity found in Eurasia, or whether it represented an endemic Hawaiian lineage. Using ancient DNA techniques, we sequenced part of the rapidly evolving mtDNA control region from the same specimen, and compared it to published range-wide control region data from White-tailed Eagles and newly generated sequences from Bald Eagles. Phylogenetic analyses indicated that the Hawaiian eagle represents a distinct (>3% divergent) mtDNA lineage most closely related to those of extant White-tailed Eagles. Based on fossil calibration, we estimate that the Hawaiian mtDNA lineage diverged from mainland sequences around the Middle Pleistocene. Although not clearly differentiated morphologically from mainland forms, the Hawaiian eagle thus likely constituted an isolated, resident population in the Hawaiian archipelago for more than 100,000 years, where it was the largest terrestrial predator. (C) 2014 Elsevier Inc. All rights reserved. C1 [Hailer, Frank; Fleischer, Robert C.] Smithsonian Conservat Biol Inst, Ctr Conservat & Evolutionary Genet, Washington, DC 20008 USA. [Hailer, Frank] Biodivers & Climate Res Ctr BiK F, Ecol Gen Senckenberg Gesell Nat Forsch, D-60325 Frankfurt, Germany. [James, Helen F.; Olson, Storrs L.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Div Birds, Washington, DC 20013 USA. RP Hailer, F (reprint author), Smithsonian Conservat Biol Inst, Ctr Conservat & Evolutionary Genet, Natl Zool Pk, Washington, DC 20008 USA. EM frashai@gmx.net; fleischerr@si.edu RI Hailer, Frank/C-9114-2012 OI Hailer, Frank/0000-0002-2340-1726 FU Smithsonian Restricted Endowment funds; Hesse's "LOEWE Landes-Offensive zur Entwicklung Wissenschaftlich-okonomischer Exzellenz"; Smithsonian Center for Conservation and Evolutionary Genetics; NSF [DEB-0643291] FX FH was supported by the Smithsonian Restricted Endowment funds and Hesse's "LOEWE Landes-Offensive zur Entwicklung Wissenschaftlich-okonomischer Exzellenz". The Smithsonian Center for Conservation and Evolutionary Genetics and NSF DEB-0643291 provided technical support and funding for lab supplies. We thank Michael W. Meyer and Walter H. Piper for kindly providing Bald Eagle samples, Nancy Rotzel McInerney for lab logistics support, Gerald Mayr for discussions, and two anonymous reviewers for their helpful comments. NR 28 TC 4 Z9 4 U1 1 U2 13 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 1055-7903 EI 1095-9513 J9 MOL PHYLOGENET EVOL JI Mol. Phylogenet. Evol. PD FEB PY 2015 VL 83 BP 40 EP 43 DI 10.1016/j.ympev.2014.11.005 PG 4 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA CC0EK UT WOS:000350008400005 PM 25463753 ER PT J AU Lemer, S Kawauchi, GY Andrade, SCS Gonzalez, VL Boyle, MJ Giribet, G AF Lemer, Sarah Kawauchi, Gisele Y. Andrade, Sonia C. S. Gonzalez, Vanessa L. Boyle, Michael J. Giribet, Gonzalo TI Re-evaluating the phylogeny of Sipuncula through transcriptomics SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article DE Annelida; Peanut worms; Phylogenomics; Systematics ID EVOLUTIONARY RELATIONSHIPS; DATA SETS; RNA-SEQ; THEMISTE-LAGENIFORMIS; MAXIMUM-LIKELIHOOD; PHYLUM SIPUNCULA; WORMS; INFERENCE; MODEL; LARVAE AB Sipunculans (also known as peanut worms) are an ancient group of exclusively marine worms with a global distribution and a fossil record that dates back to the Early Cambrian. The systematics of sipunculans, now considered a distinct subclade of Annelida, has been studied for decades using morphological and molecular characters, and has reached the limits of Sanger-based approaches. Here, we reevaluate their family-level phylogeny by comparative transcriptomic analysis of eight species representing all known families within Sipuncula. Two data matrices with alternative gene occupancy levels (large matrix with 675 genes and 62% missing data; reduced matrix with 141 genes and 23% missing data) were analysed using concatenation and gene-tree methods, yielding congruent results and resolving each internal node with maximum support. We thus corroborate prior phylogenetic work based on molecular data, resolve outstanding issues with respect to the familial relationships of Aspidosiphonidae, Antillesomatidae and Phascolosomatidae, and highlight the next area of focus for sipunculan systematics. (C) 2014 Elsevier Inc. All rights reserved. C1 [Lemer, Sarah; Kawauchi, Gisele Y.; Andrade, Sonia C. S.; Gonzalez, Vanessa L.; Giribet, Gonzalo] Harvard Univ, Dept Organism & Evolutionaly Biol, Museum Comparat Zool, Cambridge, MA 02138 USA. [Kawauchi, Gisele Y.] Univ Sao Paulo, CEBIMar, Sao Paulo, Brazil. [Andrade, Sonia C. S.] ESALQ USP, Dept Zootecnia, Sao Paulo, Brazil. [Gonzalez, Vanessa L.] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20013 USA. [Boyle, Michael J.] Smithsonian Trop Res Inst, Naos Marine Labs, Panama City 084303092, Panama. RP Lemer, S (reprint author), Harvard Univ, Dept Organism & Evolutionaly Biol, Museum Comparat Zool, 26 Oxford St, Cambridge, MA 02138 USA. EM sarah.lemer@gmail.com RI Giribet, Gonzalo/P-1086-2015; Andrade, Sonia/F-8267-2014 OI Giribet, Gonzalo/0000-0002-5467-8429; FU National Science Foundation, NSF [DEB-0844881]; NSF [DEB-0732903] FX Many colleagues have assisted with fieldwork, specimens, and laboratory protocols, especially Marta Novo for the Phascolopsis library. FedEx is acknowledged for the reliable delivery of live sipunculans for RNA work. Rosa Fernandez, Christopher Laumer and Horacio Montenegro assisted with analyses and scripts. The Bauer Core from the Faculty of Arts and Sciences at Harvard and the Research Computing Group, also from Harvard, are deeply acknowledged for their assistance at many stages of the data acquisition and analyses. We are grateful to Mary Rice for use of the Life Histories Laboratory at the Smithsonian Marine Station. The editor and two anonymous reviewers provided constructive criticism that helped to improve this article. This work was funded by the National Science Foundation, NSF #DEB-0844881 (Collaborative Research: Resolving old questions in Mollusc phylogenetics with new EST data and developing general phylogenomic tools) and NSF #DEB-0732903 (Collaborative Research: AToL: Phylogeny on the half-shell-Assembling the Bivalve Tree of Life) to G.G. This publication is Smithsonian Marine Station contribution no. 965. NR 98 TC 13 Z9 13 U1 5 U2 27 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 FEB PY 2015 VL 83 BP 174 EP 183 DI 10.1016/j.ympev.2014.10.019 PG 10 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA CC0EK UT WOS:000350008400016 PM 25450098 ER PT J AU Carvalho, M Vari, RP AF Carvalho, Murilo Vari, Richard P. TI Development of the splanchnocranium in Prochilodus argenteus (Teleostei: Characiformes) with a discussion of the basal developmental patterns in the Otophysi SO ZOOLOGY LA English DT Article DE Actinopterygii; Ostariophysi; Splanchnocranium; Comparative morphology; Ontogeny ID EARLY-STAGE LARVAE; OSTEOLOGICAL DEVELOPMENT; CEPHALIC SKELETON; PHYLOGENETIC-RELATIONSHIPS; ENDOCHONDRAL OSSIFICATION; POSTEMBRYONIC DEVELOPMENT; INTRASPECIFIC VARIATION; CYPRINIFORM FISHES; FEEDING APPARATUS; ARCH SKELETON AB Development of the mandibular, hyoid and gill arches, which constitute the splanchnocranium, are described for Prochilodus argenteus, order Characiformes, one of the basal lineages of the Otophysi. Development was examined from just hatched larvae through juveniles using whole specimens cleared and counterstained for cartilage and bone as well as histological preparations. Observations are compared with the developmental trends reported for Cypriniformes, the basalmost clade of the Otophysi. Shortened developmental sequences for Prochilodus compared to the cypriniform Catostomus were discovered in the ontogeny of the ceratohyals, ceratobranchials 1-5, epibranchials 1-4 and the symplectic portion of the hyosymplectic. Prochilodus also differs from Catostomus in having the basihyal plus the anterior copula appearing at different stages of ontogeny rather than simultaneously. Contrary to previous assumptions, developmental information indicates that hypobranchial 4 as well as likely basibranchial 5 are present in Prochilodus. Various developmental patterns in Prochilodus considered basal for the Otophysi, the predominant component of the Ostariophysi, are likely conserved from patterns prevalent in basal groups in the Actinopterygii. (C) 2014 Elsevier GmbH. All rights reserved. C1 [Carvalho, Murilo] Univ Sao Paulo, Dept Biol, Lab Ictiol Ribeirao Preto LIRP, PPG Biol Comparada, BR-14040901 Sao Paulo, Brazil. [Vari, Richard P.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20013 USA. RP Carvalho, M (reprint author), Univ Sao Paulo, Inst Biociencias, Dept Zool, Lab Ictiol, Rua Matao,Travessa 14 101, BR-05508900 Sao Paulo, SP, Brazil. EM mcarvalho79@gmail.com OI Carvalho, Murilo/0000-0001-6881-5271 FU Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPq) [140415/2006-8]; Fundacao de Amparo a Pesquisa do Estado de Sao Paulo (FAPESP) [2012/05152-0]; National Science Foundation [DEB-1257898] FX Special thanks to Yoshimi Sato who reared and collected the developmental series at the larviculture laboratory, Hydrobiology and Hatchery Station at Tres Marias - CODEVASF. We thank Vani M.A. Correa, Laboratory of Histotechnology, Department of Cellular and Molecular Biology of Pathogenic Bioagents, who helped with histological preparations; Paulo Tambasco de Oliveira, Department of Morphology, Stomatology and Physiology, Faculty of Dentistry of Ribeirao Preto, who greatly assisted with interpreting histological sections and the identification of cell types; Maria Isabel P. A. Balbi and Dalton S. Amorim for sharing and assisting with image capturing equipment; and Nair S. de Oliveira (Biblioteca Central de Ribeirao Preto, USP) and the librarians of the Programa de Comutacao Bibliografica (COMUT) who located critical references. Mario C. C. de Pinna and Osvaldo T. Oyakawa (MZUSP) provided access to material. MC is deeply indebted to Flavio Bockmann who encouraged this project. Thanks to Marcelo R. de Carvalho and Jose Xavier-Neto for suggestions on the manuscript. G. Arratia and two anonymous reviewers provided very valuable comments on an earlier draft of the paper. Funding for this study was provided by the Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPq, 140415/2006-8) and Fundacao de Amparo a Pesquisa do Estado de Sao Paulo (FAPESP, 2012/05152-0) to M.C., and by the National Science Foundation (DEB-1257898) to R.P.V. NR 68 TC 3 Z9 3 U1 0 U2 6 PU ELSEVIER GMBH, URBAN & FISCHER VERLAG PI JENA PA OFFICE JENA, P O BOX 100537, 07705 JENA, GERMANY SN 0944-2006 J9 ZOOLOGY JI Zoology PD FEB PY 2015 VL 118 IS 1 BP 34 EP 50 DI 10.1016/j.zool.2014.10.002 PG 17 WC Zoology SC Zoology GA CC2OR UT WOS:000350185000005 PM 25595854 ER PT J AU Xu, XW Wu, JW Qi, MX Lu, QX Lee, PF Lutz, S Ge, S Wen, J AF Xu, Xin-Wei Wu, Jin-Wei Qi, Mei-Xia Lu, Qi-Xiang Lee, Peter F. Lutz, Sue Ge, Song Wen, Jun TI COMPARATIVE PHYLOGEOGRAPHY OF THE WILD-RICE GENUS ZIZANIA (POACEAE) IN EASTERN ASIA AND NORTH AMERICA SO AMERICAN JOURNAL OF BOTANY LA English DT Article DE cpDNA; eastern Asia; intercontinental disjunction; microsatellite; North America; phylogeography; Zizania ID MOLECULAR EVOLUTION; SPECIES-DIVERSITY; GENETIC DIVERSITY; FLOWERING PLANTS; COLONIZATION; POPULATIONS; SEQUENCES; SOFTWARE; HISTORY; TEXANA AB Premise of the study: Comparative phylogeography of intercontinental disjunct taxa allowed us not only to elucidate their diversification and evolution following geographic isolation, but also to understand the effect of climatic and geological histories on the evolutionary processes of closely related species. A phylogeographic analysis was conducted on the eastern Asian-North American disjunct genus Zizania to compare intracontinental phylogeographic patterns between different continents. Methods: Surveys were conducted of 514 individuals using three chloroplast DNA fragments and three nuclear microsatellite loci. These individuals included 246 from 45 populations of Zizania latifolia in eastern Asia, and the following from North America: 154 individuals from 26 populations of Z. aquatica, 84 individuals from 14 populations of Z. palustris, and 30 individuals from one population of Z. texana. Key results: The genetic diversity of North American Zizania was significantly higher than that of eastern Asian Zizania. High levels of genetic differentiation among populations and no signal of population expansion were detected in three widespread species. No phylogeographic structure was observed in Zizania latifolia, and discordant patterns of cpDNA and microsatellite markers were observed in North American Zizania. Conclusions: Reduced variation in Zizania latifolia likely reflects its perennial life history, the North American origin of Zizania, and the relative homogeneity of aquatic environments. High levels of genetic differentiation suggest limited dispersal among populations in all Zizania species. The more complex patterns of diversification and evolution in North American Zizania may be driven by the greater impact of glaciation in North America relative to eastern Asia. C1 [Xu, Xin-Wei; Wu, Jin-Wei; Qi, Mei-Xia; Lu, Qi-Xiang] Wuhan Univ, Coll Life Sci, Natl Field Stn Freshwater Ecosyst Liangzi Lake, Wuhan 430072, Peoples R China. [Lee, Peter F.] Lakehead Univ, Dept Biol, Thunder Bay, ON P7B 5E1, Canada. [Lutz, Sue; Wen, Jun] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA. [Ge, Song] Chinese Acad Sci, Inst Bot, State Key Lab Systemat & Evolutionary Bot, Beijing 100093, Peoples R China. RP Xu, XW (reprint author), Wuhan Univ, Coll Life Sci, Natl Field Stn Freshwater Ecosyst Liangzi Lake, Wuhan 430072, Peoples R China. EM xuxw@whu.edu.cn; wenj@si.edu FU National Natural Science Foundation of China [31070190, 31270265]; Laboratory of Analytical Biology of the Smithsonian Institution FX This study was supported by grants from the National Natural Science Foundation of China (31070190 and 31270265) to X.-W. Xu and from the Laboratory of Analytical Biology of the Smithsonian Institution. The authors thank the members of Dan Yu's group, D. Cohen and S. Orr for field assistance, and M. L. Alexander, M. Hunter, S. Steneck, and A. Soejima for providing samples. We also thank J. Jernstedt, J. Freudenstein, and two anonymous reviewers for their comments on the manuscript. NR 59 TC 1 Z9 1 U1 8 U2 48 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 FEB PY 2015 VL 102 IS 2 BP 239 EP 247 DI 10.3732/ajb.1400323 PG 9 WC Plant Sciences SC Plant Sciences GA CB3PF UT WOS:000349539800009 PM 25667077 ER PT J AU Martinez, C Carvalho, MR Madrinan, S Jaramillo, CA AF Martinez, Camila Carvalho, Monica R. Madrinan, Santiago Jaramillo, Carlos A. TI A LATE CRETACEOUS PIPER (PIPERACEAE) FROM COLOMBIA AND DIVERSIFICATION PATTERNS FOR THE GENUS SO AMERICAN JOURNAL OF BOTANY LA English DT Article DE Colombia; dated phylogeny; fossil leaves; Guaduas Formation; Late Cretaceous; paleobotany; Piper; Piperaceae; radiation ID NEOTROPICAL RAIN-FOREST; SPECIES-RICH GENUS; PEPEROMIA PIPERACEAE; SOUTH-AMERICA; CERREJON FORMATION; BASAL ANGIOSPERMS; MOLECULAR CLOCK; LATE PALEOCENE; EVOLUTION; PHYLOGENY AB Premise of the study: Documented fossil floras in the neotropics are sparse, yet their records provide evidence on the spatial and temporal occurrence of taxa, allowing for testing of biogeographical and diversification scenarios on individual lineages. A new fossil Piper from the Late Cretaceous of Colombia is described here, and its importance for assessing diversification patterns in the genus is addressed. Methods: Leaf architecture of 32 fossil leaf compressions from the Guaduas Formation was compared with that of 294 extant angiosperm species. The phylogenetic position of the fossil named Piper margaritae sp. nov. was established based on leaf traits and a molecular scaffold of Piper. The age of the fossil was independently used as a calibration point for divergence time estimations. Key results: Natural affinities of Piper margaritae to the Schilleria clade of Piper indicate that the genus occurred in tropical America by the Late Cretaceous. Estimates of age divergence and lineage accumulation reveal that most of the extant diversity of the genus accrued during the last similar to 30 Myr. Conclusions: The recent radiation of Piper is coeval with both the Andean uplift and the emergence of Central America, which have been proposed as important drivers of diversity. This pattern could exemplify a recurrent theme among many neotropical plant lineages. C1 [Martinez, Camila; Madrinan, Santiago] Univ Los Andes, Lab Bot & Sistemat, Bogota, Colombia. [Martinez, Camila; Carvalho, Monica R.; Jaramillo, Carlos A.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Martinez, Camila; Carvalho, Monica R.] Cornell Univ, Dept Plant Biol, LH Bailey Hortorium, Ithaca, NY 14850 USA. RP Martinez, C (reprint author), Univ Los Andes, Lab Bot & Sistemat, Apartado Aereo 4976, Bogota, Colombia. EM camilamartineza@gmail.com FU Jose Cuatrecasas Fellowship Award from The Smithsonian Institution; Faculty of Sciences research seed grant from Universidad de los Andes; University of Missouri-Columbia; Yale University Edward P. Bass Distinguished Visiting Environmental Scholarship; Fulbright-Colciencias Fellowship; Schlumberger Faculty for the Future Foundation FX The authors thank M. Gutierrez who collected the fossils, R. Callejas for valuable collaboration during the study, S. Wing who was the first to suggest the taxonomic affinity of the fossil, and F. Herrera for reviewing the manuscript. They are grateful to the staff of US, NCLC-W, HUA, and COL for access to their collections. This project was supported by a Jose Cuatrecasas Fellowship Award from The Smithsonian Institution and a Faculty of Sciences research seed grant from the Universidad de los Andes to C.M.; the University of Missouri-Columbia provided research funds through A. Jaramillo to C.M. in an early stage of this project; the Yale University Edward P. Bass Distinguished Visiting Environmental Scholarship to C.A.J. C.M. is supported by a Fulbright-Colciencias Fellowship and M.R.C. is supported by the Schlumberger Faculty for the Future Foundation. NR 94 TC 0 Z9 0 U1 3 U2 17 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 FEB PY 2015 VL 102 IS 2 BP 273 EP 289 DI 10.3732/ajb.1400427 PG 17 WC Plant Sciences SC Plant Sciences GA CB3PF UT WOS:000349539800012 PM 25667080 ER PT J AU Mikolajewska, J Caldwell, N Shara, MM Ilkiewicz, K AF Mikolajewska, Joanna Caldwell, Nelson Shara, Michael M. Ilkiewicz, Krystian TI CHARACTERIZATION OF THE MOST LUMINOUS STAR IN M33: A SUPER SYMBIOTIC BINARY SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE binaries: symbiotic; galaxies: individual (M33); H II regions; stars: evolution; stars: massive ID LARGE-MAGELLANIC-CLOUD; MASSIVE STARS; ULTRAVIOLET EXTINCTION; INFRARED PHOTOMETRY; IIN SUPERNOVAE; SPITZER; PROGENITORS; TRANSIENTS; CATALOG; CENSUS AB We present the first spectrum of the most luminous infrared star in M33, and use it to demonstrate that the object is almost certainly a binary composed of a massive O star and a dust-enshrouded red hypergiant. This is the most luminous symbiotic binary ever discovered. Its radial velocity is an excellent match to that of the hydrogen gas in the disk of M33, supporting our interpretation that it is a very young and massive binary star. C1 [Mikolajewska, Joanna; Ilkiewicz, Krystian] Nicholas Copernicus Astron Ctr, PL-00716 Warsaw, Poland. [Caldwell, Nelson] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Shara, Michael M.] Amer Museum Nat Hist, Dept Astrophys, New York, NY 10024 USA. [Ilkiewicz, Krystian] Univ Warsaw Observ, PL-00478 Warsaw, Poland. RP Mikolajewska, J (reprint author), Nicholas Copernicus Astron Ctr, Bartycka 18, PL-00716 Warsaw, Poland. EM mikolaj@camk.edu.pl OI Mikolajewska, Joanna/0000-0003-3457-0020 FU Polish NCN [DEC-2013/10/M/ST9/00086]; Canadian Space Agency FX This study has been supported in part by the Polish NCN grant DEC-2013/10/M/ST9/00086. We gratefully acknowledge the fine support at the MMT Observatory and The Local Group Galaxy Survey conducted at NOAO by Phil Massey and collaborators. This research used the facilities of the Canadian Astronomy Data Center operated by the National Research Council of Canada with the support of the Canadian Space Agency. We thank Michael Schwartz and Paulo Holvorcem for support in obtaining recent Tenagra images of Object X, and Dave Zurek for support in accessing the LGGS archival images. We also thank Scott Kenyon for pointing out the similarity between Object X and the VV Cep stars. NR 25 TC 2 Z9 2 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD FEB 1 PY 2015 VL 799 IS 2 AR L16 DI 10.1088/2041-8205/799/2/L16 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CB0KS UT WOS:000349315400002 ER PT J AU Tanaka, YT Doi, A Inoue, Y Cheung, CC Stawarz, L Fukazawa, Y Gurwell, MA Tahara, M Kataoka, J Itoh, R AF Tanaka, Y. T. Doi, A. Inoue, Y. Cheung, C. C. Stawarz, L. Fukazawa, Y. Gurwell, M. A. Tahara, M. Kataoka, J. Itoh, R. TI SIX YEARS OF FERMI-LAT AND MULTI-WAVELENGTH MONITORING OF THE BROAD-LINE RADIO GALAXY 3C 120: JET DISSIPATION AT SUB-PARSEC SCALES FROM THE CENTRAL ENGINE SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: active; galaxies: individual (3C 120); galaxies: jets; radiation mechanisms: non-thermal; radio continuum: galaxies; gamma-rays: galaxies ID ACTIVE GALACTIC NUCLEI; GAMMA-RAY EMISSION; RELATIVISTIC JETS; BLACK-HOLE; ACCRETION DISKS; ORIGIN; POWER; VARIABILITY; CONNECTION; LUMINOSITY AB We present multi-wavelength monitoring results for the broad-line radio galaxy 3C 120 in the MeV/GeV, sub-millimeter, and 43 GHz bands over 6 yr. Over the past 2 yr, the Fermi-Large Area Telescope sporadically detected 3C 120 with high significance and the 230 GHz data also suggest an enhanced activity of the source. After the MeV/GeV detection from 3C 120 in MJD 56240-56300, 43 GHz Very Long Baseline Array (VLBA) monitoring revealed a brightening of the radio core, followed by the ejection of a superluminal knot. Since we observed the gamma-ray and VLBA phenomena in temporal proximity to each other, it is naturally assumed that they are physically connected. This assumption was further supported by the subsequent observation that the 43 GHz core brightened again after a gamma-ray flare occurred around MJD 56560. We can then infer that the MeV/GeV emission took place inside an unresolved 43 GHz core of 3C 120 and that the jet dissipation occurred at sub-parsec distances from the central black hole (BH), if we take the distance of the 43 GHz core from the central BH as similar to 0.5 pc, as previously estimated from the time lag between X-ray dips and knot ejections. Based on our constraints on the relative locations of the emission regions and energetic arguments, we conclude that the gamma rays are more favorably produced via the synchrotron self-Compton process, rather than inverse Compton scattering of external photons coming from the broad line region or hot dusty torus. We also derived the electron distribution and magnetic field by modeling the simultaneous broadband spectrum. C1 [Tanaka, Y. T.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Higashihiroshima 7398526, Japan. [Doi, A.; Inoue, Y.; Stawarz, L.] JAXA, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2525210, Japan. [Cheung, C. C.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA. [Stawarz, L.] Jagiellonian Univ, Astron Observ, PL-30244 Krakow, Poland. [Fukazawa, Y.; Itoh, R.] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan. [Gurwell, M. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Tahara, M.; Kataoka, J.] Waseda Univ, Res Inst Sci & Engn, Tokyo 1698555, Japan. RP Tanaka, YT (reprint author), Hiroshima Univ, Hiroshima Astrophys Sci Ctr, 1-3-1 Kagamiyama, Higashihiroshima 7398526, Japan. EM ytanaka@hep01.hepl.hiroshima-u.ac.jp OI Inoue, Yoshiyuki/0000-0002-7272-1136 FU NASA; DOE (United States); CEA/Irfu; IN2P3/CNRS (France); ASI; INFN (Italy); MEXT (Japan); KEK (Japan); JAXA (Japan); K. A. Wallenberg Foundation; Swedish Research Council; National Space Board (Sweden); INAF (Italy); CNES (France); NASA through the Fermi-LAT Guest Investigator Program; Smithsonian Institution; Academia Sinica; NASA DPR [S-15633]; Polish NSC [DEC-2012/04/A/ST9/00083] FX The Fermi-LAT Collaboration acknowledges support for LAT development, operation, and data analysis from NASA and DOE (United States), CEA/Irfu, and IN2P3/CNRS (France), ASI and INFN (Italy), MEXT, KEK, and JAXA (Japan), and the K. A. Wallenberg Foundation, the Swedish Research Council and the National Space Board (Sweden). Science analysis support in the operations phase from INAF (Italy) and CNES (France) is also gratefully acknowledged. This study makes use of 43 GHz VLBA data from the VLBA-BU Blazar Monitoring Program (VLBA-BU-BLAZAR; http://www.bu.edu/blazars/VLBAproject.html), funded by NASA through the Fermi-LAT Guest Investigator Program. The VLBA is an instrument of the National Radio Astronomy Observatory, a facility of the National Science Foundation operated by Associated Universities, Inc. 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. C.C.C. was supported at NRL by NASA DPR S-15633 Y.L.S. was supported by Polish NSC grant DEC-2012/04/A/ST9/00083. NR 32 TC 7 Z9 7 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD FEB 1 PY 2015 VL 799 IS 2 AR L18 DI 10.1088/2041-8205/799/2/L18 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CB0KS UT WOS:000349315400004 ER PT J AU Yan, H Soon, W Wang, YH AF Yan, Hong Soon, Willie Wang, Yuhong TI A composite sea surface temperature record of the northern South China Sea for the past 2500 years: A unique look into seasonality and seasonal climate changes during warm and cold periods SO EARTH-SCIENCE REVIEWS LA English DT Article DE South China Sea; Coral; Tridacna gigas; Sea surface temperature; Seasonal climate; Late Holocene ID ASIAN WINTER MONSOON; CORAL DELTA-O-18 RECORDS; TRIDACNA-GIGAS BIVALVES; GREAT-BARRIER-REEF; MID-LATE HOLOCENE; PALEOCLIMATIC IMPLICATIONS; GLACIER FLUCTUATIONS; SUMMER TEMPERATURES; ARCTICA-ISLANDICA; LEIZHOU PENINSULA AB High-resolution late Holocene climate records that can resolve seasonality are essential for confirming past climatic dynamics, understanding the late 20th century global warming and predicting future climate. Here a new composite record of the sea surface temperature, SST, variation in the northern South China Sea (SCS) during the late Holocene is constructed by combining seven seasonally-resolved coral and Tridacna gigas Sr/Ca-based SST time-windows with the instrumental SST record from modern interval between 1990 and 2000. This composite multi-proxy marine record, together with the reconstructions from mainland China and tropical Western Pacific, indicates that the late Holocene warm periods, the Roman Warm Period (RWP) and Medieval Warm Period (MWP), were prominently imprinted and documented in the climatic and environmental history of the East Asia-Western Pacific region. Meanwhile, substantial and significant SST seasonality variations during the late Holocene were observed in the composite record. The observed increase in seasonality (or amplitude of seasonal cycles) during the cold periods around our study area was probably caused by the different amplitudes between winter versus summer SST variations in northern SCS, with much larger SST variation during winters than during summers for the late Holocene. In addition, the distinctive warm, cold and neutral climatic episodes identified in our northern SCS composite SST record correspond well with other paleo reconstructions from mainland China and especially well with the Northern Hemisphere-wide composites by Moberg et al. (2005) and Ljungqvist (2010). The overall agreement however also calls for more information and insights on how seasonal temperatures and their ranges vary on decadal-centennial timescales. (C) 2014 Elsevier B.V. All rights reserved. C1 [Yan, Hong] Chinese Acad Sci, Inst Earth Environm, State Key Lab Loess & Quaternary Geol, Xian 710075, Peoples R China. [Soon, Willie] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Wang, Yuhong] Fudan Univ, Dept Chem, Shanghai 200433, Peoples R China. [Wang, Yuhong] Fudan Univ, Laser Chem Inst, Shanghai 200433, Peoples R China. RP Yan, H (reprint author), Chinese Acad Sci, Inst Earth Environm, State Key Lab Loess & Quaternary Geol, Xian 710075, Peoples R China. EM yanhong@ieecas.cn FU Natural Science Foundation of China (NSFC) [41403018]; Major State Basic Research Development Program of China (973 Program) [2013CB955900]; West Light Foundation of The Chinese Academy of Sciences [29Y42909101]; Key Programs of the Chinese Academy of Sciences [55ZZBS1304101] FX Financial support for this research was provided by the Natural Science Foundation of China (NSFC) (41403018), Major State Basic Research Development Program of China (973 Program) (2013CB955900), the West Light Foundation of The Chinese Academy of Sciences (29Y42909101) and the Key Programs of the Chinese Academy of Sciences (55ZZBS1304101). We are grateful to Professor Kefu Yu and Gangjian Wei for the constructive comments on earlier versions of the manuscript, as well as useful comments from the editor and three anonymous reviewers. NR 89 TC 10 Z9 10 U1 12 U2 65 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0012-8252 EI 1872-6828 J9 EARTH-SCI REV JI Earth-Sci. Rev. PD FEB PY 2015 VL 141 BP 122 EP 135 DI 10.1016/j.earscirev.2014.12.003 PG 14 WC Geosciences, Multidisciplinary SC Geology GA CB4GL UT WOS:000349586100007 ER PT J AU Castillo-Cardenas, MF Diaz-Gonzales, F Ceron-Souza, I Sanjur, O Toro-Perea, N AF Fernanda Castillo-Cardenas, Maria Diaz-Gonzales, Fernando Ceron-Souza, Ivania Sanjur, Oris Toro-Perea, Nelson TI Jumping a geographic barrier: diversification of the mangrove species Pelliciera rhizophorae (Tetrameristaceae) across the Central American Isthmus SO TREE GENETICS & GENOMES LA English DT Article DE Central American Isthmus; Chloroplast DNA; Microsatellite; Neotropical mangroves; Pelliciera rhizophorae; Phylogeographic structure ID POPULATION-STRUCTURE; GENETIC-STRUCTURE; GLOBAL PHYLOGEOGRAPHY; MITOCHONDRIAL-DNA; CARIBBEAN COAST; OCEAN CURRENTS; LAND BARRIERS; DISPERSAL; SEA; DIFFERENTIATION AB The Central American Isthmus (CAI) is an important geographic barrier in the Neotropics. Its role in the diversification of marine and coastal species has been detected in fishes, turtles, sea urchins, and mangroves. We evaluated the CAI's influence on the diversification of the most ancient neotropical mangrove species Pelliciera rhizophorae across populations from the Caribbean and Pacific coasts, based on the analysis of ten nuclear microsatellite loci and two noncoding chloroplast DNA regions. The two molecular markers showed concordant patterns of diversification in this mangrove species. Contrary to our expectations, this study did not reveal significant genetic structure among populations separated by the CAI. Two major genetic variants (cluster I and cluster II) were found on both coasts, but the two were not found intermixed in the same population. Within each coastal region, breaking of gene flow among populations was found at two points in the Pacific Basin and one point in the Caribbean Basin, separating the Colombian and Panamanian populations. Our study revealed a transisthmian connection among populations of P. rhizophorae. This result, together with the reduced genetic diversity in the Caribbean reported in our previous study, suggests the recent origin of these populations, probably due to reintroduction of P. rhizophorae from the Pacific coast. Taking into account that these introductions are random events, this study raises a new question: Why are genetic variants not intermixed within the Caribbean populations? Our hypotheses suggest the influence of environmental factors and/or anthropogenic impact on the establishment of these Caribbean patches. C1 [Fernanda Castillo-Cardenas, Maria; Sanjur, Oris] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Diaz-Gonzales, Fernando; Toro-Perea, Nelson] Univ Valle, Dept Biol, Cali, Colombia. [Ceron-Souza, Ivania] Oregon State Univ, Dept Bot & Plant Pathol, Corvallis, OR 97331 USA. RP Castillo-Cardenas, MF (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Ancon, Panama. EM mfcastillo@gmail.com RI Diaz, Fernando/I-6209-2016 FU International Foundation for Science (IFS) [D-3238]; Smithsonian Tropical Research Institute (STRI) FX We are grateful to Universidad del Valle (Colombia) for institutional support, to the International Foundation for Science (IFS) for financial support, grant no. D-3238, and to Smithsonian Tropical Research Institute (STRI) in Panama for logistical and financial support in field and laboratory work. For collaboration in field work, we are grateful to "Molecular Biology and Ecogenetic Studies Team" (Universidad del Valle) in Colombia, Biol. O. Lopez (STRI) in Panama, Ing. A. Bodero and Ing. AC. Ceballos in Ecuador, Lianna Mora and Biol. Albert Rojas from Organizacion de Estudios Tropicales (OTS) in Costa Rica. NR 72 TC 0 Z9 0 U1 0 U2 11 PU SPRINGER HEIDELBERG PI HEIDELBERG PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY SN 1614-2942 EI 1614-2950 J9 TREE GENET GENOMES JI Tree Genet. Genomes PD FEB PY 2015 VL 11 IS 1 AR 822 DI 10.1007/s11295-014-0822-1 PG 11 WC Forestry; Genetics & Heredity; Horticulture SC Forestry; Genetics & Heredity; Agriculture GA CB3UD UT WOS:000349553500042 ER PT J AU Guan, TP Wang, F Li, S McShea, WJ AF Guan, Tianpei Wang, Fang Li, Sheng McShea, William J. TI Nature reserve requirements for landscape-dependent ungulates: The case of endangered takin (Budorcas taxicolor) in Southwestern China SO BIOLOGICAL CONSERVATION LA English DT Article DE Species distribution models; Large herbivores; Autologistic regression; Conservation strategy; Habitat suitability map; Protected area network ID GIANT PANDAS; QINLING MOUNTAINS; PROTECTED AREAS; LARGE HERBIVORE; GOLDEN TAKIN; SPATIAL AUTOCORRELATION; PLANT PHENOLOGY; LARGE MAMMALS; CONSERVATION; MIGRATION AB Large ungulates commonly perform seasonal or annual movements that encompass considerable land area and various habitat types. Effective conservation of these species relies not only on insights on their basic ecology, but also an understanding on their requirements to move across landscapes. To determine the key landscape characteristics of the endangered takin (Budorcas taxicolor), we systematically surveyed for their occurrence in the Northern MinShan Mountains, China, during 2010-2011. We then modeled takin distribution at a regional scale using autologistic regression models, and produced a predictive map for their distribution. The results showed that occurrence probabilities for takin were higher in areas with a larger range of elevation, closer to protected areas, farther from townships, and with more forest coverage. There was a considerable overlap between highly suitable takin habitat and the network of protected forest formed by nature reserves originally established to conserve giant panda (Ailuropoda melanoleuca). A broad elevation gradient and the protected area network were essential landscape characteristics in predicting takin distributions and our results suggested that takin should be considered landscape- and conservation-dependent species. The results of this study are applicable to the conservation of large ungulates throughout the mountains bordering the Tibetan Plateau and to a broader suite of mammals that conduct seasonal migrations. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Guan, Tianpei] Mianyang Normal Univ, Ecol Secur & Protect Key Lab Sichuan Prov, Mianyang 621000, Peoples R China. [Wang, Fang; McShea, William J.] Natl Zool Pk, Smithsonian Conservat Biol Inst, Conservat Ecol Ctr, Front Royal, VA 22630 USA. [Wang, Fang; Li, Sheng] Peking Univ, Sch Life Sci, Beijing 100871, Peoples R China. RP Li, S (reprint author), Peking Univ, Sch Life Sci, 5 Yiheyuan RD, Beijing 100871, Peoples R China. EM shengli@pku.edu.cn FU Mohamed bin Zayed Species Conservation Fund; Friends of the National Zoo; National Geographic Society; National Natural Science Foundation of China [31300319]; Mianyang Normal University [QD2012A12b] FX We thank Dr. Gong Minghao, Dr. Gu Xiaodong, Mr. Qiu Jian, Mr. Dai Bo for contacting local administrations to support these field surveys. We appreciate great help from Sichuan Forestry Department, World Wildlife Fund, Tangjiahe National Nature reserve, Wanglang National Nature reserve, Baishuijiang National Nature reserve for providing monitor records on takin and assisting field survey. This study was supported by Mohamed bin Zayed Species Conservation Fund, Friends of the National Zoo, National Geographic Society, National Natural Science Foundation of China (31300319), and Mianyang Normal University (QD2012A12b). NR 63 TC 2 Z9 3 U1 7 U2 43 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0006-3207 EI 1873-2917 J9 BIOL CONSERV JI Biol. Conserv. PD FEB PY 2015 VL 182 BP 63 EP 71 DI 10.1016/j.biocon.2014.11.041 PG 9 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA CB3AY UT WOS:000349501400009 ER PT J AU Turner, W Rondinini, C Pettorelli, N Mora, B Leidner, AK Szantoi, Z Buchanan, G Dech, S Dwyer, J Herold, M Koh, LP Leimgruber, P Taubenboeck, H Wegmann, M Wikelski, M Woodcock, C AF Turner, W. Rondinini, C. Pettorelli, N. Mora, B. Leidner, A. K. Szantoi, Z. Buchanan, G. Dech, S. Dwyer, J. Herold, M. Koh, L. P. Leimgruber, P. Taubenboeck, H. Wegmann, M. Wikelski, M. Woodcock, C. TI Free and open-access satellite data are key to biodiversity conservation SO BIOLOGICAL CONSERVATION LA English DT Article DE Satellite; Remote sensing; Biodiversity; Conservation; Monitoring; Landsat ID LANDSAT IMAGERY; COVER CHANGE; SCIENCE; OPPORTUNITIES; CHALLENGES; SUPPORT; SYSTEM AB Satellite remote sensing is an important tool for monitoring the status of biodiversity and associated environmental parameters, including certain elements of habitats. However, satellite data are currently underused within the biodiversity research and conservation communities. Three factors have significant impact on the utility of remote sensing data for tracking and understanding biodiversity change. They are its continuity, affordability, and access. Data continuity relates to the maintenance of long-term satellite data products. Such products promote knowledge of how biodiversity has changed over time and why. Data affordability arises from the cost of the imagery. New data policies promoting free and open access to government satellite imagery are expanding the use of certain imagery but the number of free and open data sets remains too limited. Data access addresses the ability of conservation biologists and biodiversity researchers to discover, retrieve, manipulate, and extract value from satellite imagery as well as link it with other types of information. Tools are rapidly improving access. Still, more cross-community interactions are necessary to strengthen ties between the biodiversity and remote sensing communities. (C) 2014 Published by Elsevier Ltd. C1 [Turner, W.; Leidner, A. K.] NASA Headquarters, Div Earth Sci, Washington, DC 20546 USA. [Rondinini, C.] Univ Roma La Sapienza, Dept Biol & Biotechnol, Rome, Italy. [Pettorelli, N.] Zool Soc London, Inst Zool, London, England. [Mora, B.; Herold, M.] GOFC GOLD Land Cover Off, Wageningen, Netherlands. [Leidner, A. K.] Univ Space Res Assoc, Houston, TX USA. [Szantoi, Z.] European Commiss, Joint Res Ctr, Inst Environm & Sustainabil, Land Resources Management Unit, Ispra, Italy. [Buchanan, G.] Royal Soc Protect Birds, Ctr Conservat Sci, Sandy, Beds, England. [Dech, S.; Taubenboeck, H.] German Aerosp Ctr DLR, German Remote Sensing Data Ctr, Cologne, Germany. [Dwyer, J.] US Geol Survey, Earth Resources Observat & Sci Ctr, Reston, VA USA. [Koh, L. P.] Univ Adelaide, Inst Environm, Adelaide, SA 5005, Australia. [Leimgruber, P.] Natl Zool Pk, Smithsonian Conservat Biol Inst, Washington, DC 20008 USA. [Wegmann, M.] Univ Wurzburg, German Aerosp Ctr DLR, CEOS Biodivers German Remote Sensing Data Ctr, Wurzburg, Germany. [Wegmann, M.] Univ Wurzburg, Dept Remote Sensing, Wurzburg, Germany. [Wikelski, M.] Univ Konstanz, Max Planck Inst Ornithol, Constance, Germany. [Wikelski, M.] Univ Konstanz, Dept Biol, Constance, Germany. [Woodcock, C.] Boston Univ, Dept Earth & Environm, Boston, MA 02215 USA. RP Turner, W (reprint author), NASA Headquarters, Div Earth Sci, Washington, DC 20546 USA. EM woody.turner@nasa.gov RI Koh, Lian Pin/A-5794-2010; Trivedi, Kruti/E-7558-2015; Herold, Martin/F-8553-2012; Leimgruber, Peter/O-1304-2015; OI Koh, Lian Pin/0000-0001-8152-3871; Herold, Martin/0000-0003-0246-6886; Leimgruber, Peter/0000-0002-3682-0153; Dwyer, John/0000-0002-8281-0896; Szantoi, Zoltan/0000-0003-2580-4382 NR 25 TC 26 Z9 30 U1 6 U2 33 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0006-3207 EI 1873-2917 J9 BIOL CONSERV JI Biol. Conserv. PD FEB PY 2015 VL 182 BP 173 EP 176 DI 10.1016/j.biocon.2014.11.048 PG 4 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA CB3AY UT WOS:000349501400022 ER PT J AU Talley, BL Muletz, CR Vredenburg, VT Fleischer, RC Lips, KR AF Talley, Brooke L. Muletz, Carly R. Vredenburg, Vance T. Fleischer, Robert C. Lips, Karen R. TI A century of Batrachochytrium dendrobatidis in Illinois amphibians (1888-1989) SO BIOLOGICAL CONSERVATION LA English DT Article DE Amphibians; Batrachochytrium dendrobatidis (Bd); Chytridiomycosis; Emerging pathogen; Illinois; Southern leopard frog (Rana (Lithobates) sphenocephala) ID CHYTRID PATHOGEN; FUNGAL PATHOGEN; KILLING FUNGUS; NATIONAL-PARK; CHYTRIDIOMYCOSIS; DYNAMICS; DISEASE; EMERGENCE; DECLINES; HOST AB The fungal pathogen, Batrachochytrium dendrobatidis (Bd), causes the disease chytridiomycosis in amphibians and is responsible for the worst epizootics in vertebrate history. In some regions of the world (e.g., the Neotropics and Western United States), Bd has caused recent reductions in amphibian population abundance and species richness, while in other regions the impacts are less clear. Although Bd is present in the Midwestern United States, its history and impact in the region is not known. We used a qPCR assay to determine historic Bd prevalence in Illinois, testing 1028 specimens representing 10 anuran species, collected 1888-1989. We used two complementary sets of samples to first assess historic prevalence with the primary set, and used a secondary set to confirm Bd presence and examine older samples with a more sensitive technique. Prevalence varied among species; in the primary dataset of 1008 samples extracted with PrepMan Ultra collected 1892-1989, Bd was found in four species (11.1%, CI: 9.3-13.2%). Rana (Lithobates) sphenocephala, the southern leopard frog, had the highest prevalence (38.3%, Cl 32.7-44.2%); prevalence among other infected species was <7%. Overall prevalence was <10% in most decades but >40% in the 1940s. In the secondary set of 50 samples extracted with Qiagen Blood and Tissue Kits (30 re-swabbed of the original 1008 and 20 additional older specimens), 17 of the 20 additional samples were Bd+ (85.0%, CI 64.0-94.8%) including the oldest Bd+ specimen, which was collected in 1888. We confirmed Bd presence by sequencing 42 Bd+ samples and found >= 99% homology with Bd sequences in Genbank. By 1900, Bd was geographically widespread throughout Illinois-40 years earlier than the current oldest estimate in the U.S. meaning that Illinois amphibians have been coexisting with Bd for at least 126 years. This long period of coexistence from our results raises new questions about the history of Bd in North America, possible coevolution between host and pathogen, and the potential role of Bd in historic population declines. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Talley, Brooke L.] So Illinois Univ, Dept Zool, Carbondale, IL 62901 USA. [Muletz, Carly R.; Lips, Karen R.] Univ Maryland, Dept Biol, College Pk, MD 20742 USA. [Vredenburg, Vance T.] San Francisco State Univ, Dept Biol, San Francisco, CA 94132 USA. [Muletz, Carly R.; Fleischer, Robert C.] Smithsonian Conservat Biol Inst, Ctr Conservat & Evolutionary Genet, Washington, DC 20008 USA. RP Talley, BL (reprint author), Florida Fish & Wildlife Conservat Commiss, Tallahassee, FL 32399 USA. EM bltalley@gmail.com OI Vredenburg, Vance/0000-0002-9682-1190; Lips, Karen/0000-0002-2719-1551 FU Illinois Department of Natural Resources; State Wildlife Grant [T-56 R-1]; National Science Foundation [DEB 0213851, 1120161, DEB 1120283] FX Thanks to the Illinois Department of Natural Resources for supporting this research with a State Wildlife Grant (#T-56 R-1). KRL (#DEB 0213851, 1120161) and VTV (#DEB 1120283) were supported by the National Science Foundation. We appreciate the four anonymous reviewers whose comments improved this manuscript. Thanks to S. Becker, T. Hill, E. Thomas, L. Torres, N. Caruso, G. DiRenzo, T. Tunstall, P. Langhammer, A. Novarro, E. Heist, J. Reeve, and E. Schauber for assistance on the project. Special thanks to C. Phillips for permission to use specimens in the INHS and UIMNH collections. NR 58 TC 14 Z9 16 U1 5 U2 36 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0006-3207 EI 1873-2917 J9 BIOL CONSERV JI Biol. Conserv. PD FEB PY 2015 VL 182 BP 254 EP 261 DI 10.1016/j.biocon.2014.12.007 PG 8 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA CB3AY UT WOS:000349501400031 ER PT J AU Stanley, CQ McKinnon, EA Fraser, KC Macpherson, MP Casbourn, G Friesen, L Marra, PP Studds, CE Ryder, TB Diggs, NE Stutchbury, BJM AF Stanley, Calandra Q. McKinnon, Emily A. Fraser, Kevin C. Macpherson, Maggie P. Casbourn, Garth Friesen, Lyle Marra, Peter P. Studds, Colin E. Ryder, T. Brandt Diggs, Nora E. Stutchbury, Bridget J. M. TI Connectivity of wood thrush breeding, wintering, and migration sites based on range-wide tracking SO CONSERVATION BIOLOGY LA English DT Article DE Central America; geolocator; Hylocichla mustelina; migration network; migration route; migratory connectivity; tropical deforestation; America Central; conectividad migratoria; deforestacion tropical; geolocalizador; red migratoria; ruta de migracion; Hylocichla mustelina ID LIGHT-LEVEL GEOLOCATORS; POPULATION-DYNAMICS; SONGBIRD; BIRDS; CONSERVATION; WARBLERS; ROUTES; CYCLE; DNA AB Many migratory animals are experiencing rapid population declines, but migration data with the geographic scope and resolution to quantify the complex network of movements between breeding and nonbreeding regions are often lacking. Determining the most frequently used migration routes and nonbreeding regions for a species is critical for understanding population dynamics and making effective conservation decisions. We tracked the migration of individual Wood Thrushes (Hylocichla mustelina) (n = 102) from across their range with light-level geolocators and, for the first time, quantified migration routes and wintering regions for distinct breeding populations. We identified regional and species-level migratory connectivity networks for this declining songbird by combining our tracking results with range-wide breeding abundance estimates and forest cover data. More than 50% of the species occupied the eastern wintering range (Honduras to Costa Rica), a region that includes only one-third of all wintering habitat and that is undergoing intensive deforestation. We estimated that half of all Wood Thrushes in North America migrate south through Florida in fall, whereas in spring approximately 73% funnel northward through a narrow span along the central U.S. Gulf Coast (88-93 degrees W). Identifying migratory networks is a critical step for conservation of songbirds and we demonstrated with Wood Thrushes how it can highlight conservation hotspots for regional populations and species as a whole. Conectividad de Sitios de Reproduccion, Invierno y Migracion del Zorzal con Base en Rastreo de Cobertura Amplia Resumen Muchos animales migratorios estan experimentando declinaciones poblacionales rapidas, pero la informacion migratoria con el enfoque geografico y la resolucion para cuantificar la red completa de movimientos entre regiones reproductivas y no reproductivas con frecuencia es carente. Determinar las rutas y las regiones no-reproductivas usadas con mayor frecuencia por una especie es critico para entender las dinamicas poblacionales y hacer decisiones de conservacion efectivas. Rastreamos la migracion individual de zorzales (Hylocichla mustelina) (n = 102) a lo largo de su extension con geolocalizadores de bajo nivel y, por primera vez, cuantificamos la conectividad de las rutas migratorias y las regiones de invierno para poblaciones reproductivas diferentes. Identificamos redes de conectividad migratoria regionales y a nivel de especie para esta ave canora en declive al combinar nuestros resultados de rastreo con los estimados de abundancia reproductiva de cobertura amplia y los datos de cubierta forestal. Mas del 50% de las especies ocuparon la cobertura occidental de invierno (de Honduras a Costa Rica), una region que incluye solo un tercio de todo el habitat de invierno y que esta sometida a una deforestacion intensiva. Estimamos que la mitad de los zorzales en America del Norte migran al sur por Florida en el otono, mientras que en la primavera aproximadamente el 73% atraviesan un camino estrecho a lo largo del centro de la costa del Golfo en los Estados Unidos (88-93 degrees W). Identificar las redes migratorias es un paso critico para la conservacion de las aves canoras y demostramos con los zorzales como puede resaltar sitios de importancia para la conservacion para poblaciones regionales y para la especie entera. C1 [Stanley, Calandra Q.; McKinnon, Emily A.; Fraser, Kevin C.; Macpherson, Maggie P.; Casbourn, Garth; Stutchbury, Bridget J. M.] York Univ, Dept Biol, Toronto, ON M3J 1P3, Canada. [Stanley, Calandra Q.; Marra, Peter P.; Studds, Colin E.; Ryder, T. Brandt; Diggs, Nora E.] Migratory Bird Ctr, Smithsonian Conservat Biol Inst, Washington, DC 20013 USA. [Stanley, Calandra Q.; McKinnon, Emily A.; Friesen, Lyle] Canadian Wildlife Serv, Burlington, ON, Canada. RP McKinnon, EA (reprint author), York Univ, Dept Biol, Toronto, ON M3J 1P3, Canada. EM emilymck@yorku.ca FU Natural Sciences and Engineering Research Council of Canada; National Geographic Society; U.S. Fish and Wildlife Service Neotropical Migratory Bird Grant; Environment Canada; Schad Foundation; Kenneth M. Molson Foundation; York University; Department of Defence's Legacy Program; Strategic Environmental Research Development Program; National Audubon Society FX We thank J. Sauer for analysis of Breeding Bird Survey data and S. Barretto for GIS analysis. We thank the following funding sources: Natural Sciences and Engineering Research Council of Canada, National Geographic Society, U.S. Fish and Wildlife Service Neotropical Migratory Bird Grant, Environment Canada, Schad Foundation, Kenneth M. Molson Foundation, York University, and proceeds from Silence of the Songbirds (Walker & Co.). P.P.M., T.B.R., and C.E.S. received support from the Department of Defence's Legacy Program and the Strategic Environmental Research Development Program. The National Audubon Society provided funding and Pro-Aves Veracruz provided assistance for fieldwork in Mexico. Tropical fieldwork was conducted at the Belize Foundation for Research and Environmental Education, La Selva in Costa Rica, and Reserva Nebliselva El Jaguar in Nicaragua. We thank J. Marlin, J. Rotenberg, L. Duriaux-Chavarria, and G. Duriaux for field support in Central America. NR 42 TC 18 Z9 20 U1 16 U2 84 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0888-8892 EI 1523-1739 J9 CONSERV BIOL JI Conserv. Biol. PD FEB PY 2015 VL 29 IS 1 BP 164 EP 174 DI 10.1111/cobi.12352 PG 11 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA CA2AX UT WOS:000348712400019 PM 25052795 ER PT J AU Lebuhn, G Droege, S Connor, EF Gemmill-Herren, B Potts, SG Minckley, RL Jean, RP Kula, E Roubik, DW Wright, KW Frankie, G Parker, F AF Lebuhn, Gretchen Droege, Sam Connor, Edward F. Gemmill-Herren, Barbara Potts, Simon G. Minckley, Robert L. Jean, Robert P. Kula, Emanuel Roubik, David W. Wright, Karen W. Frankie, Gordon Parker, Frank TI Evidence-based conservation: reply to Tepedino et al. SO CONSERVATION BIOLOGY LA English DT Editorial Material C1 [Lebuhn, Gretchen; Connor, Edward F.] San Francisco State Univ, Dept Biol, San Francisco, CA 94132 USA. [Droege, Sam] USGS Patuxent Wildlife Res Ctr, Laurel, MD 20708 USA. [Gemmill-Herren, Barbara] Food & Agr Org United Nations, I-00100 Rome, Italy. [Potts, Simon G.] Univ Reading, Sch Agr Policy & Dev, Ctr Agri Environm Res CAER, Reading RG6 6AR, Berks, England. [Minckley, Robert L.] Univ Rochester, Dept Biol, Rochester, NY 14627 USA. [Jean, Robert P.] St Mary Of The Woods Coll, Dept Sci & Math, St Mary Of The Woods, IN 47876 USA. [Kula, Emanuel] Mendel Univ Brno, Fac Forestry & Wood Technol, Brno 134127, Czech Republic. [Roubik, David W.] Smithsonian Trop Res Inst, Balboa Ancon, Panama. [Wright, Karen W.] Univ New Mexico, Dept Biol, Sevilleta LTER, Albuquerque, NM 87131 USA. [Frankie, Gordon] Univ Calif Berkeley, Dept Environm Sci Policy & Management, Berkeley, CA 94720 USA. [Parker, Frank] Utah State Univ, ARS, USDA, Bee Biol & Systemat Lab, Logan, UT 84322 USA. RP Lebuhn, G (reprint author), San Francisco State Univ, Dept Biol, San Francisco, CA 94132 USA. EM lebuhn@sfsu.edu FU Biotechnology and Biological Sciences Research Council NR 7 TC 2 Z9 2 U1 3 U2 19 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0888-8892 EI 1523-1739 J9 CONSERV BIOL JI Conserv. Biol. PD FEB PY 2015 VL 29 IS 1 BP 283 EP 285 DI 10.1111/cobi.12438 PG 3 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA CA2AX UT WOS:000348712400031 PM 25545768 ER PT J AU Moore, A Burch, J Duda, TF AF Moore, Alexandria C. Burch, John B. Duda, Thomas F., Jr. TI Recognition of a highly restricted freshwater snail lineage (Physidae: Physella) in southeastern Oregon: convergent evolution, historical context, and conservation considerations SO CONSERVATION GENETICS LA English DT Article DE Freshwater gastropods; Physidae; Convergent evolution; COI; ITS1; ITS2 ID BIOMPHALARIA GASTROPODA; PULMONATA; BIOGEOGRAPHY; BASOMMATOPHORA; INVERTEBRATES; PLANORBIDAE; HYGROPHILA; CHALLENGES; PHYLOGENY AB Non-marine mollusks have the highest number of documented extinctions of any major taxonomic group. Given their conservation status and the numerous cases of taxonomic uncertainty concerning freshwater mollusks in particular, the recognition of potentially endangered species is critically important. Here, we evaluate the genetic distinctiveness and phylogenetic position of a freshwater snail restricted to a series of geothermal springs within the Owyhee River drainage in Oregon (the 'Owyhee wet-rock physa'). Because these snails closely resemble Physella (Petrophysa) zionis, a wet-rock physa that occurs in a small area in Zion National Park (Utah), the Owyhee wet-rock physa is presumably either closely related to or represents a disjunct population of P. zionis. However, phylogenetic analyses of sequences of mitochondrial cytochrome oxidase I and nuclear first and second internal transcribed spacer gene regions indicate that the Owyhee wet-rock physa is genetically distinct from other physid species. Despite exhibiting similar morphologies, the Owyhee wet-rock physa and P. zionis are distantly related physids; instead, the Owyhee wet-rock physa is most closely related to a population of physids from central California. These results suggest that convergent evolution may be responsible for the similar shell morphologies of the Owyhee wet-rock physa and P. zionis. Furthermore, the close relationship between physid populations in southeastern Oregon and central California suggests a historical connection between the Owyhee River and river drainages to the south. Finally, we recommend that the Owyhee wet-rock physa be considered critically endangered based on its extremely limited distribution. C1 [Moore, Alexandria C.; Burch, John B.; Duda, Thomas F., Jr.] Univ Michigan, Dept Ecol & Evolutionary Biol, Ann Arbor, MI 48109 USA. [Moore, Alexandria C.; Burch, John B.; Duda, Thomas F., Jr.] Univ Michigan, Museum Zool, Ann Arbor, MI 48109 USA. [Duda, Thomas F., Jr.] Smithsonian Trop Res Inst, Ancon, Panama. RP Moore, A (reprint author), Univ Michigan, Dept Ecol & Evolutionary Biol, 1109 Geddes Ave, Ann Arbor, MI 48109 USA. EM mooreale@umich.edu FU University of Michigan Department of Ecology and Evolutionary Biology; Rackham Graduate School FX We thank D. Hopper (U.S. Fish and Wildlife Service) and G.R. Smith (University of Michigan) for their varied expertise, assistance, and suggestions. We are also grateful to A. Wethington (Chowan University), B. Dayrat (Pennsylvania State University), W.H. Clark and S.J. Lysne (Orma J. Smith Museum of Natural History), and E. Kools (California Academy of Sciences) for providing specimens used in this work. The University of Michigan Department of Ecology and Evolutionary Biology and the Rackham Graduate School provided financial support. We also thank C. Dick and J. Pappas (University of Michigan) for the support and feedback that they provided on this work. This manuscript was also considerably improved based on input received from T. Lee (University of Michigan) and three anonymous reviewers. NR 43 TC 1 Z9 1 U1 2 U2 17 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 2015 VL 16 IS 1 BP 113 EP 123 DI 10.1007/s10592-014-0645-5 PG 11 WC Biodiversity Conservation; Genetics & Heredity SC Biodiversity & Conservation; Genetics & Heredity GA AZ6XF UT WOS:000348360700009 ER PT J AU Sonsthagen, S Tibbitts, T Gill, R Williams, I Talbot, S AF Sonsthagen, Sarah A. Tibbitts, T. Lee Gill, Robert E., Jr. Williams, Ian Talbot, Sandra L. TI Spatial genetic structure of bristle-thighed curlews (Numenius tahitiensis): breeding area differentiation not reflected on the non-breeding grounds SO CONSERVATION GENETICS LA English DT Article DE Alaska; Bristle-thighed curlew; Migratory connectivity; Numenius; Oceania; Population genetic structure ID MAXIMUM-LIKELIHOOD-ESTIMATION; MIGRATORY CONNECTIVITY; POPULATION-STRUCTURE; COALESCENT APPROACH; MITOCHONDRIAL-DNA; ALASKA; SELECTION; BIODIVERSITY; INDIVIDUALS; INFERENCE AB Migratory birds occupy geographically and ecologically disparate areas during their annual cycle with conditions on breeding and non-breeding grounds playing separate and important roles in population dynamics. We used data from nuclear microsatellite and mitochondrial DNA control region loci to assess the breeding and non-breeding spatial genetic structure of a transoceanic migrant shorebird, the bristle-thighed curlew. We found spatial variance in the distribution of allelic and haplotypic frequencies between the curlew's two breeding areas in Alaska but did not observe this spatial structure throughout its non-breeding range on low-lying tropical and subtropical islands in the Central Pacific (Oceania). This suggests that the two breeding populations do not spatially segregate during the non-breeding season. Lack of migratory connectivity is likely attributable to the species' behavior, as bristle-thighed curlews exhibit differential timing of migration and some individuals move among islands during non-breeding months. Given the detrimental impact of many past and current human activities on island ecosystems, admixture of breeding populations in Oceania may render the bristle-thighed curlew less vulnerable to perturbations there, as neither breeding population will be disproportionally affected by local habitat losses or by stochastic events. Furthermore, lack of migratory connectivity may enable bristle-thighed curlews to respond to changing island ecosystems by altering their non-breeding distribution. However, availability of suitable non-breeding habitat for curlews in Oceania is increasingly limited on both low-lying and high islands by habitat loss, sea level rise, and invasive mammalian predators that pose a threat to flightless and flight-compromised curlews during the molting period. C1 [Sonsthagen, Sarah A.; Tibbitts, T. Lee; Gill, Robert E., Jr.; Williams, Ian; Talbot, Sandra L.] US Geol Survey, Alaska Sci Ctr, Anchorage, AK 99508 USA. [Sonsthagen, Sarah A.] Smithsonian Inst, Labs Analyt Biol, Washington, DC 20560 USA. [Sonsthagen, Sarah A.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Sonsthagen, S (reprint author), US Geol Survey, Alaska Sci Ctr, 4210 Univ Dr, Anchorage, AK 99508 USA. EM ssonsthagen@usgs.gov FU U.S. Geological Survey Alaska Science Center; Laboratories of Analytical Biology, National Museum of Natural History, Smithsonian Institution; U.S. Fish and Wildlife Service FX Funding for this research was provided by the U.S. Geological Survey Alaska Science Center and Laboratories of Analytical Biology, National Museum of Natural History, Smithsonian Institution. Technological support was provided the University of Alaska Life Science Informatics computer cluster (NIH P20RR016466). Richard Lanctot, U.S. Fish and Wildlife Service, helped design the study and Sue Thomas, U.S. Fish and Wildlife Service, procured initial funding. We thank the James Dean, National Museum of Natural History, Smithsonian Institution, for subsampling specimens. George Sage and Judy Gust, U.S. Geological Survey, provided laboratory assistance. David Douglas, U.S. Geological Survey, provided advice on the spatial analysis. Comments by Robert Wilson, University of Alaska Fairbanks, John Pearce, U.S. Geological Survey, and three anonymous reviewers, improved the manuscript. Any use of trade, product, or firm names is for descriptive purposes only and does not imply endorsement by the U.S. Government. NR 64 TC 1 Z9 1 U1 9 U2 20 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 2015 VL 16 IS 1 BP 223 EP 233 DI 10.1007/s10592-014-0654-4 PG 11 WC Biodiversity Conservation; Genetics & Heredity SC Biodiversity & Conservation; Genetics & Heredity GA AZ6XF UT WOS:000348360700017 ER PT J AU Adey, WH Hernandez-Kantun, JJ Johnson, G Gabrielson, PW AF Adey, Walter H. Hernandez-Kantun, Jazmin J. Johnson, Gabriel Gabrielson, Paul W. TI DNA SEQUENCING, ANATOMY, AND CALCIFICATION PATTERNS SUPPORT A MONOPHYLETIC, SUBARCTIC, CARBONATE REEF-FORMING CLATHROMORPHUM (HAPALIDIACEAE, CORALLINALES, RHODOPHYTA) SO JOURNAL OF PHYCOLOGY LA English DT Article DE anatomy; Callilithophytum; ecology; evolution; Leptophytum; Melobesioideae; Neopolyporolithon; psbA; rbcL; SSU ID NORTHWESTERN NORTH ATLANTIC; RED ALGAE FLORIDEOPHYCEAE; APPLYING AVAILABLE NAMES; RNA GENE-SEQUENCES; CRUSTOSE CORALLINES; LEPTOPHYTUM CORALLINACEAE; MARINE-ALGAE; PACIFIC; MELOBESIOIDEAE; GIGARTINALES AB For the first time, morpho-anatomical characters that were congruent with DNA sequence data were used to characterize several genera in Hapalidiaceae -the major eco-engineers of Subarctic carbonate ecosystems. DNA sequencing of three genes (SSU, rbcL, ribulose-1, 5-bisphosphate carboxylase/oxygenase large subunit gene and psbA, photosystem II D1 protein gene), along with patterns of cell division, cell elongation, and calcification supported a monophyletic Clathromorphum. Two characters were diagnostic for this genus: (i) cell division, elongation, and primary calcification occurred only in intercalary meristematic cells and in a narrow vertical band (1-2 mu m wide) resulting in a "meristem split" and (ii) a secondary calcification of interfilament crystals was also produced. Neopolyporolithon was resurrected for N. reclinatum, the generitype, and Clathromorphum loculosum was transferred to this genus. Like Clathromorphum, cell division, elongation, and calcification occurred only in intercalary meristematic cells, but in a wider vertical band (over 10-20 mu m), and a "meristem split" was absent. Callilithophytum gen. nov. was proposed to accommodate Clathromorphum parcum, the obligate epiphyte of the northeast Pacific endemic geniculate coralline, Calliarthron. Diagnostic for this genus were epithallial cells terminating all cell filaments (no dorsi-ventrality was present), and a distinct "foot" was embedded in the host. Leptophytum, based on its generitype, L. laeve, was shown to be a distinct genus more closely related to Clathromorphum than to Phymatolithon. All names of treated species were applied unequivocally by linking partial rbcL sequences from holotype, isotype, or epitype specimens with field-collected material. Variation in rbcL and psbA sequences suggested that multiple species may be passing under each currently recognized species of Clathromorphum and Neopolyporolithon. C1 [Adey, Walter H.; Hernandez-Kantun, Jazmin J.] Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, Washington, DC 20560 USA. [Johnson, Gabriel] Smithsonian Inst, Natl Museum Nat Hist, Lab Analyt Biol, Washington, DC 20560 USA. [Gabrielson, Paul W.] Univ N Carolina, Dept Biol, Chapel Hill, NC USA. [Gabrielson, Paul W.] Univ N Carolina, Herbarium, Chapel Hill, NC USA. RP Adey, WH (reprint author), Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, Washington, DC 20560 USA. EM adeyw@si.edu FU Ecological Systems Technology; Natural Science and Engineering Research Council of Canada; Botany Department of the Smithsonian's National Museum of Natural History; Smithsonian Institution FX We are very grateful to the curators at S (Ms. Marianne Hamnede), TRH (Dr. Kristian Hassel), UBC (Dr. Sandra Lindstrom), UC (the late Dr. Paul C. Silva), and UPS (Dr. Stefan Ekman) for the loan of type material critical to this study; equally grateful to the following for collecting specimens: J. Estes, S. M. E. Gabrielson, A. Galloway, J. Halfar, S. C. Lindstrom, K. A. Miller, K. M. Miklasz, P. T. Martone, R. S. Steneck, and T. Suskiewicz. A portion of this study was done while PWG was a visiting professor at the Friday Harbor Laboratories, University of Washington. PWG also thanks Dr. Todd Vision (University of North Carolina, Chapel Hill) for the use of lab space and equipment. This research was funded in part by a family trust to P. W. G. and by Ecological Systems Technology, The Natural Science and Engineering Research Council of Canada, and the Botany Department of the Smithsonian's National Museum of Natural History to W. H. A. J. H.-K. is grateful to the Smithsonian Institution for a postdoctoral fellowship. NR 68 TC 16 Z9 16 U1 3 U2 16 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0022-3646 EI 1529-8817 J9 J PHYCOL JI J. Phycol. PD FEB PY 2015 VL 51 IS 1 BP 189 EP 203 DI 10.1111/jpy.12266 PG 15 WC Plant Sciences; Marine & Freshwater Biology SC Plant Sciences; Marine & Freshwater Biology GA CB1PU UT WOS:000349400900015 PM 26986268 ER PT J AU Callahan, MK Rains, MC Bellino, JC Walker, CM Baird, SJ Whigham, DF King, RS AF Callahan, Michael K. Rains, Mark C. Bellino, Jason C. Walker, Coowe M. Baird, Steven J. Whigham, Dennis F. King, Ryan S. TI CONTROLS ON TEMPERATURE IN SALMONID-BEARING HEADWATER STREAMS IN TWO COMMON HYDROGEOLOGIC SETTINGS, KENAI PENINSULA, ALASKA SO JOURNAL OF THE AMERICAN WATER RESOURCES ASSOCIATION LA English DT Article DE surface-water; groundwater interactions; surface water hydrology; groundwater hydrology; geomorphology; watershed management; anadromous fish ID WATER TEMPERATURE; JUVENILE SALMONIDS; THERMAL REFUGIA; STORM RUNOFF; HABITAT; USA; LOWLANDS; RIVER; GEOMORPHOLOGY; ECOSYSTEMS AB Headwater streams are the most numerous in terms of both number and length in the conterminous United States and play important roles as spawning and rearing grounds for numerous species of anadromous fish. Stream temperature is a controlling variable for many physical, chemical, and biological processes and plays a critical role in the overall health and integrity of a stream. We investigated the controls on stream temperature in salmon-bearing headwater streams in two common hydrogeologic settings on the Kenai Peninsula, Alaska: (1) drainage-ways, which are low-gradient streams that flow through broad valleys; and (2) discharge-slopes, which are high gradient streams that flow through narrow valleys. We hypothesize local geomorphology strongly influences surface-water and groundwater interactions, which control streamflow at the network scale and stream temperatures at the reach scale. The results of this study showed significant differences in stream temperatures between the two hydrogeologic settings. Observed stream temperatures were higher in drainage-way sites than in discharge-slope sites, and showed strong correlations as a continuous function with the calculated topographic metric flow-weighted slope. Additionally, modeling results indicated the potential for groundwater discharge to moderate stream temperature is not equal between the two hydrogeologic settings, with groundwater having a greater moderating effect on stream temperature at the drainage-way sites. C1 [Callahan, Michael K.; Rains, Mark C.] Univ S Florida, Sch Geosci, Tampa, FL 33620 USA. [Bellino, Jason C.] Univ S Florida, Tampa, FL 33620 USA. [Walker, Coowe M.; Baird, Steven J.] Kachemak Bay Natl Estuarine Res Reserve, Homer, AK 99603 USA. [Whigham, Dennis F.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [King, Ryan S.] Baylor Univ, Dept Biol, Waco, TX 76798 USA. RP Callahan, MK (reprint author), Univ S Florida, Sch Geosci, 4202 E Fowler Ave, Tampa, FL 33620 USA. EM mkcallah@mail.usf.edu OI Whigham, Dennis/0000-0003-1488-820X FU USEPA [CD-96011801-0]; Baylor University, Kachemak Bay Research Reserve; University of South Florida FX This project was funded by USEPA grant number CD-96011801-0 and with significant cost-sharing from Baylor University, Kachemak Bay Research Reserve, and the University of South Florida. We would like to thank the numerous staff and volunteers of KBRR, especially Amy Alderfer and Kim Cooney, for providing invaluable administrative and logistical support. We would also like to thank Becky Shaftel, Douglas Reynolds, and Molly Tedeschi for their help in the field. We are grateful to the Ninilchik Tribal Association and the private landowners who gave us permission to access their lands. We would also like to acknowledge the anonymous reviewers for their constructive comments. Finally, we'd like to recognize the valuable insights and encouragement of Phil North, who helped make this research possible. NR 65 TC 1 Z9 1 U1 3 U2 16 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1093-474X EI 1752-1688 J9 J AM WATER RESOUR AS JI J. Am. Water Resour. Assoc. PD FEB PY 2015 VL 51 IS 1 BP 84 EP 98 DI 10.1111/jawr.12235 PG 15 WC Engineering, Environmental; Geosciences, Multidisciplinary; Water Resources SC Engineering; Geology; Water Resources GA CA8FF UT WOS:000349151900006 ER PT J AU DeVience, SJ Pham, LM Lovchinsky, I Sushkov, AO Bar-Gill, N Belthangady, C Casola, F Corbett, M Zhang, HL Lukin, M Park, H Yacoby, A Walsworth, RL AF DeVience, Stephen J. Pham, Linh M. Lovchinsky, Igor Sushkov, Alexander O. Bar-Gill, Nir Belthangady, Chinmay Casola, Francesco Corbett, Madeleine Zhang, Huiliang Lukin, Mikhail Park, Hongkun Yacoby, Amir Walsworth, Ronald L. TI Nanoscale NMR spectroscopy and imaging of multiple nuclear species SO NATURE NANOTECHNOLOGY LA English DT Article ID MAGNETIC-RESONANCE; AMBIENT CONDITIONS; ELECTRONIC SPIN; DIAMOND; MAGNETOMETRY; MICROSCOPY; RESOLUTION; COHERENCE; DYNAMICS; QUBIT AB Nuclear magnetic resonance (NMR) spectroscopy and magnetic resonance imaging (MRI) provide non-invasive information about multiple nuclear species in bulk matter, with wide-ranging applications from basic physics and chemistry to biomedical imaging(1). However, the spatial resolution of conventional NMR and MRI is limited(2) to several micrometres even at large magnetic fields (>1T), which is inadequate for many frontier scientific applications such as single-molecule NMR spectroscopy and in vivo MRI of individual biological cells. A promising approach for nanoscale NMR and MRI exploits optical measurements of nitrogen-vacancy (NV) colour centres in diamond, which provide a combination of magnetic field sensitivity and nanoscale spatial resolution unmatched by any existing technology, while operating under ambient conditions in a robust, solid-state system(3-5). Recently, single, shallow NV centres were used to demonstrate NMR of nanoscale ensembles of proton spins, consisting of a statistical polarization equivalent to similar to 100-1,000 spins in uniform samples covering the surface of a bulk diamond chip6,7. Here, we realize nanoscale NMR spectroscopy and MRI of multiple nuclear species (H-1, F-19, P-31) in non-uniform (spatially structured) samples under ambient conditions and at moderate magnetic fields (similar to 20 mT) using two complementary sensor modalities. C1 [DeVience, Stephen J.; Sushkov, Alexander O.; Park, Hongkun; Walsworth, Ronald L.] Harvard Univ, Dept Chem & Chem Biol, Cambridge, MA 02138 USA. [Pham, Linh M.; Belthangady, Chinmay; Casola, Francesco; Walsworth, Ronald L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lovchinsky, Igor; Sushkov, Alexander O.; Zhang, Huiliang; Lukin, Mikhail; Park, Hongkun; Yacoby, Amir; Walsworth, Ronald L.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Bar-Gill, Nir] Hebrew Univ Jerusalem, Dept Appl Phys, Jerusalem, Israel. [Bar-Gill, Nir] Hebrew Univ Jerusalem, Racah Inst Phys, IL-91904 Jerusalem, Israel. [Corbett, Madeleine; Yacoby, Amir] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA. [Park, Hongkun; Walsworth, Ronald L.] Harvard Univ, Ctr Brain Sci, Cambridge, MA 02138 USA. RP Walsworth, RL (reprint author), Harvard Univ, Dept Chem & Chem Biol, 12 Oxford St, Cambridge, MA 02138 USA. EM rwalsworth@cfa.harvard.edu RI DeVience, Stephen/D-7274-2012 OI DeVience, Stephen/0000-0003-3142-7296 FU National Science Foundation; Defense Advanced Research Projects Agency QuASAR programme; Swiss National Science Foundation; National Defense Science and Engineering Graduate fellowship FX This work was supported by the National Science Foundation and the Defense Advanced Research Projects Agency QuASAR programme. F.C. acknowledges support from the Swiss National Science Foundation. I.L. acknowledges support from a National Defense Science and Engineering Graduate fellowship. NR 37 TC 46 Z9 46 U1 17 U2 118 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 1748-3387 EI 1748-3395 J9 NAT NANOTECHNOL JI Nat. Nanotechnol. PD FEB PY 2015 VL 10 IS 2 BP 129 EP 134 DI 10.1038/nnano.2014.313 PG 6 WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary SC Science & Technology - Other Topics; Materials Science GA CB2OV UT WOS:000349468200010 PM 25559712 ER PT J AU Lambers, H Hayes, PE Laliberte, E Oliveira, RS Turner, BL AF Lambers, Hans Hayes, Patrick E. Laliberte, Etienne Oliveira, Rafael S. Turner, Benjamin L. TI Leaf manganese accumulation and phosphorus-acquisition efficiency SO TRENDS IN PLANT SCIENCE LA English DT Review DE carboxylates; exudation; manganese; phosphorus; phosphorus-acquisition efficiency ID ACINOSA ROXB. PHYTOLACCACEAE; PLANT CHENGIOPANAX-SCIADOPHYLLOIDES; LUPINUS-ALBUS L; METAL TRANSPORTER; WHITE LUPIN; NUTRIENT CONCENTRATIONS; ARBUSCULAR MYCORRHIZAL; MN HYPERACCUMULATORS; BIDWILLII MYRTACEAE; FUNCTIONAL TRAITS AB Plants that deploy a phosphorus (P)-mobilising strategy based on the release of carboxylates tend to have high leaf manganese concentrations ([Mn]). This occurs because the carboxylates mobilise not only soil inorganic and organic P. but also a range of micronutrients, including Mn. Concentrations of most other micronutrients increase to a small extent, but Mn accumulates to significant levels, even when plants grow in soil with low concentrations of exchangeable Mn availability. Here, we propose that leaf [Mn] can be used to select for genotypes that are more efficient at acquiring P when soil P availability is low. Likewise, leaf [Mn] can be used to screen for belowground functional traits related to nutrient-acquisition strategies among species in low-P habitats. C1 [Lambers, Hans; Hayes, Patrick E.; Laliberte, Etienne; Oliveira, Rafael S.; Turner, Benjamin L.] Univ Western Australia, Sch Plant Biol, Crawley Perth, WA 6009, Australia. [Oliveira, Rafael S.] Univ Estadual Campinas, Dept Biol Vegetal, BR-13083862 Campinas, SP, Brazil. [Turner, Benjamin L.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Lambers, H (reprint author), Univ Western Australia, Sch Plant Biol, Stirling Highway, Crawley Perth, WA 6009, Australia. EM hans.lambers@uwa.edu.au RI Laliberte, Etienne/B-6855-2008; Turner, Benjamin/E-5940-2011; Hayes, Patrick/D-4679-2014; Lambers, Hans/A-1544-2008; Oliveira, Rafael/B-3422-2013 OI Laliberte, Etienne/0000-0002-3167-2622; Turner, Benjamin/0000-0002-6585-0722; Hayes, Patrick/0000-0001-7554-4588; Lambers, Hans/0000-0002-4118-2272; Oliveira, Rafael/0000-0002-6392-2526 FU Australian Research Council (ARC) [DP0985685, DP110101120]; Australian Postgraduate Award through the University of Western Australia; DECRA from the ARC [DE120100352]; Sao Paulo Research Foundation [Fapesp 2010/172040, Fapesp 2011/520720] FX H.L. was supported by the Australian Research Council (ARC; DP0985685 and DP110101120); P.E.H. was supported by an Australian Postgraduate Award through the University of Western Australia; E.L. was supported by a DECRA (DE120100352) from the ARC; and R.S.O. was supported by Sao Paulo Research Foundation (Fapesp 2010/172040 and Fapesp 2011/520720). NR 105 TC 24 Z9 26 U1 24 U2 86 PU ELSEVIER SCIENCE LONDON PI LONDON PA 84 THEOBALDS RD, LONDON WC1X 8RR, ENGLAND SN 1360-1385 J9 TRENDS PLANT SCI JI Trends Plant Sci. PD FEB PY 2015 VL 20 IS 2 BP 83 EP 90 DI 10.1016/j.tplants.2014.10.007 PG 8 WC Plant Sciences SC Plant Sciences GA CB3CD UT WOS:000349504900006 PM 25466977 ER PT J AU Brodu, E Balat-Pichelin, M Sans, JL Kasper, JC AF Brodu, E. Balat-Pichelin, M. Sans, J. -L. Kasper, J. C. TI Evolution of the emissivity of tungsten at high temperature with and without proton bombardment SO ACTA MATERIALIA LA English DT Article DE Emissivity; Tungsten; High temperature; Proton bombardment; Surface topography ID SOLAR PROBE PLUS; RADIATIVE PROPERTIES; MOLYBDENUM; HELIUM; VACUUM AB The Solar Probe Plus mission (NASA) will be the first mission to enter the solar corona. The spacecraft will orbit the Sun at 8.5 solar radii from the Sun's surface at closest approach. Some metallic parts of the two on-board instruments, SWEAP (a Faraday cup) and FIELDS (antennas), will directly face the Sun, while the rest of the payload will be protected by a heat shield. For application to these instruments, a candidate refractory material, tungsten, was studied, confronting conditions similar to the ones expected close to the Sun: high radiative flux leading to high temperatures (1100-2500 K) and proton bombardment (1 and 4 keV; 10(16), 10(17) and 10(18) ions m(-2) s(-1)) to simulate the solar wind in high vacuum (10(-4) Pa). Total directional and hemispherical emissivities in the two wavelength ranges 0.6-2.8 and 0.6-40 mu m were recorded in situ during treatments. Material characterization was performed before and after each high temperature and bombardment experiment to correlate a possible emissivity evolution to other material properties: mainly the microstructure and the surface topography. This paper reports some results on the evolution of the emissivity at high temperature for two different tungsten materials elaborated by two manufacturers - having thus different initial surface states, impurity contents and microstructures - and also with the addition of proton bombardment to the high temperature. However, the proton bombardment showed no effect on the surface topography or the emissivity, despite the fact that the ion fluxes used in our experiments were up to three orders of magnitude higher than the one expected from the solar winds. (C) 2014 Acta Materialia Inc. Published by Elsevier Ltd. All rights reserved. C1 [Brodu, E.; Balat-Pichelin, M.; Sans, J. -L.] PROMES CNRS, Lab Procides Mat & Energie Solaire, F-66120 Font Romeu, France. [Brodu, E.; Kasper, J. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Balat-Pichelin, M (reprint author), PROMES CNRS, Lab Procides Mat & Energie Solaire, 7 Rue Four Solaire, F-66120 Font Romeu, France. EM marianne.balat@promes.cnrs.fr NR 27 TC 3 Z9 3 U1 2 U2 10 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1359-6454 EI 1873-2453 J9 ACTA MATER JI Acta Mater. PD FEB 1 PY 2015 VL 84 BP 305 EP 316 DI 10.1016/j.actamat.2014.10.050 PG 12 WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Materials Science; Metallurgy & Metallurgical Engineering GA CA1RC UT WOS:000348688300028 ER PT J AU Brown, A Neff, JE Ayres, TR Kowalski, A Hawley, S Berdyugina, S Harper, GM Korhonen, H Piskunov, N Saar, S Walkowicz, L Wells, MA AF Brown, Alexander Neff, James E. Ayres, Thomas R. Kowalski, Adam Hawley, Suzanne Berdyugina, Svetlana Harper, Graham M. Korhonen, Heidi Piskunov, Nikolai Saar, Steven Walkowicz, Lucianne Wells, Mark A. TI SERENDIPITOUS DISCOVERY OF A DWARF NOVA IN THE KEPLER FIELD NEAR THE G DWARF KIC 5438845 SO ASTRONOMICAL JOURNAL LA English DT Article DE stars: dwarf novae; stars: individual (KIC 5438845) ID SU UMA-TYPE; V344 LYRAE; INSTABILITY; SUPERHUMPS; OUTBURSTS; MODEL AB The Kepler satellite provides a unique window into stellar temporal variability by observing a wide variety of stars with multi-year, near-continuous, high precision, optical photometric time series. While most Kepler targets are faint stars with poorly known physical properties, many unexpected discoveries should result from a long photometric survey of such a large area of sky. During our Kepler Guest Observer programs that monitored late-type stars for starspot and flaring variability, we discovered a previously unknown dwarf nova that lies within a few arcseconds of the mid-G dwarf star KIC 5438845. This dwarf nova underwent nine outbursts over a 4 year time span. The two largest outbursts lasted similar to 17-18 days and show strong modulations with a 110.8 minute period and a declining amplitude during the outburst decay phase. These properties are characteristic of an SU UMa-type cataclysmic variable. By analogy with other dwarf nova light curves, we associate the 110.8 minute (1.847 hr) period with the superhump period, close to but slightly longer than the orbital period of the binary. No precursor outbursts are seen before the super-outbursts and the overall super-outburst morphology corresponds to Osaki & Meyer "Case B" outbursts, which are initiated when the outer edge of the disk reaches the tidal truncation radius. "Case B" outbursts are rare within the Kepler light curves of dwarf novae. The dwarf nova is undergoing relatively slow mass transfer, as evidenced by the long intervals between outbursts, but the mass transfer rate appears to be steady, because the smaller "normal" outbursts show a strong correlation between the integrated outburst energy and the elapsed time since the previous outburst. At super-outburst maximum the system was at V similar to 18, but in quiescence it is fainter than V similar to 22, which will make any detailed quiescent follow-up of this system difficult. C1 [Brown, Alexander; Ayres, Thomas R.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. [Neff, James E.; Wells, Mark A.] Coll Charleston, Dept Phys & Astron, Charleston, SC 29424 USA. [Kowalski, Adam] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Kowalski, Adam; Hawley, Suzanne] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Berdyugina, Svetlana] Univ Freiburg, Kiepenheuer Inst Sonnenphys, D-79104 Freiburg, Germany. [Harper, Graham M.] Univ Dublin Trinity Coll, Sch Phys, Dublin 2, Ireland. [Korhonen, Heidi] Univ Turku, Finnish Ctr Astron ESO FINCA, FI-21500 Piikkio, Finland. [Korhonen, Heidi] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Piskunov, Nikolai] Uppsala Univ, Dept Astron & Space Phys, SE-75120 Uppsala, Sweden. [Saar, Steven] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Walkowicz, Lucianne] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Wells, Mark A.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. RP Brown, A (reprint author), Univ Colorado, Ctr Astrophys & Space Astron, 593 UCB, Boulder, CO 80309 USA. EM Alexander.Brown@colorado.edu RI Korhonen, Heidi/E-3065-2016 OI Korhonen, Heidi/0000-0003-0529-1161 FU NASA Kepler Cycle 1/2/3/4 Guest Observer grants [NNX10AC51G, NNX11AC79G, NNX12AC85, NNX13AC31G]; GALEX Cycle 4 Guest Observer grant [NNX09AM47 G]; NSF [AST-1109695]; South Carolina Space Grant consortium; NASA Office of Space Science [NNX13AC07 G] FX This work was supported by NASA Kepler Cycle 1/2/3/4 Guest Observer grants NNX10AC51G, NNX11AC79G, NNX12AC85 G, and NNX13AC31G, and GALEX Cycle 4 Guest Observer grant NNX09AM47 G to the University of Colorado. We acknowledge support by NSF grant AST-1109695 to the College of Charleston, and by the South Carolina Space Grant consortium. The Kepler data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST). Support to MAST for non-HST data is provided by the NASA Office of Space Science via grant NNX13AC07 G and by other grants and contracts. This paper is based in part on observations obtained with the Apache Point Observatory 3.5 m telescope, which is owned and operated by the Astrophysical Research Consortium. NR 16 TC 2 Z9 2 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD FEB PY 2015 VL 149 IS 2 AR 67 DI 10.1088/0004-6256/149/2/67 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CB1BA UT WOS:000349360200032 ER PT J AU Johnson, CI McDonald, I Pilachowski, CA Mateo, M Bailey, JI Cordero, MJ Zijlstra, AA Crane, JD Olszewski, E Shectman, SA Thompson, I AF Johnson, Christian I. McDonald, Iain Pilachowski, Catherine A. Mateo, Mario Bailey, John I., III Cordero, Maria J. Zijlstra, Albert A. Crane, Jeffrey D. Olszewski, Edward Shectman, Stephen A. Thompson, Ian TI AGB SODIUM ABUNDANCES IN THE GLOBULAR CLUSTER 47 TUCANAE (NGC 104) SO ASTRONOMICAL JOURNAL LA English DT Article DE globular clusters: general; globular clusters: individual (47 Tucanae, NGC 104); stars: abundances ID RED GIANT BRANCH; MULTIPLE STELLAR POPULATIONS; MAIN-SEQUENCE STARS; SELF-ENRICHMENT SCENARIO; COLOR-MAGNITUDE DIAGRAM; PROTON-CAPTURE ELEMENTS; BLUE HORIZONTAL-BRANCH; LTE LINE FORMATION; HELIUM ABUNDANCE; TURN-OFF AB A recent analysis comparing the [Na/Fe] distributions of red giant branch (RGB) and asymptotic giant branch (AGB) stars in the Galactic globular cluster NGC 6752 found that the ratio of Na-poor to Na-rich stars changes from 30: 70 on the RGB to 100: 0 on the AGB. The surprising paucity of Na-rich stars on the AGB in NGC 6752 warrants additional investigations to determine if the failure of a significant fraction of stars to ascend the AGB is an attribute common to all globular clusters. Therefore, we present radial velocities, [Fe/H], and [Na/Fe] abundances for 35 AGB stars in the Galactic globular cluster 47 Tucanae (47 Tuc; NGC 104), and compare the AGB [Na/Fe] distribution with a similar RGB sample published previously. The abundances and velocities were derived from high-resolution spectra obtained with the Michigan/Magellan Fiber System and MSpec spectrograph on the Magellan-Clay 6.5 m telescope. We find the average heliocentric radial velocity and [Fe/H] values to be < RVhelio.> = -18.56 km s(-1) (sigma = 10.21 km s-1) and <[Fe/H]> = -0.68 (sigma = 0.08), respectively, in agreement with previous literature estimates. The average [Na/Fe] abundance is 0.12 dex lower in the 47 Tuc AGB sample compared to the RGB sample, and the ratio of Na-poor to Na-rich stars is 63: 37 on the AGB and 45: 55 on the RGB. However, in contrast to NGC 6752, the two 47 Tuc populations have nearly identical [Na/Fe] dispersion and interquartile range values. The data presented here suggest that only a small fraction (less than or similar to 20%) of Na-rich stars in 47 Tuc may fail to ascend the AGB, which is a similar result to that observed in M13. Regardless of the cause for the lower average [Na/Fe] abundance in AGB stars, we find that Na-poor stars and at least some Na-rich stars in 47 Tuc evolve through the early AGB phase. The contrasting behavior of Na-rich stars in 47 Tuc and NGC 6752 suggests that the RGB [Na/Fe] abundance alone is insufficient for predicting if a star will ascend the AGB. C1 [Johnson, Christian I.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [McDonald, Iain; Zijlstra, Albert A.] Jodrell Bank, Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Pilachowski, Catherine A.] Indiana Univ, Dept Astron, Bloomington, IN 47405 USA. [Mateo, Mario; Bailey, John I., III] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Cordero, Maria J.] Heidelberg Univ, Zentrum Astron, Heidelberg, Germany. [Crane, Jeffrey D.; Shectman, Stephen A.; Thompson, Ian] Carnegie Inst Washington Observ, Pasadena, CA 91101 USA. [Olszewski, Edward] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. RP Johnson, CI (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-15, Cambridge, MA 02138 USA. EM cjohnson@cfa.harvard.edu; iain.mcdonald-2@manchester.ac.uk; catyp@astro.indiana.edu; mmateo@umich.edu; baileyji@umich.edu; mjcorde@lsw.uni-heidelberg.de; albert.zijlstra@manchester.ac.uk; crane@obs.carnegiescience.edu; eolszewski@as.arizona.edu; shec@obs.carnegiescience.edu; ian@obs.carnegiescience.edu FU National Aeronautics and Space Administration; National Science Foundation; Clay Fellowship; Daniel Kirkwood Research Fund at Indiana University; German Research Foundation (DFG) [Sonderforschungs-bereich SFB 881]; National Science Foundation [AST-0923160, AST-1312997] FX We thank the anonymous referee for a thoughtful and constructive report that led to improvement of the manuscript. This research has made use of NASA's Astrophysics Data System Bibliographic Services. This publication has made 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. C.I.J. gratefully acknowledges support from the Clay Fellowship, administered by the Smithsonian Astrophysical Observatory. C.I.J. would like to thank Andrea Dupree and Nelson Caldwell for helpful discussions regarding data reduction. C.A.P. gratefully acknowledges support from the Daniel Kirkwood Research Fund at Indiana University. M.C. is supported by Sonderforschungs-bereich SFB 881 "The Milky Way System" (subproject A5) of the German Research Foundation (DFG). M.M. is grateful for support from the National Science Foundation to develop M2FS (AST-0923160) and carry out the observations reported here (AST-1312997) and to the University of Michigan for its direct support of M2FS construction and operation. NR 114 TC 18 Z9 18 U1 1 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 2015 VL 149 IS 2 AR 71 DI 10.1088/0004-6256/149/2/71 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CB1BA UT WOS:000349360200036 ER PT J AU Kimmig, B Seth, A Ivans, II Strader, J Caldwell, N Anderton, T Gregersen, D AF Kimmig, Brian Seth, Anil Ivans, Inese I. Strader, Jay Caldwell, Nelson Anderton, Tim Gregersen, Dylan TI MEASURING CONSISTENT MASSES FOR 25 MILKY WAY GLOBULAR CLUSTERS SO ASTRONOMICAL JOURNAL LA English DT Article DE globular clusters: general; globular clusters: individual (M2, M3, M14, M71, NGC 4147, NGC 5053, NGC 5466, NGC 6934, 47Tuc, M5, NGC 6441, M12, M15, M53, M92, NGC 6752, M4, M22, M30, M54, M55, M68, NGC 288, NGC 362) ID NA-O ANTICORRELATION; TO-LIGHT RATIOS; STELLAR POPULATION SYNTHESIS; COMPACT DWARF GALAXIES; STAR-CLUSTERS; HORIZONTAL BRANCHES; BLACK-HOLE; STRUCTURAL PARAMETERS; VELOCITY DISPERSIONS; ELLIPTIC GALAXIES AB We present central velocity dispersions, masses, mass-to-light ratios (M/Ls), and rotation strengths for 25 Galactic globular clusters (GCs). We derive radial velocities of 1951 stars in 12 GCs from single order spectra taken with Hectochelle on the MMT telescope. To this sample we add an analysis of available archival data of individual stars. For the full set of data we fit King models to derive consistent dynamical parameters for the clusters. We find good agreement between single-mass King models and the observed radial dispersion profiles. The large, uniform sample of dynamical masses we derive enables us to examine trends of M/L with cluster mass and metallicity. The overall values of M/L and the trends with mass and metallicity are consistent with existing measurements from a large sample of M31 clusters. This includes a clear trend of increasing M/L with cluster mass and lower than expected M/Ls for the metal-rich clusters. We find no clear trend of increasing rotation with increasing cluster metallicity suggested in previous work. C1 [Kimmig, Brian; Seth, Anil; Ivans, Inese I.; Anderton, Tim; Gregersen, Dylan] Univ Utah, SLC, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Strader, Jay] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Caldwell, Nelson] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kimmig, B (reprint author), Univ Utah, SLC, Dept Phys & Astron, Salt Lake City, UT 84112 USA. OI Seth, Anil/0000-0003-0248-5470 NR 69 TC 15 Z9 15 U1 1 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 2015 VL 149 IS 2 AR 53 DI 10.1088/0004-6256/149/2/53 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CB1BA UT WOS:000349360200018 ER PT J AU Sun, XH Rudnick, L Akahori, T Anderson, CS Bell, MR Bray, JD Farnes, JS Ideguchi, S Kumazaki, K O'Brien, T O'Sullivan, SP Scaife, AMM Stepanov, R Stil, J Takahashi, K van Weeren, RJ Wolleben, M AF Sun, X. H. Rudnick, L. Akahori, Takuya Anderson, C. S. Bell, M. R. Bray, J. D. Farnes, J. S. Ideguchi, S. Kumazaki, K. O'Brien, T. O'Sullivan, S. P. Scaife, A. M. M. Stepanov, R. Stil, J. Takahashi, K. van Weeren, R. J. Wolleben, M. TI COMPARISON OF ALGORITHMS FOR DETERMINATION OF ROTATION MEASURE AND FARADAY STRUCTURE. I. 1100-1400MHZ SO ASTRONOMICAL JOURNAL LA English DT Article DE ISM: magnetic fields; magnetic fields; polarization; radio continuum: general; techniques: polarimetric ID INTERGALACTIC MAGNETIC-FIELD; EXTRAGALACTIC RADIO-SOURCES; LARGE-MAGELLANIC-CLOUD; SIMILAR-TO 1; POLARIZED EMISSION; 350 MHZ; DEPOLARIZATION; GALAXIES; POLARIMETRY; TOMOGRAPHY AB Faraday rotation measures (RMs) and more general Faraday structures are key parameters for studying cosmic magnetism and are also sensitive probes of faint ionized thermal gas. A definition of which derived quantities are required for various scientific studies is needed, as well as addressing the challenges in determining Faraday structures. A wide variety of algorithms has been proposed to reconstruct these structures. In preparation for the Polarization Sky Survey of the Universe ' s Magnetism (POSSUM) to be conducted with the Australian Square Kilometre Array Pathfinder and the ongoing Galactic Arecibo L-band Feeds Array Continuum Transit Survey (GALFACTS), we run a Faraday structure determination data challenge to benchmark the currently available algorithms, including Faraday synthesis (previously called RM synthesis in the literature), wavelet, compressive sampling, and QU-fitting. The input models include sources with one Faraday thin component, two Faraday thin components, and one Faraday thick component. The frequency set is similar to POSSUM/GALFACTS with a 300 MHz bandwidth from 1.1 to 1.4 GHz. We define three figures of merit motivated by the underlying science: (1) an average RM weighted by polarized intensity, RMwtd, (2) the separation Df of two Faraday components, and (3) the reduced chi-squared c r 2. Based on the current test data with a signal-to-noise ratio of about 32, we find the following. (1) When only one Faraday thin component is present, most methods perform as expected, with occasional failures where two components are incorrectly found. (2) For two Faraday thin components, QU-fitting routines perform the best, with errors close to the theoretical ones for RMwtd but with significantly higher errors for Df. All other methods, including standard Faraday synthesis, frequently identify only one component when Df is below or near the width of the Faraday point-spread function. (3) No methods as currently implemented work well for Faraday thick components due to the narrow bandwidth. (4) There exist combinations of two Faraday components that produce a large range of acceptable fits and hence large uncertainties in the derived single RMs; in these cases, different RMs lead to the same Q, U behavior, so no method can recover a unique input model. Further exploration of all these issues is required before upcoming surveys will be able to provide reliable results on Faraday structures. C1 [Sun, X. H.; Akahori, Takuya; Anderson, C. S.; Farnes, J. S.; O'Sullivan, S. P.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia. [Rudnick, L.; O'Brien, T.] Univ Minnesota, Sch Phys & Astron, Minnesota Inst Astrophys, Minneapolis, MN 55455 USA. [Bell, M. R.] Max Planck Inst Astrophys, D-85748 Garching, Germany. [Bray, J. D.; Scaife, A. M. M.] Univ Southampton, Dept Phys & Astron, Southampton SO17 1BJ, Hants, England. [Ideguchi, S.; Kumazaki, K.] Nagoya Univ, Chikusa Ku, Nagoya, Aichi 4648601, Japan. [Stepanov, R.] Inst Continuous Media Mech, Perm 614061, Russia. [Stepanov, R.] Perm Natl Res Polytech Univ, Perm 614990, Russia. [Stil, J.; Wolleben, M.] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada. [Takahashi, K.] Kumamoto Univ, Kumamoto 8608555, Japan. [van Weeren, R. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Sun, XH (reprint author), Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia. EM x.sun@physics.usyd.edu.au; larry@umn.edu RI Stepanov, Rodion/D-2221-2009; Takahashi, Keitaro/L-5930-2015; OI Stepanov, Rodion/0000-0001-8098-0720; Farnes, Jamie/0000-0002-2809-4032; van Weeren, Reinout/0000-0002-0587-1660 NR 61 TC 7 Z9 7 U1 2 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD FEB PY 2015 VL 149 IS 2 AR 60 DI 10.1088/0004-6256/149/2/60 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CB1BA UT WOS:000349360200025 ER PT J AU Tingay, SJ Macquart, JP Collier, JD Rees, G Callingham, JR Stevens, J Carretti, E Wayth, RB Wong, GF Trott, CM McKinley, B Bernardi, G Bowman, JD Briggs, F Cappallo, RJ Corey, BE Deshpande, AA Emrich, D Gaensler, BM Goeke, R Greenhill, LJ Hazelton, BJ Johnston-Hollitt, M Kaplan, DL Kasper, JC Kratzenberg, E Lonsdale, CJ Lynch, MJ McWhirter, SR Mitchell, DA Morales, MF Morgan, E Oberoi, D Ord, SM Prabu, T Rogers, AEE Roshi, A Shankar, NU Srivani, KS Subrahmanyan, R Waterson, M Webster, RL Whitney, AR Williams, A Williams, CL AF Tingay, S. J. Macquart, J. -P. Collier, J. D. Rees, G. Callingham, J. R. Stevens, J. Carretti, E. Wayth, R. B. Wong, G. F. Trott, C. M. McKinley, B. Bernardi, G. Bowman, J. D. Briggs, F. Cappallo, R. J. Corey, B. E. Deshpande, A. A. Emrich, D. Gaensler, B. M. Goeke, R. Greenhill, L. J. Hazelton, B. J. Johnston-Hollitt, M. Kaplan, D. L. Kasper, J. C. Kratzenberg, E. Lonsdale, C. J. Lynch, M. J. McWhirter, S. R. Mitchell, D. A. Morales, M. F. Morgan, E. Oberoi, D. Ord, S. M. Prabu, T. Rogers, A. E. E. Roshi, A. Shankar, N. Udaya Srivani, K. S. Subrahmanyan, R. Waterson, M. Webster, R. L. Whitney, A. R. Williams, A. Williams, C. L. TI THE SPECTRAL VARIABILITY OF THE GHZ-PEAKED SPECTRUM RADIO SOURCE PKS 1718-649 AND A COMPARISON OF ABSORPTION MODELS SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: individual (NGC 6328, PKS 1718-649); radiation mechanisms: general; radio continuum: galaxies ID INTERSTELLAR SCINTILLATION; IMAGING SURVEY; SOUTHERN SKY; COMPACT; CATALOG; DESIGN; SUMSS AB Using the new wideband capabilities of the ATCA, we obtain spectra for PKS 1718-649, a well-known gigahertz-peaked spectrum radio source. The observations, between approximately 1 and 10 GHz over 3 epochs spanning approximately 21 months, reveal variability both above the spectral peak at similar to 3 GHz and below the peak. The combination of the low-and high-frequency variability cannot be easily explained using a single absorption mechanism, such as free-free absorption or synchrotron self-absorption. We find that the PKS 1718-649 spectrum and its variability are best explained by variations in the free-free optical depth on our line of sight to the radio source at low frequencies (below the spectral peak) and the adiabatic expansion of the radio source itself at high frequencies (above the spectral peak). The optical depth variations are found to be plausible when X-ray continuum absorption variability seen in samples of active galactic nuclei is considered. We find that the cause of the peaked spectrum in PKS 1718-649 is most likely due to free-free absorption. In agreement with previous studies, we find that the spectrum at each epoch of observation is best fit by a free-free absorption model characterized by a power-law distribution of free-free absorbing clouds. This agreement is extended to frequencies below the 1 GHz lower limit of the ATCA by considering new observations with Parkes at 725 MHz and 199 MHz observations with the newly operational Murchison Widefield Array. These lower frequency observations argue against families of absorption models (both free-free and synchrotron self-absorption) that are based on simple homogenous structures. C1 [Tingay, S. J.; Macquart, J. -P.; Wayth, R. B.; Trott, C. M.; Emrich, D.; Lynch, M. J.; Ord, S. M.; Waterson, M.; Williams, A.] Curtin Univ, Int Ctr Radio Astron Res, Bentley, WA 6102, Australia. [Collier, J. D.; Wong, G. F.] Univ Western Sydney, Penrith, NSW 2751, Australia. [Collier, J. D.; Rees, G.; Stevens, J.; Carretti, E.; Wong, G. F.; Mitchell, D. A.] CSIRO Astron & Space Sci CASS, Epping, NSW 1710, Australia. [Rees, G.] Macquarie Univ, N Ryde, NSW 2109, Australia. [Callingham, J. R.; Gaensler, B. M.] Univ Sydney, Sydney Inst Astron, Sch Phys SiFA, Sydney, NSW 2006, Australia. [Callingham, J. R.; Trott, C. M.; Gaensler, B. M.; Mitchell, D. A.; Subrahmanyan, R.; Webster, R. L.] ARC Ctr Excellence All Sky Astrophys CAASTRO, Sydney, NSW, Australia. [McKinley, B.; Briggs, F.] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia. [Bernardi, G.] Sq Kilometre Array South Africa, ZA-7405 Cape Town, South Africa. [Bowman, J. D.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Cappallo, R. J.; Corey, B. E.; Kratzenberg, E.; Lonsdale, C. J.; McWhirter, S. R.; Rogers, A. E. E.; Whitney, A. R.] MIT, Haystack Observ, Westford, MA 01886 USA. [Deshpande, A. A.; Prabu, T.; Shankar, N. Udaya; Srivani, K. S.; Subrahmanyan, R.] Raman Res Inst, Bangalore 560080, Karnataka, India. [Goeke, R.; Morgan, E.; Williams, C. L.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Greenhill, L. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hazelton, B. J.; Morales, M. F.] Univ Washington, Dept Phys, Seattle, WA 98195 USA. [Johnston-Hollitt, M.] Victoria Univ Wellington, Sch Chem & Phys Sci, Wellington 6140, New Zealand. [Kaplan, D. L.] Univ Wisconsin, Dept Phys, Milwaukee, WI 53201 USA. [Kasper, J. C.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Oberoi, D.] Tata Inst Fundamental Res, Natl Ctr Radio Astrophys, Pune 411007, Maharashtra, India. [Roshi, A.] Natl Radio Astron Observ, Charlottesville, VA USA. [Webster, R. L.] Univ Melbourne, Sch Phys, Parkville, Vic 3010, Australia. RP Tingay, SJ (reprint author), Curtin Univ, Int Ctr Radio Astron Res, Bentley, WA 6102, Australia. EM s.tingay@curtin.edu.au RI Williams, Andrew/K-2931-2013; M, Manjunath/N-4000-2014; Deshpande, Avinash/D-4868-2012; Udayashankar , N/D-4901-2012; Wayth, Randall/B-2444-2013; Emrich, David/B-7002-2013; Subrahmanyan, Ravi/D-4889-2012; Trott, Cathryn/B-5325-2013; OI Gaensler, Bryan/0000-0002-3382-9558; Williams, Andrew/0000-0001-9080-0105; M, Manjunath/0000-0001-8710-0730; Wayth, Randall/0000-0002-6995-4131; Emrich, David/0000-0002-4058-1837; Trott, Cathryn/0000-0001-6324-1766; Carretti, Ettore/0000-0002-3973-8403; Callingham, Joseph/0000-0002-7167-1819 FU U.S. National Science Foundation [AST-0457585, PHY-0835713, CAREER-0847753, AST-0908884]; Australian Research Council [LE0775621, LE0882938]; U.S. Air Force Office of Scientific Research [FA9550-0510247]; Centre for All-sky Astrophysics (an Australian Research Council Centre of Excellence) [CE110001020]; Smithsonian Astrophysical Observatory; MIT School of Science; Raman Research Institute; Australian National University; Victoria University of Wellington (New Zealand Ministry of Economic Development) [MED-E1799]; Victoria University of Wellington (IBM Shared University Research Grant) [MED-E1799]; Australian Federal government via the CSIRO; National Collaborative Research Infrastructure Strategy; Education Investment Fund; Australia India Strategic Research Fund; Astronomy Australia Limited; NVIDIA at Harvard University; International Centre for Radio Astronomy Research (ICRAR), a Joint Venture of Curtin University; University of Western Australia; Western Australian State government; Western Australian Government; Commonwealth of Australia FX This scientific work makes use of the Murchison Radio-astronomy Observatory, operated by the Commonwealth Scientific and Industrial Research Organisation (CSIRO). We acknowledge the Wajarri Yamatji people as the traditional owners of the Observatory site. Support for the MWA comes from the U.S. National Science Foundation (grants AST-0457585, PHY-0835713, CAREER-0847753, and AST-0908884), the Australian Research Council (LIEF grants LE0775621 and LE0882938), the U.S. Air Force Office of Scientific Research (grant FA9550-0510247), and the Centre for All-sky Astrophysics (an Australian Research Council Centre of Excellence funded by grant CE110001020). Support is also provided by the Smithsonian Astrophysical Observatory, the MIT School of Science, the Raman Research Institute, the Australian National University, and the Victoria University of Wellington (via grant MED-E1799 from the New Zealand Ministry of Economic Development and an IBM Shared University Research Grant). The Australian Federal government provides additional support via the CSIRO, National Collaborative Research Infrastructure Strategy, Education Investment Fund, the Australia India Strategic Research Fund, and Astronomy Australia Limited, under contract to Curtin University. We acknowledge the iVEC Petabyte Data Store, the Initiative in Innovative Computing and the CUDA Center for Excellence sponsored by NVIDIA at Harvard University, and the International Centre for Radio Astronomy Research (ICRAR), a Joint Venture of Curtin University and The University of Western Australia, funded by the Western Australian State government. SJT acknowledges support from the Western Australian Government via a Premier's Research Fellowship. The Australia Telescope Compact Array is part of the Australia Telescope National Facility which is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. The Parkes Radio Telescope is part of the Australia Telescope National Facility which is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. NR 28 TC 12 Z9 12 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD FEB PY 2015 VL 149 IS 2 AR 74 DI 10.1088/0004-6256/149/2/74 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CB1BA UT WOS:000349360200039 ER PT J AU Barriere, NM Krivonos, R Tomsick, JA Bachetti, M Boggs, SE Chakrabarty, D Christensen, FE Craig, WW Hailey, CJ Harrison, FA Hong, J Mori, K Stern, D Zhang, WW AF Barriere, Nicolas M. Krivonos, Roman Tomsick, John A. Bachetti, Matteo Boggs, Steven E. Chakrabarty, Deepto Christensen, Finn E. Craig, William W. Hailey, Charles J. Harrison, Fiona A. Hong, Jaesub Mori, Kaya Stern, Daniel Zhang, William W. TI NuSTAR OBSERVATION OF A TYPE I X-RAY BURST FROM GRS 1741.9-2853 SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion; accretion disks; nuclear reactions; nucleosynthesis; abundances; stars: neutron; X-rays: binaries; X-rays: bursts; X-rays: individual (GRS 1741.9-2853) ID GALACTIC-CENTER REGION; PHOTOSPHERIC RADIUS EXPANSION; ACCRETING NEUTRON-STARS; ABSORPTION-LINES; SHELL FLASHES; EXO 0748-676; MILKY-WAY; SPECTRA; BINARY; DISCOVERY AB We report on two NuSTAR observations of GRS 1741.9-2853, a faint neutron star (NS) low-mass X-ray binary burster located 10 ' away from the Galactic center. NuSTAR detected the source serendipitously as it was emerging from quiescence: its luminosity was 6x10(34) erg s(-1) on 2013 July 31 and 5x10(35) erg s(-1) in a second observation on 2013 August 3. A bright, 800 s long, H-triggered mixed H/He thermonuclear Type I burst with mild photospheric radius expansion (PRE) was present during the second observation. Assuming that the luminosity during the PRE was at the Eddington level, an H mass fraction X = 0.7 in the atmosphere, and an NS mass M = 1.4 M-circle dot, we determine a new lower limit on the distance for this source of 6.3 +/- 0.5 kpc. Combining with previous upper limits, this places GRS 1741.9-2853 at a distance of 7 kpc. Energy independent (achromatic) variability is observed during the cooling of the NS, which could result from the disturbance of the inner accretion disk by the burst. The large dynamic range of this burst reveals a long power-law decay tail. We also detect, at a 95.6% confidence level (1.7 sigma), a narrow absorption line at 5.46 +/- 0.10 keV during the PRE phase of the burst, reminiscent of the detection by Waki et al. We propose that the line, if real, is formed in the wind above the photosphere of the NS by a resonant K alpha transition from H-like Cr gravitationally redshifted by a factor 1 + z = 1.09, corresponding to a radius range of 29.0-41.4 km for a mass range of 1.4-2.0 M-circle dot. C1 [Barriere, Nicolas M.; Krivonos, Roman; Tomsick, John A.; Boggs, Steven E.; Craig, William W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Bachetti, Matteo] Inst Rech Astrophys & Plantol, UMR 5277, Toulouse, France. [Chakrabarty, Deepto] MIT, MIT Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Christensen, Finn E.] Tech Univ Denmark, Natl Space Inst, Copenhagen, Denmark. [Craig, William W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Hailey, Charles J.; Mori, Kaya] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Harrison, Fiona A.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Hong, Jaesub] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Zhang, William W.] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA. RP Barriere, NM (reprint author), Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. EM barriere@ssl.berkeley.edu RI Boggs, Steven/E-4170-2015; OI Boggs, Steven/0000-0001-9567-4224; Bachetti, Matteo/0000-0002-4576-9337 FU NASA [NNG08FD60C]; National Aeronautics and Space Administration FX This work was supported under NASA contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTAR-DAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). The authors thank Nevin Weinberg for useful discussions, and the anonymous referee for constructive comments. NR 69 TC 5 Z9 5 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2015 VL 799 IS 2 AR 123 DI 10.1088/0004-637X/799/2/123 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CA3QH UT WOS:000348820900010 ER PT J AU Batygin, K Morbidelli, A Holman, MJ AF Batygin, Konstantin Morbidelli, Alessandro Holman, Mathew J. TI CHAOTIC DISINTEGRATION OF THE INNER SOLAR SYSTEM SO ASTROPHYSICAL JOURNAL LA English DT Article DE celestial mechanics; planets and satellites: dynamical evolution and stability ID MEAN MOTION RESONANCES; PLANET-PLANET SCATTERING; OUTER ASTEROID BELT; LARGE-SCALE CHAOS; SECULAR RESONANCES; 3-BODY PROBLEM; DYNAMICAL INSTABILITIES; SUCCESSIVE ELIMINATION; ANALYTIC MODEL; GIANT PLANETS AB On timescales that greatly exceed an orbital period, typical planetary orbits evolve in a stochastic yet stable fashion. On even longer timescales, however, planetary orbits can spontaneously transition from bounded to unbound chaotic states. Large-scale instabilities associated with such behavior appear to play a dominant role in shaping the architectures of planetary systems, including our own. Here we show how such transitions are possible, focusing on the specific case of the long-term evolution of Mercury. We develop a simple analytical model for Mercury's dynamics and elucidate the origins of its short-term stochastic behavior as well as of its sudden progression to unbounded chaos. Our model allows us to estimate the timescale on which this transition is likely to be triggered, i.e., the dynamical lifetime of the solar system as we know it. The formulated theory is consistent with the results of numerical simulations and is broadly applicable to extrasolar planetary systems dominated by secular interactions. These results constitute a significant advancement in our understanding of the processes responsible for sculpting of the dynamical structures of generic planetary systems. C1 [Batygin, Konstantin] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Morbidelli, Alessandro] Observ Cote Azur, Dept Lagrange, F-06304 Nice, France. [Holman, Mathew J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Batygin, K (reprint author), CALTECH, Div Geol & Planetary Sci, 1200 East Calif Blvd, Pasadena, CA 91125 USA. NR 104 TC 12 Z9 12 U1 2 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2015 VL 799 IS 2 AR 120 DI 10.1088/0004-637X/799/2/120 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CA3QH UT WOS:000348820900007 ER PT J AU Bocquet, S Saro, A Mohr, JJ Aird, KA Ashby, MLN Bautz, M Bayliss, M Bazin, G Benson, BA Bleem, LE Brodwin, M Carlstrom, JE Chang, CL Chiu, I Cho, HM Clocchiatti, A Crawford, TM Crites, AT Desai, S de Haan, T Dietrich, JP Dobbs, MA Foley, RJ Forman, WR Gangkofner, D George, EM Gladders, MD Gonzalez, AH Halverson, NW Hennig, C Hlavacek-Larrondo, J Holder, GP Holzapfel, WL Hrubes, JD Jones, C Keisler, R Knox, L Lee, AT Leitch, EM Liu, J Lueker, M Luong-Van, D Marrone, DP McDonald, M McMahon, JJ Meyer, SS Mocanu, L Murray, SS Padin, S Pryke, C Reichardt, CL Rest, A Ruel, J Ruhl, JE Saliwanchik, BR Sayre, JT Schaffer, KK Shirokoff, E Spieler, HG Stalder, B Stanford, SA Staniszewski, Z Stark, AA Story, K Stubbs, CW Vanderlinde, K Vieira, JD Vikhlinin, A Williamson, R Zahn, O Zenteno, A AF Bocquet, S. Saro, A. Mohr, J. J. Aird, K. A. Ashby, M. L. N. Bautz, M. Bayliss, M. Bazin, G. Benson, B. A. Bleem, L. E. Brodwin, M. Carlstrom, J. E. Chang, C. L. Chiu, I. Cho, H. M. Clocchiatti, A. Crawford, T. M. Crites, A. T. Desai, S. de Haan, T. Dietrich, J. P. Dobbs, M. A. Foley, R. J. Forman, W. R. Gangkofner, D. George, E. M. Gladders, M. D. Gonzalez, A. H. Halverson, N. W. Hennig, C. Hlavacek-Larrondo, J. Holder, G. P. Holzapfel, W. L. Hrubes, J. D. Jones, C. Keisler, R. Knox, L. Lee, A. T. Leitch, E. M. Liu, J. Lueker, M. Luong-Van, D. Marrone, D. P. McDonald, M. McMahon, J. J. Meyer, S. S. Mocanu, L. Murray, S. S. Padin, S. Pryke, C. Reichardt, C. L. Rest, A. Ruel, J. Ruhl, J. E. Saliwanchik, B. R. Sayre, J. T. Schaffer, K. K. Shirokoff, E. Spieler, H. G. Stalder, B. Stanford, S. A. Staniszewski, Z. Stark, A. A. Story, K. Stubbs, C. W. Vanderlinde, K. Vieira, J. D. Vikhlinin, A. Williamson, R. Zahn, O. Zenteno, A. TI MASS CALIBRATION AND COSMOLOGICAL ANALYSIS OF THE SPT-SZ GALAXY CLUSTER SAMPLE USING VELOCITY DISPERSION sigma(v) AND X-RAY Y-X MEASUREMENTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic background radiation; cosmology: observations; galaxies: clusters: individual; large-scale structure of universe ID SOUTH-POLE TELESCOPE; BARYON ACOUSTIC-OSCILLATIONS; DIGITAL SKY SURVEY; HUBBLE-SPACE-TELESCOPE; 720 SQUARE DEGREES; GREATER-THAN 1; SCALING RELATIONS; OBSERVED GROWTH; CONSTRAINTS; CATALOG AB We present a velocity-dispersion-based mass calibration of the South Pole Telescope Sunyaev-Zel'dovich effect survey (SPT-SZ) galaxy cluster sample. Using a homogeneously selected sample of 100 cluster candidates from 720 deg(2) of the survey along with 63 velocity dispersion (sigma(v)) and 16 X-ray Y-X measurements of sample clusters, we simultaneously calibrate the mass-observable relation and constrain cosmological parameters. Our method accounts for cluster selection, cosmological sensitivity, and uncertainties in the mass calibrators. The calibrations using sigma(v) and Y-X are consistent at the 0.6 sigma level, with the sigma(v) calibration preferring similar to 16% higher masses. We use the full SPTCL data set (SZ clusters+sigma(v)+Y-X) to measure sigma(8)(Omega(m)/0.27)(0.3) = 0.809 +/- 0.036 within a flat ACDM model. The SPT cluster abundance is lower than preferred by either the WMAP9 or Planck+WMAP9 polarization (WP) data, but assuming that the sum of the neutrino masses is Sigma m(upsilon) = 0.06 eV, we find the data sets to be consistent at the 1.0 sigma level for WMAP9 and 1.5 sigma for Planck+WP. Allowing for larger Sigma m(upsilon) further reconciles the results. When we combine the SPTCL and Planck+WP data sets with information from baryon acoustic oscillations and Type Ia supernovae, the preferred cluster masses are 1.9 sigma higher than the Y-X calibration and 0.8 sigma higher than the sigma(v) calibration. Given the scale of these shifts (similar to 44% and similar to 23% in mass, respectively), we execute a goodness-of-fit test; it reveals no tension, indicating that the best-fit model provides an adequate description of the data. Using the multi-probe data set, we measure Omega(m) = 0.299 +/- 0.009 and sigma(8) = 0.829 +/- 0.011. Within upsilon CDM model we find Sigma m(upsilon) = 0.148 +/- 0.081 eV. We present a consistency test of the cosmic growth rate using SPT clusters. Allowing both the growth index gamma and the dark energy equation-of-state parameter w to vary, we find gamma = 0.73 +/- 0.28 and w = -1.007 +/- 0.065, demonstrating that the expansion and the growth histories are consistent with ACDM universe (gamma = 0.55; w = -1). C1 [Bocquet, S.; Saro, A.; Mohr, J. J.; Bazin, G.; Chiu, I.; Desai, S.; Dietrich, J. P.; Gangkofner, D.; Hennig, C.; Liu, J.; Zenteno, A.] Univ Munich, Dept Phys, D-81679 Munich, Germany. [Bocquet, S.; Mohr, J. J.; Desai, S.; Dietrich, J. P.; Gangkofner, D.; Liu, J.] Excellence Cluster Univ, D-85748 Garching, Germany. [Mohr, J. J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Aird, K. A.; Hrubes, J. D.; Luong-Van, D.] Univ Chicago, Chicago, IL 60637 USA. [Ashby, M. L. N.; Bayliss, M.; Foley, R. J.; Forman, W. R.; Jones, C.; Murray, S. S.; Stalder, B.; Stark, A. A.; Stubbs, C. W.; Vikhlinin, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bautz, M.; McDonald, M.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Bayliss, M.; Ruel, J.; Stubbs, C. W.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Benson, B. A.] Fermilab Natl Accelerator Lab, Batavia, IL 60510 USA. [Benson, B. A.; Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.; Crawford, T. M.; Crites, A. T.; Gladders, M. D.; Keisler, R.; Leitch, E. M.; Meyer, S. S.; Mocanu, L.; Padin, S.; Schaffer, K. K.; Story, K.; Williamson, R.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Benson, B. A.; Carlstrom, J. E.; Crawford, T. M.; Crites, A. T.; Gladders, M. D.; Leitch, E. M.; Meyer, S. S.; Mocanu, L.; Padin, S.; Williamson, R.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Bleem, L. E.; Carlstrom, J. E.; Keisler, R.; Meyer, S. S.; Story, K.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA. [Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.] Argonne Natl Lab, Div High Energy Phys, Argonne, IL 60439 USA. [Brodwin, M.] Univ Missouri, Dept Phys & Astron, Kansas City, MO 64110 USA. [Carlstrom, J. E.; Chang, C. L.; Meyer, S. S.; Schaffer, K. K.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Cho, H. M.] NIST, Quantum Devices Grp, Boulder, CO 80305 USA. [Clocchiatti, A.] Pontificia Univ Catolica Chile, Dept Astron & Astrosif, Santiago, Chile. [Crites, A. T.; Lueker, M.; Padin, S.; Shirokoff, E.; Staniszewski, Z.; Williamson, R.] CALTECH, Pasadena, CA 91125 USA. [de Haan, T.; Dobbs, M. A.; Holder, G. P.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Foley, R. J.; Vieira, J. D.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA. [Foley, R. J.; Vieira, J. D.] Univ Illinois, Dept Phys, Urbana, IL 61801 USA. [George, E. M.; Holzapfel, W. L.; Lee, A. T.; Lueker, M.; Reichardt, C. L.; Shirokoff, E.; Zahn, O.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Gonzalez, A. H.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Halverson, N. W.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. [Halverson, N. W.] Univ Colorado, Dept Phys, Boulder, CO 80309 USA. [Hlavacek-Larrondo, J.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Hlavacek-Larrondo, J.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Knox, L.; Stanford, S. A.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Lee, A. T.; Spieler, H. G.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Phys, Berkeley, CA 94720 USA. [Marrone, D. P.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [McMahon, J. J.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Pryke, C.] Univ Minnesota, Dept Phys, Minneapolis, MN 55455 USA. [Reichardt, C. L.] Univ Melbourne, Sch Phys, Melbourne, Vic 3010, Australia. [Rest, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Ruhl, J. E.; Saliwanchik, B. R.; Sayre, J. T.; Staniszewski, Z.] Case Western Reserve Univ, Ctr Educ & Res Cosmol & Astrophys, Dept Phys, Cleveland, OH 44106 USA. [Schaffer, K. K.] Sch Art, Inst Chicago, Liberal Arts Dept, Chicago, IL 60603 USA. [Stanford, S. A.] Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94551 USA. [Vanderlinde, K.] Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Vanderlinde, K.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Zahn, O.] Univ Calif Berkeley, Dept Phys, Berkeley Ctr Cosmol Phys, Berkeley, CA 94720 USA. [Zahn, O.] Lawrence Berkeley Natl Labs, Berkeley, CA 94720 USA. [Zenteno, A.] Cerro Tololo Interamer Observ, La Serena, Chile. RP Bocquet, S (reprint author), Univ Munich, Dept Phys, Scheinerstr 1, D-81679 Munich, Germany. EM bocquet@usm.lmu.de RI Williamson, Ross/H-1734-2015; Holzapfel, William/I-4836-2015; OI Williamson, Ross/0000-0002-6945-2975; Marrone, Daniel/0000-0002-2367-1080 FU DFG Cluster of Excellence "Origin and Structure of the Universe"; Transregio program TR33 "The Dark Universe"; NASA; National Science Foundation [PLR-1248097]; NSF Physics Frontier Center [PHY-1125897]; Kavli Foundation; Gordon and Betty Moore Foundation [GBMF 947]; NSF [AST-1009012, AST-1009649, MRI-0723073]; UChicago Argonne, LLC, Operator of Argonne National Laboratory ("Argonne"); Argonne, a U.S. Department of Energy Office of Science Laboratory [DE-AC02-06CH11357]; National Sciences and Engineering Research Council of Canada; Canada Research Chairs Program; Canadian Institute for Advanced Research FX We acknowledge the support of the DFG Cluster of Excellence "Origin and Structure of the Universe" and the Transregio program TR33 "The Dark Universe." The calculations have been carried out on the computing facilities of the Computational Center for Particle and Astrophysics (C2PAP) and of the Leibniz Supercomputer Center (LRZ). Optical spectroscopic data from VLT programs 086.A-0741 and 286.A-5021 and Gemini program GS-2009B-Q-16 were included in this work. Additional data were obtained with the 6.5 m Magellan Telescopes, which is located at the Las Campanas Observatory in Chile. 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 South Pole Telescope is supported by the National Science Foundation through grant PLR-1248097. Partial support is also provided by the NSF Physics Frontier Center grant PHY-1125897 to the Kavli Institute of Cosmological Physics at the University of Chicago, the Kavli Foundation and the Gordon and Betty Moore Foundation grant GBMF 947. Galaxy cluster research at Harvard is supported by NSF grant AST-1009012, and research at SAO is supported in part by NSF grants AST-1009649 and MRI-0723073. Work at Argonne National Lab is supported by UChicago Argonne, LLC, Operator of Argonne National Laboratory ("Argonne"). Argonne, a U.S. Department of Energy Office of Science Laboratory, is operated under Contract No. DE-AC02-06CH11357. The McGill group acknowledges funding from the National Sciences and Engineering Research Council of Canada, Canada Research Chairs Program, and the Canadian Institute for Advanced Research. NR 83 TC 29 Z9 29 U1 1 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2015 VL 799 IS 2 AR 214 DI 10.1088/0004-637X/799/2/214 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CA3QH UT WOS:000348820900101 ER PT J AU Cleeves, LI Bergin, EA Qi, CH Adams, FC Oberg, KI AF Cleeves, L. Ilsedore Bergin, Edwin A. Qi, Chunhua Adams, Fred C. Oeberg, Karin I. TI CONSTRAINING THE X-RAY AND COSMIC-RAY IONIZATION CHEMISTRY OF THE TW Hya PROTOPLANETARY DISK: EVIDENCE FOR A SUB-INTERSTELLAR COSMIC-RAY RATE SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; astrochemistry; circumstellar matter; stars: pre-main sequence ID MAIN-SEQUENCE STARS; TAURI STARS; CIRCUMSTELLAR DISKS; HYDRAE ASSOCIATION; MAGNETOROTATIONAL INSTABILITY; RADIATIVE-TRANSFER; ACCRETION DISKS; FAR-ULTRAVIOLET; SOLAR NEBULA; YOUNG STARS AB We present an observational and theoretical study of the primary ionizing agents (cosmic rays (CRs) and X-rays) in the TW Hya protoplanetary disk. We use a set of resolved and unresolved observations of molecular ions and other molecular species, encompassing 11 lines total, in concert with a grid of disk chemistry models. The molecular ion constraints comprise new data from the Submillimeter Array on HCO+, acquired at unprecedented spatial resolution, and data from the literature, including ALMA observations of N2H+. We vary the model incident CR flux and stellar X-ray spectra and find that TW Hya's HCO+ and N2H+ emission are best-fit by a moderately hard X-ray spectra, as would be expected during the "flaring" state of the star, and a low CR ionization rate, zeta CR less than or similar to 10(-19) s(-1). This low CR rate is the first indication of the presence of CR exclusion by winds and/or magnetic fields in an actively accreting T Tauri disk system. With this new constraint, our best-fit ionization structure predicts a low turbulence "dead-zone" extending from the inner edge of the disk out to 50-65 AU. This region coincides with an observed concentration of millimeter grains, and we propose that the inner region of TW Hya is a dust (and possibly planet) growth factory as predicted by previous theoretical work. C1 [Cleeves, L. Ilsedore; Bergin, Edwin A.; Adams, Fred C.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Qi, Chunhua; Oeberg, Karin I.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Adams, Fred C.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. RP Cleeves, LI (reprint author), Univ Michigan, Dept Astron, 1085 South Univ Ave, Ann Arbor, MI 48109 USA. OI Cleeves, L. Ilsedore/0000-0003-2076-8001 FU Simons Collaboration on the Origins of Life (SCOL) program; NASA Origins of solar systems [NNX11AK63G]; [AST-1008800] FX The authors wish to thank the anonymous referee and editor for their helpful comments. L.I.C. and E.A.B. acknowledge grant AST-1008800 and K.O. acknowledges support from the Simons Collaboration on the Origins of Life (SCOL) program. C.Q. acknowledges grant NASA Origins of solar systems, grant number NNX11AK63G. The Atacama Large Millimeter/submillimeter Array (ALMA), an international astronomy facility, is a partnership of Europe, North America, and East Asia in cooperation with the Republic of Chile. This paper makes use of the following ALMA Science Verification data: ADS/JAO.ALMA#2011.0.00001.SV. NR 144 TC 25 Z9 25 U1 1 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2015 VL 799 IS 2 AR 204 DI 10.1088/0004-637X/799/2/204 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CA3QH UT WOS:000348820900091 ER PT J AU George, EM Reichardt, CL Aird, KA Benson, BA Bleem, LE Carlstrom, JE Chang, CL Cho, HM Crawford, TM Crites, AT de Haan, T Dobbs, MA Dudley, J Halverson, NW Harrington, NL Holder, GP Holzapfel, WL Hou, Z Hrubes, JD Keisler, R Knox, L Lee, AT Leitch, EM Lueker, M Luong-Van, D McMahon, JJ Mehl, J Meyer, SS Millea, M Mocanu, LM Mohr, JJ Montroy, TE Padin, S Plagge, T Pryke, C Ruhl, JE Schaffer, KK Shaw, L Shirokoff, E Spieler, HG Staniszewski, Z Stark, AA Story, KT van Engelen, A Vanderlinde, K Vieira, JD Williamson, R Zahn, O AF George, E. M. Reichardt, C. L. Aird, K. A. Benson, B. A. Bleem, L. E. Carlstrom, J. E. Chang, C. L. Cho, H-M. Crawford, T. M. Crites, A. T. de Haan, T. Dobbs, M. A. Dudley, J. Halverson, N. W. Harrington, N. L. Holder, G. P. Holzapfel, W. L. Hou, Z. Hrubes, J. D. Keisler, R. Knox, L. Lee, A. T. Leitch, E. M. Lueker, M. Luong-Van, D. McMahon, J. J. Mehl, J. Meyer, S. S. Millea, M. Mocanu, L. M. Mohr, J. J. Montroy, T. E. Padin, S. Plagge, T. Pryke, C. Ruhl, J. E. Schaffer, K. K. Shaw, L. Shirokoff, E. Spieler, H. G. Staniszewski, Z. Stark, A. A. Story, K. T. van Engelen, A. Vanderlinde, K. Vieira, J. D. Williamson, R. Zahn, O. TI A MEASUREMENT OF SECONDARY COSMIC MICROWAVE BACKGROUND ANISOTROPIES FROM THE 2500 SQUARE-DEGREE SPT-SZ SURVEY SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic background radiation; cosmology: observations; dark ages, reionization, first stars; diffuse radiation; large-scale structure of universe ID SOUTH-POLE TELESCOPE; STAR-FORMING GALAXIES; BARYON ACOUSTIC-OSCILLATIONS; ATACAMA COSMOLOGY TELESCOPE; ZELDOVICH POWER SPECTRUM; SUNYAEV-ZELDOVICH; CLUSTER PHYSICS; SOURCE CATALOG; DUST EMISSION; INHOMOGENEOUS REIONIZATION AB We present measurements of secondary cosmic microwave background (CMB) anisotropies and cosmic infrared background (CIB) fluctuations using data from the South Pole Telescope (SPT) covering the complete 2540 deg(2) SPT-SZ survey area. Data in the three SPT-SZ frequency bands centered at 95, 150, and 220 GHz, are used to produce six angular power spectra (three single-frequency auto-spectra and three cross-spectra) covering the multipole range 2000 < l < 11,000 (angular scales 5' greater than or similar to theta greater than or similar to 1'). These are the most precise measurements of the angular power spectra at l > 2500 at these frequencies. The main contributors to the power spectra at these angular scales and frequencies are the primary CMB, CIB, thermal and kinematic Sunyaev-Zel'dovich effects (tSZ and kSZ), and radio galaxies. We include a constraint on the tSZ power from a measurement of the tSZ bispectrum from 800 deg(2) of the SPT-SZ survey. We measure the tSZ power at 143 GHz to be D-3000(tSZ) = 4.08(-0.67)(+0.58) mu K-2 and the kSZ power to be D-3000(kSZ) = 2.9 +/- 1.3 mu K-2. The data prefer positive kSZ power at 98.1% CL. We measure a correlation coefficient of xi = 0.113(-0.054)(+0.057) between sources of tSZ and CIB power, with xi < 0 disfavored at a confidence level of 99.0%. The constraint on kSZ power can be interpreted as an upper limit on the duration of reionization. When the post-reionization homogeneous kSZ signal is accounted for, we find an upper limit on the duration Delta z < 5.4 at 95% CL. C1 [George, E. M.; Reichardt, C. L.; Harrington, N. L.; Holzapfel, W. L.; Lee, A. T.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [George, E. M.; Mohr, J. J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Reichardt, C. L.] Univ Melbourne, Sch Phys, Parkville, Vic 3010, Australia. [Aird, K. A.; Hrubes, J. D.; Luong-Van, D.] Univ Chicago, Chicago, IL 60637 USA. [Benson, B. A.; Carlstrom, J. E.; Crawford, T. M.; Crites, A. T.; Leitch, E. M.; Meyer, S. S.; Mocanu, L. M.; Padin, S.; Plagge, T.; Shirokoff, E.; Williamson, R.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Benson, B. A.; Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.; Crawford, T. M.; Crites, A. T.; Keisler, R.; Leitch, E. M.; Mehl, J.; Meyer, S. S.; Mocanu, L. M.; Padin, S.; Plagge, T.; Schaffer, K. K.; Shirokoff, E.; Story, K. T.; Williamson, R.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Benson, B. A.] Fermilab Natl Accelerator Lab, Batavia, IL 60510 USA. [Bleem, L. E.; Carlstrom, J. E.; Keisler, R.; Meyer, S. S.; Story, K. T.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA. [Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.; Mehl, J.] Argonne Natl Lab, Argonne, IL 60439 USA. [Carlstrom, J. E.; Chang, C. L.; Meyer, S. S.; Schaffer, K. K.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Cho, H-M.] NIST, Quantum Devices Grp, Boulder, CO 80305 USA. [Crites, A. T.; Lueker, M.; Padin, S.] CALTECH, Pasadena, CA 91125 USA. [de Haan, T.; Dobbs, M. A.; Dudley, J.; Holder, G. P.; Shaw, L.; van Engelen, A.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Halverson, N. W.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. [Halverson, N. W.] Univ Colorado, Dept Phys, Boulder, CO 80309 USA. [Hou, Z.; Knox, L.; Millea, M.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Keisler, R.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Keisler, R.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Lee, A. T.; Spieler, H. G.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Phys, Berkeley, CA 94720 USA. [McMahon, J. J.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Mohr, J. J.] Univ Munich, Dept Phys, D-81679 Munich, Germany. [Mohr, J. J.] Excellence Cluster Universe, D-85748 Garching, Germany. [Montroy, T. E.; Ruhl, J. E.; Staniszewski, Z.] Case Western Reserve Univ, Dept Phys, Ctr Educ & Res Cosmol & Astrophys, Cleveland, OH 44106 USA. [Pryke, C.] Univ Minnesota, Dept Phys, Minneapolis, MN 55455 USA. [Schaffer, K. K.] Sch Art Inst Chicago, Liberal Arts Dept, Chicago, IL 60603 USA. [Stark, A. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Vanderlinde, K.] Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Vanderlinde, K.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Vieira, J. D.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA. [Vieira, J. D.] Univ Illinois, Dept Phys, Urbana, IL 61801 USA. [Zahn, O.] Univ Calif Berkeley, Berkeley Ctr Cosmol Phys, Dept Phys, Berkeley, CA 94720 USA. [Zahn, O.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. RP George, EM (reprint author), Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. EM lizinvt@berkeley.edu RI Williamson, Ross/H-1734-2015; Holzapfel, William/I-4836-2015; OI Williamson, Ross/0000-0002-6945-2975; Aird, Kenneth/0000-0003-1441-9518; Reichardt, Christian/0000-0003-2226-9169; Stark, Antony/0000-0002-2718-9996 FU National Science Foundation [PLR-1248097]; NSF Physics Frontier Center [PHY-1125897]; Kavli Foundation; Gordon and Betty Moore Foundation [GBMF 947]; National Sciences and Engineering Research Council of Canada; Canada Research Chairs program; Canadian Institute for Advanced Research; NASA Hubble Fellowship [HF-51275.01]; Alfred P. Sloan Research Fellowship; Office of Science of the U.S. Department of Energy [DE-AC02-05CH11231]; NASA Office of Space Science FX The South Pole Telescope is supported by the National Science Foundation through grant PLR-1248097. Partial support is also provided by the NSF Physics Frontier Center grant PHY-1125897 to the Kavli Institute of Cosmological Physics at the University of Chicago, the Kavli Foundation, and the Gordon and Betty Moore Foundation grant GBMF 947. The McGill group acknowledges funding from the National Sciences and Engineering Research Council of Canada, Canada Research Chairs program, and the Canadian Institute for Advanced Research. R. Keisler acknowledges support from NASA Hubble Fellowship grant HF-51275.01. M. Dobbs acknowledges support from an Alfred P. Sloan Research Fellowship. This research used resources of the National Energy Research Scientific Computing Center, which is supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231. We acknowledge the use of the Legacy Archive for Microwave Background Data Analysis (LAMBDA). Support for LAMBDA is provided by the NASA Office of Space Science. NR 102 TC 41 Z9 41 U1 2 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2015 VL 799 IS 2 AR 177 DI 10.1088/0004-637X/799/2/177 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CA3QH UT WOS:000348820900064 ER PT J AU Kozarev, KA Raymond, JC Lobzin, VV Hammer, M AF Kozarev, K. A. Raymond, J. C. Lobzin, V. V. Hammer, M. TI PROPERTIES OF A CORONAL SHOCK WAVE AS A DRIVER OF EARLY SEP ACCELERATION SO ASTROPHYSICAL JOURNAL LA English DT Article DE acceleration of particles; Sun: coronal mass ejections (CMEs); shock waves; Sun: flares; Sun: radio radiation; Sun: UV radiation ID EMISSION MEASURE ANALYSIS; EXTREME-ULTRAVIOLET WAVE; SOLAR PARTICLE EVENTS; MASS EJECTIONS; ACTIVE REGIONS; HIGH-ENERGIES; SDO/AIA; FRONTS; ORIGIN; IMAGES AB Coronal mass ejectmons (CMEs) are thought to drive collisionless shocks in the solar corona, which in turn have been shown to be capable of accelerating solar energetic particles (SEPs) in minutes. It has been notoriously difficult to extract information about energetic particle spectra in the corona, owing to a lack of in situ measurements. It is possible, however, to combine remote observations with data-driven models in order to deduce coronal shock properties relevant to the local acceleration of SEPs and their heliospheric connectivity to near-Earth space. We present such novel analysis applied to the 2011 May 11 CME event on the western solar limb, focusing on the evolution of the eruption-driven, dome-like shock wave observed by the Atmospheric Imaging Assembly (AIA) EUV telescopes on board the Solar Dynamics Observatory spacecraft. We analyze the shock evolution and estimate its strength using emission measure modeling. We apply a new method combining a geometric model of the shock front with a potential field source surface model to estimate time-dependent field-to-shock angles and heliospheric connectivity during shock passage in the low corona. We find that the shock was weak, with an initial speed of similar to 450 km s(-1). It was initially mostly quasi-parallel, but a significant portion of it turned quasi-perpendicular later in the event. There was good magnetic connectivity to near-Earth space toward the end of the event as observed by the AIA instrument. The methods used in this analysis hold a significant potential for early characterization of coronal shock waves and forecasting of SEP spectra based on remote observations. C1 [Kozarev, K. A.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Raymond, J. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lobzin, V. V.] Learmonth Solar Observ, Exmouth, WA 6707, Australia. [Hammer, M.] Cornell Univ, Dept Phys, Ithaca, NY 14853 USA. [Lobzin, V. V.] Univ Sydney, Sch Phys, Sydney, NSW 2006, Australia. RP Kozarev, KA (reprint author), Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. EM kkozarev@cfa.harvard.edu FU AIA subcontract from Lockheed-Martin [SP02H1701R]; NASA; Star Jack Eddy Postdoctoral Fellowship Program FX We acknowledge support under AIA subcontract SP02H1701R from Lockheed-Martin. K. A. K. was supported under the NASA Living with a Star Jack Eddy Postdoctoral Fellowship Program, administered by the UCAR Visiting Scientist Programs. NR 24 TC 4 Z9 4 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2015 VL 799 IS 2 AR 167 DI 10.1088/0004-637X/799/2/167 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CA3QH UT WOS:000348820900054 ER PT J AU Martin-Drumel, MA Hindle, F Mouret, G Cuisset, A Cernicharo, J AF Martin-Drumel, M. A. Hindle, F. Mouret, G. Cuisset, A. Cernicharo, J. TI A COMPLETE SPECTROSCOPIC CHARACTERIZATION OF SO AND ITS ISOTOPOLOGUES UP TO THE TERAHERTZ DOMAIN SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: lines and bands; ISM: molecules; line: identification; molecular data ID EXCITED VIBRATIONAL-STATES; SULFUR MONOXIDE; MICROWAVE-SPECTRUM; ELECTRONIC STATES; DUNHAM COEFFICIENTS; HYPERFINE-STRUCTURE; ISOTOPE DEPENDENCE; WAVE SPECTROSCOPY; LASER PHOTOLYSIS; BAND AB In order to obtain accurate terahertz center frequencies for SO and its isotopologues, we have studied the absorption spectrum of SO, (SO)-S-34, and (SO)-S-33 up to 2.5 THz using continuous-wave terahertz photomixing based on a frequency comb providing an accuracy down to 10 kHz. Sulfur monoxide was produced in a radio frequency discharge of air in a cell containing pure sulfur. Together with the strong absorption signal of the main isotopologue, transitions of (SO)-S-34 (S-34: 4.21%) and 33SO (S-33: 0.75%) were observed in natural abundance. The newly observed transitions constitute an extension of the observed rotational quantum numbers of the molecule toward higher N values, allowing an improvement of the molecular parameters for the three species. An isotopically invariant fit has been performed based on pure rotational and ro-vibrational transitions of all SO isotopologues, enabling their accurate line position prediction at higher frequencies. Thanks to this new set of parameters, it is now possible to predict with very high accuracy the frequencies of the ro-vibrational lines. This should enable the research of SO in the mid-IR using ground-based IR telescopes, space-based telescope archives (Infrared Space Observatory, Spitzer), and future space missions such as the James Webb Space Telescope. This set of parameters is particularly well adapted for the detection of SO lines in O-rich evolved stars or in molecular clouds in absorption against bright IR sources. C1 [Martin-Drumel, M. A.; Hindle, F.; Mouret, G.; Cuisset, A.] Univ Littoral Cote dOpale, EA 4493, Lab Physicochim Atmosphere, F-59140 Dunkerque, France. [Cernicharo, J.] CSIC, ICMM, Grp Mol Astrophys, E-28049 Madrid, Spain. RP Martin-Drumel, MA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mmartin@cfa.harvard.edu RI Hindle, Francis/B-3261-2009; OI Hindle, Francis/0000-0001-9925-4497; Martin-Drumel, Marie-Aline/0000-0002-5460-4294 FU Communaute urbaine de Dunkerque; Region Nord-Pas de Calais; Ministere de l'education nationale, de l'enseignement superieur et de la recherche; European funds of the IRENI (Institut de Recherche en ENvironnement Industriel); Spanish MINECO program [CSD2009-00038, AYA2009-07304, AYA2012-32032]; European Research Council under the European Union's Seventh Framework Program [610256 NANOCOSMOS, ERC-2013-SyG]; European funds InterregIVA "Cleantech" program FX The authors gratefully acknowledge Caroline C. Womack for her helpful comments on the manuscript. The THz spectrometer was funded by the Communaute urbaine de Dunkerque, the Region Nord-Pas de Calais, the Ministere de l'education nationale, de l'enseignement superieur et de la recherche, and European funds in the context of the IRENI (Institut de Recherche en ENvironnement Industriel) and InterregIVA "Cleantech" programs. J. Cernicharo thanks the Spanish MINECO program for funding support through grants CSD2009-00038 (CONSOLIDER program "ASTROMOL"), AYA2009-07304, and AYA2012-32032, and the European Research Council for funding under the European Union's Seventh Framework Program (FP/2007-2013) / ERC-2013-SyG, Grant Agreement No. 610256 NANOCOSMOS. NR 45 TC 1 Z9 1 U1 2 U2 13 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2015 VL 799 IS 2 AR 115 DI 10.1088/0004-637X/799/2/115 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CA3QH UT WOS:000348820900002 ER PT J AU Pillepich, A Madau, P Mayer, L AF Pillepich, Annalisa Madau, Piero Mayer, Lucio TI BUILDING LATE-TYPE SPIRAL GALAXIES BY IN-SITU AND EX-SITU STAR FORMATION SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: formation; galaxies: structure; Galaxy: evolution; Galaxy: formation; Galaxy: halo; methods: numerical ID SIMULATED DISC GALAXIES; DARK-MATTER HALOES; MILKY-WAY; FORMATION HISTORIES; STELLAR HALOES; GALACTIC DISKS; THICK DISK; COSMOLOGICAL SIMULATIONS; CIRCUMGALACTIC MEDIUM; SECULAR EVOLUTION AB We analyze the formation and evolution of the stellar components in "Eris," a 120 pc resolution cosmological hydrodynamic simulation of a late-type spiral galaxy. The simulation includes the effects of a uniform UV background, a delayed-radiative-cooling scheme for supernova feedback, and a star formation recipe based on a high gas density threshold. It allows a detailed study of the relative contributions of "in-situ" (within the main host) and "ex-situ" (within satellite galaxies) star formation to each major Galactic component in a close Milky Way analog. We investigate these two star-formation channels as a function of galactocentric distance, along different lines of sight above and along the disk plane, and as a function of cosmic time. We find that: (1) approximately 70% of today's stars formed in-situ; (2) more than two thirds of the ex-situ stars formed within satellites after infall; (3) the majority of ex-situ stars are found today in the disk and in the bulge; (4) the stellar halo is dominated by ex-situ stars, whereas in-situ stars dominate the mass profile at distances less than or similar to 5 kpc from the center at high latitudes; and (5) approximately 25% of the inner, r less than or similar to 0 kpc, halo is composed of in-situ stars that have been displaced from their original birth sites during Eris' early assembly history. C1 [Pillepich, Annalisa] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Pillepich, Annalisa; Madau, Piero] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Mayer, Lucio] Univ Zurich, Inst Computat Sci, Ctr Theoret Astrophys & Cosmol, CH-9057 Zurich, Switzerland. RP Pillepich, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. FU NSF [OIA-1124453, AST-1229745]; NASA [NNX12AF87G] FX Support for this work was provided by the NSF through grants OIA-1124453 and AST-1229745, and by NASA through grant NNX12AF87G. The Eris Simulation was carried out at NASA's Pleiades supercomputer. A.P. thanks Alexander Knebe for providing support and input on the Amiga Halo Finder, and Sijing Shen, Alis Deason, Ryan Cooke, and Connie Rockosi for many stimulating discussions on the topic of this paper. NR 69 TC 20 Z9 20 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2015 VL 799 IS 2 AR 184 DI 10.1088/0004-637X/799/2/184 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CA3QH UT WOS:000348820900071 ER PT J AU Saliwanchik, BR Montroy, TE Aird, KA Bayliss, M Benson, BA Bleem, LE Bocquet, S Brodwin, M Carlstrom, JE Chang, CL Cho, HM Clocchiatti, A Crawford, TM Crites, AT de Haan, T Desai, S Dobbs, MA Dudley, JP Foley, RJ Forman, WR George, EM Gladders, MD Gonzalez, AH Halverson, NW Hlavacek-Larrondo, J Holder, GP Holzapfel, WL Hrubes, JD Jones, C Keisler, R Knox, L Lee, AT Leitch, EM Liu, J Lueker, M Luong-Van, D Mantz, A Marrone, DP McDonald, M McMahon, JJ Mehl, J Meyer, SS Mocanu, L Mohr, JJ Murray, SS Nurgaliev, D Padin, S Patej, A Pryke, C Reichardt, CL Rest, A Ruel, J Ruhl, JE Saro, A Sayre, JT Schaffer, KK Shirokoff, E Spieler, HG Stalder, B Stanford, SA Staniszewski, Z Stark, AA Story, K Stubbs, CW Vanderlinde, K Vieira, JD Vikhlinin, A Williamson, R Zahn, O Zenteno, A AF Saliwanchik, B. R. Montroy, T. E. Aird, K. A. Bayliss, M. Benson, B. A. Bleem, L. E. Bocquet, S. Brodwin, M. Carlstrom, J. E. Chang, C. L. Cho, H. M. Clocchiatti, A. Crawford, T. M. Crites, A. T. de Haan, T. Desai, S. Dobbs, M. A. Dudley, J. P. Foley, R. J. Forman, W. R. George, E. M. Gladders, M. D. Gonzalez, A. H. Halverson, N. W. Hlavacek-Larrondo, J. Holder, G. P. Holzapfel, W. L. Hrubes, J. D. Jones, C. Keisler, R. Knox, L. Lee, A. T. Leitch, E. M. Liu, J. Lueker, M. Luong-Van, D. Mantz, A. Marrone, D. P. McDonald, M. McMahon, J. J. Mehl, J. Meyer, S. S. Mocanu, L. Mohr, J. J. Murray, S. S. Nurgaliev, D. Padin, S. Patej, A. Pryke, C. Reichardt, C. L. Rest, A. Ruel, J. Ruhl, J. E. Saro, A. Sayre, J. T. Schaffer, K. K. Shirokoff, E. Spieler, H. G. Stalder, B. Stanford, S. A. Staniszewski, Z. Stark, A. A. Story, K. Stubbs, C. W. Vanderlinde, K. Vieira, J. D. Vikhlinin, A. Williamson, R. Zahn, O. Zenteno, A. TI MEASUREMENT OF GALAXY CLUSTER INTEGRATED COMPTONIZATION AND MASS SCALING RELATIONS WITH THE SOUTH POLE TELESCOPE SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: general; methods: data analysis; X-rays: galaxies: clusters ID SUNYAEV-ZELDOVICH ARRAY; MICROWAVE BACKGROUND ANISOTROPIES; X-RAY; EXTRAGALACTIC SOURCES; COSMOLOGICAL CONSTRAINTS; RELATIVISTIC CORRECTIONS; SAMPLE; GAS; CATALOG; DEG(2) AB We describe a method formeasuring the integrated Comptonization ( YSZ) of clusters of galaxies from measurements of the Sunyaev- Zel'dovich ( SZ) effect in multiple frequency bands and use this method to characterize a sample of galaxy clusters detected in the South Pole Telescope ( SPT) data. We use a Markov Chain Monte Carlo method to fit a beta- model source profile and integrate YSZ within an angular aperture on the sky. In simulated observations of an SPT- like survey that include cosmic microwave background anisotropy, point sources, and atmospheric and instrumental noise at typical SPT- SZ survey levels, we show that we can accurately recover beta- model parameters for inputted clusters. We measure YSZ for simulated semi- analytic clusters and find that YSZ is most accurately determined in an angular aperture comparable to the SPT beam size. We demonstrate the utility of this method to measure YSZ and to constrain mass scaling relations using X- ray mass estimates for a sample of 18 galaxy clusters from the SPT- SZ survey. Measuring YSZ within a 0. 75 radius aperture, we find an intrinsic log- normal scatter of 21% 11% in YSZ at a fixed mass. Measuring YSZ within a 0.3 Mpc projected radius ( equivalent to 0. 75 at the survey median redshift z = 0.6), we find a scatter of 26% 9%. Prior to this study, the SPT observable found to have the lowest scatter with mass was cluster detection significance. We demonstrate, from both simulations and SPT observed clusters that YSZ measured within an aperture comparable to the SPT beam size is equivalent, in terms of scatter with cluster mass, to SPT cluster detection significance. C1 [Saliwanchik, B. R.; Montroy, T. E.; Ruhl, J. E.; Sayre, J. T.; Staniszewski, Z.] Case Western Reserve Univ, Dept Phys, Ctr Educ & Res Cosmol & Astrophys, Cleveland, OH 44106 USA. [Aird, K. A.; Hrubes, J. D.; Luong-Van, D.] Univ Chicago, Chicago, IL 60637 USA. [Bayliss, M.; Nurgaliev, D.; Patej, A.; Ruel, J.; Stubbs, C. W.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Bayliss, M.; Foley, R. J.; Forman, W. R.; Jones, C.; Murray, S. S.; Stalder, B.; Stark, A. A.; Stubbs, C. W.; Vikhlinin, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Benson, B. A.; Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.; Crawford, T. M.; Crites, A. T.; Gladders, M. D.; Keisler, R.; Leitch, E. M.; Mantz, A.; Mehl, J.; Meyer, S. S.; Mocanu, L.; Padin, S.; Schaffer, K. K.; Story, K.; Williamson, R.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Benson, B. A.; Carlstrom, J. E.; Chang, C. L.; Schaffer, K. K.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Benson, B. A.] Fermilab Natl Accelerator Lab, Ctr Particle Astrophys, Batavia, IL 60510 USA. [Bleem, L. E.; Carlstrom, J. E.; Keisler, R.; Meyer, S. S.; Story, K.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA. [Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.] Argonne Natl Lab, Argonne, IL 60439 USA. [Bocquet, S.; Desai, S.; Liu, J.; Mohr, J. J.; Saro, A.] Univ Munich, Dept Phys, D-81679 Munich, Germany. [Bocquet, S.; Desai, S.; Liu, J.; Mohr, J. J.; Zenteno, A.] Excellence Cluster Universe, D-85748 Garching, Germany. [Brodwin, M.] Univ Missouri, Dept Phys & Astron, Kansas City, MO 64110 USA. [Carlstrom, J. E.; Crawford, T. M.; Crites, A. T.; Gladders, M. D.; Leitch, E. M.; Mehl, J.; Meyer, S. S.; Mocanu, L.; Padin, S.; Williamson, R.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Cho, H. M.] NIST, Quantum Devices Grp, Boulder, CO 80305 USA. [Clocchiatti, A.] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago, Chile. [de Haan, T.; Dobbs, M. A.; Dudley, J. P.; Holder, G. P.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Foley, R. J.; Vieira, J. D.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA. [Foley, R. J.] Univ Illinois, Dept Phys, Urbana, IL 61801 USA. [George, E. M.; Holzapfel, W. L.; Lee, A. T.; Lueker, M.; Reichardt, C. L.; Shirokoff, E.; Zahn, O.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Gonzalez, A. H.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Halverson, N. W.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. [Halverson, N. W.] Univ Colorado, Dept Phys, Boulder, CO 80309 USA. [Hlavacek-Larrondo, J.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Hlavacek-Larrondo, J.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Knox, L.; Stanford, S. A.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Lee, A. T.; Spieler, H. G.; Zahn, O.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Phys, Berkeley, CA 94720 USA. [Lueker, M.; Padin, S.; Shirokoff, E.; Vieira, J. D.] CALTECH, Pasadena, CA 91125 USA. [Marrone, D. P.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [McDonald, M.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [McMahon, J. J.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Mohr, J. J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Pryke, C.] Univ Minnesota, Dept Phys, Minneapolis, MN 55455 USA. [Rest, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Schaffer, K. K.] Sch Art Inst Chicago, Liberal Arts Dept, Chicago, IL 60603 USA. [Stanford, S. A.] Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94551 USA. [Vanderlinde, K.] Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Vanderlinde, K.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Zahn, O.] Univ Calif Berkeley, Berkeley Ctr Cosmol Phys, Berkeley, CA 94720 USA. RP Saliwanchik, BR (reprint author), Case Western Reserve Univ, Dept Phys, Ctr Educ & Res Cosmol & Astrophys, Cleveland, OH 44106 USA. EM benjamin.saliwanchik@case.edu RI Williamson, Ross/H-1734-2015; Holzapfel, William/I-4836-2015; OI Williamson, Ross/0000-0002-6945-2975; Marrone, Daniel/0000-0002-2367-1080; Aird, Kenneth/0000-0003-1441-9518; Reichardt, Christian/0000-0003-2226-9169; Forman, William/0000-0002-9478-1682; Stark, Antony/0000-0002-2718-9996 FU NSF [AST-1009012] FX We acknowledge the use of the Legacy Archive for Microwave Background Data Analysis ( LAMBDA). Support for LAMBDA is provided by the NASA Office of Space Science. Galaxy cluster research at Harvard is supported by NSF grant AST-1009012. Galaxy cluster research at SAO is supported in part by NSF grants AST- 1009649 and MRI- 0723073. The McGill group acknowledges funding from theNational Sciences and Engineering Research Council of Canada, Canada Research Chairs program, and the Canadian Institute for Advanced Research. The Munich group was supported by The Cluster of Excellence " Origin and Structure of the Universe," funded by the Excellence Initiative of the Federal Government of Germany, EXC project number 153. R. J. F. is supported by a Clay Fellowship, and B. A. B. is supported by aKICP Fellowship. A. P. is supported by an NSF Graduate Research Fellowship under grant No. DGE- 1144152. J. H. L. is supported by NASA through the Einstein Fellowship Program under grant No. PF2- 130094. M. M. acknowledges support provided by NASA through aHubble Fellowship grant from STScI. M. D. acknowledges support from an Alfred P. Sloan Research Fellowship, W. F. and C. J. acknowledge support from the Smithsonian Institution, and B. S. acknowledges support from the Brinson Foundation. NR 76 TC 2 Z9 2 U1 1 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2015 VL 799 IS 2 AR 137 DI 10.1088/0004-637X/799/2/137 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CA3QH UT WOS:000348820900024 ER PT J AU Sanders, NE Soderberg, AM Gezari, S Betancourt, M Chornock, R Berger, E Foley, RJ Challis, P Drout, M Kirshner, RP Lunnan, R Marion, GH Margutti, R McKinnon, R Milisavljevic, D Narayan, G Rest, A Kankare, E Mattila, S Smartt, SJ Huber, ME Burgett, WS Draper, PW Hodapp, KW Kaiser, N Kudritzki, RP Magnier, EA Metcalfe, N Morgan, JS Price, PA Tonry, JL Wainscoat, RJ Waters, C AF Sanders, N. E. Soderberg, A. M. Gezari, S. Betancourt, M. Chornock, R. Berger, E. Foley, R. J. Challis, P. Drout, M. Kirshner, R. P. Lunnan, R. Marion, G. H. Margutti, R. McKinnon, R. Milisavljevic, D. Narayan, G. Rest, A. Kankare, E. Mattila, S. Smartt, S. J. Huber, M. E. Burgett, W. S. Draper, P. W. Hodapp, K. W. Kaiser, N. Kudritzki, R. P. Magnier, E. A. Metcalfe, N. Morgan, J. S. Price, P. A. Tonry, J. L. Wainscoat, R. J. Waters, C. TI TOWARD CHARACTERIZATION OF THE TYPE IIP SUPERNOVA PROGENITOR POPULATION: A STATISTICAL SAMPLE OF LIGHT CURVES FROM Pan-STARRS1 SO ASTROPHYSICAL JOURNAL LA English DT Article DE supernovae: general; surveys ID CORE-COLLAPSE SUPERNOVAE; M-CIRCLE-DOT; GALACTIC CHEMICAL EVOLUTION; MASSIVE STAR EVOLUTION; DIGITAL SKY SURVEY; P SUPERNOVAE; PLATEAU SUPERNOVAE; IA SUPERNOVAE; PHYSICAL-PROPERTIES; INTERSTELLAR-MEDIUM AB In recent years, wide-field sky surveys providing deep multiband imaging have presented a new path for indirectly characterizing the progenitor populations of core-collapse supernovae (SNe): systematic light-curve studies. We assemble a set of 76 grizy-band Type IIP SN light curves from Pan-STARRS1, obtained over a constant survey program of 4 yr and classified using both spectroscopy and machine-learning-based photometric techniques. We develop and apply a new Bayesian model for the full multiband evolution of each light curve in the sample. We find no evidence of a subpopulation of fast-declining explosions (historically referred to as "Type IIL" SNe). However, we identify a highly significant relation between the plateau phase decay rate and peak luminosity among our SNe IIP. These results argue in favor of a single parameter, likely determined by initial stellar mass, predominantly controlling the explosions of red supergiants. This relation could also be applied for SN cosmology, offering a standardizable candle good to an intrinsic scatter of less than or similar to 0.2mag. We compare each light curve to physical models from hydrodynamic simulations to estimate progenitor initial masses and other properties of the Pan-STARRS1 Type IIP SN sample. We show that correction of systematic discrepancies between modeled and observed SN IIP light-curve properties and an expanded grid of progenitor properties are needed to enable robust progenitor inferences from multiband light-curve samples of this kind. This work will serve as a pathfinder for photometric studies of core-collapse SNe to be conducted through future wide-field transient searches. C1 [Sanders, N. E.; Soderberg, A. M.; Chornock, R.; Berger, E.; Challis, P.; Drout, M.; Kirshner, R. P.; Lunnan, R.; Marion, G. H.; Margutti, R.; McKinnon, R.; Milisavljevic, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gezari, S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Betancourt, M.] Univ Warwick, Dept Stat, Coventry CV4 7AL, W Midlands, England. [Foley, R. J.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA. [Foley, R. J.] Univ Illinois, Dept Phys, Urbana, IL 61801 USA. [Narayan, G.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Rest, A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Kankare, E.; Mattila, S.] Univ Turku, Finnish Ctr Astron ESO FINCA, Piikkio 21500, Finland. [Smartt, S. J.] Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland. [Huber, M. E.; Burgett, W. S.; Hodapp, K. W.; Kaiser, N.; Kudritzki, R. P.; Magnier, E. A.; Morgan, J. S.; Tonry, J. L.; Wainscoat, R. J.; Waters, C.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Draper, P. W.; Metcalfe, N.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Price, P. A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. RP Sanders, NE (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM nsanders@cfa.harvard.edu OI Lunnan, Ragnhild/0000-0001-9454-4639; Narayan, Gautham/0000-0001-6022-0484 FU David and Lucile Packard Foundation Fellowship for Science and Engineering awarded; EPSRC grant [EP/J016934/1] FX Support for this work was provided by the David and Lucile Packard Foundation Fellowship for Science and Engineering awarded to A.M.S. M.B. is supported under EPSRC grant EP/J016934/1 NR 98 TC 37 Z9 37 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 1 PY 2015 VL 799 IS 2 AR 208 DI 10.1088/0004-637X/799/2/208 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CA3QH UT WOS:000348820900095 ER PT J AU Schlafly, EF Green, G Finkbeiner, DP Rix, HW Burgett, WS Chambers, KC Draper, PW Kaiser, N Martin, NF Metcalfe, N Morgan, JS Price, PA Tonry, JL Wainscoat, RJ Waters, C AF Schlafly, E. F. Green, G. Finkbeiner, D. P. Rix, H. -W. Burgett, W. S. Chambers, K. C. Draper, P. W. Kaiser, N. Martin, N. F. Metcalfe, N. Morgan, J. S. Price, P. A. Tonry, J. L. Wainscoat, R. J. Waters, C. TI THREE-DIMENSIONAL DUST MAPPING REVEALS THAT ORION FORMS PART OF A LARGE RING OF DUST SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; ISM: bubbles; ISM: clouds ID SURROUNDING LAMBDA-ORIONIS; HIGH GALACTIC LATITUDE; MILKY-WAY TOMOGRAPHY; PAN-STARRS 1; MOLECULAR CLOUDS; SUPERNOVA-REMNANTS; H-I; INTERSTELLAR EXTINCTION; ERIDANUS SUPERBUBBLE; MULTIBAND PHOTOMETRY AB The Orion Molecular Complex is the nearest site of ongoing high-mass star formation, making it one of the most extensively studied molecular complexes in the Galaxy. We have developed a new technique for mapping the three-dimensional distribution of dust in the Galaxy using Pan-STARRS1 photometry. We isolate the dust at the distance to Orion using this technique, revealing a large (100 pc, 14 degrees diameter), previously unrecognized ring of dust, which we term the "Orion dust ring." The ring includes Orion A and B, and is not coincident with current Ha features. The circular morphology suggests formation as an ancient bubble in the interstellar medium, though we have not been able to conclusively identify the source of the bubble. This hint at the history of Orion may have important consequences for models of high-mass star formation and triggered star formation. C1 [Schlafly, E. F.; Rix, H. -W.; Martin, N. F.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Green, G.; Finkbeiner, D. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Finkbeiner, D. P.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Burgett, W. S.; Chambers, K. C.; Kaiser, N.; Morgan, J. S.; Tonry, J. L.; Wainscoat, R. J.; Waters, C.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Draper, P. W.; Metcalfe, N.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Martin, N. F.] CNRS, UMR 7550, Observ Astron Strasbourg, F-67000 Strasbourg, France. [Price, P. A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. RP Schlafly, EF (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. OI Green, Gregory/0000-0001-5417-2260; Chambers, Kenneth /0000-0001-6965-7789; Schlafly, Edward Ford/0000-0002-3569-7421 FU Sonderforschungs-bereich of the German Research Foundation (DFG) [SFB 881]; NASA [NNX10AD69G]; NSF [AST-1312891]; CNRS [PICS06183]; National Aeronautics and Space Administration [NNX08AR22G]; National Science Foundation [AST-1238877] FX This work has been greatly facilitated by valuable discussions with J. Bally, W.P. Chen, C. Heiles, E. Mamajek, C. McKee, and A. Stutz. E.S. acknowledges funding by Sonderforschungs-bereich SFB 881 "The Milky Way System" (subproject A3) of the German Research Foundation (DFG). D.F. acknowledges support of NASA grant NNX10AD69G. GMG and DPF are partially supported by NSF grant AST-1312891. N.F.M. gratefully acknowledges the CNRS for support through PICS project PICS06183. The Pan-STARRS1 Surveys (PS1) have been made possible through contributions of the Institute for Astronomy, the University of Hawaii, the Pan-STARRS Project Office, the Max-Planck Society and its participating institutes, the Max Planck Institute for Astronomy, Heidelberg and the Max Planck Institute for Extraterrestrial Physics, Garching, The Johns Hopkins University, Durham University, the University of Edinburgh, Queen's University Belfast, the Harvard-Smithsonian Center for Astrophysics, the Las Cumbres Observatory Global Telescope Network Incorporated, the National Central University of Taiwan, the Space Telescope Science Institute, the National Aeronautics and Space Administration under grant No. NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate, the National Science Foundation under grant No. AST-1238877, the University of Maryland, and Eotvos Lorand University (ELTE). NR 81 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 1 PY 2015 VL 799 IS 2 AR 116 DI 10.1088/0004-637X/799/2/116 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CA3QH UT WOS:000348820900003 ER PT J AU Slane, P Lee, SH Ellison, DC Patnaude, DJ Hughes, JP Eriksen, KA Castro, D Nagataki, S AF Slane, P. Lee, S. -H. Ellison, D. C. Patnaude, D. J. Hughes, J. P. Eriksen, K. A. Castro, D. Nagataki, S. TI A CR-HYDRO-NEI MODEL OF THE STRUCTURE AND BROADBAND EMISSION FROM TYCHO'S SUPERNOVA REMNANT (vol 33, 783, 2014) SO ASTROPHYSICAL JOURNAL LA English DT Correction C1 [Slane, P.; Patnaude, D. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lee, S. -H.; Nagataki, S.] RIKEN, Astrophys Big Bang Lab, Wako, Saitama 3510198, Japan. [Ellison, D. C.] N Carolina State Univ, Dept Phys, Raleigh, NC 27695 USA. [Hughes, J. P.; Eriksen, K. A.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Eriksen, K. A.] Los Alamos Natl Lab, XTD IDA, Los Alamos, NM 87545 USA. [Castro, D.] MIT, Kavli Ctr Astrophys & Space Res, Cambridge, MA 02139 USA. RP Slane, P (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM slane@cfa.harvard.edu; shiu-hang.lee@riken.jp; don_ellison@ncsu.edu; dpatnaude@cfa.harvard.edu; jph@physics.rutgers.edu; castro@mit.edu; shigehiro.nagataki@riken.jp NR 2 TC 0 Z9 0 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2015 VL 799 IS 2 AR 238 DI 10.1088/0004-637X/799/2/238 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CA3QH UT WOS:000348820900124 ER PT J AU Soria, R Kuntz, KD Long, KS Blair, WP Plucinsky, PP Winkler, PF AF Soria, Roberto Kuntz, K. D. Long, Knox S. Blair, William P. Plucinsky, Paul P. Winkler, P. Frank TI THE SLIM-DISK STATE OF THE ULTRALUMINOUS X-RAY SOURCE IN M83 SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; galaxies: individual (M83); X-rays: binaries ID MASS BLACK-HOLES; SUPER-EDDINGTON ACCRETION; NEARBY SPIRAL GALAXIES; SPECTRAL VARIABILITY; GRO J1655-40; MODEL; OSCILLATIONS; CANDIDATES; ABUNDANCES; 4U-1630-47 AB The transient ULX in M83 that went into outburst in, or shortly before, 2010 is still active. Our new XMM-Newton spectra show that it has a curved spectrum typical of the upper end of the high/soft state or slim-disk state. It appears to be spanning the gap between Galactic stellar-mass black holes (BHs) and the ultraluminous state, at X-ray luminosities of approximate to 1-3 x 10(39) erg s(-1) (a factor of two lower than in the 2010 and 2011 Chandra observations). From its broadened disk-like spectral shape at that luminosity, and from the fitted inner-disk radius and temperature, we argue that the accreting object is an ordinary stellar-mass BH with M similar to 10-20 M-circle dot. We suggest that in the 2010 and 2011 Chandra observations, the source was seen at a higher accretion rate, resulting in a power-law-dominated spectrum with a soft excess at large radii. C1 [Soria, Roberto] Curtin Univ, Int Ctr Radio Astron Res, Perth, WA 6845, Australia. [Kuntz, K. D.; Blair, William P.] Johns Hopkins Univ, Henry A Rowland Dept Phys & Astron, Baltimore, MD 21218 USA. [Long, Knox S.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Plucinsky, Paul P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Winkler, P. Frank] Middlebury Coll, Dept Phys, Middlebury, VT 05753 USA. RP Soria, R (reprint author), Curtin Univ, Int Ctr Radio Astron Res, GPO Box U1987, Perth, WA 6845, Australia. EM roberto.soria@curtin.edu.au FU National Aeronautics and Space Administration [GO1-12115] FX We thank our additional colleagues on the companion multi-wavelength surveys of M83 for useful discussions. We thank the anonymous referee for useful suggestions that have improved our discussion. R.S. also thanks Chris Done, Hua Feng, Fabien Grise, Matthew Middleton, and Tim Roberts for useful discussions on ULX spectral states relevant to this work. Support for this work was provided by the National Aeronautics and Space Administration through Chandra grant No. GO1-12115, issued by the Chandra X-Ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of NASA under contract NAS8-03060. R.S. acknowledges an Australian Research Council grant DP120102393. W.P.B. and K.K. acknowledge Chandra grant No. GO1-12115C to Johns Hopkins University. P.F.W. also acknowledges financial support from the National Science Foundation through grant AST-0908566. NR 59 TC 5 Z9 5 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2015 VL 799 IS 2 AR 140 DI 10.1088/0004-637X/799/2/140 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CA3QH UT WOS:000348820900027 ER PT J AU Udalski, A Yee, JC Gould, A Carey, S Zhu, W Skowron, J Kozllowski, S Poleski, R Pietrukowicz, P Pietrzynski, G Szymanski, MK Mroz, P Soszynski, I Ulaczyk, K Wyrzykowski, L Han, C Novati, SC Pogge, RW AF Udalski, A. Yee, J. C. Gould, A. Carey, S. Zhu, W. Skowron, J. Kozllowski, S. Poleski, R. Pietrukowicz, P. Pietrzynski, G. Szymanski, M. K. Mroz, P. Soszynski, I. Ulaczyk, K. Wyrzykowski, L. Han, C. Novati, S. Calchi Pogge, R. W. TI SPITZER AS A MICROLENS PARALLAX SATELLITE: MASS MEASUREMENT FOR THE OGLE-2014-BLG-0124L PLANET AND ITS HOST STAR SO ASTROPHYSICAL JOURNAL LA English DT Article DE gravitational lensing: micro; planetary systems ID GRAVITATIONAL LENSING EXPERIMENT; JUPITER/SATURN ANALOG; GALACTIC BULGE; OGLE-III; SYSTEMS; PHOTOMETRY; MILKY AB We combine Spitzer and ground-based observations to measure the microlens parallax vector pi(E), and thus the mass and distance of OGLE-2014-BLG-0124L, making it the first microlensing planetary system with a space-based parallax measurement. The planet and star have masses of m similar to 0.5M(jup) and M similar to 0.7M(circle dot) and are separated by a(perpendicular to) similar to 3.1AU in projection. The main source of uncertainty in all of these numbers (approximately 30%, 30%, and 20%) is the relatively poor measurement of the Einstein radius theta(E), rather than uncertainty in pE, which is measured with 2.5% precision. This compares to 22% based on OGLE data alone, implying that the Spitzer data provide not only a substantial improvement in the precision of the pE measurement, but also the first independent test of a ground-based pE measurement. C1 [Udalski, A.; Skowron, J.; Kozllowski, S.; Poleski, R.; Pietrukowicz, P.; Pietrzynski, G.; Szymanski, M. K.; Mroz, P.; Soszynski, I.; Ulaczyk, K.; Wyrzykowski, L.] Univ Warsaw Observ, PL-00478 Warsaw, Poland. [Yee, J. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Zhu, W.; Poleski, R.; Pogge, R. W.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Carey, S.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Pietrzynski, G.] Univ Concepcion, Dept Astron, Concepcion, Chile. [Wyrzykowski, L.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Han, C.] Chungbuk Natl Univ, Dept Phys, Cheongju 371763, South Korea. [Novati, S. Calchi] CALTECH, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Novati, S. Calchi] Univ Salerno, Dipartimento Fis ER Caianiello, I-84084 Fisciano, SA, Italy. [Novati, S. Calchi] IIASS, I-84019 Vietri Sul Mare, SA, Italy. RP Udalski, A (reprint author), Univ Warsaw Observ, Al Ujazdowskie 4, PL-00478 Warsaw, Poland. RI Skowron, Jan/M-5186-2014; OI Skowron, Jan/0000-0002-2335-1730; Kozlowski, Szymon/0000-0003-4084-880X FU European Research Council under the European Community/ERC [246678]; California Institute of Technology (Caltech)/Jet Propulsion Laboratory (JPL); NASA [NNX12AB99G]; NSF [AST 1103471]; JPL [1500811]; Creative Research Initiative Program of the National Research Foundation of Korea [2009-0081561] FX The OGLE project has received funding from the European Research Council under the European Community's Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement No. 246678 to A.U. Work by J.C.Y. was performed under contract with the California Institute of Technology (Caltech)/Jet Propulsion Laboratory (JPL) funded by NASA through the Sagan Fellowship Program executed by the NASA Exoplanet Science Institute. A.G. was supported by NSF grant AST 1103471 and NASA grant NNX12AB99G. Work by J.C.Y., A.G., and S.C. was supported by JPL grant 1500811. Work by C.H. was supported by the Creative Research Initiative Program (2009-0081561) of the National Research Foundation of Korea. 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. NR 34 TC 25 Z9 25 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2015 VL 799 IS 2 AR 237 DI 10.1088/0004-637X/799/2/237 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CA3QH UT WOS:000348820900123 ER PT J AU Williams, PKG Berger, E Irwin, J Berta-Thompson, ZK Charbonneau, D AF Williams, P. K. G. Berger, E. Irwin, J. Berta-Thompson, Z. K. Charbonneau, D. TI SIMULTANEOUS MULTIWAVELENGTH OBSERVATIONS OF MAGNETIC ACTIVITY IN ULTRACOOL DWARFS. IV. THE ACTIVE, YOUNG BINARY NLTT 33370 AB (=2MASS J13142039+1320011) SO ASTROPHYSICAL JOURNAL LA English DT Article ID LOW-MASS STARS; DIGITAL SKY SURVEY; X-RAY-EMISSION; QUIESCENT RADIO-EMISSION; ELECTRON-CYCLOTRON MASER; FULLY CONVECTIVE STARS; MAIN-SEQUENCE STARS; LSPM-NORTH CATALOG; L FIELD DWARFS; BROWN DWARFS AB We present multi-epoch simultaneous radio, optical, H alpha, UV, and X-ray observations of the active, young, low-mass binary NLTT 33370 AB (blended spectral type M7e). This system is remarkable for its extreme levels of magnetic activity: it is the most radio-luminous ultracool dwarf (UCD) known, and here we show that it is also one of the most X-ray luminous UCDs known. We detect the system in all bands and find a complex phenomenology of both flaring and periodic variability. Analysis of the optical light curve reveals the simultaneous presence of two periodicities, 3.7859 +/- 0.0001 and 3.7130 +/- 0.0002 hr. While these differ by only similar to 2%, studies of differential rotation in the UCD regime suggest that it cannot be responsible for the two signals. The system's radio emission consists of at least three components: rapid 100% polarized flares, bright emission modulating periodically in phase with the optical emission, and an additional periodic component that appears only in the 2013 observational campaign. We interpret the last of these as a gyrosynchrotron feature associated with large-scale magnetic fields and a cool, equatorial plasma torus. However, the persistent rapid flares at all rotational phases imply that small-scale magnetic loops are also present and reconnect nearly continuously. We present a spectral energy distribution of the blended system spanning more than 9 orders of magnitude in wavelength. The significant magnetism present in NLTT 33370 AB will affect its fundamental parameters, with the components' radii and temperatures potentially altered by similar to+20% and similar to-10%, respectively. Finally, we suggest spatially resolved observations that could clarify many aspects of this system's nature. C1 [Williams, P. K. G.; Berger, E.; Irwin, J.; Charbonneau, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Berta-Thompson, Z. K.] MIT Kavli Inst, Cambridge, MA 02139 USA. RP Williams, PKG (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM pwilliams@cfa.harvard.edu OI Berta-Thompson, Zachory/0000-0002-3321-4924 FU National Science Foundation [AST-1008361, AST-0807690, AST-1109468, AST-1004488]; Torres Fellowship for Exoplanetary Research; David and Lucile Packard Fellowship for Science and Engineering; John Templeton Foundation; National Aeronautics and Space Administration FX We thank Jan Forbrich for sharing preliminary VLBI results and helpful suggestions. P.K.G.W. and E.B. acknowledge support for this work from the National Science Foundation through Grant AST-1008361. Z.K.B.-T. acknowledges support from the Torres Fellowship for Exoplanetary Research. The VLA is operated by the National Radio Astronomy Observatory, a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France, and NASA's Astrophysics Data System. This research has made use of the XRT Data Analysis Software (XRTDAS) developed under the responsibility of the ASI Science Data Center (ASDC), Italy.; This paper makes use of data from the MEarth Project, which is a collaboration between Harvard University and the Smithsonian Astrophysical Observatory. The MEarth Project acknowledges funding from the David and Lucile Packard Fellowship for Science and Engineering and the National Science Foundation under grants AST-0807690, AST-1109468, and AST-1004488 (Alan T. Waterman Award), and a grant from the John Templeton Foundation.; This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. NR 165 TC 13 Z9 13 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2015 VL 799 IS 2 AR 192 DI 10.1088/0004-637X/799/2/192 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CA3QH UT WOS:000348820900079 ER PT J AU Yen, HW Koch, PM Takakuwa, S Ho, PTP Ohashi, N Tang, YW AF Yen, Hsi-Wei Koch, Patrick M. Takakuwa, Shigehisa Ho, Paul T. P. Ohashi, Nagayoshi Tang, Ya-Wen TI OBSERVATIONS OF INFALLING AND ROTATIONAL MOTIONS ON A 1000 AU SCALE AROUND 17 CLASS 0 AND 0/I PROTOSTARS: HINTS OF DISK GROWTH AND MAGNETIC BRAKING? SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; ISM: kinematics and dynamics; ISM: molecules; stars: formation; stars: low-mass ID LOW-MASS PROTOSTARS; YOUNG STELLAR OBJECTS; MOLECULAR CLOUD CORE; KEPLERIAN CIRCUMBINARY DISK; 111 PROTOSTELLAR SYSTEM; SELF-SIMILAR COLLAPSE; C2D LEGACY CLOUDS; L1551 IRS 5; STAR-FORMATION; DENSE CORES AB We perform imaging and analyses of SMA 1.3 mm continuum, (CO)-O-18(2-1) and (CO)-C-12(2-1) line data of 17Class 0 and 0/I protostars to study their gas kinematics on a 1000 AU scale. Continuum and (CO)-O-18 (2-1) emission are detected toward all the sample sources and show central primary components with sizes of similar to 600-1500 AU associated with protostars. The velocity gradients in (CO)-O-18 (2-1) have wide ranges of orientations from parallel to perpendicular to the outflows, with magnitudes from similar to 1 to similar to 530 km s(-1) pc(-1). We construct a simple kinematic model to reproduce the observed velocity gradients, estimate the infalling and rotational velocities, and infer the disk radii and the protostellar masses. The inferred disk radii range from <5 AU to >500 AU with estimated protostellar masses from <0.1 M-circle dot to >1 M-circle dot. Our results hint that both large and small disks are possibly present around Class 0 protostars, which could be a sign of disk growth at the Class 0 stage. In addition, the directions of the overall velocity gradients in 7 out of the 17 sources are close to perpendicular to their outflow axes (Delta theta > 65 degrees), which is a signature of significant rotational motions. From our model fitting, the specific angular momenta in these sources are estimated to be >2 x 10(-4) km s(-1) pc, suggesting that magnetic braking is unlikely efficient on a 1000 AU scale in these Class 0 and 0/I sources. In a sub-sample with observed magnetic field orientations, we find no source with large specific angular momenta together with closely aligned magnetic field and outflow axes. This possibly hints that the magnetic field, if originally aligned with the rotational axis, can play a role in removing angular momentum from infalling material at the Class 0 stage. We discuss our results in comparison with theoretical models of collapsing dense cores with and without magnetic fields in the context of disk formation. C1 [Yen, Hsi-Wei; Koch, Patrick M.; Takakuwa, Shigehisa; Ho, Paul T. P.; Ohashi, Nagayoshi; Tang, Ya-Wen] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Ho, Paul T. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ohashi, Nagayoshi] Natl Astron Observ Japan, Subaru Telescope, Hilo, HI 96720 USA. RP Yen, HW (reprint author), Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 10617, Taiwan. EM hwyen@asiaa.sinica.edu.tw FU Smithsonian Institute; Academia Sinica; Ministry of Science and Technology (MOST) of Taiwan [MOST 102-2119-M-001-012-MY3]; [MOST 103-2119-M-001-009] FX We thank all the SMA staff supporting this work. 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. S.T. acknowledges a grant from the Ministry of Science and Technology (MOST) of Taiwan (MOST 102-2119-M-001-012-MY3) in support of this work. P.M.K. acknowledges support through grant MOST 103-2119-M-001-009. NR 154 TC 16 Z9 16 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2015 VL 799 IS 2 AR 193 DI 10.1088/0004-637X/799/2/193 PG 26 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CA3QH UT WOS:000348820900080 ER PT J AU Young, PR Tian, H Jaeggli, S AF Young, Peter R. Tian, Hui Jaeggli, Sarah TI THE 2014 MARCH 29 X-FLARE: SUBARCSECOND RESOLUTION OBSERVATIONS OF Fe XXI lambda 1354.1 SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: activity; Sun: chromosphere; Sun: corona; Sun: flares; Sun: UV radiation ID IMAGING-SPECTROGRAPH IRIS; SOLAR-FLARE; CHROMOSPHERIC EVAPORATION; FORBIDDEN LINES; ATOMIC DATABASE; DOPPLER SHIFTS; EMISSION-LINES; SUPRA-ARCADE; PLASMA; REGION AB The Interface Region Imaging Spectrometer (IRIS) is the first solar instrument to observe similar to 10 MK plasma at subarcsecond spatial resolution through imaging spectroscopy of the Fe XXI lambda 1354.1 forbidden line. IRIS observations of the X1 class flare that occurred on 2014 March 29 at 17:48 UT reveal Fe XXI emission from both the flare ribbons and the post-flare loop arcade. Fe XXI appears at all of the chromospheric ribbon sites, although typically with a delay of one raster (75 s) and sometimes offset by up to 1(2). 100-200 km s(-1) blue-shifts are found at the brightest ribbons, suggesting hot plasma upflow into the corona. The Fe XXI ribbon emission is compact with a spatial extent of <2(2), and can extend beyond the chromospheric ribbon locations. Examples are found of both decreasing and increasing blue-shift in the direction away from the ribbon locations, and blue-shifts were present for at least six minutes after the flare peak. The post-flare loop arcade, seen in Atmospheric Imaging Assembly 131 angstrom filtergram images that are dominated by Fe XXI, exhibited bright loop-tops with an asymmetric intensity distribution. The sizes of the loop-tops are resolved by IRIS at (3)1(2), and line widths in the loop-tops are not broader than in the loop-legs suggesting the loop-tops are not sites of enhanced turbulence. Line-of-sight speeds in the loop arcade are typically <10 km s(-1), and mean non-thermal motions fall from 43 km s(-1) at the flare peak to 26 km s(-1) six minutes later. If the average velocity in the loop arcade is assumed to be at rest, then it implies a new reference wavelength for the Fe XXI line of 1354.106 +/- 0.023 angstrom. C1 [Young, Peter R.] George Mason Univ, Coll Sci, Fairfax, VA 22030 USA. [Tian, Hui] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Jaeggli, Sarah] Montana State Univ, Dept Phys, Bozeman, MT 59717 USA. RP Young, PR (reprint author), George Mason Univ, Coll Sci, Fairfax, VA 22030 USA. FU NASA [NNX13AE06G]; National Science Foundation [AGS-1159353]; LMSAL [8100002705, SP02H1701R]; Norwegian Space Center (NSC, Norway) through ESA PRODEX contract FX P.R.Y. acknowledges funding from NASA grant NNX13AE06G and National Science Foundation grant AGS-1159353. H.T. is supported by contracts 8100002705 and SP02H1701R from LMSAL to SAO. IRIS is a NASA small explorer mission developed and operated by LMSAL with mission operations executed at NASA Ames Research center and major contributions to downlink communications funded by the Norwegian Space Center (NSC, Norway) through an ESA PRODEX contract. SDO is a mission for NASA's Living With a Star program, and data are provided courtesy of NASA/SDO and the AIA and HMI science teams. NR 42 TC 27 Z9 27 U1 1 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2015 VL 799 IS 2 AR 218 DI 10.1088/0004-637X/799/2/218 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CA3QH UT WOS:000348820900105 ER PT J AU Anderson-Teixeira, KJ Davies, SJ Bennett, AC Gonzalez-Akre, EB Muller-Landau, HC Wright, SJ Abu Salim, K Zambrano, AMA Alonso, A Baltzer, JL Basset, Y Bourg, NA Broadbent, EN Brockelman, WY Bunyavejchewin, S Burslem, DFRP Butt, N Cao, M Cardenas, D Chuyong, GB Clay, K Cordell, S Dattaraja, HS Deng, XB Detto, M Du, XJ Duque, A Erikson, DL Ewango, CEN Fischer, GA Fletcher, C Foster, RB Giardina, CP Gilbert, GS Gunatilleke, N Gunatilleke, S Hao, ZQ Hargrove, WW Hart, TB Hau, BCH He, FL Hoffman, FM Howe, RW Hubbell, SP Inman-Narahari, FM Jansen, PA Jiang, MX Johnson, DJ Kanzaki, M Kassim, AR Kenfack, D Kibet, S Kinnaird, MF Korte, L Kral, K Kumar, J Larson, AJ Li, YD Li, XK Liu, SR Lum, SKY Lutz, JA Ma, KP Maddalena, DM Makana, JR Malhi, Y Marthews, T Serudin, RM McMahon, SM McShea, WJ Memiaghe, HR Mi, XC Mizuno, T Morecroft, M Myers, JA Novotny, V de Oliveira, AA Ong, PS Orwig, DA Ostertag, R den Ouden, J Parker, GG Phillips, RP Sack, L Sainge, MN Sang, WG Sri-ngernyuang, K Sukumar, R Sun, IF Sungpalee, W Suresh, HS Tan, S Thomas, SC Thomas, DW Thompson, J Turner, BL Uriarte, M Valencia, R Vallejo, MI Vicentini, A Vrska, T Wang, XH Wang, XG Weiblen, G Wolf, A Xu, H Yap, S Zimmerman, J AF Anderson-Teixeira, Kristina J. Davies, Stuart J. Bennett, Amy C. Gonzalez-Akre, Erika B. Muller-Landau, Helene C. Wright, S. Joseph Abu Salim, Kamariah Zambrano, Angelica M. Almeyda Alonso, Alfonso Baltzer, Jennifer L. Basset, Yves Bourg, Norman A. Broadbent, Eben N. Brockelman, Warren Y. Bunyavejchewin, Sarayudh Burslem, David F. R. P. Butt, Nathalie Cao, Min Cardenas, Dairon Chuyong, George B. Clay, Keith Cordell, Susan Dattaraja, Handanakere S. Deng, Xiaobao Detto, Matteo Du, Xiaojun Duque, Alvaro Erikson, David L. Ewango, Corneille E. N. Fischer, Gunter A. Fletcher, Christine Foster, Robin B. Giardina, Christian P. Gilbert, Gregory S. Gunatilleke, Nimal Gunatilleke, Savitri Hao, Zhanqing Hargrove, William W. Hart, Terese B. Hau, Billy C. H. He, Fangliang Hoffman, Forrest M. Howe, Robert W. Hubbell, Stephen P. Inman-Narahari, Faith M. Jansen, Patrick A. Jiang, Mingxi Johnson, Daniel J. Kanzaki, Mamoru Kassim, Abdul Rahman Kenfack, David Kibet, Staline Kinnaird, Margaret F. Korte, Lisa Kral, Kamil Kumar, Jitendra Larson, Andrew J. Li, Yide Li, Xiankun Liu, Shirong Lum, Shawn K. Y. Lutz, James A. Ma, Keping Maddalena, Damian M. Makana, Jean-Remy Malhi, Yadvinder Marthews, Toby Serudin, Rafizah Mat McMahon, Sean M. McShea, William J. Memiaghe, Herve R. Mi, Xiangcheng Mizuno, Takashi Morecroft, Michael Myers, Jonathan A. Novotny, Vojtech de Oliveira, Alexandre A. Ong, Perry S. Orwig, David A. Ostertag, Rebecca den Ouden, Jan Parker, Geoffrey G. Phillips, Richard P. Sack, Lawren Sainge, Moses N. Sang, Weiguo Sri-ngernyuang, Kriangsak Sukumar, Raman Sun, I-Fang Sungpalee, Witchaphart Suresh, Hebbalalu Sathyanarayana Tan, Sylvester Thomas, Sean C. Thomas, Duncan W. Thompson, Jill Turner, Benjamin L. Uriarte, Maria Valencia, Renato Vallejo, Marta I. Vicentini, Alberto Vrska, Tomas Wang, Xihua Wang, Xugao Weiblen, George Wolf, Amy Xu, Han Yap, Sandra Zimmerman, Jess TI CTFS-ForestGEO: a worldwide network monitoring forests in an era of global change SO GLOBAL CHANGE BIOLOGY LA English DT Review DE biodiversity; Center for Tropical Forest Science (CTFS); climate change; demography; forest dynamics plot; Forest Global Earth Observatory (ForestGEO); long-term monitoring; spatial analysis ID TROPICAL TREE COMMUNITY; LONG-TERM NITROGEN; RAIN-FOREST; NEOTROPICAL FOREST; FUNCTIONAL TRAITS; SPATIAL-PATTERNS; EL-NINO; PHYLOGENETIC STRUCTURE; SEEDLING RECRUITMENT; DISPERSAL LIMITATION AB Global change is impacting forests worldwide, threatening biodiversity and ecosystem services including climate regulation. Understanding how forests respond is critical to forest conservation and climate protection. This review describes an international network of 59 long-term forest dynamics research sites (CTFS-ForestGEO) useful for characterizing forest responses to global change. Within very large plots (median size 25ha), all stems 1cm diameter are identified to species, mapped, and regularly recensused according to standardized protocols. CTFS-ForestGEO spans 25 degrees S-61 degrees N latitude, is generally representative of the range of bioclimatic, edaphic, and topographic conditions experienced by forests worldwide, and is the only forest monitoring network that applies a standardized protocol to each of the world's major forest biomes. Supplementary standardized measurements at subsets of the sites provide additional information on plants, animals, and ecosystem and environmental variables. CTFS-ForestGEO sites are experiencing multifaceted anthropogenic global change pressures including warming (average 0.61 degrees C), changes in precipitation (up to +/- 30% change), atmospheric deposition of nitrogen and sulfur compounds (up to 3.8g Nm(-2)yr(-1) and 3.1g Sm(-2)yr(-1)), and forest fragmentation in the surrounding landscape (up to 88% reduced tree cover within 5km). The broad suite of measurements made at CTFS-ForestGEO sites makes it possible to investigate the complex ways in which global change is impacting forest dynamics. Ongoing research across the CTFS-ForestGEO network is yielding insights into how and why the forests are changing, and continued monitoring will provide vital contributions to understanding worldwide forest diversity and dynamics in an era of global change. C1 [Anderson-Teixeira, Kristina J.; Davies, Stuart J.; Muller-Landau, Helene C.; Wright, S. Joseph; Basset, Yves; Detto, Matteo; Gilbert, Gregory S.; Hubbell, Stephen P.; Jansen, Patrick A.; Kenfack, David; McMahon, Sean M.; Turner, Benjamin L.] Smithsonian Trop Res Inst, Ctr Trop Forest Sci, Forest Global Earth Observ, Panama City, Panama. [Anderson-Teixeira, Kristina J.; Bennett, Amy C.; Gonzalez-Akre, Erika B.; Zambrano, Angelica M. Almeyda; Bourg, Norman A.; Broadbent, Eben N.; McShea, William J.] Natl Zool Pk, Conservat Ecol Ctr, Smithsonian Conservat Biol Inst, Front Royal, VA USA. [Davies, Stuart J.; Erikson, David L.; Kenfack, David] Natl Museum Nat Hist, Dept Bot, Washington, DC 20560 USA. [Abu Salim, Kamariah] Univ Brunei Darussalam, Fac Sci, BE-1410 Bandar Seri Begawan, Brunei. [Zambrano, Angelica M. Almeyda; Broadbent, Eben N.] Stanford Univ, Stanford Woods Inst Environm, Stanford, CA 94305 USA. [Zambrano, Angelica M. Almeyda; Broadbent, Eben N.] Univ Alabama, Dept Geog, Tuscaloosa, AL USA. [Alonso, Alfonso; Korte, Lisa] Smithsonian Inst, Natl Zool Pk, Ctr Conservat Educ & Sustainabil, Smithsonian Conservat Biol Inst, Washington, DC 20008 USA. [Baltzer, Jennifer L.] Wilfrid Laurier Univ, Dept Biol, Waterloo, ON N2L 3C5, Canada. [Brockelman, Warren Y.] Mahidol Univ, Dept Biol, Bangkok 10700, Thailand. [Bunyavejchewin, Sarayudh] Dept Natl Pk Wildlife & Plant Conservat, Res Off, Bangkok, Thailand. [Burslem, David F. R. P.] Univ Aberdeen, Sch Biol Sci, Aberdeen, Scotland. [Butt, Nathalie] Univ Queensland, Sch Biol Sci, St Lucia, Qld 4072, Australia. [Butt, Nathalie; Malhi, Yadvinder; Marthews, Toby] Univ Oxford, Environm Change Inst, Sch Geog & Environm, Oxford, England. [Cao, Min; Deng, Xiaobao] Chinese Acad Sci, Key Lab Trop Forest Ecol, Xishuangbanna Trop Bot Garden, Kunming 650223, Peoples R China. [Cardenas, Dairon] Inst Amazon Invest Cient Sinchi, Bogota, Colombia. [Chuyong, George B.] Univ Buea, Dept Bot & Plant Physiol, Buea, Cameroon. [Clay, Keith; Johnson, Daniel J.; Phillips, Richard P.] Indiana Univ, Dept Biol, Bloomington, IN USA. [Cordell, Susan; Giardina, Christian P.] US Forest Serv, Inst Pacific Isl Forestry, USDA, Hilo, HI USA. [Dattaraja, Handanakere S.; Sukumar, Raman; Suresh, Hebbalalu Sathyanarayana] Indian Inst Sci, Ctr Ecol Sci, Bangalore 560012, Karnataka, India. [Du, Xiaojun; Ma, Keping; Mi, Xiangcheng; Sang, Weiguo] Chinese Acad Sci, Inst Bot, Beijing 100093, Peoples R China. [Duque, Alvaro] Univ Nacl Colombia, Dept Ciencias Forestales, Medellin, Colombia. [Ewango, Corneille E. N.] Reserve Faune Okapis, Ctr Format & Rech Conservat Forestiere CEFRECOF E, Ituri Forest, Epulu, DEM REP CONGO. [Fischer, Gunter A.] Kadoorie Farm & Bot Garden, Tai Po, Hong Kong, Peoples R China. [Fletcher, Christine; Kassim, Abdul Rahman] Forest Res Inst Malaysia, Selangor, Malaysia. [Foster, Robin B.] Field Museum Nat Hist, Dept Bot, Chicago, IL 60605 USA. [Gilbert, Gregory S.] Univ Calif Santa Cruz, Dept Environm Studies, Santa Cruz, CA 95064 USA. [Gunatilleke, Nimal; Gunatilleke, Savitri] Univ Peradeniya, Fac Sci, Dept Bot, Peradeniya, Sri Lanka. [Hao, Zhanqing] Chinese Acad Sci, Inst Appl Ecol, State Key Lab Forest & Soil Ecol, Shenyang 110164, Peoples R China. [Hargrove, William W.] US Forest Serv, Eastern Forest Environm Threat Assessment Ctr, USDA, Stn Headquarters, Asheville, NC USA. [Hart, Terese B.; Wang, Xugao] Lukuru Wildlife Res Fdn, Tshuapa Lomami Lualaba Project, Kinshasa, DEM REP CONGO. [Hau, Billy C. H.] Univ Hong Kong, Kadoorie Inst, Pokfulam, Hong Kong, Peoples R China. [Hau, Billy C. H.] Univ Hong Kong, Sch Biol Sci, Pokfulam, Hong Kong, Peoples R China. [He, Fangliang] Univ Alberta, Dept Renewable Resources, Edmonton, AB, Canada. [Hoffman, Forrest M.; Kumar, Jitendra; Maddalena, Damian M.] Oak Ridge Natl Lab, Computat Earth Sci Grp, Oak Ridge, TN USA. [Howe, Robert W.] Univ Wisconsin, Dept Nat & Appl Sci, Green Bay, WI 54311 USA. [Hubbell, Stephen P.; Sack, Lawren] Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA USA. [Inman-Narahari, Faith M.] Univ Hawaii Manoa, Coll Trop Agr & Human Resources, Honolulu, HI 96822 USA. [Jansen, Patrick A.] Wageningen Univ, Resource Ecol Grp, NL-6700 AP Wageningen, Netherlands. [Jiang, Mingxi] Chinese Acad Sci, Wuhan Bot Garden, Wuhan 430074, Peoples R China. [Kanzaki, Mamoru; Mizuno, Takashi] Kyoto Univ, Grad Sch Agr, Kyoto, Japan. [Kibet, Staline] Natl Museums Kenya, Nairobi, Kenya. [Kibet, Staline] Univ Nairobi, Land Resource Management & Agr Technol Dept, Nairobi, Kenya. [Kinnaird, Margaret F.] Mpala Res Ctr, Nanyuki 10400, Kenya. [Kinnaird, Margaret F.] Wildlife Conservat Soc, Global Conservat Programs, Bronx, NY 10460 USA. [Kral, Kamil; Vrska, Tomas] Silva Tarouca Res Inst, Dept Forest Ecol, Brno, Czech Republic. [Larson, Andrew J.] Univ Montana, Coll Forestry & Conservat, Dept Forest Management, Missoula, MT 59812 USA. [Li, Yide; Xu, Han] Chinese Acad Forestry, Res Inst Trop Forestry, Guangzhou, Guangdong, Peoples R China. [Li, Xiankun] Chinese Acad Sci, Guangxi Inst Bot, Guilin, Guangxi, Peoples R China. [Liu, Shirong] Chinese Acad Forestry, Res Inst Forest Ecol Environm & Protect, Beijing, Peoples R China. [Lum, Shawn K. Y.] Nanyang Technol Univ, Natl Inst Educ, Nat Sci & Sci Educ Acad Grp, Singapore 639798, Singapore. [Lutz, James A.] Utah State Univ, Wildland Resources Dept, Logan, UT 84322 USA. [Makana, Jean-Remy] Wildlife Conservat Soc, Brazzaville, DEM REP CONGO. [Serudin, Rafizah Mat] Univ Brunei Darussalam, Fac Sci, BE-1410 Bandar Seri Begawan, Brunei. [McMahon, Sean M.; Parker, Geoffrey G.] Smithsonian Environm Res Ctr, Forest Ecol Grp, Edgewater, MD 21037 USA. [Memiaghe, Herve R.] Ctr Natl Rech Sci & Technol, Inst Rech Ecol Tropicale, Libreville, Gabon. [Morecroft, Michael] Nat England, Sheffield, S Yorkshire, England. [Myers, Jonathan A.] Washington Univ, Dept Biol, St Louis, MO 63130 USA. [Novotny, Vojtech] New Guinea Binatang Res Ctr, Madang, Papua N Guinea. [Novotny, Vojtech] Acad Sci Czech Republic, Ctr Biol, Ceske Budejovice 37005, Czech Republic. [Novotny, Vojtech] Univ South Bohemia, Fac Sci, Ceske Budejovice 37005, Czech Republic. [de Oliveira, Alexandre A.] Univ Sao Paulo, Dept Ecol, Inst Biociencias, Sao Paulo, Brazil. [Ong, Perry S.; Yap, Sandra] Univ Philippines Diliman, Inst Biol, Quezon City, Philippines. [Orwig, David A.] Harvard Univ, Harvard Forest, Petersham, MA USA. [Ostertag, Rebecca] Univ Hawaii, Dept Biol, Hilo, HI 96720 USA. [den Ouden, Jan] Wageningen Univ, Forest Ecol & Forest Management Grp, NL-6700 AP Wageningen, Netherlands. [Sainge, Moses N.] Trop Plant Explorat Grp TroPEG, Mundemba, Southwest Regio, Cameroon. [Sun, I-Fang] Natl Dong Hwa Univ, Dept Nat Resources & Environm Studies, Hualien, Taiwan. [Tan, Sylvester] Sarawak Forest Dept, Kuching, Sarawak, Malaysia. [Thomas, Sean C.] Univ Toronto, Fac Forestry, Toronto, ON M5S 3B3, Canada. [Thomas, Duncan W.] Washington State Univ, Sch Biol Sci, Vancouver, WA USA. [Thompson, Jill] Ctr Ecol & Hydrol, Penicuik EH26 0QB, Midlothian, Scotland. [Thompson, Jill; Zimmerman, Jess] Univ Puerto Rico, Inst Trop Ecosyst Studies, Dept Environm Sci, San Juan, PR 00936 USA. [Uriarte, Maria] Columbia Univ, Dept Ecol Evolut & Environm Biol, New York, NY USA. [Valencia, Renato] Pontifical Catholic Univ Ecuador, Dept Biol Sci, Quito, Ecuador. [Vallejo, Marta I.] Inst Alexander von Humboldt, Bogota, Colombia. [Vicentini, Alberto] Inst Nacl de Pesquisas da Amazonia, Manaus, Amazonas, Brazil. [Wang, Xihua] E China Normal Univ, Sch Ecol & Environm Sci, Shanghai 200062, Peoples R China. [Weiblen, George] Univ Minnesota, Dept Plant Biol, St Paul, MN USA. [Wolf, Amy] UW Green Bay, Dept Biol, Green Bay, WI 54311 USA. [Wolf, Amy] UW Green Bay, Dept Nat & Appl Sci, Green Bay, WI 54311 USA. RP Anderson-Teixeira, KJ (reprint author), Smithsonian Trop Res Inst, Ctr Trop Forest Sci, Forest Global Earth Observ, Panama City, Panama. EM teixeirak@si.edu RI Hoffman, Forrest/B-8667-2012; Sack, Lawren/A-5492-2008; Basset, Yves/B-6642-2014; Giardina, Christian/C-3120-2011; Kral, Kamil/E-4415-2014; Turner, Benjamin/E-5940-2011; Jansen, Patrick/G-2545-2015; wang, xugao/B-1111-2015; Novotny, Vojtech/G-9434-2014; Thompson, Jill/K-2200-2012; Kumar, Jitendra/G-8601-2013; Wright, Stuart/M-3311-2013 OI Almeyda Zambrano, Angelica/0000-0001-5081-9936; Bourg, Norman/0000-0002-7443-1992; Oliveira, Alexandre/0000-0001-5526-8109; Parker, Geoffrey/0000-0001-7055-6491; Burslem, David/0000-0001-6033-0990; Hoffman, Forrest/0000-0001-5802-4134; Sack, Lawren/0000-0002-7009-7202; Giardina, Christian/0000-0002-3431-5073; Turner, Benjamin/0000-0002-6585-0722; Jansen, Patrick/0000-0002-4660-0314; wang, xugao/0000-0003-1207-8852; Novotny, Vojtech/0000-0001-7918-8023; Thompson, Jill/0000-0002-4370-2593; Kumar, Jitendra/0000-0002-0159-0546; Wright, Stuart/0000-0003-4260-5676 FU Smithsonian Competitive Grants Program for Science; Smithsonian Institution; Smithsonian Tropical Research Institute; Arnold Arboretum of Harvard University; National Science Foundation; Rockefeller Foundation; John Merck Fund; John D. and Catherine T. MacArthur Foundation; Andrew W. Mellon Foundation; Frank Levinson Family Foundation; HSBC Climate Partnership; Bromley Charitable Trust; John Swire Sons Pty Ltd; Celerity; F.H. Levinson Fund; Small World Institute Fund FX We thank everyone involved in the collection of the vast quantity of data and information in the CTFS-ForestGEO network; to F. Dentener and W. Laurance for providing data; E. Leigh, Y. Lin, J. McGarvey and A. Miller for helpful comments; E. Aikens, L. Gonzalez and M. Azimi for help with analysis and figures. Study on this manuscript was funded in part by a Smithsonian Competitive Grants Program for Science award to KJAT. The CTFS-ForestGEO network has received major support from the Smithsonian Institution - particularly the Smithsonian Tropical Research Institute, the Arnold Arboretum of Harvard University, the National Science Foundation (multiple grants), the Rockefeller Foundation, the John Merck Fund, the John D. and Catherine T. MacArthur Foundation, the Andrew W. Mellon Foundation, the Frank Levinson Family Foundation, the HSBC Climate Partnership, the Bromley Charitable Trust, John Swire & Sons Pty Ltd, Celerity, F.H. Levinson Fund, Small World Institute Fund and Jennifer and Greg Johnson. Site-specific support is listed in Table S8. NR 199 TC 61 Z9 67 U1 41 U2 207 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1354-1013 EI 1365-2486 J9 GLOBAL CHANGE BIOL JI Glob. Change Biol. PD FEB PY 2015 VL 21 IS 2 BP 528 EP 549 DI 10.1111/gcb.12712 PG 22 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA CA1DE UT WOS:000348652400004 PM 25258024 ER PT J AU Hong, T AF Hong, Terry TI The Four Books SO LIBRARY JOURNAL LA English DT Book Review C1 [Hong, Terry] Smithsonian BookDragon, Washington, DC 20024 USA. RP Hong, T (reprint author), Smithsonian BookDragon, Washington, DC 20024 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 2015 VL 140 IS 2 BP 78 EP 78 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA CA1UN UT WOS:000348697000104 ER PT J AU Wright, A Tobin, M Mangan, S Schnitzer, SA AF Wright, Alexandra Tobin, Mike Mangan, Scott Schnitzer, Stefan A. TI Unique competitive effects of lianas and trees in a tropical forest understory SO OECOLOGIA LA English DT Article DE Procedural control; Community composition; Global change; Seedling regeneration; Aboveground competition ID BELOW-GROUND COMPETITION; BARRO-COLORADO ISLAND; LIGHT ENVIRONMENTS; GROWTH DYNAMICS; PANAMA; REGENERATION; SEEDLINGS; TOLERANCE; ABUNDANCE; PATTERNS AB Lianas are an important component of tropical forests, contributing up to 25 % of the woody stems and 35 % of woody species diversity. Lianas invest less in structural support but more in leaves compared to trees of similar biomass. These physiological and morphological differences suggest that lianas may interact with neighboring plants in ways that are different from similarly sized trees. However, the vast majority of past liana competition studies have failed to identify the unique competitive effects of lianas by controlling for the amount of biomass removed. We assessed liana competition in the forest understory over the course of 3 years by removing liana biomass and an equal amount of tree biomass in 40 plots at 10 sites in a secondary tropical moist forest in central Panama. We found that growth of understory trees and lianas, as well as planted seedlings, was limited due to competitive effects from both lianas and trees, though the competitive impacts varied by species, season, and size of neighbors. The removal of trees resulted in greater survival of planted seedlings compared to the removal of lianas, apparently related to a greater release from competition for light. In contrast, lianas had a species-specific negative effect on drought-tolerant Dipteryx oleifera seedlings during the dry season, potentially due to competition for water. We conclude that, at local scales, lianas and trees have unique and differential effects on understory dynamics, with lianas potentially competing more strongly during the dry season, and trees competing more strongly for light. C1 [Wright, Alexandra; Tobin, Mike; Mangan, Scott; Schnitzer, Stefan A.] Univ Wisconsin, Sch Freshwater Sci, Milwaukee, WI 53201 USA. [Wright, Alexandra] Bard Coll, Annandale On Hudson, NY 12504 USA. [Tobin, Mike] Univ Houston Downtown, Dept Nat Sci, Houston, TX USA. [Mangan, Scott] Washington Univ, Dept Biol, St Louis, MO 63130 USA. [Schnitzer, Stefan A.] Smithsonian Trop Res Inst, Ancon, Panama. RP Wright, A (reprint author), Bard Coll, Annandale On Hudson, NY 12504 USA. EM sashajwright@gmail.com OI Schnitzer, Stefan/0000-0002-2715-9455 FU National Science Foundation [NSF-DEB 0613666, NSF-DEB 0845071, NSF-DEB 1019436]; University of Wisconsin-Milwaukee Advanced Opportunity Fellowship; UWM Center for Latin American and Caribbean Studies; UWM graduate school; UWM Department of Biological Sciences FX The experiment presented here complies with the current laws of Panama where the experiment was performed. This research was made possible through support from the National Science Foundation (grants NSF-DEB 0613666, NSF-DEB 0845071, and NSF-DEB 1019436 to SAS), a University of Wisconsin-Milwaukee Advanced Opportunity Fellowship, the UWM Center for Latin American and Caribbean Studies, the UWM graduate school and scholarship funds from the UWM Department of Biological Sciences. We thank G. Rutten, A. Katherina, A. Domeyko, E. Sanchez, S. Yorke, and J. Mascaro for support and feedback on these ideas. NR 38 TC 1 Z9 1 U1 7 U2 35 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0029-8549 EI 1432-1939 J9 OECOLOGIA JI Oecologia PD FEB PY 2015 VL 177 IS 2 BP 561 EP 569 DI 10.1007/s00442-014-3179-0 PG 9 WC Ecology SC Environmental Sciences & Ecology GA CA5XK UT WOS:000348981500023 PM 25502290 ER PT J AU Clay, NA Donoso, DA Kaspari, M AF Clay, Natalie A. Donoso, David A. Kaspari, Michael TI Urine as an important source of sodium increases decomposition in an inland but not coastal tropical forest SO OECOLOGIA LA English DT Article DE Urea; Nutrient subsidies; Brown food web; Latrine; Landscape heterogeneity; Biogeography; Biogeochemistry; Isoptera ID BODY-SIZE; POPULATION-DENSITY; RAIN-FOREST; NATIONAL-PARK; PLANT-LITTER; SOIL; NUTRIENTS; BEHAVIOR; FERTILIZATION; EQUIVALENCE AB Nutrient pulses can profoundly impact ecosystem processes and urine is a frequently deposited source of N and K, and Na. Na is unimportant to plants, but its addition can increase decomposition and change invertebrate community structure in Na-poor tropical forests. Here we used synthetic urine to separate the effects of Na from urine's other nutrients and contrasted their roles in promoting decomposition and detritivore recruitment in both a Na-poor inland Ecuadorian and Na-rich coastal Panamanian tropical forest. After 2 days, invertebrate communities did not vary among +Na, H2O, Urine+Na, and Urine-Na treatments. But after 2 weeks, Ecuador wood, but not cellulose, decomposition was twofold higher on Urine+Na and +Na plots compared to H2O and Urine-Na plots accompanied by > 20-fold increases in termite abundance on these plots. Panama, in contrast, showed no effect of Na on decomposition. In both forests, plots fertilized with urine had nearly twofold decrease in detritivores after 2 weeks that was likely a shock effect from ammonification. Moreover, the non-Na nutrients in urine did not enhance decomposition at this time scale. On control plots, Panama had higher decomposition rates for both cellulose and wood than Ecuador, but the addition of Na in Ecuador alleviated these differences. These results support the hypothesis that in Na-poor tropical forests, urine can enhance wood decomposition and generate an important source of heterogeneity in the abundance and activity of brown food webs. C1 [Clay, Natalie A.; Kaspari, Michael] Univ Oklahoma, Dept Biol, Norman, OK 73019 USA. [Donoso, David A.] Univ Tecn Particular Loja San Cayetano, Dept Ciencias Nat, Museo Colecc Biol MUTPL, Loja, Ecuador. [Kaspari, Michael] Smithsonian Trop Res Inst, Balboa, Panama. RP Clay, NA (reprint author), Mississippi State Univ, Dept Biochem Mol Biol Entomol & Plant Pathol, Clay Lyle Entomol Bldg,Room 110,Box 9775, Mississippi State, MS 39762 USA. EM naclay@ou.edu RI Donoso, David/A-2059-2016; OI Donoso, David/0000-0002-3408-1457; Kaspari, Michael/0000-0002-9717-5768 FU NSF [DEB-0948762] FX We thank D. Flatt, K. Tholt, J. Burks and D. Rinehart for help in the laboratory. Special thanks to N. Velasco and T. Zumbusch, who were invaluable in the field. We also thank Oris Acevedo and Belkys Jimenez and Smithsonian Tropical Research Institute staff on BCI, Panama, and ANAM for permit SEX/AP-309. Miguel Rodriquez and Alvaro Barragan provided logistical help in Quito and Yasuni. We thank the Ministerio de Ambiente del Ecuador for research permit 0020-2010-IC-FUN-DPO-MA. All experiments comply with the current laws of the countries in which the experiments were performed. Funding was provided from NSF DEB-0948762 (principal investigator M. Kaspari). NR 63 TC 3 Z9 3 U1 2 U2 20 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0029-8549 EI 1432-1939 J9 OECOLOGIA JI Oecologia PD FEB PY 2015 VL 177 IS 2 BP 571 EP 579 DI 10.1007/s00442-014-3183-4 PG 9 WC Ecology SC Environmental Sciences & Ecology GA CA5XK UT WOS:000348981500024 PM 25519175 ER PT J AU Scarpa, F Cossu, P Sanna, D Lai, T Norenburg, JL Curini-Galletti, M Casu, M AF Scarpa, Fabio Cossu, Piero Sanna, Dania Lai, Tiziana Norenburg, Jon L. Curini-Galletti, Marco Casu, Marco TI An 18S and 28S-based clock calibration for marine Proseriata (Platyhelminthes) SO JOURNAL OF EXPERIMENTAL MARINE BIOLOGY AND ECOLOGY LA English DT Article DE Meiofauna; Isthmus of Panama; Mutation rates; Relaxed molecular clock; Divergence time; Calibration point ID OXIDASE SUBUNIT-I; MOLECULAR CLOCK; MAXIMUM-LIKELIHOOD; NORTHEAST ATLANTIC; DIVERGENCE TIMES; SPECIES COMPLEX; TAXONOMY; DIVERSITY; ISTHMUS; PANAMA AB Geminate species are a powerful tool for calibrating the molecular clock in marine organisms, and their adoption is mandatory for soft-bodied taxa, which lack fossil records. The first attempt to calibrate the molecular clock in taxa belonging to meiofaunal microturbellaria (Platyhelminthes: Proseriata) based on geminate species is presented here. We used two species pairs from both sides of the Isthmus of Panama: Minona gemella (Caribbean) and Minona cf gemella (Pacific); Parotoplana sp. nov. 1 (Caribbean) and Parotoplana sp. nov. 2 (Pacific). The mutation rates per million years were estimated for both geminate species pairs on two ribosomal regions, the complete nuclear small subunit rDNA (18S) gene and the partial nuclear large subunit rDNA (28S) gene fragment (spanning variable domains D1-D6). Similar values of mutation rates per million years were found in both species pairs, ranging 0.12-0.16% for 18S and 0.49-0.52% for 28S. The values obtained were used as calibration points at minimum age, in order to estimate the divergence times within the phylogenetic tree of the whole dataset, and tested on three cases of trans-American (not-geminate) species from Pacific Panama and S-E Brazil, belonging to the genera Kata, Archimonocelis and Duplominona. They consistently showed higher divergence times (ranging 9.4-17.9 Myr) than geminate, trans-isthmian pairs. These results suggest potential usefulness of our molecular clock calibration, for future research on phylogeography and evolution of Proseriata. (C) 2014 Elsevier B.V. All rights reserved. C1 [Scarpa, Fabio; Cossu, Piero; Sanna, Dania; Lai, Tiziana; Curini-Galletti, Marco; Casu, Marco] Univ Sassari, Dipartimento Sci Nat Territorio, Sez Zool, I-07100 Sassari, Italy. [Norenburg, Jon L.] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. RP Casu, M (reprint author), Univ Sassari, Dipartimento Sci Nat Territorio, Sez Zool, Via Muroni 25, I-07100 Sassari, Italy. EM marcasu@uniss.it RI Norenburg, Jon/K-3481-2015; OI Norenburg, Jon/0000-0001-7776-1527; CASU, Marco/0000-0002-5042-4851; LAI, Tiziana/0000-0003-0731-1656 FU Smithsonian Institution's Marine Science Network; ASSEMBLE [227799] FX We acknowledge partial funding support of the field work by an award from the Smithsonian Institution's Marine Science Network to JLN. We are grateful to the staff at the Smithsonian Tropical Research Institute's Naos Marine Laboratory for space and assistance of many sorts. We also acknowledge for partial funding support ASSEMBLE grant agreement no. 227799 for specimens sampled in Roscoff and in Faro. Finally we are grateful to Prof. Ulf Jondelius and to an anonymous referee for their constructive suggestions who helped to improve the paper. [SS] NR 79 TC 4 Z9 4 U1 2 U2 13 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0022-0981 EI 1879-1697 J9 J EXP MAR BIOL ECOL JI J. Exp. Mar. Biol. Ecol. PD FEB PY 2015 VL 463 BP 22 EP 31 DI 10.1016/j.jembe.2014.10.020 PG 10 WC Ecology; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA CA0TD UT WOS:000348628400004 ER PT J AU Gomez, CG Guzman, HM Gonzalez, A AF Gomez, Catalina G. Guzman, Hector M. Gonzalez, Andrew TI Population decline and the effects of disturbances on the structure and recovery of octocoral communities (Coelenterata: Octocorallia) in Pacific Panama SO JOURNAL OF THE MARINE BIOLOGICAL ASSOCIATION OF THE UNITED KINGDOM LA English DT Article DE coral community ecology; octocorals; species relative abundance; disturbance; diversity; Coiba National Park; Panama ID SPECIES ABUNDANCE DISTRIBUTIONS; EASTERN TROPICAL PACIFIC; ANTHOZOA OCTOCORALLIA; RELATIVE-ABUNDANCE; GORGONIIDAE; DIVERSITY; REVISION; REEFS; CONSERVATION; VERRILL AB Community structure, species composition, and changes over time after disturbances are frequently studied using common descriptors. We used rank abundance distribution plots (RADs), Renyi entropy plots, common theoretical community models, ordination analysis of similarities (ANOSIM and Clusters), and abundance spectra analyses to study the effects of a gradual natural population decline and an anthropogenic punctuated disturbance on the structure of octocoral communities in Panama, considered a hot spot area for octocoral diversity in the Tropical Eastern Pacific. Over a 17-month period, no significant change was found in community structure after a natural yearly population decline of 25.2%. After a disturbance, however, different recovery trajectories were observed in various coral communities. Possible physical and biological explanations for the observed differences include initial local species diversity and abundance, species life history patterns, colony morphology, and the geographical location of the community. Differences in community structure between study sites were best described using a combination of community descriptors, RADs, and abundance spectra. Renyi plots were useful in identifying changes in community structure, whereas the extent of the changes was best evaluated using ANOSIM and cluster analysis. C1 [Gomez, Catalina G.; Guzman, Hector M.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Gonzalez, Andrew] McGill Univ, Dept Biol, Montreal, PQ H3A 1B1, Canada. RP Gomez, CG (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Ancon, Panama. EM gomezc@si.edu FU Secretaria Nacional de Ciencia, Tecnologia e Innovacion-Panama (SENACYT) [PNCOIBA-08-024]; Smithsonian Tropical Research Institute; McGill-STRI NEO Program FX This research was partially sponsored by Secretaria Nacional de Ciencia, Tecnologia e Innovacion-Panama (SENACYT-Grant No, PNCOIBA-08-024), the Smithsonian Tropical Research Institute, and the McGill-STRI NEO Program. NR 46 TC 0 Z9 0 U1 2 U2 11 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0025-3154 EI 1469-7769 J9 J MAR BIOL ASSOC UK JI J. Mar. Biol. Assoc. U.K. PD FEB PY 2015 VL 95 IS 1 BP 81 EP 90 DI 10.1017/S0025315414000915 PG 10 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA AZ2AR UT WOS:000348037500009 ER PT J AU Kuntner, M Agnarsson, I Li, DQ AF Kuntner, Matjaz Agnarsson, Ingi Li, Daiqin TI The eunuch phenomenon: adaptive evolution of genital emasculation in sexually dimorphic spiders SO BIOLOGICAL REVIEWS LA English DT Article DE genital mutilation; terminal investment; monogyny; sexual selection; sperm competition; antagonistic co-evolution; sexual size dimorphism; SSD; female gigantism; mate choice; plugging; sexual cannibalism; sexual conflict ID ORB-WEB SPIDER; MALE MATE CHOICE; CANNIBALISTIC SPIDER; PHYLOGENETIC PLACEMENT; SPERM COMPETITION; NEPHILID SPIDERS; REDBACK SPIDERS; MALE ADAPTATION; WEAVING SPIDER; MALE SACRIFICE AB Under natural and sexual selection traits often evolve that secure paternity ormaternity through self-sacrifice to predators, rivals, offspring, or partners. Emasculation-males removing their genitals-is an unusual example of such behaviours. Known only in insects and spiders, the phenomenon's adaptiveness is difficult to explain, yet its repeated origins and association with sexual size dimorphism (SSD) and sexual cannibalism suggest an adaptive significance. In spiders, emasculation of paired male sperm-transferring organs - secondary genitals -(hereafter, palps), results in 'eunuchs'. This behaviour has been hypothesized to be adaptive because (i) males plug female genitals with their severed palps (plugging hypothesis), (ii) males remove their palps to become better fighters in male-male contests (better-fighter hypothesis), perhaps reaching higher agility due to reduced total body mass (gloves-off hypothesis), and (iii) males achieve prolonged sperm transfer through severed genitals (remote-copulation hypothesis). Prior research has provided evidence in support of these hypotheses in some orb-weaving spiders but these explanations are far from general. Seeking broad macroevolutionary patterns of spider emasculation, we review the known occurrences, weigh the evidence in support of the hypotheses in each known case, and redefine more precisely the particular cases of emasculation depending on its timing in relation to maturation and mating: 'pre-maturation', 'mating', and 'post-mating'. We use a genus-level spider phylogeny to explore emasculation evolution and to investigate potential evolutionary linkage between emasculation, SSD, lesser genital damage (embolic breakage), and sexual cannibalism (females consuming their mates). We find a complex pattern of spider emasculation evolution, all cases confined to Araneoidea: emasculation evolved at least five and up to 11 times, was lost at least four times, and became further modified at least once. We also find emasculation, as well as lesser genital damage and sexual cannibalism, to be significantly associated with SSD. These behavioural and morphological traits thus likely co-evolve in spiders. Emasculation can be seen as an extreme form of genital mutilation, or even a terminal investment strategy linked to the evolution of monogyny. However, as different emasculation cases in araneoid spiders are neither homologous nor biologically identical, and may or may not serve as paternity protection, the direct link to monogyny is not clear cut. Understanding better the phylogenetic patterns of emasculation and its constituent morphologies and behaviours, a clearer picture of the intricate interplay of natural and sexual selection may arise. With the here improved evolutionary resolution of spider eunuch behaviour, we can more specifically tie the evidence from adaptive hypotheses to independent cases, and propose promising avenues for further research of spider eunuchs, and of the evolution of monogyny. C1 [Kuntner, Matjaz] Slovenian Acad Sci & Arts, Ctr Sci Res, Inst Biol, Ljubljana 1000, Slovenia. [Kuntner, Matjaz; Li, Daiqin] Hubei Univ, Coll Life Sci, Ctr Behav Ecol & Evolut, Wuhan 430062, Peoples R China. [Kuntner, Matjaz; Agnarsson, Ingi] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. [Agnarsson, Ingi] Univ Vermont, Dept Biol, Burlington, VT 05405 USA. [Li, Daiqin] Natl Univ Singapore, Dept Biol Sci, Singapore 117543, Singapore. RP Kuntner, M (reprint author), Slovenian Acad Sci & Arts, Ctr Sci Res, Inst Biol, Novi Trg 2, Ljubljana 1000, Slovenia. EM kuntner@gmail.com RI Li, Daiqin/D-6922-2013 OI Li, Daiqin/0000-0001-8269-7734 FU Raffles Museum for Biodiversity Research (RMBR) Short-term Fellowship; Slovenian Research Agency [P10236, MU-PROM/12-001]; NSFC [31272324]; Singapore Ministry of Education (MOE) AcRF grant [R-154-000-476-112]; Ah Meng Conservation Fund [R-154-518-720] FX We thank Barbara Thaler-Knoflach for kindly providing all images in Fig. 2 and for checking our interpretations of theridiid emasculation, Peter Michalik and an anonymous reviewer for constructive comments, and R.-C. Cheng, D. Court, M. Gregoric, J. Koh, S. Kralj-Fiser, Q.Q. Lee, J. Oh, U. Pristovsek, J. Schneider, and S. Zhang for kindly sharing data, observations and insight. This work was made possible by a Raffles Museum for Biodiversity Research (RMBR) Short-term Fellowship and the grants P10236 and MU-PROM/12-001 from the Slovenian Research Agency to M.K. and by the NSFC grant (31272324) as well as Singapore Ministry of Education (MOE) AcRF grant (R-154-000-476-112) and Ah Meng Conservation Fund (R-154-518-720) to D.L. NR 111 TC 11 Z9 11 U1 4 U2 66 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1464-7931 EI 1469-185X J9 BIOL REV JI Biol. Rev. PD FEB PY 2015 VL 90 IS 1 BP 279 EP 296 DI 10.1111/brv.12109 PG 18 WC Biology SC Life Sciences & Biomedicine - Other Topics GA AZ7RL UT WOS:000348415500017 PM 24809822 ER PT J AU Aisenberg, A Barrantes, G Eberhard, WG AF Aisenberg, Anita Barrantes, Gilbert Eberhard, William G. TI Hairy kisses: tactile cheliceral courtship affects female mating decisions in Leucauge mariana (Araneae, Tetragnathidae) SO BEHAVIORAL ECOLOGY AND SOCIOBIOLOGY LA English DT Article DE Sexual selection; Cryptic female choice; Experimental manipulation; Cheliceral clasp; Leucauge ID ORB-WEAVING SPIDER; SEXUAL SELECTION; MALE ARCHISEPSIS; FRONT LEGS; SEPSIDAE; DIPTERA; SPERM; STIMULATION; COEVOLUTION; COPULATION AB Sexual selection is thought to be an important force driving the evolution of sexually dimorphic morphology and behavior, but direct experimental tests of the functions of species-specific details of morphology are rare and usually incomplete. The males of most species of the large spider family Tetragnathidae possess large sexually dimorphic chelicerae that are used when the sexes lock together before and during mating. In Leucauge mariana, the female's chelicerae clasp those of the male; mating does not begin until the female's chelicerae seize the male and does not end until they release him. In addition, females contribute material to form genital plugs in the female's genitalia. Male chelicerae have sexually dimorphic and species-specific setae and ledges in areas that contact the female during cheliceral clasps. We tested the hypothesis that stimuli from these structures trigger mating processes that are controlled by the female which could increase male reproductive success. We reduced or eliminated possible stimulation of the female in two ways: removing male cheliceral setae that contact the female, and removing setae on the female's chelicerae and endites that are contacted by and could thus be stimulated by the male's chelicerae and their setae. Both male and female modifications had similar effects that likely reduced the male's chances of paternity: female receptivity to re-mating increased, copulatory plug formation decreased, and interruptions during copulation became more frequent. As expected under the stimulation hypothesis, blocking female sensory abilities generally had greater effects on these responses than modifying male stimulatory structures. C1 [Aisenberg, Anita] Inst Invest Biol Clemente Estable, Lab Etol Ecol & Evoluc, Montevideo, Uruguay. [Barrantes, Gilbert; Eberhard, William G.] Univ Costa Rica, Escuela Biol, Facio Brenes, Costa Rica. [Eberhard, William G.] Louisiana State Univ, Smithsonian Trop Res Inst, Dept Biol, Baton Rouge, LA 70803 USA. RP Aisenberg, A (reprint author), Inst Invest Biol Clemente Estable, Lab Etol Ecol & Evoluc, Ave Italia 3318,CP 11600, Montevideo, Uruguay. EM anita.aisenberg@gmail.com FU Sistema Nacional de Investigadores (Agencia Nacional de Investigacion e Innovacion); Programa de Desarrollo de las Ciencias Basicas; Vicerrectoria de Investigacion of the Universidad de Costa Rica; Smithsonian Tropical Research Institute FX We thank the Sistema Nacional de Investigadores (Agencia Nacional de Investigacion e Innovacion) and Programa de Desarrollo de las Ciencias Basicas (AA), the Vicerrectoria de Investigacion of the Universidad de Costa Rica (GB, WGE), and the Smithsonian Tropical Research Institute (WGE) for financial support. The editor and two anonymous reviewers improved the final version of the manuscript. NR 41 TC 1 Z9 1 U1 1 U2 28 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0340-5443 EI 1432-0762 J9 BEHAV ECOL SOCIOBIOL JI Behav. Ecol. Sociobiol. PD FEB PY 2015 VL 69 IS 2 BP 313 EP 323 DI 10.1007/s00265-014-1844-2 PG 11 WC Behavioral Sciences; Ecology; Zoology SC Behavioral Sciences; Environmental Sciences & Ecology; Zoology GA AY8QM UT WOS:000347818500015 ER PT J AU Van Bocxlaer, B Albrecht, C AF Van Bocxlaer, Bert Albrecht, Christian TI Ecosystem change and establishment of an invasive snail alter gastropod communities in long-lived Lake Malawi SO HYDROBIOLOGIA LA English DT Article DE Melanoides tuberculata; Exotic or alien species; Ancient Lake Malawi; Faunal interaction; Freshwater Cerithioidea; Bulinus ID SCHISTOSOME INTERMEDIATE HOST; SOFT-SEDIMENT GASTROPODS; CAPE MACLEAR; TREMATOCRANUS-PLACODON; BULINUS-NYASSANUS; ASSEMBLAGE; RESISTANCE; STRESSORS; DIVERSITY; VICTORIA AB Biotic invasions can have far-reaching effects in isolated, eco-insular systems such as the African Great Lakes, certainly in synergy with other anthropogenic stressors that affect ecosystem stability. Interactions between invasive and indigenous taxa across trophic levels often tend to propagate throughout the ecosystem, but also those at the same trophic level may affect biodiversity. Here, we examine faunal interactions between an invasive Asian morph of the cerithioidean gastropod Melanoides tuberculata and indigenous gastropods in long-lived Lake Malawi. Studying quantitative samples, we document a negative spatial correlation between the established invader and endemic Melanoides species, and positive ones between invasive and native M. tuberculata, and between native Melanoides and schistosome-transmitting Bulinus. Comparison of modern and fossil samples indicates that Melanoides communities have changed since the middle Holocene from consisting predominantly of endemic taxa (95%) toward a dominance by non-endemics (80%). External evidence suggests that ecosystem change, such as increased sedimentation and eutrophication, and interactions between the invasive and endemic Melanoides species are the most likely causes for these changes. More in-depth study of the benthic ecosystem is required to document interaction mechanisms better, but the invasive taxon is playing an important role in reshaping communities and diversity in Lake Malawi. C1 [Van Bocxlaer, Bert] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol & Invertebrate Zool, Washington, DC 20560 USA. [Van Bocxlaer, Bert] Univ Ghent, Dept Geol & Soil Sci, Res Unit Palaeontol, B-9000 Ghent, Belgium. [Van Bocxlaer, Bert; Albrecht, Christian] Univ Giessen, Dept Anim Ecol & Systemat, D-35392 Giessen, Germany. RP Van Bocxlaer, B (reprint author), Univ Giessen, Dept Anim Ecol & Systemat, Heinrich Buff Ring 26-32 IFZ, D-35392 Giessen, Germany. EM vanbocxlaerb@si.edu RI Van Bocxlaer, Bert/N-1965-2016 OI Van Bocxlaer, Bert/0000-0003-2033-326X FU Flanders Research Foundation; Leopold III-Fund; Belgian American Educational Foundation; Peter Buck Fellowship of the Smithsonian Institution; Alexander von Humboldt Fellowship; DFG [AL 1076/6-2, 7-1, 8-1] FX Martin Genner kindly shared data. Thies Geertz, Nore Praet, Wout Salenbien, Friedemann Schrenk, Roland Schultheiss, Danny Simbeye, Joseph Tembo, and Jacques Verniers provided help with fieldwork. Two anonymous reviewers provided many valuable suggestions that improved the manuscript considerably. Funding was received from the Flanders Research Foundation, the Leopold III-Fund, the Belgian American Educational Foundation, a Peter Buck Fellowship of the Smithsonian Institution, and an Alexander von Humboldt Fellowship to B.V.B., and DFG Grants AL 1076/6-2, 7-1, 8-1 to C.A. NR 37 TC 3 Z9 3 U1 4 U2 45 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0018-8158 EI 1573-5117 J9 HYDROBIOLOGIA JI Hydrobiologia PD FEB PY 2015 VL 744 IS 1 BP 307 EP 316 DI 10.1007/s10750-014-2093-0 PG 10 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA AW3JH UT WOS:000346182100022 ER PT J AU Brodu, E Balat-Pichelin, M Meneses, DD Sans, JL AF Brodu, E. Balat-Pichelin, M. Meneses, D. De Sousa Sans, J. -L. TI Reducing the temperature of a C/C composite heat shield for solar probe missions with an optically selective semi-transparent pyrolytic boron nitride (pBN) coating SO CARBON LA English DT Article ID EMISSIVITY; BOUNDARY AB Two solar missions are designed to plunge into the solar corona, and respectively get as close as 8.5 and 3 Rs (solar radii) from the Sun's surface. Heat shields will protect the pay-loads within their umbra from the thermal radiation and solar winds. We report the high temperature behavior of a pBN coating on a C/C composite. We established thanks to spectral emissivity measurements at high temperature that covering the C/C composite with pBN leads to a strong decrease of the ratio alpha/epsilon of the solar absorptivity to the total emissivity. The alpha/epsilon ratios calculated from the spectral emissivity measurements are correlated to the ones obtained from integrated emissivity measurements. A resulting surface temperature reduction of 200 K is estimated at 8.5 solar radii between uncoated C/C and pBN coated C/C. In the semi-transparent region of the spectral emissivity of pBN, located in the solar spectrum, the substrate C/C keeps a strong contribution in the spectral emissivity of the assembly pBN + C/C. The level of this contribution is function of the pBN coating thickness. Finally, material characterizations performed before and after treatment at 2200 K showed that the pBN coating has a good stability at high temperature. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Brodu, E.; Balat-Pichelin, M.; Sans, J. -L.] CNRS, PROMES, Lab Proc Mat & Energie Solaire, F-66120 Font Romeu, France. [Brodu, E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Meneses, D. De Sousa] CNRS, CEMHTI, F-45071 Orleans, France. RP Balat-Pichelin, M (reprint author), CNRS, PROMES, Lab Proc Mat & Energie Solaire, 7 Rue Four Solaire, F-66120 Font Romeu, France. EM marianne.balat@promes.cnrs.fr FU PhD of Etienne Brodu and Daniele Perarnau; CNES (Centre National d'Etudes Spatiales, France) FX The authors gratefully acknowledge CNES (Centre National d'Etudes Spatiales, France) and particularly J.Y. Prado for the support of the PhD of Etienne Brodu and Daniele Perarnau for XRD measurements. NR 21 TC 4 Z9 4 U1 4 U2 46 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0008-6223 EI 1873-3891 J9 CARBON JI Carbon PD FEB PY 2015 VL 82 BP 39 EP 50 DI 10.1016/j.carbon.2014.10.022 PG 12 WC Chemistry, Physical; Materials Science, Multidisciplinary SC Chemistry; Materials Science GA AU5ZZ UT WOS:000345683100005 ER PT J AU Luque, J AF Luque, Javier TI A puzzling frog crab (Crustacea: Decapoda: Brachyura) from the Early Cretaceous Santana Group of Brazil: frog first or crab first? SO JOURNAL OF SYSTEMATIC PALAEONTOLOGY LA English DT Article DE evolution; Neotropics; Raninoidia; South America; Raninoida; Albian ID PHYLOGENETIC ANALYSIS; FAMILY; CLASSIFICATION; PODOTREMATA; RANINIDAE; COLOMBIA; RANINOIDA; REVISION; EXTINCT; GENERA AB The evolutionary origin of frog crabs (Raninoida) remains puzzling partly due to their astonishing morphological disparity, ranging from broad and heavily ornamented 'crab-like' extinct families (necrocarcinids and allies), to elongate and smoother 'frog-like' extant ones (raninids and allies). However, an ancient Cretaceous clade (Palaeocorystidae) displays a combination of plesiomorphic and apomorphic traits that might advocate for either evolutionary scenario: from 'crab-like' to 'frog-like', or vice versa. This lack of agreement is partly fuelled by the scarcity of Early Cretaceous fossils, a time from which the first raninoidans are known. A close re-examination of an Early Cretaceous fossil from the Santana Group of Brazil, Araripecarcinus ferreirai Martins-Neto, 1987, combined with phylogenetic analysis including all main clades of podotreme crabs, reinforces its raninoidan condition, and rejects the initial hypothesis of a Portunoidea affinity. Furthermore, comparisons with other raninoidans support the hypothesis that a more 'crab-like' body plan is the plesiomorphic condition for raninoidans, and that the 'frog-like' architecture of Palaeocorystidae, and perhaps the Raninoidea as a whole, reflects a derived condition related to a specialized burrowing lifestyle. Phylogenetic analyses are fundamental to evaluate the position of Palaeocorystidae with respect to raninoidean and necrocarcinid-like families, helping to better resolve the Raninoida evolutionary tree of life, and to gain a broader understanding on their relatedness by common ancestry throughout geological time. C1 [Luque, Javier] Univ Alberta, Dept Biol Sci, Edmonton, AB T6G 2E9, Canada. [Luque, Javier] Smithsonian Trop Res Inst, Panama City, Panama. RP Luque, J (reprint author), Univ Alberta, Dept Biol Sci, Edmonton, AB T6G 2E9, Canada. EM luque@ualberta.ca OI Luque, Javier/0000-0002-4391-5951 FU Natural Science and Engineering Research Council of Canada Graduate Scholarship (NSERC CGS-D); NSERC Canada [A7245] FX This work was supported by the Natural Science and Engineering Research Council of Canada Graduate Scholarship (NSERC CGS-D). My deepest thanks to Carlos Jaramillo (STRI), Daniele Guinot (MHNH), Kecia Kerr (McGill University), A. Richard Palmer (University of Alberta) and Hiroaki Karasawa (Mizunami Fossil Museum, Japan) for intellectual support; to Paula Sucerquia (Universidade de Sao Paulo) for providing photos and a cast of the holotype and sole specimen of Araripecarcinus ferreirai; to Rodney M. Feldmann (Kent State University, USA) for providing photos of the cast of Araripecarcinus and the specimen of Cenomanocarcinus sp., plus valuable comments that improved an early version of the manuscript; to Barry Van Bakel (Oertijdmuseum De Groene Poort, Boxtel, The Netherlands) for thoughtful discussions and providing photos of Silvacarcinus; to Roger Portell (FLMNH) and the Invertebrate Paleontology Division, Florida Museum of Natural History, University of Florida, for the photo of Corazzatocarcinus; and to John Maisey, Lorraine Meeker and Chester Tarka (AMNH, USA) for the photos of the Cretaceous brachyuran larva preserved as stomach contents. I am very grateful to Carrie E. Schweitzer (Kent State University, USA), an anonymous reviewer, and the JSP editors for improving the quality of the manuscript. Partial funding for this project was provided by an NSERC Canada Discovery Grant A7245 to A. Richard Palmer. NR 78 TC 8 Z9 8 U1 0 U2 24 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 1477-2019 EI 1478-0941 J9 J SYST PALAEONTOL JI J. Syst. Palaeontol. PD FEB 1 PY 2015 VL 13 IS 2 BP 153 EP 166 DI 10.1080/14772019.2013.871586 PG 14 WC Evolutionary Biology; Paleontology SC Evolutionary Biology; Paleontology GA AW5ZJ UT WOS:000346349100004 ER PT J AU Hiremath, KM Manjunath, H Soon, W AF Hiremath, K. M. Manjunath, Hegde Soon, Willie TI Indian summer monsoon rainfall: Dancing with the tunes of the sun SO NEW ASTRONOMY LA English DT Article DE Solar variability; Indian summer monsoon variability; Solar activity forcing on monsoon; Simulations of monsoon rainfall ID MULTISCALE SOLAR-ACTIVITY; GALACTIC COSMIC-RAYS; CORONAL HOLE AREA; EMPIRICAL-EVIDENCE; WAVELET ANALYSIS; SUNSPOT CYCLE; ASIAN MONSOON; CLIMATE; VARIABILITY; HOLOCENE AB There is strong statistical evidence that solar activity influences the Indian summer monsoon rainfall. To search for a physical link between the two, we consider the coupled cloud hydrodynamic equations, and derive an equation for the rate of precipitation that is similar to the equation of a forced harmonic oscillator, with cloud and rain water mixing ratios as forcing variables. Those internal forcing variables are parameterized in terms of the combined effect of external forcing as measured by sunspot and coronal hole activities with several well known solar periods (9, 13 and 27 days; 1.3, 5, 11 and 22 years). The equation is then numerically solved and the results show that the variability of the simulated rate of precipitation captures very well the actual variability of the Indian monsoon rainfall, yielding vital clues for a physical understanding that has so far eluded analyses based on statistical correlations alone. We also solved the precipitation equation by allowing for the effects of long-term variation of aerosols. We tentatively conclude that the net effects of aerosols variation are small, when compared to the solar factors, in terms of explaining the observed rainfall variability covering the full Indian monsoonal geographical domains. (C) 2014 Elsevier B.V. All rights reserved. C1 [Hiremath, K. M.; Manjunath, Hegde] Indian Inst Astrophys, Bengaluru 560034, Karnataka, India. [Soon, Willie] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Hiremath, KM (reprint author), Indian Inst Astrophys, Bengaluru 560034, Karnataka, India. EM hiremath@iiap.res.in FU Indian Space Research Organization (ISRO), Government of India FX This research has been carried out under "CAWSES India Phase-II program of Theme 1" sponsored by Indian Space Research Organization (ISRO), Government of India. We are grateful to both Professor Peter Conti, the editor and, the referee for useful and helpful comments that improved this manuscript substantially. NR 99 TC 4 Z9 4 U1 1 U2 19 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 1384-1076 EI 1384-1092 J9 NEW ASTRON JI New Astron. PD FEB PY 2015 VL 35 BP 8 EP 19 DI 10.1016/j.newast.2014.08.002 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AS7HN UT WOS:000344427700002 ER PT J AU Corstanje, A Schellart, P Nelles, A Buitink, S Enriquez, JE Falcke, H Frieswijk, W Horandel, JR Krause, M Rachen, JP Scholten, O ter Veen, S Thoudam, S Trinh, TNG van den Akker, M Alexov, A Anderson, J Avruch, IM Bell, ME Bentum, MJ Bernardi, G Best, P Bonafede, A Breitling, F Broderick, J Brugen, M Butcher, HR Ciardi, B de Gasperin, F de Geus, E de Vos, M Duscha, S Eisloffel, J Engels, D Fallows, RA Ferrari, C Garrett, MA Griessmseier, J Gunst, AW Hamaker, JP Hoeft, M Homeffer, A Icobelli, M Juette, E Karastergiou, A Kohler, J Kondratiev, VI Kuniyoshi, M Kuper, G Maat, P Mann, G McFadden, R McKay-Bukowski, D Mevius, M Munk, H Norden, MJ Orru, E Paas, H Pandey-Pommier, M Pandey, VN Pizzo, R Polatidis, AG Reich, W Rottgering, H Scaife, AMM Schwarz, D Smirnov, O Stewart, A Steinmetz, M Swinbank, J Tagger, M Tang, Y Tasse, C Toribio, C Vermeulen, R Vocks, C van Weeren, RJ Wijnholds, SJ Wucknitz, O Yatawatta, S Zarka, P AF Corstanje, A. Schellart, P. Nelles, A. Buitink, S. Enriquez, J. E. Falcke, H. Frieswijk, W. Horandel, J. R. Krause, M. Rachen, J. P. Scholten, O. ter Veen, S. Thoudam, S. Trinh, T. N. G. van den Akker, M. Alexov, A. Anderson, J. Avruch, I. M. Bell, M. E. Bentum, M. J. Bernardi, G. Best, P. Bonafede, A. Breitling, F. Broderick, J. Bruegen, M. Butcher, H. R. Ciardi, B. de Gasperin, F. de Geus, E. de Vos, M. Duscha, S. Eisloeffel, J. Engels, D. Fallows, R. A. Ferrari, C. Garrett, M. A. Griessmseier, J. Gunst, A. W. Hamaker, J. P. Hoeft, M. Homeffer, A. Icobelli, M. Juette, E. Karastergiou, A. Kohler, J. Kondratiev, V. I. Kuniyoshi, M. Kuper, G. Maat, P. Mann, G. McFadden, R. McKay-Bukowski, D. Mevius, M. Munk, H. Norden, M. J. Orru, E. Paas, H. Pandey-Pommier, M. Pandey, V. N. Pizzo, R. Polatidis, A. G. Reich, W. Rottgering, H. Scaife, A. M. M. Schwarz, D. Smirnov, O. Stewart, A. Steinmetz, M. Swinbank, J. Tagger, M. Tang, Y. Tasse, C. Toribio, C. Vermeulen, R. Vocks, C. van Weeren, R. J. Wijnholds, S. J. Wucknitz, O. Yatawatta, S. Zarka, P. TI The shape of the radio wavefront of extensive air showers as measured with LOFAR SO ASTROPARTICLE PHYSICS LA English DT Article DE Cosmic rays; Extensive air showers; Radio emission; Wavefront shape ID EMISSION; RADIATION; PULSES; ARRAY AB Extensive air showers, induced by high energy cosmic rays impinging on the Earth's atmosphere, produce radio emission that is measured with the LOFAR radio telescope. As the emission comes from a finite distance of a few kilometers, the incident wavefront is non-planar. A spherical, conical or hyperbolic shape of the wavefront has been proposed, but measurements of individual air showers have been inconclusive so far. For a selected high-quality sample of 161 measured extensive air showers, we have reconstructed the wavefront by measuring pulse arrival times to sub-nanosecond precision in 200 to 350 individual antennas. For each measured air shower, we have fitted a conical, spherical, and hyperboloid shape to the arrival times. The fit quality and a likelihood analysis show that a hyperboloid is the best parameterization. Using a non-planar wavefront shape gives an improved angular resolution, when reconstructing the shower arrival direction. Furthermore, a dependence of the wavefront shape on the shower geometry can be seen. This suggests that it will be possible to use a wavefront shape analysis to get an additional handle on the atmospheric depth of the shower maximum, which is sensitive to the mass of the primary particle. (C) 2014 Elsevier B.V. All rights reserved. C1 [Corstanje, A.; Schellart, P.; Nelles, A.; Buitink, S.; Enriquez, J. E.; Falcke, H.; Horandel, J. R.; Krause, M.; Rachen, J. P.; ter Veen, S.; Thoudam, S.; van den Akker, M.] Radboud Univ Nijmegen, IMAPP, Dept Astrophys, NL-6500 GL Nijmegen, Netherlands. [Falcke, H.; Frieswijk, W.; Bentum, M. J.; de Geus, E.; de Vos, M.; Duscha, S.; Fallows, R. A.; Garrett, M. A.; Gunst, A. W.; Hamaker, J. P.; Kondratiev, V. I.; Kuper, G.; Maat, P.; McFadden, R.; Mevius, M.; Munk, H.; Norden, M. J.; Orru, E.; Pandey, V. N.; Pizzo, R.; Polatidis, A. G.; Tang, Y.; Toribio, C.; Vermeulen, R.; Wijnholds, S. J.; Yatawatta, S.] Netherlands Inst Radio Astron ASTRON, NL-7990 AA Dwingeloo, Netherlands. [Nelles, A.; Falcke, H.; Horandel, J. R.] Nikhef, Sci Pk Amsterdam, NL-1098 XG Amsterdam, Netherlands. [Falcke, H.; Homeffer, A.; Kohler, J.; Kuniyoshi, M.; Reich, W.; Wucknitz, O.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Scholten, O.; Trinh, T. N. G.] Univ Groningen, NL-9700 AB Groningen, Netherlands. [Alexov, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Anderson, J.; Breitling, F.; Mann, G.; Vocks, C.] Leibniz Inst Astrophys Potsdam AIP, D-14482 Potsdam, Germany. [Avruch, I. M.] SRON Netherlands Insitute Space Res, NL-9700 AV Groningen, Netherlands. [Avruch, I. M.; Mevius, M.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Bell, M. E.] Univ Sydney, ARC Ctr Excellence All Sky Astrophys CAASTRO, Sydney Inst Astron, Sydney, NSW 2006, Australia. [Bernardi, G.; van Weeren, R. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Best, P.] Univ Edinburgh, Royal Observ Edinburgh, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. [Bonafede, A.; Bruegen, M.; de Gasperin, F.] Univ Hamburg, D-21029 Hamburg, Germany. [Broderick, J.; Scaife, A. M. M.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Butcher, H. R.] Australian Natl Univ, Mt Stromlo Obs, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. [Ciardi, B.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [de Geus, E.] SmarterVis BV, NL-9401 JX Assen, Netherlands. [Eisloeffel, J.; Hoeft, M.] Thuringer Landessternwarte, D-07778 Tautenburg, Germany. [Engels, D.] Hamburger Sternwarte, D-21029 Hamburg, Germany. [Ferrari, C.] Univ Nice Sophia Antipolis, CNRS, Observ Cote Azur, Lab Lagrange,UMR7293, F-06300 Nice, France. [Garrett, M. A.; Icobelli, M.; Rottgering, H.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Griessmseier, J.; Tagger, M.] Univ Orleans, CNRS, LPC2E, F-45067 Orleans, France. [Griessmseier, J.] Univ Orleans, OSUC, CNRS INSU, Observ Paris,Stn Radioastron Nancay,USR 704, F-18330 Nancy, France. [Juette, E.] Ruhr Univ Bochum, Astron Inst, D-44780 Bochum, Germany. [Karastergiou, A.; Stewart, A.] Univ Oxford, Oxford OX1 3RH, England. [Kondratiev, V. I.] Lebedev Phys Inst, Ctr Astro Space, Moscow 117997, Russia. [McKay-Bukowski, D.] Univ Oulu, Sodankyla Geophys Observ, Sodankyla 99600, Finland. [McKay-Bukowski, D.] STFC Rutherford Appleton Lab, Harwell Sci & Innovat Campus, Didcot OX11 0QX, Oxon, England. [Paas, H.] Univ Groningen, CIT, NL-9700 AB Groningen, Netherlands. [Pandey-Pommier, M.] Observ Lyon, Ctr Rech Astrophys Lyon, F-69561 St Genis Laval, France. [Schwarz, D.] Univ Bielefeld, Fak Phys, Lehrstuhl Genet, D-33501 Bielefeld, Germany. [Smirnov, O.] Rhodes Univ, Dept Phys & Elelct, ZA-6140 Grahamstown, South Africa. [Smirnov, O.] SKA South Africa, ZA-7405 Pinelands, South Africa. [Swinbank, J.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands. [Tasse, C.; Zarka, P.] Observ Paris, LESIA, UMR CNRS 8109, F-92195 Meudon, France. RP Schellart, P (reprint author), Radboud Univ Nijmegen, IMAPP, Dept Astrophys, POB 9010, NL-6500 GL Nijmegen, Netherlands. EM A.Corstanje@astro.ru.nl; P.Schellart@astro.ru.nl; A.Nelles@astro.ru.nl RI Tagger, Michel/O-6615-2014; Ciardi, Benedetta/N-7625-2015; Yatawatta, Sarod/E-6037-2013; Kondratiev, Vladislav/N-1105-2015 OI Tagger, Michel/0000-0003-2962-3220; Swinbank, John/0000-0001-9445-1846; Yatawatta, Sarod/0000-0001-5619-4017; Krause, Maria/0000-0001-7595-0914; de Gasperin, Francesco/0000-0003-4439-2627; van Weeren, Reinout/0000-0002-0587-1660; Kondratiev, Vladislav/0000-0001-8864-7471 FU Netherlands Research School for Astronomy (NOVA); Samenwerkingsverband Noord-Nederland (SNN); Foundation for Fundamental Research on Matter (FOM); Netherlands Organization for Scientific Research (NWO) [639-041-130]; Advanced Grant of the European Research Council under the European Union [227610]; Agence Nationale de la Recherche [ANR-09-JCJC-0001-01] FX Furthermore, we acknowledge financial support from the Netherlands Research School for Astronomy (NOVA), the Samenwerkingsverband Noord-Nederland (SNN) and the Foundation for Fundamental Research on Matter (FOM) as well as support from the Netherlands Organization for Scientific Research (NWO), VENI grant 639-041-130. We acknowledge funding from an Advanced Grant of the European Research Council under the European Union's Seventh Framework Program (FP/2007-2013)/ERC Grant Agreement n. 227610. Chiara Ferrari acknowledges financial support by the "Agence Nationale de la Recherche" through grant ANR-09-JCJC-0001-01. NR 25 TC 15 Z9 15 U1 3 U2 23 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0927-6505 EI 1873-2852 J9 ASTROPART PHYS JI Astropart Phys. PD FEB PY 2015 VL 61 BP 22 EP 31 DI 10.1016/j.astropartphys.2014.06.001 PG 10 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA AR2CM UT WOS:000343391200004 ER PT J AU Milisavljevic, D Fesen, RA AF Milisavljevic, Dan Fesen, Robert A. TI The bubble-like interior of the core-collapse supernova remnant Cassiopeia A SO SCIENCE LA English DT Article ID 3-DIMENSIONAL STRUCTURE; A SUPERNOVA; EJECTA; EXPLOSIONS; INSTABILITIES; ASYMMETRY; TURBULENT; SHELL; IRON; AGE AB The death of massive stars is believed to involve aspheric explosions initiated by the collapse of an iron core. The specifics of these catastrophic explosions remain uncertain, due partly to limited observational constraints on asymmetries deep inside the star. Here we present near-infrared observations of the young supernova remnant Cassiopeia A, descendant of a type IIb core-collapse explosion, and a three-dimensional map of its interior unshocked ejecta. The remnant's interior has a bubble-like morphology that smoothly connects to and helps explain the multiringed structures seen in the remnant's bright reverse-shocked main shell of expanding debris. This internal structure may originate from turbulent mixing processes that encouraged outwardly expanding plumes of radioactive Ni-56-rich ejecta. If this is true, substantial amounts of its decay product, Fe-56, may still reside in these interior cavities. C1 [Milisavljevic, Dan] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Fesen, Robert A.] Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA. RP Milisavljevic, D (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM dmilisav@cfa.harvard.edu FU National Science Foundation [AST-0908237]; Guest Observer program [10286]; NASA [NAS 5-26555] FX This material is based on work supported by the National Science Foundation under grant no. AST-0908237, as well as observations made with the NASA/European Space Agency HST associated with Guest Observer program 10286 (Principal Investigator, R. Fesen) and obtained from the data archive at the Space Telescope Science Institute (STScI). STScI is operated by the Association of Universities for Research in Astronomy under NASA contract NAS 5-26555. Visual modeling of our observations was aided with the use of MeshLab (http://meshlab.sourceforge.net), a tool developed with the support of the 3D-CoForm project. We thank anonymous reviewers for providing suggestions that improved the content and presentation of the manuscript and D. Patnaude for helpful discussions. NR 33 TC 11 Z9 11 U1 0 U2 4 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 EI 1095-9203 J9 SCIENCE JI Science PD JAN 30 PY 2015 VL 347 IS 6221 BP 526 EP 530 DI 10.1126/science.1261949 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CA0YK UT WOS:000348639300047 PM 25635094 ER PT J AU Meibom, S Barnes, SA Platais, I Gilliland, RL Latham, DW Mathieu, RD AF Meibom, Soren Barnes, Sydney A. Platais, Imants Gilliland, Ronald L. Latham, David W. Mathieu, Robert D. TI A spin-down clock for cool stars from observations of a 2.5-billion-year-old cluster SO NATURE LA English DT Article ID WIYN OPEN CLUSTER; ANGULAR-MOMENTUM LOSS; TIME-SERIES ANALYSIS; MAIN-SEQUENCE STARS; OLD OPEN CLUSTER; SOLAR-TYPE STARS; NGC 6819; STELLAR ROTATION; ERROR-CORRECTION; CCD PHOTOMETRY AB The ages of the most common stars-low-mass (cool) stars like the Sun, and smaller-are difficult to derive(1,2) because traditional dating methods use stellar properties that either change little as the stars age(3,4) or are hard to measure(5-8). The rotation rates of all cool stars decrease substantially with time as the stars steadily lose their angular momenta. If properly calibrated, rotation therefore can act as a reliable determinant of their ages based on the method of gyrochronology(2,9-11). To calibrate gyrochronology, the relationship between rotation period and age must be determined for cool stars of different masses, which is best accomplished with rotation period measurements for stars in clusters with well-known ages. Hitherto, such measurements have been possible only in clusters with ages of less than about one billion years(12-16), and gyrochronology ages for older stars have been inferred from model predictions(2,7,11,17). Here we report rotation period measurements for 30 cool stars in the 2.5-billion-year-old cluster NGC 6819. The periods reveal a well-defined relationship between rotation period and stellar mass at the cluster age, suggesting that ages with a precision of order 10 per cent can be derived for large numbers of cool Galactic field stars. C1 [Meibom, Soren; Latham, David W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Barnes, Sydney A.] Leibniz Inst Astrophys, D-14482 Potsdam, Germany. [Barnes, Sydney A.] Space Sci Inst, Boulder, CO 80301 USA. [Platais, Imants] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Gilliland, Ronald L.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA. [Mathieu, Robert D.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. RP Meibom, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM smeibom@cfa.harvard.edu FU NASA [NNX09AH18A]; NSF [1312882]; Smithsonian Institution's Competitive Grants Program for Science; German Science Foundation (DFG); Research in Astronomy, Inc., under NASA [NAS5-26555]; NASA Office of Space Science [NNX13AC07G] FX S.M. acknowledges support through NASA grant NNX09AH18A (The Kepler ClusterStudy), NSF grant 1312882 (The Kepler ClusterStudy: Planets and Gyrochronology) and the Smithsonian Institution's Competitive Grants Program for Science in 2012 and 2013. S.A.B. acknowledges support from the German Science Foundation (DFG) during a crucial phase of this work via a Mercator Guest Professorship at the University of Potsdam and the Leibniz Institute for Astrophysics Potsdam, Germany. This paper includes data collected by the Kepler mission. Kepler was competitively selected as the tenth Discovery mission. Funding for the Kepler mission is provided by the NASA Science Mission directorate. Some or all of the data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST). STScl is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant NNX13AC07G and by other grants and contracts. Spectroscopic observations of NGC 6819 with the Hectochelle spectrograph were obtained at the MMT Observatory, a joint facility of the Smithsonian Institution and the University of Arizona. NR 45 TC 43 Z9 43 U1 0 U2 4 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 EI 1476-4687 J9 NATURE JI Nature PD JAN 29 PY 2015 VL 517 IS 7536 BP 589 EP U347 DI 10.1038/nature14118 PG 15 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CA2ZL UT WOS:000348775000037 PM 25539085 ER PT J AU Luan, L Grinolds, MS Hong, SK Maletinsky, P Walsworth, RL Yacoby, A AF Luan, Lan Grinolds, Michael S. Hong, Sungkun Maletinsky, Patrick Walsworth, Ronald L. Yacoby, Amir TI Decoherence imaging of spin ensembles using a scanning single-electron spin in diamond SO SCIENTIFIC REPORTS LA English DT Article ID NUCLEAR-MAGNETIC-RESONANCE; NITROGEN-VACANCY SPIN; TOPOLOGICAL INSULATORS; AMBIENT CONDITIONS; MAGNETOMETRY; RESOLUTION; COHERENCE; DYNAMICS; CENTERS; SENSOR AB The nitrogen-vacancy (NV) defect center in diamond has demonstrated great capability for nanoscale magnetic sensing and imaging for both static and periodically modulated target fields. However, it remains a challenge to detect and image randomly fluctuating magnetic fields. Recent theoretical and numerical works have outlined detection schemes that exploit changes in decoherence of the detector spin as a sensitive measure for fluctuating fields. Here we experimentally monitor the decoherence of a scanning NV center in order to image the fluctuating magnetic fields from paramagnetic impurities on an underlying diamond surface. We detect a signal corresponding to roughly 800 mu(B) in 2 s of integration time, without any control on the target spins, and obtain magnetic-field spectral information using dynamical decoupling techniques. The extracted spatial and temporal properties of the surface paramagnetic impurities provide insight to prolonging the coherence of near-surface qubits for quantum information and metrology applications. C1 [Luan, Lan; Grinolds, Michael S.; Hong, Sungkun; Yacoby, Amir] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Hong, Sungkun] Univ Vienna, Fac Phys, Vienna Ctr Quantum Sci & Technol VCQ, A-1090 Vienna, Austria. [Maletinsky, Patrick] Univ Basel, Dept Phys, CH-4056 Basel, Switzerland. [Walsworth, Ronald L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Yacoby, A (reprint author), Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. EM yacoby@physics.harvard.edu RI Maletinsky, Patrick/L-1851-2015 OI Maletinsky, Patrick/0000-0003-1699-388X FU Department of Defense (NDSEG programme); National Science Foundation; Kwanjeong Scholarship Foundation; DARPA QuEST programme; QuASAR programme; MURI QuISM FX The authors thank Element Six for providing diamond samples for both the sensor and targets. M.S.G. is supported through fellowships from the Department of Defense (NDSEG programme) and the National Science Foundation. S.H. acknowledges support from the Kwanjeong Scholarship Foundation when at Harvard University. This work was supported by the DARPA QuEST and QuASAR programmes and the MURI QuISM. NR 38 TC 10 Z9 10 U1 6 U2 56 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 2045-2322 J9 SCI REP-UK JI Sci Rep PD JAN 29 PY 2015 VL 5 AR 8119 DI 10.1038/srep08119 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AZ8ZQ UT WOS:000348501100010 PM 25631646 ER PT J AU Kristiansen, NI Prata, AJ Stohl, A Carn, SA AF Kristiansen, N. I. Prata, A. J. Stohl, A. Carn, S. A. TI Stratospheric volcanic ash emissions fromthe 13 February 2014 Kelut eruption SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE volcanic ash; satellite observations; transport modeling; inversion techniques; aircraft encounter; stratospheric ID EYJAFJALLAJOKULL ERUPTION; SULFUR-DIOXIDE; DISPERSION; TRANSPORT; RETRIEVAL; GRIMSVOTN; AIRCRAFT; CLOUDS AB Mount Kelut (Indonesia) erupted explosively around 15:50 UT on 13 February 2014 sending ash and gases into the stratosphere. Satellite ash retrievals and dispersion transport modeling are combined within an inversion framework to estimate the volcanic ash source term and to study ash transport. The estimated source term suggests that most of the ash was injected to altitudes of 16-17km, in agreement with space-based lidar data. Modeled ash concentrations along the flight track of a commercial aircraft that encountered the ash cloud indicate that it flew under the main ash cloud and encountered maximum ash concentrations of 93mgm(-3), mean concentrations of 21mgm(-3)over a period of 10-11min of the flight, giving a dosage of 1.20.3gsm(-3). Satellite data could not be used directly to observe the ash cloud encountered by the aircraft, whereas inverse modeling revealed its presence. C1 [Kristiansen, N. I.; Prata, A. J.; Stohl, A.] Norwegian Inst Air Res, Kjeller, Norway. [Prata, A. J.] Nicarn Aviat, Kjeller, Norway. [Carn, S. A.] Michigan Technol Univ, Dept Geol & Min Engn & Sci, Houghton, MI 49931 USA. [Carn, S. A.] Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DE USA. RP Kristiansen, NI (reprint author), Norwegian Inst Air Res, Kjeller, Norway. EM nik@nilu.no RI Stohl, Andreas/A-7535-2008 OI Stohl, Andreas/0000-0002-2524-5755 FU European Space Agency; NASA [NNX11AF42G, NNX13AF50G] FX We thank the Japan Meteorological Agency (JMA) and Wataru Takeuchi (University of Tokyo) for supplying the MTSAT 2 data and Manfred Birnfeld (AIRBUS) for helpful advice regarding the aircraft flight track. NASA provided the data from MODIS, CALIOP, and MLS used in this study. This work was partially funded by the European Space Agency under the VAST project. S.A.C. acknowledges support from NASA through the Aura Science Team (grant NNX11AF42G) and MEaSUREs (grant NNX13AF50G) programs. The data used to produce Figure 2c (source term) are provided as supporting information to this manuscript. NR 25 TC 11 Z9 11 U1 2 U2 12 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JAN 28 PY 2015 VL 42 IS 2 BP 588 EP 596 DI 10.1002/2014GL062307 PG 9 WC Geosciences, Multidisciplinary SC Geology GA CB9MO UT WOS:000349956000050 ER PT J AU Hagedorn, M Carter, V Zuchowicz, N Phillips, M Penfield, C Shamenek, B Vallen, EA Kleinhans, FW Peterson, K White, M Yancey, PH AF Hagedorn, Mary Carter, Virginia Zuchowicz, Nikolas Phillips, Micaiah Penfield, Chelsea Shamenek, Brittany Vallen, Elizabeth A. Kleinhans, Frederick W. Peterson, Kelly White, Meghan Yancey, Paul H. TI Trehalose Is a Chemical Attractant in the Establishment of Coral Symbiosis SO PLOS ONE LA English DT Article ID LARVAL SETTLEMENT; ALGAL SYMBIONTS; HOST; SYMBIODINIUM; ZOOXANTHELLAE; RECOGNITION; BEHAVIOR; LIGHT; ACQUISITION; DIVERSITY AB Coral reefs have evolved with a crucial symbiosis between photosynthetic dinoflagellates (genus Symbiodinium) and their cnidarian hosts (Scleractinians). Most coral larvae take up Symbiodinium from their environment; however, the earliest steps in this process have been elusive. Here we demonstrate that the disaccharide trehalose may be an important signal from the symbiont to potential larval hosts. Symbiodinium freshly isolated from Fungia scutaria corals constantly released trehalose (but not sucrose, maltose or glucose) into seawater, and released glycerol only in the presence of coral tissue. Spawning Fungia adults increased symbiont number in their immediate area by excreting pellets of Symbiodinium, and when these naturally discharged Symbiodinium were cultured, they also released trehalose. In Y-maze experiments, coral larvae demonstrated chemoattractant and feeding behaviors only towards a chamber with trehalose or glycerol. Concomitantly, coral larvae and adult tissue, but not symbionts, had significant trehalase enzymatic activities, suggesting the capacity to utilize trehalose. Trehalase activity was developmentally regulated in F. scutaria larvae, rising as the time for symbiont uptake occurs. Consistent with the enzymatic assays, gene finding demonstrated the presence of a trehalase enzyme in the genome of a related coral, Acropora digitifera, and a likely trehalase in the transcriptome of F. scutaria. Taken together, these data suggest that adult F. scutaria seed the reef with Symbiodinium during spawning and the exuded Symbiodinium release trehalose into the environment, which acts as a chemoattractant for F. scutaria larvae and as an initiator of feeding behavior-the first stages toward establishing the coral-Symbiodinium relationship. Because trehalose is a fixed carbon compound, this cue would accurately demonstrate to the cnidarian larvae the photosynthetic ability of the potential symbiont in the ambient environment. To our knowledge, this is the first report of a chemical cue attracting the motile coral larvae to the symbiont. C1 [Hagedorn, Mary; Carter, Virginia; Zuchowicz, Nikolas; Phillips, Micaiah; Penfield, Chelsea; Shamenek, Brittany] Smithsonian Conservat Biol Inst, Dept Reprod Sci, Front Royal, VA 22630 USA. [Hagedorn, Mary; Carter, Virginia; Zuchowicz, Nikolas; Phillips, Micaiah; Penfield, Chelsea; Shamenek, Brittany] Univ Hawaii, Hawaii Inst Marine Biol, Kaneohe, HI USA. [Vallen, Elizabeth A.] Swarthmore Coll, Dept Biol, Swarthmore, PA USA. [Kleinhans, Frederick W.] Indiana Univ Purdue Univ Indianapolis, Dept Phys, Indianapolis, IN USA. [Peterson, Kelly; White, Meghan; Yancey, Paul H.] Dept Biol, Whitman Coll, Walla Walla, WA USA. RP Hagedorn, M (reprint author), Smithsonian Conservat Biol Inst, Dept Reprod Sci, Front Royal, VA 22630 USA. EM hagedomm@si.edu FU Roddenberry Foundation; Anela Kolohe Foundation; Taronga Conservation Society Australia; Whitman College Perry Grant; NIH [1F33GM096488-01]; NSF FX These experiments were funded through funds from the Roddenberry Foundation (MH), the Anela Kolohe Foundation (MH), the Taronga Conservation Society Australia (MH), Whitman College Perry Grant (PY) and NIH 1F33GM096488-01 (EAV) and NSF (EAV). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 57 TC 4 Z9 4 U1 6 U2 27 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD JAN 28 PY 2015 VL 10 IS 1 AR e0117087 DI 10.1371/journal.pone.0117087 PG 18 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CA2IM UT WOS:000348732100062 PM 25629699 ER PT J AU Wray, LA Huang, SW Xia, YQ Hasan, MZ Mathy, C Eisaki, H Hussain, Z Chuang, YD AF Wray, L. Andrew Huang, Shih-Wen Xia, Yuqi Hasan, M. Zahid Mathy, Charles Eisaki, Hiroshi Hussain, Zahid Chuang, Yi-De TI Experimental signatures of phase interference and subfemtosecond time dynamics on the incident energy axis of resonant inelastic x-ray scattering SO PHYSICAL REVIEW B LA English DT Article ID ONE-DIMENSIONAL SRCUO2; ELECTRONIC-STRUCTURE; EXCITATIONS; NIO; PHOTOEMISSION; EMISSION AB Core hole resonance is used in x-ray spectroscopy to incisively probe the local electronic states of many-body systems. Here, resonant inelastic x-ray scattering (RIXS) is studied as a function of incident photon energy on Mott insulators SrCuO2 and NiO to examine how resonance states decay into different excitation symmetries at the transition-metal M, L, and K edges. Quantum interference patterns characteristic of the two major RIXS mechanisms are identified within the data, and used to distinguish the attosecond scale scattering dynamics by which fundamental excitations of a many-body system are created. A function is proposed to experimentally evaluate whether a particular excitation has constructive or destructive interference in the RIXS cross section, and corroborates other evidence that an anomalous excitation is present at the leading edge of the Mott gap in quasi-one-dimensional SrCuO2. C1 [Wray, L. Andrew] NYU, Dept Phys, New York, NY 10003 USA. [Huang, Shih-Wen; Hussain, Zahid; Chuang, Yi-De] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Adv Light Source, Berkeley, CA 94720 USA. [Xia, Yuqi; Hasan, M. Zahid] Princeton Univ, Dept Phys, Joseph Henry Labs, Princeton, NJ 08544 USA. [Mathy, Charles] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. [Eisaki, Hiroshi] Natl Inst Adv Ind Sci & Technol, Nanoelect Res Inst, Tsukuba, Ibaraki 3058568, Japan. RP Wray, LA (reprint author), NYU, Dept Phys, 4 Washington Pl, New York, NY 10003 USA. EM lawray@nyu.edu FU US DOE/BES Grant [DE-FG02-05ER46200]; Office of Science, Office of Basic Energy Sciences, of the US Department of Energy [DE-AC02-05CH11231]; Argonne National Laboratory [DE-AC02-06CH11357] FX We are grateful for discussions with K. Wohlfeld, B. Moritz, T. Devereaux, K. Ishii, I. Jarrige, R. Eder, D.-H. Lee, S. Roy, and P. Shafer. M. Z. H. was supported by US DOE/BES Grant No. DE-FG02-05ER46200. The Advanced Light Source is supported by the Director, Office of Science, Office of Basic Energy Sciences, of the US Department of Energy under Contract No. DE-AC02-05CH11231. This research used resources of the Advanced Photon Source, a US Department of Energy (DOE) Office of Science User Facility operated for the DOE Office of Science by Argonne National Laboratory under Contract No. DE-AC02-06CH11357. NR 37 TC 3 Z9 3 U1 3 U2 21 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2469-9950 EI 2469-9969 J9 PHYS REV B JI Phys. Rev. B PD JAN 27 PY 2015 VL 91 IS 3 AR 035131 DI 10.1103/PhysRevB.91.035131 PG 11 WC Physics, Condensed Matter SC Physics GA CA3WF UT WOS:000348834400001 ER PT J AU Abramowski, A Aharonian, F Benkhali, FA Akhperjanian, AG Anguner, EO Backes, M Balenderan, S Balzer, A Barnacka, A Becherini, Y Becker-Tjus, J Berge, D Bernhard, S Bernlohr, K Birsin, E Biteau, J Bottcher, M Boisson, C Bolmont, J Bordas, P Bregeon, J Brun, F Brun, P Bryan, M Bulik, T Carrigan, S Casanova, S Chadwick, PM Chakraborty, N Chalme-Calvet, R Chaves, RCG Chretien, M Colafrancesco, S Cologna, G Conrad, J Couturier, C Cui, Y Dalton, M Davids, ID Degrange, B Deil, C de Wilt, P Djannati-Atai, A Domainko, W Donath, A Drury, LO Dubus, G Dutson, K Dyks, J Dyrda, M Edwards, T Egberts, K Eger, P Espigat, P Farnier, C Fegan, S Feinstein, F Fernandes, MV Fernandez, D Fiasson, A Fontaine, G Forster, A Fussling, M Gabici, S Gajdus, M Gallant, YA Garrigoux, T Giavitto, G Giebels, B Glicenstein, JF Gottschall, D Grondin, MH Grudzinska, M Hadasch, D Haffner, S Hahn, J Harris, J Heinzelmann, G Henri, G Hermann, G Hervet, O Hillert, A Hinton, JA Hofmann, W Hofverberg, P Holler, M Horns, D Ivascenko, A Jacholkowska, A Jahn, C Jamrozy, M Janiak, M Jankowsky, F Jung, I Kastendieck, MA Katarzynski, K Katz, U Kaufmann, S Khelifi, B Kieffer, M Klepser, S Klochkov, D Kluzniak, W Kolitzus, D Komin, N Kosack, K Krakau, S Krayzel, F Kruger, PP Laffon, H Lamanna, G Lefaucheur, J Lefranc, V Lemiere, A Lemoine-Goumard, M Lenain, JP Lohse, T Lopatin, A Lu, CC Marandon, V Marcowith, A Marx, R Maurin, G Maxted, N Mayer, M McComb, TJL Mehault, J Meintjes, PJ Menzler, U Meyer, M Mitchell, AMW Moderski, R Mohamed, M Mora, K Moulin, E Murach, T de Naurois, M Niemiec, J Nolan, SJ Oakes, L Odaka, H Ohm, S Opitz, B Ostrowski, M Oya, I Panter, M Parsons, RD Arribas, MP Pekeur, NW Pelletier, G Perez, J Petrucci, PO Peyaud, B Pita, S Poon, H Puhlhofer, G Punch, M Quirrenbach, A Raab, S Reichardt, I Reimer, A Reimer, O Renaud, M de los Reyes, R Rieger, F Rob, L Romoli, C Rosier-Lees, S Rowell, G Rudak, B Rulten, CB Sahakian, V Salek, D Sanchez, DA Santangelo, A Schlickeiser, R Schussler, F Schulz, A Schwanke, U Schwarzburg, S Schwemmer, S Sol, H Spanier, F Spengler, G Spies, F Stawarz, L Steenkamp, R Stegmann, C Stinzing, F Stycz, K Sushch, I Tavernet, JP Tavernier, T Taylor, AM Terrier, R Tluczykont, M Trichard, C Valerius, K van Eldik, C van Soelen, B Vasileiadis, G Veh, J Venter, C Viana, A Vincent, P Vink, J Volk, HJ Volpe, F Vorster, M Vuillaume, T Wagner, SJ Wagner, P Wagner, RM Ward, M Weidinger, M Weitzel, Q White, R Wierzcholska, A Willmann, P Wornlein, A Wouters, D Yang, R Zabalza, V Zaborov, D Zacharias, M Zdziarski, AA Zech, A Zechlin, HS AF Abramowski, A. Aharonian, F. Benkhali, F. Ait Akhperjanian, A. G. Anguener, E. O. Backes, M. Balenderan, S. Balzer, A. Barnacka, A. Becherini, Y. Becker-Tjus, J. Berge, D. Bernhard, S. Bernloehr, K. Birsin, E. Biteau, J. Boettcher, M. Boisson, C. Bolmont, J. Bordas, P. Bregeon, J. Brun, F. Brun, P. Bryan, M. Bulik, T. Carrigan, S. Casanova, S. Chadwick, P. M. Chakraborty, N. Chalme-Calvet, R. Chaves, R. C. G. Chretien, M. Colafrancesco, S. Cologna, G. Conrad, J. Couturier, C. Cui, Y. Dalton, M. Davids, I. D. Degrange, B. Deil, C. de Wilt, P. Djannati-Atai, A. Domainko, W. Donath, A. Drury, L. O'C. Dubus, G. Dutson, K. Dyks, J. Dyrda, M. Edwards, T. Egberts, K. Eger, P. Espigat, P. Farnier, C. Fegan, S. Feinstein, F. Fernandes, M. V. Fernandez, D. Fiasson, A. Fontaine, G. Foerster, A. Fuessling, M. Gabici, S. Gajdus, M. Gallant, Y. A. Garrigoux, T. Giavitto, G. Giebels, B. Glicenstein, J. F. Gottschall, D. Grondin, M-H. Grudzinska, M. Hadasch, D. Haeffner, S. Hahn, J. Harris, J. Heinzelmann, G. Henri, G. Hermann, G. Hervet, O. Hillert, A. Hinton, J. A. Hofmann, W. Hofverberg, P. Holler, M. Horns, D. Ivascenko, A. Jacholkowska, A. Jahn, C. Jamrozy, M. Janiak, M. Jankowsky, F. Jung, I. Kastendieck, M. A. Katarzynski, K. Katz, U. Kaufmann, S. Khelifi, B. Kieffer, M. Klepser, S. Klochkov, D. Kluzniak, W. Kolitzus, D. Komin, Nu. Kosack, K. Krakau, S. Krayzel, F. Krueger, P. P. Laffon, H. Lamanna, G. Lefaucheur, J. Lefranc, V. Lemiere, A. Lemoine-Goumard, M. Lenain, J-P. Lohse, T. Lopatin, A. Lu, C-C. Marandon, V. Marcowith, A. Marx, R. Maurin, G. Maxted, N. Mayer, M. McComb, T. J. L. Mehault, J. Meintjes, P. J. Menzler, U. Meyer, M. Mitchell, A. M. W. Moderski, R. Mohamed, M. Mora, K. Moulin, E. Murach, T. de Naurois, M. Niemiec, J. Nolan, S. J. Oakes, L. Odaka, H. Ohm, S. Opitz, B. Ostrowski, M. Oya, I. Panter, M. Parsons, R. D. Arribas, M. Paz Pekeur, N. W. Pelletier, G. Perez, J. Petrucci, P-O. Peyaud, B. Pita, S. Poon, H. Puehlhofer, G. Punch, M. Quirrenbach, A. Raab, S. Reichardt, I. Reimer, A. Reimer, O. Renaud, M. de los Reyes, R. Rieger, F. Rob, L. Romoli, C. Rosier-Lees, S. Rowell, G. Rudak, B. Rulten, C. B. Sahakian, V. Salek, D. Sanchez, D. A. Santangelo, A. Schlickeiser, R. Schuessler, F. Schulz, A. Schwanke, U. Schwarzburg, S. Schwemmer, S. Sol, H. Spanier, F. Spengler, G. Spies, F. Stawarz, L. Steenkamp, R. Stegmann, C. Stinzing, F. Stycz, K. Sushch, I. Tavernet, J-P. Tavernier, T. Taylor, A. M. Terrier, R. Tluczykont, M. Trichard, C. Valerius, K. van Eldik, C. van Soelen, B. Vasileiadis, G. Veh, J. Venter, C. Viana, A. Vincent, P. Vink, J. Voelk, H. J. Volpe, F. Vorster, M. Vuillaume, T. Wagner, S. J. Wagner, P. Wagner, R. M. Ward, M. Weidinger, M. Weitzel, Q. White, R. Wierzcholska, A. Willmann, P. Woernlein, A. Wouters, D. Yang, R. Zabalza, V. Zaborov, D. Zacharias, M. Zdziarski, A. A. Zech, A. Zechlin, H-S. CA HESS Collaboration TI The exceptionally powerful TeV gamma-ray emitters in the Large Magellanic Cloud SO SCIENCE LA English DT Article ID YOUNG SUPERNOVA-REMNANTS; LARGE-AREA TELESCOPE; PARTICLE-ACCELERATION; MILKY-WAY; CRAB-NEBULA; SN 1987A; SPECTROSCOPY; SUPERBUBBLES; ASTRONOMY; EMISSION AB The Large Magellanic Cloud, a satellite galaxy of the Milky Way, has been observed with the High Energy Stereoscopic System (H.E.S.S.) above an energy of 100 billion electron volts for a deep exposure of 210 hours. Three sources of different types were detected: the pulsar wind nebula of the most energetic pulsar known, N 157B; the radio-loud supernova remnant N 132D; and the largest nonthermal x-ray shell, the superbubble 30 Dor C. The unique object SN 1987A is, unexpectedly, not detected, which constrains the theoretical framework of particle acceleration in very young supernova remnants. These detections reveal the most energetic tip of a g-ray source population in an external galaxy and provide via 30 Dor C the unambiguous detection of g-ray emission from a superbubble. C1 [Abramowski, A.; Fernandes, M. V.; Heinzelmann, G.; Horns, D.; Kastendieck, M. A.; Opitz, B.; Spies, F.; Tluczykont, M.; Zechlin, H-S.] Univ Hamburg Inst Expt Phys, D-22761 Hamburg, Germany. [Aharonian, F.; Benkhali, F. Ait; Bernloehr, K.; Carrigan, S.; Casanova, S.; Chakraborty, N.; Deil, C.; Domainko, W.; Donath, A.; Edwards, T.; Eger, P.; Foerster, A.; Grondin, M-H.; Hahn, J.; Hermann, G.; Hillert, A.; Hofmann, W.; Hofverberg, P.; Lu, C-C.; Marandon, V.; Marx, R.; Mitchell, A. M. W.; Odaka, H.; Panter, M.; Parsons, R. D.; Poon, H.; de los Reyes, R.; Rieger, F.; Viana, A.; Voelk, H. J.; Volpe, F.; Weitzel, Q.; Yang, R.; Zabalza, V.] Max Planck Inst Kernphys, D-69029 Heidelberg, Germany. [Aharonian, F.; Drury, L. O'C.; Romoli, C.; Taylor, A. M.] Dublin Inst Adv Studies, Dublin 2, Ireland. [Aharonian, F.; Akhperjanian, A. G.; Sahakian, V.] Natl Acad Sci Republ Armenia, Yerevan 0019, Armenia. [Akhperjanian, A. G.; Sahakian, V.] Yerevan Phys Inst, Yerevan 375036, Armenia. [Anguener, E. O.; Bernloehr, K.; Birsin, E.; Gajdus, M.; Lohse, T.; Murach, T.; Oakes, L.; Oya, I.; Arribas, M. Paz; Schwanke, U.; Sushch, I.; Wagner, P.] Humboldt Univ, Inst Phys, D-12489 Berlin, Germany. [Backes, M.; Davids, I. D.; Steenkamp, R.] Univ Namibia, Dept Phys, Windhoek, Namibia. [Balenderan, S.; Chadwick, P. M.; Harris, J.; McComb, T. J. L.; Nolan, S. J.; Ward, M.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Balzer, A.; Bryan, M.; Vink, J.] Univ Amsterdam, Astron Inst Anton Pannekoek, Gravitat Astroparticle Phys Amsterdam GRAPPA, NL-1098 XH Amsterdam, Netherlands. [Barnacka, A.; Jamrozy, M.; Ostrowski, M.; Stawarz, L.] Uniwersytet Jagiellonski, Obserwatorium Astronomiczne, PL-30244 Krakow, Poland. [Barnacka, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Becherini, Y.] Linnaeus Univ, Dept Phys & Elect Engn, S-35195 Vaxjo, Sweden. [Becker-Tjus, J.; Krakau, S.; Menzler, U.; Schlickeiser, R.; Weidinger, M.] Ruhr Univ Bochum, Inst Theoret Phys, Lehrstuhl Weltraum & Astrophys 4, D-44780 Bochum, Germany. [Berge, D.] Univ Amsterdam, Astron Inst Anton Pannekoek, GRAPPA, NL-1098 XH Amsterdam, Netherlands. [Berge, D.] Univ Amsterdam, Inst High Energy Phys, NL-1098 XH Amsterdam, Netherlands. [Bernhard, S.; Hadasch, D.; Kolitzus, D.; Perez, J.; Reimer, A.; Reimer, O.] Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria. [Biteau, J.; Degrange, B.; Fegan, S.; Fontaine, G.; Giebels, B.; Holler, M.; de Naurois, M.; Zaborov, D.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France. [Biteau, J.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Boettcher, M.; Davids, I. D.; Ivascenko, A.; Krueger, P. P.; Pekeur, N. W.; Spanier, F.; Sushch, I.; Venter, C.; Vorster, M.] North West Univ, Ctr Space Res, ZA-2520 Potchefstroom, South Africa. [Boisson, C.; Hervet, O.; Rulten, C. B.; Sol, H.; Zech, A.] Univ Paris Diderot, CNRS, Observ Paris, Lab Univ & Theories LUTH, F-92190 Meudon, France. [Bolmont, J.; Chalme-Calvet, R.; Chretien, M.; Couturier, C.; Garrigoux, T.; Jacholkowska, A.; Kieffer, M.; Lenain, J-P.; Tavernet, J-P.; Vincent, P.] Univ Paris 07, Univ Paris 06, LPNHE, CNRS,IN2P3, F-75252 Paris 5, France. [Bordas, P.; Cui, Y.; Gottschall, D.; Klochkov, D.; Puehlhofer, G.; Santangelo, A.; Schwarzburg, S.] Univ Tubingen, Inst Astron & Astrophys, D-72076 Tubingen, Germany. [Bregeon, J.; Chaves, R. C. G.; Feinstein, F.; Fernandez, D.; Gallant, Y. A.; Marcowith, A.; Renaud, M.; Vasileiadis, G.] Univ Montpellier 2, CNRS, Lab Univ & Particules Montpellier, IN2P3, F-34095 Montpellier 5, France. [Brun, F.; Brun, P.; Glicenstein, J. F.; Kosack, K.; Lefranc, V.; Moulin, E.; Peyaud, B.; Schuessler, F.; Wouters, D.] CEA Saclay, DSM Irfu, F-91191 Gif Sur Yvette, France. [Bulik, T.; Grudzinska, M.] Univ Warsaw, Astron Observ, PL-00478 Warsaw, Poland. [Casanova, S.; Dyrda, M.; Niemiec, J.; Wierzcholska, A.] Inst Fizyki Jadrowej PAN, PL-31342 Krakow, Poland. [Colafrancesco, S.; Komin, Nu.] Univ Witwatersrand, Sch Phys, ZA-2050 Johannesburg, South Africa. [Cologna, G.; Grondin, M-H.; Jankowsky, F.; Kaufmann, S.; Mohamed, M.; Quirrenbach, A.; Schwemmer, S.; Wagner, S. J.; Zacharias, M.] Heidelberg Univ, Landessternwarte, D-69117 Heidelberg, Germany. [Conrad, J.; Farnier, C.; Meyer, M.; Mora, K.; Spengler, G.; Wagner, R. M.] Stockholm Univ, Albanova Univ Ctr, Dept Phys, Oskar Klein Ctr, SE-10691 Stockholm, Sweden. [Dalton, M.; Laffon, H.; Lemoine-Goumard, M.; Mehault, J.] Univ Bordeaux 1, CNRS, IN2P3, Ctr Etud Nucl Borde HESS Collaborationaux Gradign, F-33175 Gradignan, France. [de Wilt, P.; Maxted, N.; Rowell, G.] Univ Adelaide, Sch Chem & Phys, Adelaide, SA 5005, Australia. [Djannati-Atai, A.; Espigat, P.; Gabici, S.; Khelifi, B.; Lefaucheur, J.; Lemiere, A.; Pita, S.; Punch, M.; Reichardt, I.; Tavernier, T.; Terrier, R.] Univ Paris Diderot, APC, CNRS, IN2P3,CEA Irfu,Observ Paris,Sorbonne Paris Cite,A, F-75205 Paris 13, France. [Dubus, G.; Henri, G.; Pelletier, G.; Petrucci, P-O.; Vuillaume, T.] Univ Grenoble Alpes, IPAG, F-38000 Grenoble, France. [Dubus, G.; Henri, G.; Pelletier, G.; Petrucci, P-O.; Vuillaume, T.] CNRS, IPAG, F-38000 Grenoble, France. [Dutson, K.; Hinton, J. A.; White, R.; Zabalza, V.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Dyks, J.; Janiak, M.; Kluzniak, W.; Moderski, R.; Rudak, B.; Zdziarski, A. A.] Nicolaus Copernicus Astron Ctr, PL-00716 Warsaw, Poland. [Egberts, K.; Fuessling, M.; Holler, M.; Mayer, M.; Stegmann, C.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany. [Fiasson, A.; Krayzel, F.; Lamanna, G.; Maurin, G.; Rosier-Lees, S.; Sanchez, D. A.; Trichard, C.] Univ Savoie, CNRS, IN2P3, Lab Annecy le Vieux Phys Particules, F-74941 Annecy Le Vieux, France. [Giavitto, G.; Klepser, S.; Ohm, S.; Schulz, A.; Stegmann, C.] Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany. [Haeffner, S.; Jahn, C.; Jung, I.; Katz, U.; Lopatin, A.; Raab, S.; Stinzing, F.; Valerius, K.; van Eldik, C.; Veh, J.; Willmann, P.; Woernlein, A.] Univ Erlangen Nurnberg, Phys Inst, D-91058 Erlangen, Germany. [Katarzynski, K.; Stycz, K.] Nicolaus Copernicus Univ, Ctr Astron, Fac Phys Astron & Informat, PL-87100 Torun, Poland. [Meintjes, P. J.; van Soelen, B.] Univ Free State, Dept Phys, ZA-9300 Bloemfontein, South Africa. [Rob, L.] Charles Univ Prague, Fac Math & Phys, Inst Particle & Nucl Phys, CR-18000 Prague 8, Czech Republic. [Salek, D.] Univ Amsterdam, Inst High Energy Phys, GRAPPA, NL-1098 XH Amsterdam, Netherlands. RP Abramowski, A (reprint author), Univ Hamburg Inst Expt Phys, Luruper Chaussee 149, D-22761 Hamburg, Germany. RI van Eldik, Christopher/C-3901-2013; Tjus, Julia/G-8145-2012; Meyer, Manuel/E-2697-2016; Reichardt, Ignasi/P-7478-2016; Komin, Nukri/J-6781-2015; Schussler, Fabian/G-5313-2013; Katarzynski, Krzysztof/G-4528-2014; Jamrozy, Marek/F-4507-2015; Katz, Uli/E-1925-2013; Casanova, Sabrina/J-8935-2013; Reimer, Olaf/A-3117-2013 OI van Eldik, Christopher/0000-0001-9669-645X; Meyer, Manuel/0000-0002-0738-7581; Reichardt, Ignasi/0000-0003-3694-3820; Komin, Nukri/0000-0003-3280-0582; Schussler, Fabian/0000-0003-1500-6571; Katz, Uli/0000-0002-7063-4418; Casanova, Sabrina/0000-0002-6144-9122; Reimer, Olaf/0000-0001-6953-1385 FU German Ministry for Education and Research (BMBF); Max Planck Society; German Research Foundation (DFG); French Ministry for Research; CNRS-IN2P3; Astroparticle Interdisciplinary Programme of the CNRS; U.K. Science and Technology Facilities Council (STFC); Institute of Particle and Nuclear Physics (IPNP) of Charles University; Czech Science Foundation; Polish Ministry of Science and Higher Education; South African Department of Science and Technology; South African National Research Foundation; University of Namibia; European Community [ERC-StG-259391] FX The support of the Namibian authorities and of the University of Namibia in facilitating the construction and operation of H.E.S.S. is gratefully acknowledged, as is the support by the German Ministry for Education and Research (BMBF), the Max Planck Society, the German Research Foundation (DFG), the French Ministry for Research, the CNRS-IN2P3 and the Astroparticle Interdisciplinary Programme of the CNRS, the U.K. Science and Technology Facilities Council (STFC), the Institute of Particle and Nuclear Physics (IPNP) of Charles University, the Czech Science Foundation, the Polish Ministry of Science and Higher Education, the South African Department of Science and Technology and National Research Foundation, and the University of Namibia. J.C. is aWallenberg Academy Fellow. M.D. and J.M. are funded by contract ERC-StG-259391 from the European Community. We appreciate the excellent work of the technical support staff in Berlin, Durham, Hamburg, Heidelberg, Palaiseau, Paris, Saclay, and Namibia in the construction and operation of the equipment. The H.E.S.S. Collaboration will make public the smoothed excess sky map and the associated correlated significance map as shown in Fig. 1, together with the source spectral points, on the H.E.S.S. website on the link to this publication: www.mpi-hd.mpg.de/hfm/HESS/pages/publications. We thank B. Katz, E. Waxman, and R. Budnik for their external proposal supporting observations of the SNR N 132D based on their work on g-ray emission from shell-type SNRs (43). NR 58 TC 14 Z9 15 U1 2 U2 20 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 EI 1095-9203 J9 SCIENCE JI Science PD JAN 23 PY 2015 VL 347 IS 6220 BP 406 EP 412 DI 10.1126/science.1261313 PG 7 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AZ4XZ UT WOS:000348225800039 ER PT J AU Becerra, F Greif, TH Springel, V Hernquist, LE AF Becerra, Fernando Greif, Thomas H. Springel, Volker Hernquist, Lars E. TI Formation of massive protostars in atomic cooling haloes SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE hydrodynamics; stars: formation galaxies: formation galaxies; high-redshift; cosmology: theory; early Universe ID SUPERMASSIVE BLACK-HOLES; POPULATION III STAR; MAGNETIC-FIELD AMPLIFICATION; DARK-MATTER HALOES; SMALL-SCALE DYNAMO; DIRECT COLLAPSE; PRIMORDIAL PROTOSTARS; VIRIAL TEMPERATURES; EARLY UNIVERSE; GRAVITATIONAL COLLAPSE AB We present the highest-resolution three-dimensional simulation to date of the collapse of an atomic cooling halo in the early Universe. We use the moving-mesh code AREPO with the primordial chemistry module introduced in Greif, which evolves the chemical and thermal rate equations for over more than 20 orders of magnitude in density. Molecular hydrogen cooling is suppressed by a strong Lyman Werner background, which facilitates the near-isothermal collapse of the gas at a temperature of about 10(4) K. Once the central gas cloud becomes optically thick to continuum emission, it settles into a Keplerian disc around the primary protostar. The initial mass of the protostar is about 0.1 M circle dot, which is an order of magnitude higher than in minihaloes that cool via molecular hydrogen. The high accretion rate and efficient cooling of the gas catalyse the fragmentation of the disc into a small protostellar system with 5-10 members. After about 12 yr, strong gravitational interactions disrupt the disc and temporarily eject the primary protostar from the centre of the cloud. By the end of the simulation, a secondary clump has collapsed at a distance of similar or equal to 150 au from the primary clump. If this clump undergoes a similar evolution as the first, the central gas cloud may evolve into a wide binary system. High accretion rates of both the primary and secondary clumps suggest that fragmentation is not a significant barrier for forming at least one massive black hole seed. C1 [Becerra, Fernando; Greif, Thomas H.; Hernquist, Lars E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Springel, Volker] Heidelberg Inst Theoret Studies, D-69118 Heidelberg, Germany. [Springel, Volker] Heidelberg Univ, ARI, Zentrum Astron, D-69120 Heidelberg, Germany. RP Becerra, F (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM fbecerra@cfa.harvard.edu FU European Research Council [ERC-StG EXAGAL-308037] FX FB would like to thank Simon Glover, Paul Clark, John Regan, Muhammad Latif, and Kohei Inayoshi for stimulating discussions and feedback during the conference 'The physics of first stars and galaxy formation' at The Higgs Centre for Theoretical Physics of the University of Edinburgh. VS acknowledges support by the European Research Council under ERC-StG EXAGAL-308037. The simulations were carried out at the Texas Advanced Computing Center (TACC) under XSEDE allocation AST130020. NR 89 TC 29 Z9 29 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 JAN 21 PY 2015 VL 446 IS 3 BP 2380 EP 2393 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CC3TG UT WOS:000350272300015 ER PT J AU D'Ammando, F Orienti, M Finke, J Raiteri, CM Hovatta, T Larsson, J Max-Moerbeck, W Perkins, J Readhead, ACS Richards, JL Beilicke, M Benbow, W Berger, K Bird, R Bugaev, V Cardenzana, JV Cerruti, M Chen, X Ciupik, L Dickinson, HJ Eisch, JD Errando, M Falcone, A Finley, JP Fleischhack, H Fortin, P Fortson, L Furniss, A Gerard, L Gillanders, GH Griffiths, ST Grube, J Gyuk, G Hakansson, N Holder, J Humensky, TB Kar, P Kertzman, M Khassen, Y Kieda, D Krennrich, F Kumar, S Lang, MJ Maier, G McCann, A Meagher, K Moriarty, P Mukherjee, R Nieto, D de Bhroithe, AO Ong, RA Otte, AN Pohl, M Popkow, A Prokoph, H Pueschel, E Quinn, J Ragan, K Reynolds, PT Richards, GT Roache, E Rousselle, J Santander, M Sembroski, GH Smith, AW Staszak, D Telezhinsky, I Tucci, JV Tyler, J Varlotta, A Vassiliev, VV Wakely, SP Weinstein, A Welsing, R Williams, DA Zitzer, B AF D'Ammando, F. Orienti, M. Finke, J. Raiteri, C. M. Hovatta, T. Larsson, J. Max-Moerbeck, W. Perkins, J. Readhead, A. C. S. Richards, J. L. Beilicke, M. Benbow, W. Berger, K. Bird, R. Bugaev, V. Cardenzana, J. V. Cerruti, M. Chen, X. Ciupik, L. Dickinson, H. J. Eisch, J. D. Errando, M. Falcone, A. Finley, J. P. Fleischhack, H. Fortin, P. Fortson, L. Furniss, A. Gerard, L. Gillanders, G. H. Griffiths, S. T. Grube, J. Gyuk, G. Hakansson, N. Holder, J. Humensky, T. B. Kar, P. Kertzman, M. Khassen, Y. Kieda, D. Krennrich, F. Kumar, S. Lang, M. J. Maier, G. McCann, A. Meagher, K. Moriarty, P. Mukherjee, R. Nieto, D. de Bhroithe, A. O'Faolain Ong, R. A. Otte, A. N. Pohl, M. Popkow, A. Prokoph, H. Pueschel, E. Quinn, J. Ragan, K. Reynolds, P. T. Richards, G. T. Roache, E. Rousselle, J. Santander, M. Sembroski, G. H. Smith, A. W. Staszak, D. Telezhinsky, I. Tucci, J. V. Tyler, J. Varlotta, A. Vassiliev, V. V. Wakely, S. P. Weinstein, A. Welsing, R. Williams, D. A. Zitzer, B. CA VERITAS Collaboration TI The most powerful flaring activity from the NLSyl PMN J0948+0022 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: active-galaxies: individual: PMN J0948+0022; galaxies: nuclei; galaxies: Seyfert; gamma-rays: general ID LINE SEYFERT 1; GAMMA-RAY EMISSION; LARGE-AREA TELESCOPE; QUASAR PKS 1510-089; EXTRAGALACTIC BACKGROUND LIGHT; SPECTRUM RADIO QUASARS; GALACTIC NUCLEI; X-RAY; MULTIWAVELENGTH OBSERVATIONS; RELATIVISTIC JETS AB We report on multifrequency observations performed during 2012 December-2013 August of the first narrow-line Seyfert 1 galaxy detected in gamma-rays, PMN J0948+0022 (z = 0.5846). A y -ray flare was observed by the Large Area Telescope on board Fermi during 2012 December-2013 January, reaching a daily peak flux in the 0.1-100 GeV energy range of (155 31) x 10 8 ph cm(-2) S-1 on 2013 January 1, corresponding to an apparent isotropic luminosity of similar to 1.5 x 1048 erg s(-1). The y -ray flaring period triggered Swift and Very Energetic Radiation Imaging Telescope Array System (VERITAS) observations in addition to radio and optical monitoring by Owens Valley Radio Observatory, Monitoring Of Jets in Active galactic nuclei with VLBA Experiments, and Catalina Real-time Transient Survey. A strong flare was observed in optical, UV, and X-rays on 2012 December 30, quasi-simultaneously to the y -ray flare, reaching a record flux for this source from optical to y gamma-rays. VERITAS observations at very high energy (E > 100 GeV) during 2013 January 6-17 resulted in an upper limit of F>0.2 Trev < 4.0 x 10(-12) ph cm(-2) s(-1). We compared the spectral energy distribution (SED) of the flaring state in 2013 January with that of an intermediate state observed in 2011. The two SEDs, modelled as synchrotron emission and an external Compton scattering of seed photons from a dust torus, can be modelled by changing both the electron distribution parameters and the magnetic field. C1 [D'Ammando, F.] Univ Bologna, Dipartimento Fis & Astron, I-40127 Bologna, Italy. [D'Ammando, F.] Inaf Ist Radioastron, I-40129 Bologna, Italy. [Finke, J.] US Naval Res Lab, Washington, DC 20375 USA. [Raiteri, C. M.] INAF Osservatorio Astrofis Torino, I-10025 Pino Torinese, TO, Italy. [Hovatta, T.; Readhead, A. C. S.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Larsson, J.] KTH, Dept Phys, SE-10691 Stockholm, Sweden. [Larsson, J.] KTH, Oskar Klein Ctr, SE-10691 Stockholm, Sweden. [Max-Moerbeck, W.] Natl Radio Astron Observ NRAO, Socorro, NM 87801 USA. [Perkins, J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Richards, J. L.; Finley, J. P.; Sembroski, G. H.; Tucci, J. V.; Varlotta, A.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Beilicke, M.; Bugaev, V.] Washington Univ, Dept Phys, St Louis, MO 63130 USA. [Benbow, W.; Cerruti, M.; Fortin, P.; Roache, E.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. [Berger, K.; Holder, J.; Kumar, S.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Berger, K.; Holder, J.; Kumar, S.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Bird, R.; Khassen, Y.; Pueschel, E.; Quinn, J.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland. [Cardenzana, J. V.; Dickinson, H. J.; Eisch, J. D.; Krennrich, F.; Weinstein, A.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Chen, X.; Hakansson, N.; Pohl, M.; Telezhinsky, I.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany. [Chen, X.; Fleischhack, H.; Gerard, L.; Maier, G.; de Bhroithe, A. O'Faolain; Pohl, M.; Prokoph, H.; Telezhinsky, I.; Welsing, R.] DESY, D-15738 Zeuthen, Germany. [Ciupik, L.; Grube, J.; Gyuk, G.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA. [Errando, M.; Mukherjee, R.; Santander, M.] Columbia Univ, Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA. [Falcone, A.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Fortson, L.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. [Furniss, A.; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Furniss, A.; Williams, D. A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA. [Gillanders, G. H.; Lang, M. J.; Moriarty, P.] Natl Univ Ireland Galway, Sch Phys, Galway, Ireland. [Griffiths, S. T.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Humensky, T. B.; Nieto, D.] Columbia Univ, Dept Phys, New York, NY 10027 USA. [Kar, P.; Kieda, D.; Smith, A. W.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Kertzman, M.] Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA. [McCann, A.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Meagher, K.; Otte, A. N.; Richards, G. T.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA. [Meagher, K.; Otte, A. N.; Richards, G. T.] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Ong, R. A.; Popkow, A.; Rousselle, J.; Vassiliev, V. V.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Ragan, K.; Staszak, D.; Tyler, J.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Reynolds, P. T.] Cork Inst Technol, Dept Appl Phys & Instrumentat, Cork, Ireland. [Wakely, S. P.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Zitzer, B.] Argonne Natl Lab, Argonne, IL 60439 USA. RP D'Ammando, F (reprint author), Univ Bologna, Dipartimento Fis & Astron, Viale Berti Pichat 6-2, I-40127 Bologna, Italy. EM dammando@ira.inaf.it; dammando@ira.inaf.it; dammando@ira.inaf.it; dammando@ira.inaf.it; dammando@ira.inaf.it; dammando@ira.inaf.it; dammando@ira.inaf.it RI Nieto, Daniel/J-7250-2015 OI Nieto, Daniel/0000-0003-3343-0755 FU US Department of Energy Office of Science; Smithsonian Institution; NSERC in Canada; Science Foundation Ireland [SFI 10/RFP/AST2748]; Science and Technology Facilities Council in the UK; NASA [NNX08AW31G, NNX11A043G]; NSF [AST-0808050, AST-1109911]; US National Science Foundation [AST-0909182]; Fermi Guest Investigator grants [NNX08AW56G, NNX09AU10G, NNX12AO93G] FX The VERITAS Collaboration is grateful to Trevor Weekes for his seminal contributions and leadership in the field of VHE gamma-ray astrophysics, which made this study possible. The work of the VERITAS Collaboration is supported by grants from the US Department of Energy Office of Science, the US National Science Foundation, and the Smithsonian Institution, by NSERC in Canada, by Science Foundation Ireland (SFI 10/RFP/AST2748) and by the Science and Technology Facilities Council in the UK. We acknowledge the excellent work of the technical support staff at the Fred Lawrence Whipple Observatory and at the collaborating institutions in the construction and operation of the instrument.; We thank the Swift team for making these observations possible, the duty scientists, and science planners. The OVRO 40 m monitoring programme is supported in part by NASA grants NNX08AW31G and NNX11A043G, and NSF grants AST-0808050 and AST-1109911. The CRTS survey is supported by the US National Science Foundation under grants AST-0909182. This research has made use of data from the MOJAVE data base that is maintained by the MOJAVE team (Lister et al. 2009). Data from the Steward Observatory spectropolarimetric monitoring project were used. This programme is supported by Fermi Guest Investigator grants NNX08AW56G, NNX09AU10G, and NNX12AO93G. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. We thank F. Schinzel, S. Digel, P. Bruel, and the referee, Anthony M. Brown, for useful comments and suggestions. NR 88 TC 9 Z9 9 U1 1 U2 11 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JAN 21 PY 2015 VL 446 IS 3 BP 2456 EP 2467 DI 10.1093/mnras/stu2251 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CC3TG UT WOS:000350272300020 ER PT J AU Murphy, T Bell, ME Kaplan, DL Gaensler, BM Offringa, AR Lenc, E Hurley-Walker, N Bernardi, G Bowman, JD Briggs, F Cappallo, RJ Corey, BE Deshpande, AA Emrich, D Goeke, R Greenhill, LJ Hazelton, BJ Hewitt, JN Johnston-Hollitt, M Kasper, JC Kratzenberg, E Lonsdale, CJ Lynch, MJ McWhirter, SR Mitchell, DA Morales, MF Morgan, E Oberoi, D Ord, SM Prabu, T Rogers, AEE Roshi, DA Shankar, NU Srivani, KS Subrahmanyan, R Tingay, SJ Waterson, M Wayth, RB Webster, RL Whitney, AR Williams, A Williams, CL AF Murphy, Tara Bell, Martin E. Kaplan, David L. Gaensler, B. M. Offringa, Andre R. Lenc, Emil Hurley-Walker, Natasha Bernardi, G. Bowman, J. D. Briggs, F. Cappallo, R. J. Corey, B. E. Deshpande, A. A. Emrich, D. Goeke, R. Greenhill, L. J. Hazelton, B. J. Hewitt, J. N. Johnston-Hollitt, M. Kasper, J. C. Kratzenberg, E. Lonsdale, C. J. Lynch, M. J. McWhirter, S. R. Mitchell, D. A. Morales, M. F. Morgan, E. Oberoi, D. Ord, S. M. Prabu, T. Rogers, A. E. E. Roshi, D. A. Shankar, N. Udaya Srivani, K. S. Subrahmanyan, R. Tingay, S. J. Waterson, M. Wayth, R. B. Webster, R. L. Whitney, A. R. Williams, A. Williams, C. L. TI Limits on low-frequency radio emission from southern exoplanets with the Murchison Widefield Array SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE radio continuum: planetary systems ID EXTRASOLAR PLANETS; MAGNETIC-FIELDS; TAU BOOTIS; SKY SURVEY; SEARCH; MHZ; STARS; JUPITER AB We present the results of a survey for low-frequency radio emission from 17 known exoplanetary systems with the Murchison Widefield Array. This sample includes 13 systems that have not previously been targeted with radio observations. We detected no radio emission at 154 MHz, and put 3 sigma upper limits in the range 15.2-112.5 mJy on this emission. We also searched for circularly polarized emission and made no detections, obtaining 3 sigma upper limits in the range 3.4-49.9 mJy. These are comparable with the best low-frequency radio limits in the existing literature and translate to luminosity limits of between 1.2 x 10(14) and 1.4 x 10(17) W if the emission is assumed to be 100 per cent circularly polarized. These are the first results from a larger program to systematically search for exoplanetary emission with the MWA. C1 [Murphy, Tara; Bell, Martin E.; Gaensler, B. M.; Lenc, Emil] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia. [Murphy, Tara; Bell, Martin E.; Gaensler, B. M.; Offringa, Andre R.; Lenc, Emil; Briggs, F.; Mitchell, D. A.; Ord, S. M.; Subrahmanyan, R.] ARC Ctr Excellence All Sky Astrophys CAASTRO, Sydney, NSW, Australia. [Bell, Martin E.] CSIRO Astron & Space Sci, Marsfield, NSW 2122, Australia. [Kaplan, David L.] Univ Wisconsin, Dept Phys, Milwaukee, WI 53201 USA. [Offringa, Andre R.; Briggs, F.; Waterson, M.] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia. [Hurley-Walker, Natasha; Emrich, D.; Lynch, M. J.; Ord, S. M.; Tingay, S. J.; Waterson, M.; Wayth, R. B.; Williams, A.] Curtin Univ, Int Ctr Radio Astron Res, Bentley, WA 6102, Australia. [Bernardi, G.; Greenhill, L. J.; Kasper, J. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bernardi, G.] SKA SA, Cape Town, South Africa. [Bernardi, G.] Rhodes Univ, Dept Phys & Elect, ZA-6140 Grahamstown, South Africa. [Bowman, J. D.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Cappallo, R. J.; Corey, B. E.; Kratzenberg, E.; Lonsdale, C. J.; McWhirter, S. R.; Rogers, A. E. E.] MIT, Haystack Observ, Westford, MA 01886 USA. [Deshpande, A. A.; Prabu, T.; Shankar, N. Udaya; Srivani, K. S.; Subrahmanyan, R.] Raman Res Inst, Bangalore 560080, Karnataka, India. [Goeke, R.; Hewitt, J. N.; Morgan, E.; Williams, C. L.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Hazelton, B. J.; Morales, M. F.] Univ Washington, Dept Phys, Seattle, WA 98195 USA. [Johnston-Hollitt, M.] Victoria Univ Wellington, Sch Chem & Phys Sci, Wellington 6140, New Zealand. [Kasper, J. C.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Oberoi, D.] Tata Inst Fundamental Res, Natl Ctr Radio Astrophys, Pune 411007, Maharashtra, India. [Roshi, D. A.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Roshi, D. A.] Greenbank, Charlottesville, VA 22903 USA. [Webster, R. L.] Univ Melbourne, Sch Phys, Parkville, Vic 3010, Australia. RP Murphy, T (reprint author), Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia. EM tara@physics.usyd.edu.au RI Williams, Andrew/K-2931-2013; M, Manjunath/N-4000-2014; Deshpande, Avinash/D-4868-2012; Udayashankar , N/D-4901-2012; Wayth, Randall/B-2444-2013; Emrich, David/B-7002-2013; Subrahmanyan, Ravi/D-4889-2012; OI Williams, Andrew/0000-0001-9080-0105; M, Manjunath/0000-0001-8710-0730; Wayth, Randall/0000-0002-6995-4131; Emrich, David/0000-0002-4058-1837; Lenc, Emil/0000-0002-9994-1593 FU US National Science Foundation [AST-0457585, PHY-0835713, CAREER-0847753, AST-0908884]; Australian Research Council [LE0775621, LE0882938]; US Air Force Office of Scientific Research [FA9550-0510247]; Centre for All-sky Astrophysics (an Australian Research Council Centre of Excellence) [CE110001020]; Smithsonian Astrophysical Observatory; MIT School of Science; Raman Research Institute; Australian National University; Victoria University of Wellington from the New Zealand Ministry of Economic Development [MED-E1799]; Victoria University of Wellington from IBM Shared University Research Grant [MED-E1799]; Australian Federal government via the CSIRO; Australian Federal government via National Collaborative Research Infrastructure Strategy, Education Investment Fund; Australian Federal government via Australia India Strategic Research Fund; Astronomy Australia Limited; NVIDIA at Harvard University; International Centre for Radio Astronomy Research (ICRAR); Western Australian State government FX We thank Elaine Sadler for useful discussions and Aina Musaeva for assistance with the data reduction. This scientific work makes use of the Murchison Radio-astronomy Observatory, operated by Commonwealth Scientific and Industrial Research Organisation (CSIRO). We acknowledge the Wajarri Yamatji people as the traditional owners of the Observatory site. Support for the MWA comes from the US National Science Foundation (grants AST-0457585, PHY-0835713, CAREER-0847753 and AST-0908884), the Australian Research Council (LIEF grants LE0775621 and LE0882938), the US Air Force Office of Scientific Research (grant FA9550-0510247) and the Centre for All-sky Astrophysics (an Australian Research Council Centre of Excellence funded by grant CE110001020). Support is also provided by the Smithsonian Astrophysical Observatory, the MIT School of Science, the Raman Research Institute, the Australian National University, and the Victoria University of Wellington (via grant MED-E1799 from the New Zealand Ministry of Economic Development and an IBM Shared University Research Grant). The Australian Federal government provides additional support via the CSIRO, National Collaborative Research Infrastructure Strategy, Education Investment Fund, and the Australia India Strategic Research Fund, and Astronomy Australia Limited, under contract to Curtin University. We acknowledge the iVEC Petabyte Data Store, the Initiative in Innovative Computing and the CUDA Center for Excellence sponsored by NVIDIA at Harvard University, and the International Centre for Radio Astronomy Research (ICRAR), a Joint Venture of Curtin University and The University of Western Australia, funded by the Western Australian State government. NR 36 TC 7 Z9 7 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 JAN 21 PY 2015 VL 446 IS 3 BP 2560 EP 2565 DI 10.1093/mnras/stu2253 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CC3TG UT WOS:000350272300028 ER PT J AU Aliu, E Archer, A Aune, T Barnacka, A Behera, B Beilicke, M Benbow, W Berger, K Bird, R Buckley, JH Bugaev, V Byrum, K Cardenzana, JV Cerruti, M Chen, X Ciupik, L Connolly, MP Cui, W Dickinson, HJ Dumm, J Eisch, JD Errando, M Falcone, A Federici, S Feng, Q Finley, JP Fortin, P Fortson, L Furniss, A Galante, N Gillanders, GH Griffin, S Griffiths, ST Grube, J Gyuk, G Hakansson, N Hanna, D Holder, J Hughes, G Humensky, TB Johnson, CA Kaaret, P Kar, P Kertzman, M Khassen, Y Kieda, D Krawczynski, H Krennrich, F Kumar, S Lang, MJ Madhavan, A McArthur, S McCann, A Meagher, K Millis, J Moriarty, P Nieto, D de Bhroithe, AO Ong, RA Orr, M Otte, AN Park, N Perkins, JS Pohl, M Popkow, A Prokoph, H Pueschel, E Quinn, J Ragan, K Rajotte, J Reyes, LC Reynolds, PT Richards, GT Roache, E Sembroski, GH Shahinyan, K Staszak, D Telezhinsky, I Tucci, JV Tyler, J Varlotta, A Vassiliev, VV Wakely, SP Weinstein, A Welsing, R Wilhelm, A Williams, DA Zitzer, B AF Aliu, E. Archer, A. Aune, T. Barnacka, A. Behera, B. Beilicke, M. Benbow, W. Berger, K. Bird, R. Buckley, J. H. Bugaev, V. Byrum, K. Cardenzana, J. V. Cerruti, M. Chen, X. Ciupik, L. Connolly, M. P. Cui, W. Dickinson, H. J. Dumm, J. Eisch, J. D. Errando, M. Falcone, A. Federici, S. Feng, Q. Finley, J. P. Fortin, P. Fortson, L. Furniss, A. Galante, N. Gillanders, G. H. Griffin, S. Griffiths, S. T. Grube, J. Gyuk, G. Hakansson, N. Hanna, D. Holder, J. Hughes, G. Humensky, T. B. Johnson, C. A. Kaaret, P. Kar, P. Kertzman, M. Khassen, Y. Kieda, D. Krawczynski, H. Krennrich, F. Kumar, S. Lang, M. J. Madhavan, A. McArthur, S. McCann, A. Meagher, K. Millis, J. Moriarty, P. Nieto, D. de Bhroithe, A. O'Faolain Ong, R. A. Orr, M. Otte, A. N. Park, N. Perkins, J. S. Pohl, M. Popkow, A. Prokoph, H. Pueschel, E. Quinn, J. Ragan, K. Rajotte, J. Reyes, L. C. Reynolds, P. T. Richards, G. T. Roache, E. Sembroski, G. H. Shahinyan, K. Staszak, D. Telezhinsky, I. Tucci, J. V. Tyler, J. Varlotta, A. Vassiliev, V. V. Wakely, S. P. Weinstein, A. Welsing, R. Wilhelm, A. Williams, D. A. Zitzer, B. TI VERITAS OBSERVATIONS OF THE BL LAC OBJECT PG 1553+113 SO ASTROPHYSICAL JOURNAL LA English DT Article DE BL Lacertae objects: general ID EXTRAGALACTIC BACKGROUND LIGHT; LACERTAE OBJECTS; GAMMA-RAYS; OPTICAL SPECTROSCOPY; BLAZARS; TELESCOPE; RADIATION; SPECTRA; PG-1553+113; MODEL AB We present results from VERITAS observations of the BL Lac object PG 1553+113 spanning the years 2010, 2011, and 2012. The time-averaged spectrum, measured between 160 and 560 GeV, is well described by a power law with a spectral index of 4.33 +/- 0.09. The time-averaged integral flux above 200 GeV measured for this period was (1.69 +/- 0.06) x 10(-11) photons cm(-2) s(-1), corresponding to 6.9% of the Crab Nebula flux. We also present the combined gamma-ray spectrum from the Fermi Large Area Telescope and VERITAS covering an energy range from 100 MeV to 560 GeV. The data are well fit by a power law with an exponential cutoff at 101.9 +/- 3.2 GeV. The origin of the cutoff could be intrinsic to PG 1553+113 or be due to the gamma-ray opacity of our universe through pair production off the extragalactic background light (EBL). Given lower limits to the redshift of z > 0.395 based on optical/UV observations of PG 1553+113, the cutoff would be dominated by EBL absorption. Conversely, the small statistical uncertainties of the VERITAS energy spectrum have allowed us to provide a robust upper limit on the redshift of PG 1553+113 of z <= 0.62. A strongly elevated mean flux of (2.50 +/- 0.14) x10(-11) photons cm(-2) s(-1) (10.3% of the Crab Nebula flux) was observed during 2012, with the daily flux reaching as high as (4.44 +/- 0.71) x10(-11) photons cm(-2) s(-1) (18.3% of the Crab Nebula flux) on MJD 56048. The light curve measured during the 2012 observing season is marginally inconsistent with a steady flux, giving a chi(2) probability for a steady flux of 0.03%. C1 [Aliu, E.; Errando, M.] Columbia Univ Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA. [Archer, A.; Beilicke, M.; Buckley, J. H.; Bugaev, V.; Krawczynski, H.] Washington Univ, Dept Phys, St Louis, MO 63130 USA. [Aune, T.; Ong, R. A.; Popkow, A.; Vassiliev, V. V.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Barnacka, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Behera, B.; Chen, X.; Federici, S.; Hughes, G.; de Bhroithe, A. O'Faolain; Pohl, M.; Prokoph, H.; Telezhinsky, I.; Welsing, R.; Wilhelm, A.] DESY, D-15738 Zeuthen, Germany. [Benbow, W.; Cerruti, M.; Fortin, P.; Galante, N.; Roache, E.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. [Berger, K.; Holder, J.; Kumar, S.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Berger, K.; Holder, J.; Kumar, S.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Bird, R.; Khassen, Y.; Pueschel, E.; Quinn, J.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland. [Byrum, K.; Zitzer, B.] Argonne Natl Lab, Argonne, IL 60439 USA. [Cardenzana, J. V.; Dickinson, H. J.; Eisch, J. D.; Krennrich, F.; Madhavan, A.; Orr, M.; Weinstein, A.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Chen, X.; Federici, S.; Hakansson, N.; Pohl, M.; Telezhinsky, I.; Wilhelm, A.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany. [Ciupik, L.; Grube, J.; Gyuk, G.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA. [Connolly, M. P.; Gillanders, G. H.; Lang, M. J.; Moriarty, P.] Natl Univ Ireland Univ Coll Galway, Sch Phys, Galway, Ireland. [Cui, W.; Feng, Q.; Finley, J. P.; Sembroski, G. H.; Tucci, J. V.; Varlotta, A.] Purdue Univ, Dept Phys & Astron, W Lafayette, IN 47907 USA. [Dumm, J.; Fortson, L.; Shahinyan, K.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. [Falcone, A.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Furniss, A.; Johnson, C. A.; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Furniss, A.; Johnson, C. A.; Williams, D. A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA. [Griffin, S.; Hanna, D.; Ragan, K.; Rajotte, J.; Staszak, D.; Tyler, J.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Griffiths, S. T.; Kaaret, P.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Humensky, T. B.; Nieto, D.] Columbia Univ, Dept Phys, New York, NY 10027 USA. [Kar, P.; Kieda, D.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Kertzman, M.] Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA. [McArthur, S.; Park, N.; Wakely, S. P.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [McCann, A.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Meagher, K.; Otte, A. N.; Richards, G. T.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA. [Meagher, K.; Otte, A. N.; Richards, G. T.] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Millis, J.] Anderson Univ, Dept Phys, Anderson, IN 46012 USA. [Moriarty, P.] Galway Mayo Inst Technol, Dept Life & Phys Sci, Galway, Ireland. [Perkins, J. S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Reyes, L. C.] Calif Polytech State Univ San Luis Obispo, Dept Phys, San Luis Obispo, CA 94307 USA. [Reynolds, P. T.] Cork Inst Technol, Dept Appl Phys & Instrumentat, Cork, Ireland. RP Aliu, E (reprint author), Columbia Univ Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA. RI Khassen, Yerbol/I-3806-2015; Nieto, Daniel/J-7250-2015; OI Khassen, Yerbol/0000-0002-7296-3100; Nieto, Daniel/0000-0003-3343-0755; Pueschel, Elisa/0000-0002-0529-1973; Cui, Wei/0000-0002-6324-5772; Bird, Ralph/0000-0002-4596-8563 FU U.S. Department of Energy Office of Science; U.S. National Science Foundation; Smithsonian Institution; NSERC in Canada; Science Foundation Ireland [SFI 10/RFP/AST2748]; STFC in the U.K. FX The VERITAS Collaboration is grateful to Trevor Weekes for his seminal contributions and leadership in the field of VHE gamma-ray astrophysics, which made this study possible. This research is supported by grants from the U.S. Department of Energy Office of Science, the U.S. National Science Foundation and the Smithsonian Institution, by NSERC in Canada, by Science Foundation Ireland (SFI 10/RFP/AST2748) and by STFC in the U.K. We acknowledge the excellent work of the technical support staff at the Fred Lawrence Whipple Observatory and at the collaborating institutions in the construction and operation of the instrument. NR 37 TC 7 Z9 7 U1 1 U2 10 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2015 VL 799 IS 1 AR 7 DI 10.1088/0004-637X/799/1/7 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AZ4SY UT WOS:000348214500007 ER PT J AU Barnacka, A Geller, MJ Dell'Antonio, IP Benbow, W AF Barnacka, Anna Geller, Margaret J. Dell'Antonio, Ian P. Benbow, Wystan TI STRONGLY LENSED JETS, TIME DELAYS, AND THE VALUE OF H-0 SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmological parameters; galaxies: active; galaxies: jets; gravitational lensing: strong; quasars: general ID ACTIVE GALACTIC NUCLEI; HUBBLE-SPACE-TELESCOPE; EARLY-TYPE GALAXIES; GRAVITATIONAL LENS; M87 JET; QUASAR Q0957+561; LIGHT CURVES; ACS SURVEY; CONSTANT; COSMOGRAIL AB In principle, the most straightforward method of estimating the Hubble constant relies on time delays between mirage images of strongly lensed sources. It is a puzzle, then, that the values of H-0 obtained with this method span a range from similar to 50-100 km s(-1)Mpc(-1). Quasars monitored to measure these time delays are multi-component objects. The variability may arise from different components of the quasar or may even originate from a jet. Misidentifying a variable-emitting region in a jet with emission from the core region may introduce an error in the Hubble constant derived from a time delay. Here, we investigate the complex structure of the sources as the underlying physical explanation of the wide spread in values of the Hubble constant based on gravitational lensing. Our Monte Carlo simulations demonstrate that the derived value of the Hubble constant is very sensitive to the offset between the center of the emission and the center of the variable emitting region. Therefore, we propose using the value of H-0 known from other techniques to spatially resolve the origin of the variable emission once the time delay is measured. We particularly advocate this method for gamma-ray astronomy, where the angular resolution of detectors reaches approximately 0 degrees.1; lensed blazars offer the only route for identify the origin of gamma-ray flares. Large future samples of gravitationally lensed sources identified with Euclid, SKA, and LSST will enable a statistical determination of H-0. C1 [Barnacka, Anna; Geller, Margaret J.; Benbow, Wystan] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Barnacka, Anna] Jagiellonian Univ, Astron Observ, Krakow, Poland. [Dell'Antonio, Ian P.] Brown Univ, Dept Phys, Providence, RI 02912 USA. RP Barnacka, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-20, Cambridge, MA 02138 USA. EM abarnacka@cfa.harvard.edu FU Department of Energy Office of Science; NASA; Smithsonian Astrophysical Observatory; NCN [DEC-2011/01/M/ST9/01891]; Smithsonian Institution FX We thank the referee for valuable comments that prompted improvements in the manuscript. We thank Markus Bottcher, Dominique Sluse, Tommaso Treu, and Jabran Zahid for the valuable comments on the manuscript. A.B. is supported by the Department of Energy Office of Science, NASA, and the Smithsonian Astrophysical Observatory with financial support from the NCN grant DEC-2011/01/M/ST9/01891. M.J.G. is supported by the Smithsonian Institution. NR 96 TC 5 Z9 5 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2015 VL 799 IS 1 AR 48 DI 10.1088/0004-637X/799/1/48 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AZ4SY UT WOS:000348214500046 ER PT J AU Bernardi, G McQuinn, M Greenhill, LJ AF Bernardi, G. McQuinn, M. Greenhill, L. J. TI FOREGROUND MODEL AND ANTENNA CALIBRATION ERRORS IN THE MEASUREMENT OF THE SKY-AVERAGED lambda 21 cm SIGNAL AT z similar to 20 SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; dark ages, reionization, first stars; early universe; intergalactic medium; methods: observational; techniques: interferometric ID 21 CENTIMETER FLUCTUATIONS; MURCHISON WIDEFIELD ARRAY; PRE-REIONIZATION ERA; INTERGALACTIC MEDIUM; HIGH REDSHIFTS; DARK-MATTER; PARAMETER-ESTIMATION; COSMIC REIONIZATION; POWER SPECTRUM; 150 MHZ AB The most promising near-term observable of the cosmic dark age prior to widespread reionization (z similar to 15-200) is the sky-averaged lambda 21 cm background arising from hydrogen in the intergalactic medium. Though an individual antenna could in principle detect the line signature, data analysis must separate foregrounds that are orders of magnitude brighter than the lambda 21 cm background (but that are anticipated to vary monotonically and gradually with frequency, e.g., they are considered "spectrally smooth"). Using more physically motivated models for foregrounds than in previous studies, we show that the intrinsic spectral smoothness of the foregrounds is likely not a concern, and that data analysis for an ideal antenna should be able to detect the lambda 21 cm signal after subtracting a similar to fifth-order polynomial in log upsilon. However, we find that the foreground signal is corrupted by the angular and frequency-dependent response of a real antenna. The frequency dependence complicates modeling of foregrounds commonly based on the assumption of spectral smoothness. Our calculations focus on the Large-aperture Experiment to detect the Dark Age, which combines both radiometric and interferometric measurements. We show that statistical uncertainty remaining after fitting antenna gain patterns to interferometric measurements is not anticipated to compromise extraction of the lambda 21 cm signal for a range of cosmological models after fitting a seventh-order polynomial to radiometric data. Our results generalize to most efforts to measure the sky-averaged spectrum. C1 [Bernardi, G.] SKA SA, ZA-7405 Pinelands, South Africa. [Bernardi, G.] Rhodes Univ, Dept Phys & Elect, ZA-6140 Grahamstown, South Africa. [Bernardi, G.; Greenhill, L. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [McQuinn, M.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. RP Bernardi, G (reprint author), SKA SA, 3rd Floor,Pk Rd, ZA-7405 Pinelands, South Africa. EM gbernardi@ska.ac.za FU National Aeronautics and Space Administration; NSF [AST 1312724, AST-1106045, AST-1105949, AST-1106059, AST-1106054] FX G.B. is grateful to Ravi Subrahmanyan for useful discussions that initiated this work and to Oleg Smirnov for useful discussions on calibration. M.M. acknowledges support by the National Aeronautics and Space Administration through the Hubble Postdoctoral Fellowship and also from NSF grant AST 1312724. LEDA is supported by NSF grants AST-1106045, AST-1105949, AST-1106059, and AST-1106054. NR 75 TC 21 Z9 21 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 JAN 20 PY 2015 VL 799 IS 1 AR 90 DI 10.1088/0004-637X/799/1/90 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AZ4SY UT WOS:000348214500088 ER PT J AU Chan, CK Psaltis, D Ozel, F Narayan, R Sadowski, A AF Chan, Chi-Kwan Psaltis, Dimitrios Oezel, Feryal Narayan, Ramesh Sadowski, Aleksander TI THE POWER OF IMAGING: CONSTRAINING THE PLASMA PROPERTIES OF GRMHD SIMULATIONS USING EHT OBSERVATIONS OF Sgr A* SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; Galaxy: center; radiative transfer ID ADVECTION-DOMINATED ACCRETION; SUPERMASSIVE BLACK-HOLE; GALACTIC-CENTER; INFRARED-EMISSION; MHD SIMULATIONS; MILLIMETER-VLBI; DISK MODEL; SAGITTARIUS; SPECTRUM; FLARES AB Recent advances in general relativistic magnetohydrodynamic simulations have expanded and improved our understanding of the dynamics of black-hole accretion disks. However, current simulations do not capture the thermodynamics of electrons in the low density accreting plasma. This poses a significant challenge in predicting accretion flow images and spectra from first principles. Because of this, simplified emission models have often been used, with widely different configurations (e.g., disk-versus jet-dominated emission), and were able to account for the observed spectral properties of accreting black holes. Exploring the large parameter space introduced by such models, however, requires significant computational power that exceeds conventional computational facilities. In this paper, we use GRay, a fast graphics processing unit (GPU) based ray-tracing algorithm, on the GPU cluster El Gato, to compute images and spectra for a set of six general relativistic magnetohydrodynamic simulations with different magnetic field configurations and black-hole spins. We also employ two different parametric models for the plasma thermodynamics in each of the simulations. We show that, if only the spectral properties of Sgr A* are used, all 12 models tested here can fit the spectra equally well. However, when combined with the measurement of the image size of the emission using the Event Horizon Telescope, current observations rule out all models with strong funnel emission, because the funnels are typically very extended. Our study shows that images of accretion flows with horizon-scale resolution offer a powerful tool in understanding accretion flows around black holes and their thermodynamic properties. C1 [Chan, Chi-Kwan; Psaltis, Dimitrios; Oezel, Feryal] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Chan, Chi-Kwan; Psaltis, Dimitrios; Oezel, Feryal] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA. [Narayan, Ramesh] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. [Sadowski, Aleksander] MIT Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. RP Chan, CK (reprint author), Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA. EM chanc@email.arizona.edu OI Narayan, Ramesh/0000-0002-1919-2730 FU NSF [AST 1312034, 1228509]; NASA/NSF TCAN [NNX14AB48G, NNX14AB47G]; Miller Institute for Basic Research in Science at the University of California Berkeley FX This research is conducted at the University of Arizona and is supported by NSF grant AST 1312034. The Arizona team and R. N. acknowledge the support of NASA/NSF TCAN awards NNX14AB48G and NNX14AB47G, respectively. All ray tracing calculations were performed in the El Gato GPU cluster that is funded by NSF award 1228509. We thank Alexander Tchekhovskoy for providing the original derivations of the coordinate transformation used in the HARM simulations. We also thank Eliot Quataert and Jason Dexter for numerous discussions. F. O. thanks the Miller Institute for Basic Research in Science at the University of California Berkeley for their support and hospitality. NR 51 TC 28 Z9 27 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 JAN 20 PY 2015 VL 799 IS 1 AR 1 DI 10.1088/0004-637X/799/1/1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AZ4SY UT WOS:000348214500001 ER PT J AU Ellsworth-Bowers, TP Rosolowsky, E Glenn, J Ginsburg, A Evans, NJ Battersby, C Shirley, YL Svoboda, B AF Ellsworth-Bowers, Timothy P. Rosolowsky, Erik Glenn, Jason Ginsburg, Adam Evans, Neal J., II Battersby, Cara Shirley, Yancy L. Svoboda, Brian TI THE BOLOCAM GALACTIC PLANE SURVEY. XII. DISTANCE CATALOG EXPANSION USING KINEMATIC ISOLATION OF DENSE MOLECULAR CLOUD STRUCTURES WITH (CO)-C-13(1-0) SO ASTROPHYSICAL JOURNAL LA English DT Article DE Galaxy: kinematics and dynamics; Galaxy: structure; ISM: clouds; methods: data analysis; stars: formation; submillimeter: ISM ID STAR-FORMING REGIONS; DUST CONTINUUM SOURCES; INFRARED DARK CLOUDS; MILKY-WAY; OUTER GALAXY; TRIGONOMETRIC PARALLAXES; RING SURVEY; CO SURVEY; SPIRAL ARM; FUNDAMENTAL PARAMETERS AB We present an expanded distance catalog for 1710 molecular cloud structures identified in the Bolocam Galactic Plane Survey (BGPS) version 2, representing a nearly threefold increase over the previous BGPS distance catalog. We additionally present a new method for incorporating extant data sets into our Bayesian distance probability density function (DPDF) methodology. To augment the dense-gas tracers (e.g., HCO+ (3-2), NH3(1,1)) used to derive line-of-sight velocities for kinematic distances, we utilize the Galactic Ring Survey (GRS) (CO)-C-13(1-0) data to morphologically extract velocities for BGPS sources. The outline of a BGPS source is used to select a region of the GRS (CO)-C-13 data, along with a reference region to subtract enveloping diffuse emission, to produce a line profile of (CO)-C-13 matched to the BGPS source. For objects with a HCO+ (3-2) velocity, approximate to 95% of the new O-13C(1-0) velocities agree with that of the dense gas. A new prior DPDF for kinematic distance ambiguity (KDA) resolution, based on a validated formalism for associating molecular cloud structures with known objects from the literature, is presented. We demonstrate this prior using catalogs of masers with trigonometric parallaxes and Hii regions with robust KDA resolutions. The distance catalog presented here contains well-constrained distance estimates for 20% of BGPS V2 sources, with typical distance uncertainties less than or similar to 0.5 kpc. Approximately 75% of the well-constrained sources lie within 6 kpc of the Sun, concentrated in the Scutum-Centaurus arm. Galactocentric positions of objects additionally trace out portions of the Sagittarius, Perseus, and Outer arms in the first and second Galactic quadrants, and we also find evidence for significant regions of interarm dense gas. C1 [Ellsworth-Bowers, Timothy P.; Glenn, Jason] Univ Colorado, CASA, Boulder, CO 80309 USA. [Rosolowsky, Erik] Univ Alberta, Dept Phys, Edmonton, AB T6G 2E1, Canada. [Ginsburg, Adam] European So Observ, D-85748 Garching, Germany. [Evans, Neal J., II] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Battersby, Cara] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Shirley, Yancy L.; Svoboda, Brian] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. RP Ellsworth-Bowers, TP (reprint author), Univ Colorado, CASA, UCB 389, Boulder, CO 80309 USA. EM timothy.ellsworthbowers@colorado.edu OI Ginsburg, Adam/0000-0001-6431-9633 FU National Science Foundation through NSF [AST-1008577]; NSF [AST-0708403, AST-0540882, AST-0838261, AST-1109116, AST-9800334, AST-0098562, AST-0100793, AST-0228993, AST-0507657]; NSERC of Canada FX This work was supported by the National Science Foundation through NSF grant AST-1008577. The BGPS project was supported in part by NSF grant AST-0708403, and was performed at the Caltech Submillimeter Observatory (CSO), which was supported by NSF grants AST-0540882 and AST-0838261. The CSO was operated by Caltech under contract from the NSF. ER is supported by a Discovery Grant from NSERC of Canada. NJE is supported by NSF grant AST-1109116. This publication makes use of molecular line data from the Boston University-FCRAO Galactic Ring Survey (GRS). The GRS is a joint project of Boston University and Five College Radio Astronomy Observatory, funded by the NSF under grants AST-9800334, AST-0098562, AST-0100793, AST-0228993, & AST-0507657. NR 72 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 JAN 20 PY 2015 VL 799 IS 1 AR 29 DI 10.1088/0004-637X/799/1/29 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AZ4SY UT WOS:000348214500028 ER PT J AU Garay, G Mardones, D Contreras, Y Pineda, JE Servajean, E Guzman, AE AF Garay, Guido Mardones, Diego Contreras, Yanett Pineda, Jaime E. Servajean, Elise Guzman, Andres E. TI G305.136+0.068: A MASSIVE AND DENSE COLD CORE IN AN EARLY STAGE OF EVOLUTION SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; ISM: clouds; stars: formation; stars: massive ID PHYSICAL CONDITIONS; RADIATIVE-TRANSFER; FORMING REGIONS; STARLESS CORES; DUST CONTINUUM; ARRAY CAMERA; EMISSION; CS; PERFORMANCE; TELESCOPE AB We report molecular line observations, made with ASTE and SEST, and dust continuum observations at 0.87 mm, made with APEX, toward the cold dust core G305.136+0.068. The molecular observations show that the core is isolated and roughly circularly symmetric and imply that it has a mass of 1.1 x 10(3) M-circle dot. A simultaneous model fitting of the spectra observed in four transitions of CS, using a non-LTE radiative transfer code, indicates that the core is centrally condensed, with the density decreasing with radius as r(-1.8), and that the turbulent velocity increases toward the center. The dust observations also indicate that the core is highly centrally condensed and that the average column density is 1.1 g cm(-2), a value slightly above the theoretical threshold required for the formation of high-mass stars. A fit to the spectral energy distribution of the emission from the core indicates a dust temperature of 17 +/- 2 K, confirming that the core is cold. Spitzer images show that the core is seen in silhouette from 3.6 to 24.0 mu m and that it is surrounded by an envelope of emission, presumably tracing an externally excited photo-dissociated region. We found two embedded sources within a region of 20 '' centered at the peak of the core, one of which is young, has a luminosity of 66 L-circle dot, and is accreting mass with a high accretion rate of similar to 1 x 10(-4) M-circle dot yr(-1). We suggest that this object corresponds to the seed of a high-mass protostar still in the process of formation. The present observations support the hypothesis that G305.136+0.068 is a massive and dense cold core in an early stage of evolution, in which the formation of a high-mass star has just started. C1 [Garay, Guido; Mardones, Diego; Contreras, Yanett; Servajean, Elise; Guzman, Andres E.] Univ Chile, Dept Astron, Santiago, Chile. [Contreras, Yanett] CSIRO Astron & Space Sci, Epping, NSW 1710, Australia. [Pineda, Jaime E.] Swiss Fed Inst Technol, Inst Astron, CH-8093 Zurich, Switzerland. [Guzman, Andres E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Garay, G (reprint author), Univ Chile, Dept Astron, Casilla 36-D, Santiago, Chile. RI Mardones, Diego/I-5719-2016; Garay, Guido/H-8840-2013; OI Garay, Guido/0000-0003-1649-7958; Guzman, Andres/0000-0003-0990-8990; Pineda, Jaime/0000-0002-3972-1978; Contreras, Yanett/0000-0002-6388-3635 FU CONICYT [BASAL PFB-06]; European Community [229517]; Swiss National Science Foundation [CRSII2-141880]; NASA [NNX12AI55G, NNX10AD68G] FX G.G., Y.C., and D.M gratefully acknowledge support from CONICYT through project BASAL PFB-06. J.E.P. acknowledges funding from the European Community Seventh Framework Programme (/FP7/2007-2013/) under grant agreement No. 229517 and support by the Swiss National Science Foundation, project number CRSII2-141880. A.E.G. acknowledges support from NASA Grants NNX12AI55G and NNX10AD68G. This publication made use of the GLIMPSE-Spitzer and Hi-GAL-Herschel database. NR 32 TC 1 Z9 1 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2015 VL 799 IS 1 AR 75 DI 10.1088/0004-637X/799/1/75 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AZ4SY UT WOS:000348214500073 ER PT J AU Giguere, MJ Fischer, DA Payne, MJ Brewer, JM Johnson, JA Howard, AW Isaacson, HT AF Giguere, Matthew J. Fischer, Debra A. Payne, Matthew J. Brewer, John M. Johnson, John Asher Howard, Andrew W. Isaacson, Howard T. TI NEWLY DISCOVERED PLANETS ORBITING HD 5319, HD 11506, HD 75784 AND HD 10442 FROM THE N2K CONSORTIUM SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; stars: individual (HD 5319, HD 11506, HD 75784, HD 10442) ID SHORT-PERIOD PLANETS; EXTRASOLAR PLANETS; TRANSITING PLANET; HOT JUPITERS; HOST STARS; EXOPLANETARY SYSTEMS; DETERMINISTIC MODEL; RADIAL-VELOCITIES; MAGNETIC ACTIVITY; STELLAR ROTATION AB Initially designed to discover short-period planets, the N2K campaign has since evolved to discover new worlds at large separations from their host stars. Detecting such worlds will help determine the giant planet occurrence at semi-major axes beyond the ice line, where gas giants are thought to mostly form. Here we report four newly discovered gas giant planets (with minimum masses ranging from 0.4 to 2.1 M-Jup) orbiting stars monitored as part of the Next 2000 target stars (N2K) Doppler Survey program. Two of these planets orbit stars already known to host planets: HD 5319 and HD 11506. The remaining discoveries reside in previously unknown planetary systems: HD 10442 and HD 75784. The refined orbital period of the inner planet orbiting HD 5319 is 641 days. The newly discovered outer planet orbits in 886 days. The large masses combined with the proximity to a 4:3 mean motion resonance make this system a challenge to explain with current formation and migration theories. HD 11506 has one confirmed planet, and here we confirm a second. The outer planet has an orbital period of 1627.5 days, and the newly discovered inner planet orbits in 223.6 days. A planet has also been discovered orbiting HD 75784 with an orbital period of 341.7 days. There is evidence for a longer period signal; however, several more years of observations are needed to put tight constraints on the Keplerian parameters for the outer planet. Lastly, an additional planet has been detected orbiting HD 10442 with a period of 1043 days. C1 [Giguere, Matthew J.; Fischer, Debra A.; Brewer, John M.] Yale Univ, Dept Astron, New Haven, CT 06511 USA. [Payne, Matthew J.; Johnson, John Asher] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Howard, Andrew W.] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. [Isaacson, Howard T.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. RP Giguere, MJ (reprint author), Yale Univ, Dept Astron, 260 Whitney Ave, New Haven, CT 06511 USA. RI Howard, Andrew/D-4148-2015; OI Howard, Andrew/0000-0001-8638-0320; Brewer, John/0000-0002-9873-1471 FU NASA Headquarters under the NASA Earth and Space Science [NNX13AM15H]; NASA [NNX08AF42G]; W. M. Keck Foundation FX We thank the referee for useful comments and suggestions. We are grateful to Geoff Marcy for his longstanding contributions to this program and for helping with the observing and data reduction. We also thank Camille Avestruz, Ana Bonaca, Kristina Douglas, Aurelia Giguere, Haven Giguere, Nicole Larsen, Jack Moriarty, and Adele Plunkett for useful discussions. We gratefully acknowledge the dedication and support of the Keck Observatory staff, in particular Grant Hill and Scott Dahm for their support with HIRES and Greg Wirth, Bob Kibrick, Craig Henry and Andrew Stemmer for supporting remote observing. We thank the NASA and Yale Telescope assignment committees for generous allocations of telescope time. This work was supported by NASA Headquarters under the NASA Earth and Space Science Fellowship Program-Grant NNX13AM15H. Fischer acknowledges support from NASA grant NNX08AF42G and NASA Keck PI data analysis funds. This research has made use of the Extrasolar Planets Encyclopedia, available at exoplanet.eu, and the Exoplanet Orbit Database at exoplanets.org. This research has also made use of the SIMBAD database, operated at CDS, Strasbourg, France. Data presented herein were obtained at the W. M. Keck Observatory from telescope time allocated to the National Aeronautics and Space Administration through the agency's scientific partnership with the California Institute of Technology and the University of California. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. The authors extend thanks to those of native Hawaiian ancestry on whose sacred mountain of Mauna Kea we are privileged to be guests. Without their generous hospitality, the Keck observations presented herein would not have been possible. NR 82 TC 3 Z9 3 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2015 VL 799 IS 1 AR 89 DI 10.1088/0004-637X/799/1/89 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AZ4SY UT WOS:000348214500087 ER PT J AU Goicoechea, JR Chavarria, L Cernicharo, J Neufeld, DA Vavrek, R Bergin, EA Cuadrado, S Encrenaz, P Etxaluze, M Melnick, GJ Polehampton, E AF Goicoechea, Javier R. Chavarria, Luis Cernicharo, Jose Neufeld, David A. Vavrek, Roland Bergin, Edwin A. Cuadrado, Sara Encrenaz, Pierre Etxaluze, Mireya Melnick, Gary J. Polehampton, Edward TI HERSCHEL FAR-INFRARED SPECTRAL-MAPPING OF ORION BN/KL OUTFLOWS: SPATIAL DISTRIBUTION OF EXCITED CO, H2O, OH, O, AND C+ IN SHOCKED GAS SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared: ISM; ISM: jets and outflows; shock waves; stars: protostars ID FOURIER-TRANSFORM SPECTROMETER; INTERSTELLAR MOLECULAR CLOUDS; EXTRAORDINARY SOURCES HEXOS; STAR-FORMING REGIONS; WATER-VAPOR EMISSION; ISO-SWS OBSERVATIONS; LINE EMISSION; DISSOCIATIVE SHOCKS; TEMPORAL EVOLUTION; KL OUTFLOWS AB We present similar to 2; x 2' spectral-maps of Orion Becklin-Neugebauer/Kleinmann-Low (BN/KL) outflows taken with Herschel at similar to 12 '' resolution. For the first time in the far-IR domain, we spatially resolve the emission associated with the bright H-2 shocked regions "Peak 1" and "Peak 2" from that of the hot core and ambient cloud. We analyze the similar to 54-310 mu m spectra taken with the PACS and SPIRE spectrometers. More than 100 lines are detected, most of them rotationally excited lines of (CO)-C-12 (up to J = 48-47), H2O, OH, (CO)-C-13, and HCN. Peaks 1/2 are characterized by a very high L(CO)/L-FIR approximate to 5 x 10(-3) ratio and a plethora of far-IR H2O emission lines. The high-J CO and OH lines are a factor of approximate to 2 brighter toward Peak 1 whereas several excited H2O lines are less than or similar to 50% brighter toward Peak 2. Most of the CO column density arises from T-k similar to 200-500 K gas that we associate with low-velocity shocks that fail to sputter grain ice mantles and show a maximum gas-phase H2O/CO less than or similar to 10(-2) abundance ratio. In addition, the very excited CO (J > 35) and H2O lines reveal a hotter gas component (T-k similar to 2500 K) from faster (v(S) > 25 km s(-1)) shocks that are able to sputter the frozen-out H2O and lead to high H2O/CO greater than or similar to 1 abundance ratios. The H2O and OH luminosities cannot be reproduced by shock models that assume high (undepleted) abundances of atomic oxygen in the preshock gas and/or neglect the presence of UV radiation in the postshock gas. Although massive outflows are a common feature in other massive star-forming cores, Orion BN/KL seems more peculiar because of its higher molecular luminosities and strong outflows caused by a recent explosive event. C1 [Goicoechea, Javier R.; Cernicharo, Jose; Cuadrado, Sara; Etxaluze, Mireya] CSIC, ICMM, E-28049 Madrid, Spain. [Goicoechea, Javier R.; Chavarria, Luis; Cernicharo, Jose; Cuadrado, Sara; Etxaluze, Mireya] CSIC INTA, Ctr Astrobiol, E-28850 Madrid, Spain. [Chavarria, Luis] Univ Chile, CONICYT, Santiago, Chile. [Neufeld, David A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Vavrek, Roland] ESA ESAC, Herschel Sci Ctr, E-28691 Madrid, Spain. [Bergin, Edwin A.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Encrenaz, Pierre] Ecole Normale Super, Observ Paris, CNRS, LERMA,UMR 8112, F-75014 Paris, France. [Melnick, Gary J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Polehampton, Edward] Rutherford Appleton Lab, RAL Space, Didcot OX11 0QX, Oxon, England. [Polehampton, Edward] Univ Lethbridge, Inst Space Imaging Sci, Lethbridge, AB T1J 1B1, Canada. RP Goicoechea, JR (reprint author), CSIC, ICMM, Sor Juana Ines de la Cruz 3, E-28049 Madrid, Spain. EM jr.goicoechea@icmm.csic.es FU Spanish MINECO [CSD2009-00038, AYA2009-07304, AYA2012-32032]; Ramon y Cajal contract FX We thank the entire HEXOS GT-KP team for many useful and vivid discussions in the last years. We thank Spanish MINECO for funding support under grants CSD2009-00038, AYA2009-07304, and AYA2012-32032. J.R.G. was supported by a Ramon y Cajal contract. NR 97 TC 15 Z9 15 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2015 VL 799 IS 1 AR 102 DI 10.1088/0004-637X/799/1/102 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AZ4SY UT WOS:000348214500100 ER PT J AU Hashimoto, J Tsukagoshi, T Brown, JM Dong, R Muto, T Zhu, Z Wisniewski, J Ohashi, N Kudo, T Kusakabe, N Abe, L Akiyama, E Brandner, W Brandt, T Carson, J Currie, T Egner, S Feldt, M Grady, CA Guyon, O Hayano, Y Hayashi, M Hayashi, S Henning, T Hodapp, K Ishii, M Iye, M Janson, M Kandori, R Knapp, G Kuzuhara, M Kwon, J Matsuo, T McElwain, MW Mayama, S Mede, K Miyama, S Morino, JI Moro-Martin, A Nishimura, T Pyo, TS Serabyn, G Suenaga, T Suto, H Suzuki, R Takahashi, Y Takami, M Takato, N Terada, H Thalmann, C Tomono, D Turner, EL Watanabe, M Yamada, T Takami, H Usuda, T Tamura, M AF Hashimoto, J. Tsukagoshi, T. Brown, J. M. Dong, R. Muto, T. Zhu, Z. Wisniewski, J. Ohashi, N. Kudo, T. Kusakabe, N. Abe, L. Akiyama, E. Brandner, W. Brandt, T. Carson, J. Currie, T. Egner, S. Feldt, M. Grady, C. A. Guyon, O. Hayano, Y. Hayashi, M. Hayashi, S. Henning, T. Hodapp, K. Ishii, M. Iye, M. Janson, M. Kandori, R. Knapp, G. Kuzuhara, M. Kwon, J. Matsuo, T. McElwain, M. W. Mayama, S. Mede, K. Miyama, S. Morino, J. -I. Moro-Martin, A. Nishimura, T. Pyo, T. -S. Serabyn, G. Suenaga, T. Suto, H. Suzuki, R. Takahashi, Y. Takami, M. Takato, N. Terada, H. Thalmann, C. Tomono, D. Turner, E. L. Watanabe, M. Yamada, T. Takami, H. Usuda, T. Tamura, M. TI THE STRUCTURE OF PRE-TRANSITIONAL PROTOPLANETARY DISKS. II. AZIMUTHAL ASYMMETRIES, DIFFERENT RADIAL DISTRIBUTIONS OF LARGE AND SMALL DUST GRAINS IN PDS 70 SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; polarization; protoplanetary disks; stars: individual (PDS 70); stars: pre-main sequence; submillimeter: general ID T-TAURI DISKS; SPECTRAL ENERGY-DISTRIBUTIONS; PLANET-FORMING REGIONS; YOUNG STELLAR OBJECTS; INDUCED GAP EDGES; TRANSITIONAL DISK; ACCRETION DISKS; GIANT PLANET; SAO 206462; CIRCUMSTELLAR DISKS AB The formation scenario of a gapped disk, i.e., transitional disk, and its asymmetry is still under debate. Proposed scenarios such as disk-planet interaction, photoevaporation, grain growth, anticyclonic vortex, eccentricity, and their combinations would result in different radial distributions of the gas and the small (sub-mu m size) and large (millimeter size) dust grains as well as asymmetric structures in a disk. Optical/near-infrared (NIR) imaging observations and (sub-)millimeter interferometry can trace small and large dust grains, respectively; therefore multi-wavelength observations could help elucidate the origin of complicated structures of a disk. Here we report Submillimeter Array observations of the dust continuum at 1.3 mm and (CO)-C-12 J = 2 -> 1 line emission of the pre-transitional protoplanetary disk around the solar-mass star PDS 70. PDS 70, a weak-lined T Tauri star, exhibits a gap in the scattered light from its disk with a radius of similar to 65 AU at NIR wavelengths. However, we found a larger gap in the disk with a radius of similar to 80 AU at 1.3 mm. Emission from all three disk components (the gas and the small and large dust grains) in images exhibits a deficit in brightness in the central region of the disk, in particular, the dust disk in small and large dust grains has asymmetric brightness. The contrast ratio of the flux density in the dust continuum between the peak position to the opposite side of the disk reaches 1.4. We suggest the asymmetries and different gap radii of the disk around PDS 70 are potentially formed by several (unseen) accreting planets inducing dust filtration. C1 [Hashimoto, J.; Wisniewski, J.] Univ Oklahoma, Dept Phys & Astron, Norman, OK 73019 USA. [Tsukagoshi, T.] Ibaraki Univ, Coll Sci, Mito, Ibaraki 3108512, Japan. [Brown, J. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Dong, R.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Muto, T.] Kogakuin Univ, Div Liberal Arts, Shinjuku Ku, Tokyo 1638677, Japan. [Zhu, Z.; Knapp, G.; Moro-Martin, A.; Turner, E. L.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Ohashi, N.; Kudo, T.; Egner, S.; Guyon, O.; Hayano, Y.; Hayashi, S.; Nishimura, T.; Pyo, T. -S.; Takato, N.; Terada, H.; Tomono, D.] Subaru Telescope, Hilo, HI 96720 USA. [Kusakabe, N.; Akiyama, E.; Hayashi, M.; Ishii, M.; Iye, M.; Kandori, R.; Morino, J. -I.; Suto, H.; Suzuki, R.; Takami, H.; Usuda, T.; Tamura, M.] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. [Abe, L.] Univ Nice Sophia Antipolis, Lab Hippolyte Fizeau, UMR6525, F-06108 Nice 02, France. [Brandner, W.; Carson, J.; Feldt, M.; Henning, T.; Janson, M.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Brandt, T.] Inst Adv Study, Dept Astrophys, Princeton, NJ 08540 USA. [Carson, J.] Coll Charleston, Dept Phys & Astron, Charleston, SC 29424 USA. [Currie, T.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON, Canada. [Grady, C. A.] Eureka Sci, Oakland, CA 96002 USA. [Grady, C. A.; McElwain, M. W.] NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA. [Hodapp, K.] Univ Hawaii, Hilo, HI 96720 USA. [Janson, M.] Queens Univ Belfast, Astrophys Res Ctr, Belfast, Antrim, North Ireland. [Kuzuhara, M.] Tokyo Inst Technol, Dept Earth & Planetary Sci, Meguro Ku, Tokyo 1528551, Japan. [Kwon, J.; Mede, K.; Tamura, M.] Univ Tokyo, Dept Astron, Bunkyo Ku, Tokyo 1130033, Japan. [Matsuo, T.] Kyoto Univ, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan. [Mayama, S.] Shonan Int Village, Grad Univ Adv Studies SOKENDAI, Hayama, Kanagawa 2400193, Japan. [Miyama, S.] Hiroshima Univ, Higashihiroshima 7398511, Japan. [Moro-Martin, A.] CAB CSIC INTA, Dept Astrophys, E-28850 Madrid, Spain. [Serabyn, G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Suenaga, T.; Takahashi, Y.] Grad Univ Adv Studies SOKENDAI, Dept Astron Sci, Mitaka, Tokyo 1818588, Japan. [Takami, M.] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Thalmann, C.] ETH, Inst Astron, CH-8093 Zurich, Switzerland. [Thalmann, C.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands. [Turner, E. L.] Univ Tokyo, Kavli Inst Phys & Math Universe, Kashiwa, Chiba 2278568, Japan. [Watanabe, M.] Hokkaido Univ, Dept Cosmosci, Sapporo, Hokkaido 0600810, Japan. [Yamada, T.] Tohoku Univ, Astron Inst, Aoba Ku, Sendai, Miyagi 9808578, Japan. RP Hashimoto, J (reprint author), Univ Oklahoma, Dept Phys & Astron, 440 West Brooks St, Norman, OK 73019 USA. EM jun.hashimoto@ou.edu RI MIYAMA, Shoken/A-3598-2015; Watanabe, Makoto/E-3667-2016 OI Watanabe, Makoto/0000-0002-3656-4081 FU MEXT Japan; Mitsubishi Foundation; U.S. National Science Foundation [1009203, 1009314]; [25-8826] FX We are grateful to an anonymous referee for providing useful comments leading to an improved paper. We appreciate support from the SMA staff. This work is partly supported by a Grant-in-Aid for Science Research in a Priority Area from MEXT Japan, by the Mitsubishi Foundation, and by the U.S. National Science Foundation under Award Nos. 1009203 and 1009314. This work is partially supported by Grant-in-Aid for JSPS Fellows (No. 25-8826). NR 94 TC 7 Z9 7 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2015 VL 799 IS 1 AR 43 DI 10.1088/0004-637X/799/1/43 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AZ4SY UT WOS:000348214500042 ER PT J AU Jiang, XJ Wang, Z Gu, QS Wang, JZ Zhang, ZY AF Jiang, Xue-Jian Wang, Zhong Gu, Qiusheng Wang, Junzhi Zhang, Zhi-Yu TI SUB-MILLIMETER TELESCOPE CO (2-1) OBSERVATIONS OF NEARBY STAR-FORMING GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: ISM; infrared: galaxies; ISM: molecules; radio lines: galaxies ID FAST ALPHA SURVEY; CO-TO-H-2 CONVERSION FACTOR; GAS DEPLETION TIME; IRAM LEGACY SURVEY; MOLECULAR GAS; MASSIVE GALAXIES; FORMATION EFFICIENCY; SCALING RELATIONS; SOURCE CATALOG; DISK GALAXIES AB We present CO J = 2-1 observations toward 32 nearby gas-rich star-forming galaxies selected from the ALFALFA and Wide-field Infrared Survey Explorer (WISE) catalogs, using the Sub-millimeter Telescope (SMT). Our sample is selected to be dominated by intermediate-M-* galaxies. The scaling relations between molecular gas, atomic gas, and galactic properties (stellar mass, NUV - r, and WISE color W3 - W2) are examined and discussed. Our results show the following. (1) In the galaxies with stellar mass M-* <= 10(10)M(circle dot), the Hi fraction (f(HI) = MHi/M-*) is significantly higher than that of more massive galaxies, while the H-2 gas fraction (f(H2) = M-H2 /M-*) remains nearly unchanged. (2) Compared to f(H2), f(HI) correlates better with both M-* and NUV - r. (3) A new parameter, WISE color W3 - W2 (12-4.6 mu m), is introduced, which is similar to NUV - r in tracing star formation activity, and we find that W3 - W2 has a tighter anti-correlation with log f(H2) than the anti-correlation of (NUV - r)-f(HI), (NUV - r)-f(H2), and (W3 - W2)-f(HI). This indicates that W3 - W2 can trace the H2 fraction in galaxies. For the gas ratio M-H2 /M-HI, only in the intermediate-M-* galaxies it appears to depend on M-* and NUV - r. We find a tight correlation between the molecular gas mass M-H2 and 12 mu m (W3) luminosities (L12 mu m), and the slope is close to unity (1.03 +/- 0.06) for the SMT sample. This correlation may reflect that the cold gas and dust are well mixed on a global galactic scale. Using the all-sky 12 mu m (W3) data available in WISE, this correlation can be used to estimate CO flux for molecular gas observations and can even predict H-2 mass for star-forming galaxies. C1 [Jiang, Xue-Jian; Gu, Qiusheng] Nanjing Univ, Sch Astron & Space Sci, Nanjing 210093, Jiangsu, Peoples R China. [Jiang, Xue-Jian; Wang, Zhong] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Jiang, Xue-Jian; Gu, Qiusheng] Nanjing Univ, Minist Educ, Key Lab Modern Astron & Astrophys, Nanjing 210093, Jiangsu, Peoples R China. [Jiang, Xue-Jian; Gu, Qiusheng] Collaborat Innovat Ctr Modern Astron & Space Expl, Nanjing 210093, Jiangsu, Peoples R China. [Wang, Junzhi] Chinese Acad Sci, Shanghai Astron Observ, Shanghai 200030, Peoples R China. [Zhang, Zhi-Yu] Royal Observ Edinburgh, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. [Zhang, Zhi-Yu] ESO, D-85748 Munich, Germany. RP Jiang, XJ (reprint author), Nanjing Univ, Sch Astron & Space Sci, Nanjing 210093, Jiangsu, Peoples R China. EM xjjiang@nju.edu.cn OI Jiang, Xue-Jian/0000-0002-8899-4673; Zhang, Zhiyu/0000-0002-7299-2876 FU Chinese Academy of Sciences (CAS) [XDB09000000]; National Natural Science Foundation of China [11273015, 11133001]; National Basic Research Program (973 program) [2013CB834905]; Specialized Research Fund for the Doctoral Program of Higher Education [20100091110009]; European Research Council (ERC) FX We thank the anonymous referee for careful review and valuable suggestions, the SMT staff for their help during the observations, Ran Wang for her help with the observation, and U. Lisenfeld for kindly making the Hi data available to us. X.J. acknowledges support for this work from the Strategic Priority Research Program "The Emergence of Cosmological Structures" of the Chinese Academy of Sciences (CAS), grant XDB09000000. This work is supported under the National Natural Science Foundation of China (grants 11273015 and 11133001), the National Basic Research Program (973 program No. 2013CB834905), and Specialized Research Fund for the Doctoral Program of Higher Education (20100091110009). Z.-Y.Z acknowledges support from the European Research Council (ERC) in the form of an Advanced Grant, COSMICISM. This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. The Arecibo Observatory is part of the National Astronomy and Ionosphere Center which is operated by Cornell University under a cooperative agreement with the National Science Foundation. Based on observations made with the NASA Galaxy Evolution Explorer (GALEX). GALEX is operated for NASA by the California Institute of Technology under NASA contract NAS5-98034. Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. The SDSS-III Web site is http://www.sdss3.org/. SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, University of Cambridge, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University. NR 48 TC 0 Z9 0 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2015 VL 799 IS 1 AR 92 DI 10.1088/0004-637X/799/1/92 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AZ4SY UT WOS:000348214500090 ER PT J AU Milisavljevic, D Margutti, R Parrent, JT Soderberg, AM Fesen, RA Mazzali, P Maeda, K Sanders, NE Cenko, SB Silverman, JM Filippenko, AV Kamble, A Chakraborti, S Drout, MR Kirshner, RP Pickering, TE Kawabata, K Hattori, T Hsiao, EY Stritzinger, MD Marion, GH Vinko, J Wheeler, JC AF Milisavljevic, D. Margutti, R. Parrent, J. T. Soderberg, A. M. Fesen, R. A. Mazzali, P. Maeda, K. Sanders, N. E. Cenko, S. B. Silverman, J. M. Filippenko, A. V. Kamble, A. Chakraborti, S. Drout, M. R. Kirshner, R. P. Pickering, T. E. Kawabata, K. Hattori, T. Hsiao, E. Y. Stritzinger, M. D. Marion, G. H. Vinko, J. Wheeler, J. C. TI THE BROAD-LINED Type Ic SN 2012ap AND THE NATURE OF RELATIVISTIC SUPERNOVAE LACKING A GAMMA-RAY BURST DETECTION SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma-ray burst: general; supernovae: general; supernovae: individual (SN 2012ap) ID CORE-COLLAPSE SUPERNOVAE; DIFFUSE INTERSTELLAR BANDS; SOUTHERN SPECTROPHOTOMETRIC STANDARDS; SWIFT ULTRAVIOLET/OPTICAL TELESCOPE; CASSIOPEIA-A SUPERNOVA; LATE-TIME SPECTRA; H-II REGIONS; STRIPPED-ENVELOPE; IB SUPERNOVAE; LIGHT CURVES AB We present ultraviolet, optical, and near-infrared observations of SN 2012ap, a broad-lined Type Ic supernova in the galaxy NGC 1729 that produced a relativistic and rapidly decelerating outflow without a gamma-ray burst signature. Photometry and spectroscopy follow the flux evolution from -13 to +272 days past the B-band maximum of -17.4 +/- 0.5mag. The spectra are dominated by Fe II, OI, and Ca II absorption lines at ejecta velocities of nu approximate to 20,000 km s(-1) that change slowly over time. Other spectral absorption lines are consistent with contributions from photospheric He I, and hydrogen may also be present at higher velocities (nu greater than or similar to 27,000 km s(-1)). We use these observations to estimate explosion properties and derive a total ejecta mass of similar to 2.7 M-circle dot, a kinetic energy of similar to 1.0 x 10(52) erg, and a Ni-56 mass of 0.1-0.2 M-circle dot. Nebular spectra (t > 200 days) exhibit an asymmetric double-peaked [O I] lambda lambda 6300, 6364 emission profile that we associate with absorption in the supernova interior, although toroidal ejecta geometry is an alternative explanation. SN 2012ap joins SN2009bb as another exceptional supernova that shows evidence for a central engine (e. g., black hole accretion or magnetar) capable of launching a non-negligible portion of ejecta to relativistic velocities without a coincident gamma-ray burst detection. Defining attributes of their progenitor systems may be related to notable observed properties including environmental metallicities of Z greater than or similar to Z(circle dot), moderate to high levels of host galaxy extinction (E(B - V) > 0.4mag), detection of high-velocity helium at early epochs, and a high relative flux ratio of [Ca II]/[O I] > 1 at nebular epochs. These events support the notion that jet activity at various energy scales may be present in a wide range of supernovae. C1 [Milisavljevic, D.; Margutti, R.; Parrent, J. T.; Soderberg, A. M.; Sanders, N. E.; Kamble, A.; Chakraborti, S.; Drout, M. R.; Kirshner, R. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Fesen, R. A.] Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA. [Mazzali, P.] Liverpool John Moores Univ, Astrophys Res Inst, Liverpool L3 5RF, Merseyside, England. [Mazzali, P.] Max Planck Inst Astrophys, D-85748 Garching, Germany. [Mazzali, P.] Osserv Astron Padova, INAF, I-35122 Padua, Italy. [Maeda, K.] Kyoto Univ, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan. [Maeda, K.] Univ Tokyo, Todai Inst Adv Study, Kavli Inst Phys & Math Universe WPI, Kashiwa, Chiba 2778583, Japan. [Cenko, S. B.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Cenko, S. B.; Filippenko, A. V.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Silverman, J. M.; Marion, G. H.; Vinko, J.; Wheeler, J. C.] Univ Texas Austin, Austin, TX 78712 USA. [Pickering, T. E.] Southern African Large Telescope, ZA-7935 Cape Town, South Africa. [Pickering, T. E.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Kawabata, K.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan. [Hattori, T.] Natl Inst Nat Sci, Natl Astron Observ Japan, Subaru Telescope, Hilo, HI 96720 USA. [Hsiao, E. Y.] Las Campanas Observ, Carnegie Observ, Colina El Pino, Chile. [Hsiao, E. Y.; Stritzinger, M. D.] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark. [Vinko, J.] Univ Szeged, Dept Opt & Quantum Elect, H-6720 Szeged, Hungary. RP Milisavljevic, D (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM dmilisav@cfa.harvard.edu OI stritzinger, maximilian/0000-0002-5571-1833 FU W.M. Keck Foundation; David and Lucile Packard Foundation; NSF Astronomy and Astrophysics Postdoctoral Fellowship [AST-1302771]; NSF [AST-1211196, AST-1109801, AST-1211916, AST-1008343, PHYS-1066293]; Richard and Rhoda Goldman Fund; Christopher R. Redlich Fund; TABASGO Foundation; World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan; Hungarian OTKA [NN-107637]; Danish Agency for Science and Technology and Innovation; [23740141]; [26800100] FX We thank an anonymous referee for helpful suggestions. Many of the observations reported in this paper were obtained with the Southern African Large Telescope. Additional 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. Some observations also came from the MMT Observatory, a joint facility of the Smithsonian Institution and the University of Arizona, as well as the 6.5 m Magellan Telescopes located at Las Campanas Observatory, Chile. Support was provided by the David and Lucile Packard Foundation Fellowship for Science and Engineering awarded to A.M.S. J.M.S. is supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-1302771. T.E.P. thanks the National Research Foundation of South Africa. R.P.K. and J.C.W. are grateful for NSF grants AST-1211196 and AST-1109801, respectively. A.V.F. and S.B.C. acknowledge generous support from Gary and Cynthia Bengier, the Richard and Rhoda Goldman Fund, the Christopher R. Redlich Fund, the TABASGO Foundation, and NSF grant AST-1211916. K.M. acknowledges financial support by Grant-in-Aid for Scientific Research for Young Scientists (23740141, 26800100). The work by K.M. is partly supported by World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan. J.V. is supported by Hungarian OTKA grant NN-107637. M.D.S. and E.Y.H. gratefully acknowledge generous support provided by the Danish Agency for Science and Technology and Innovation realized through a Sapere Aude Level 2 grant. E.Y.H. also acknowledges support from NSF grant AST-1008343. D. Sahu and G. Pignata kindly provided archival spectra of SN 2007ru and SN 2009bb, respectively. This paper made extensive use of the SUSPECT database (www.nhn.ou.edu/similar to suspect/) and the Weizmann interactive supernova data repository (www.weizmann.ac.il/astrophysics/wiserep). This work was supported in part by NSF grant No. PHYS-1066293 and the hospitality of the Aspen Center for Physics. NR 185 TC 9 Z9 9 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2015 VL 799 IS 1 AR 51 DI 10.1088/0004-637X/799/1/51 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AZ4SY UT WOS:000348214500049 ER PT J AU Price, EM Rogers, LA Johnson, JA Dawson, RI AF Price, Ellen M. Rogers, Leslie A. Johnson, John Asher Dawson, Rebekah I. TI HOW LOW CAN YOU GO? THE PHOTOECCENTRIC EFFECT FOR PLANETS OF VARIOUS SIZES SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; techniques: photometric ID TRANSITING EXTRASOLAR PLANETS; ORBITAL ECCENTRICITIES; LIGHT CURVES; GIANT PLANETS; M-DWARF; PARAMETERS; STELLAR; CANDIDATES; EXOPLANET; SYSTEM AB It is well-known that the light curve of a transiting planet contains information about the planet's orbital period and size relative to the host star. More recently, it has been demonstrated that a tight constraint on an individual planet's eccentricity can sometimes be derived from the light curve via the "photoeccentric effect," the effect of a planet's eccentricity on the shape and duration of its light curve. This has only been studied for large planets and high signal-to-noise scenarios, raising the question of how well it can be measured for smaller planets or low signal-to-noise cases. We explore the limits of the photoeccentric effect over a wide range of planet parameters. The method hinges upon measuring g directly from the light curve, where g is the ratio of the planet's speed (projected on the plane of the sky) during transit to the speed expected for a circular orbit. We find that when the signal-to-noise in the measurement of g is <10, the ability to measure eccentricity with the photoeccentric effect decreases. We develop a "rule of thumb" that for per-point relative photometric uncertainties sigma = {10(-3), 10(-4), 10(-5)}, the critical values of the planet-star radius ratio are R-p/R-star approximate to {0.1, 0.05, 0.03} for Kepler-like 30 minute integration times. We demonstrate how to predict the best-case uncertainty in eccentricity that can be found with the photoeccentric effect for any light curve. This clears the path to study eccentricities of individual planets of various sizes in the Kepler sample and future transit surveys. C1 [Price, Ellen M.] CALTECH, Pasadena, CA 91125 USA. [Rogers, Leslie A.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Rogers, Leslie A.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Johnson, John Asher] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Dawson, Rebekah I.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. RP Price, EM (reprint author), CALTECH, 1200 East Calif Blvd, Pasadena, CA 91125 USA. FU Carolyn Ash SURF Fellowship; NASA through Hubble Fellowship - Space Telescope Science Institute [HF-51313.01]; NASA [NAS 5-26555]; Alfred P. Sloan foundation; David & Lucile Packard foundation; Miller Institute for Basic Research in Science at University of California, Berkeley FX We thank A. Pal and H. Knutson for use of their photometry data. E.M.P. acknowledges funding provided by Shirley and Carl Larson for her 2013 Carolyn Ash SURF Fellowship. L.A.R. acknowledges support provided by NASA through Hubble Fellowship grant HF-51313.01 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. J.A.J. is grateful for the generous grant support provided by the Alfred P. Sloan and David & Lucile Packard foundations. R.I.D. gratefully acknowledges support by the Miller Institute for Basic Research in Science at University of California, Berkeley. NR 40 TC 3 Z9 3 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 JAN 20 PY 2015 VL 799 IS 1 AR 17 DI 10.1088/0004-637X/799/1/17 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AZ4SY UT WOS:000348214500016 ER PT J AU Qi, CH Hogerheijde, MR Jewitt, D Gurwell, MA Wilner, DJ AF Qi, Chunhua Hogerheijde, Michiel R. Jewitt, David Gurwell, Mark A. Wilner, David J. TI PECULIAR NEAR-NUCLEUS OUTGASSING OF COMET 17P/HOLMES DURING ITS 2007 OUTBURST SO ASTROPHYSICAL JOURNAL LA English DT Article DE comets: general; comets: individual (17P/Holmes); radio lines: planetary systems; submillimeter: planetary systems; techniques: interferometric ID CHEMICAL-COMPOSITION; HALE-BOPP; PHOTOMETRY; RATES AB We present high angular resolution Submillimeter Array observations of the outbursting Jupiter family comet 17P/Holmes on 2007 October 26-29, achieving a spatial resolution of 2 ''.5, or similar to 3000 km at the comet distance. The observations resulted in detections of the rotational lines CO 3-2, HCN 4-3, (HCN)-C-13 4-3, CS 7-6, H2CO 3(1,2)-2(1,1), H2S 2(2,0)-2(1,1), and multiple CH3OH lines, along with the associated dust continuum at 221 and 349 GHz. The continuum has a spectral index of 2.7 +/- 0.3, slightly steeper than blackbody emission from large dust particles. From the imaging data, we identify two components in the molecular emission. One component is characterized by a relatively broad line width (similar to 1 km s(-1) FWHM) exhibiting a symmetric outgassing pattern with respect to the nucleus position. The second component has a narrower line width (<0.5 km s(-1) FWHM) with the line center redshifted by 0.1-0.2 km s-1 (cometocentric frame), and shows a velocity shift across the nucleus position with the position angle gradually changing from 66 degrees to 30 degrees within the four days of observations. We determine distinctly different CO/HCN ratios for each of the components. For the broad-line component we find CO/HCN < 7, while in the narrow-line component, CO/HCN = 40 +/- 5. We hypothesize that the narrow-line component originates from the ice grain halo found in near-nucleus photometry, believed to be created by sublimating recently released ice grains around the nucleus during the outburst. In this interpretation, the high CO/HCN ratio of this component reflects the more pristine volatile composition of nucleus material released in the outburst. C1 [Qi, Chunhua; Gurwell, Mark A.; Wilner, David J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hogerheijde, Michiel R.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Jewitt, David] Univ Calif Los Angeles, Dept Earth Planetary & Space Sci, Los Angeles, CA 90095 USA. [Jewitt, David] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. RP Qi, CH (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 42, Cambridge, MA 02138 USA. EM cqi@cfa.harvard.edu FU Smithsonian Institution; Academia Sinica; NASA FX The SMA is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. We thank SMA Director Raymond Blundell for quick allocation of the DDT time for the above observations and the SMA staff, especially Ken (Taco) Young and Nimesh Patel, for observational supports. D.J. acknowledges support from NASA's Origins program. NR 26 TC 1 Z9 1 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 20 PY 2015 VL 799 IS 1 AR 110 DI 10.1088/0004-637X/799/1/110 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AZ4SY UT WOS:000348214500108 ER PT J AU Tozzi, P Santos, JS Jee, MJ Fassbender, R Rosati, P Nastasi, A Forman, W Sartoris, B Borgani, S Boehringer, H Altieri, B Pratt, GW Nonino, M Jones, C AF Tozzi, P. Santos, J. S. Jee, M. J. Fassbender, R. Rosati, P. Nastasi, A. Forman, W. Sartoris, B. Borgani, S. Boehringer, H. Altieri, B. Pratt, G. W. Nonino, M. Jones, C. TI CHANDRA DEEP OBSERVATION OF XDCP J0044.0-2033, A MASSIVE GALAXY CLUSTER AT z > 1.5 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: intracluster medium; galaxies: individual (XDCP J0044.0-2033); large-scale structure of universe; X-rays: galaxies: clusters ID HUBBLE-SPACE-TELESCOPE; X-RAY-PROPERTIES; SOUTH-POLE TELESCOPE; WEAK-LENSING MASSES; ACT-CL J0102-4915; SIMILAR-TO 1; SCALING RELATIONS; DARK-MATTER; XMM-NEWTON; HIGH-REDSHIFT AB We report the analysis of the Chandra observation of XDCP J0044.0-2033, a massive, distant (z = 1.579) galaxy cluster discovered in the XDCP survey. The total exposure time of 380 ks with Chandra ACIS-S provides the deepest X-ray observation currently achieved on a massive, high-redshift cluster. Extended emission from the intra clustermedium (ICM) is detected at a very high significance level (S/N similar to 20) on a circular region with a 44 '' radius, corresponding to R-ext = 375 kpc at the cluster redshift. We perform an X-ray spectral fit of the ICM emission modeling the spectrum with a single-temperature thermal mekal model. Our analysis provides a global temperature kT = 6.7+(+1.3)(-0.9) keV, and a iron abundance Z(Fe) = 0.41(-0.26)(+0.29)Z(Fe circle dot) (error bars correspond to 1 sigma). We fit the background-subtracted surface brightness profile with a single beta-model out to 44 '', finding a rather flat profile with no hints of a cool core. We derive the deprojected electron density profile and compute the ICM mass within the extraction radius R-ext = 375 kpc to beM(ICM)(r < R-ext) = (1.48 +/- 0.20) x10(13)M(circle dot). Under the assumption of hydrostatic equilibrium and assuming isothermality within R-ext, the total mass is M-2500 = 1.23(-0.27)(+0.46) x 10(14)M(circle dot) for R-2500 = 240(-20)(+30) kpc. Extrapolating the profile at radii larger than the extraction radius R-ext we find M500 = 3.2(-0.6)(+0.9) x 10(14)M(circle dot) for R-500 = 562(-37)(+50) kpc. This analysis establishes the existence of virialized, massive galaxy clusters at redshift z similar to 1.6, paving the way to the investigation of the progenitors of the most massive clusters today. Given its mass and the XDCP survey volume, XDCP J0044.0-2033 does not create significant tension with the WMAP-7.CDM cosmology. C1 [Tozzi, P.; Santos, J. S.; Rosati, P.] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. [Jee, M. J.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Fassbender, R.] INAF Osservatorio Astron Roma OAR, I-00040 Monte Porzio Catone, Italy. [Rosati, P.] Univ Ferrara, I-44121 Ferrara, Italy. [Nastasi, A.] Univ Paris 11, CNRS, Ist Astrophys Spatiale, F-91405 Orsay, France. [Forman, W.; Jones, C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Sartoris, B.; Borgani, S.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy. [Borgani, S.; Nonino, M.] INAF Osservatorio Astron Trieste, I-34143 Trieste, Italy. [Boehringer, H.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Altieri, B.] European Space Agcy, ESAC, E-28691 Madrid, Spain. [Pratt, G. W.] CEA Saclay, Serv Astrophys, F-91191 Gif Sur Yvette, France. RP Tozzi, P (reprint author), INAF Osservatorio Astrofis Arcetri, Largo E Fermi 5, I-50125 Florence, Italy. OI Nonino, Mario/0000-0001-6342-9662; Tozzi, Paolo/0000-0003-3096-9966 FU PRIN MIUR; DFG; Munich Excellence Cluster 'Structure and Evolution of the Universe"; Chandra Program [14800360]; European Union [267251]; [PRIN INAF 2012] FX We acknowledge financial contribution from contract PRIN INAF 2012 ("A unique data set to address the most compelling open questions about X-ray galaxy clusters"), and PRIN MIUR 2009 ("Tracing the growth of structures in the Universe"). H.B. acknowledges support from the DFG Transregio program "Dark Universe" and the Munich Excellence Cluster 'Structure and Evolution of the Universe". This work was carried out with Chandra Program 14800360 obtained in AO14. J.S.S. acknowledges funding from the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement number 267251 Astronomy Fellowships in Italy (AstroFIt). We acknowledge the hospitality of Villa Il Gioiello (Arcetri, Florence), which is part of the agreement regarding the Colle di Galileo, where some of the results presented here were discussed. Finally, we thank the referee, Pasquale Mazzotta, for his careful and critical reading of this manuscript. NR 99 TC 11 Z9 11 U1 2 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2015 VL 799 IS 1 AR 93 DI 10.1088/0004-637X/799/1/93 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AZ4SY UT WOS:000348214500091 ER PT J AU Vikhlinin, A Kravtsov, A Forman, W Jones, C Markevitch, M Murray, SS Van Speybroeck, L AF Vikhlinin, A. Kravtsov, A. Forman, W. Jones, C. Markevitch, M. Murray, S. S. Van Speybroeck, L. TI CHANDRA SAMPLE OF NEARBY RELAXED GALAXY CLUSTERS: MASS, GAS FRACTION, AND MASS-TEMPERATURE RELATION (vol 640, pg 691, 2006) SO ASTROPHYSICAL JOURNAL LA English DT Correction C1 [Vikhlinin, A.; Forman, W.; Jones, C.; Markevitch, M.; Murray, S. S.; Van Speybroeck, L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Vikhlinin, A.; Markevitch, M.] Space Res Inst, Moscow, Russia. [Kravtsov, A.] Univ Chicago, Dept Astron & Astrophys, Kavli Inst Cosmol Phys, Enrico Fermi Inst, Chicago, IL 60637 USA. RP Vikhlinin, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM avikhlinin@cfa.harvard.edu NR 1 TC 0 Z9 0 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2015 VL 799 IS 1 AR 113 DI 10.1088/0004-637X/799/1/113 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AZ4SY UT WOS:000348214500111 ER PT J AU Barthel, M Flesch, R Ruhl, E McLaughlin, BM AF Barthel, Mathias Flesch, Roman Ruehl, Eckart McLaughlin, Brendan M. TI Photoionization of the 3s(2)3p(4) P-3 and the 3s(2)3p(4) D-1, S-1 states of sulfur: Experiment and theory SO PHYSICAL REVIEW A LA English DT Article ID R-MATRIX METHOD; CROSS-SECTION; VACUUM-ULTRAVIOLET; ATOMIC SULFUR; ENERGY-LEVELS; 193 NM; DES DISCHWEFELMONOXIDS; ELECTRON-SCATTERING; ABSORPTION-SPECTRUM; PLANETARY-NEBULAE AB Photoionization of neutral atomic sulfur in the ground and metastable states was studied experimentally at a photon energy resolution of 44 meV (full width at half maximum). Relative cross section measurements were recorded by using tunable vacuum ultraviolet radiation in the energy range 9-30 eV obtained from a laser-produced plasma and the atomic species were generated by photolysis of molecular precursors. Photoionization of this atom is characterized by multiple Rydberg series of autoionizing resonances superimposed on a direct photoionization continuum. A wealth of resonance features observed in the experimental spectra are spectroscopically assigned and their energies and quantum defects tabulated. The cross section measurements are comparedwith state-of-the-art theoretical cross section calculations obtained from the Dirac Coulomb R-matrix method. Resonance series in the spectra are identified and compared, indicating similar features in both the theoretical and experimental spectra. C1 [Barthel, Mathias; Flesch, Roman; Ruehl, Eckart] Free Univ Berlin, D-14195 Berlin, Germany. [McLaughlin, Brendan M.] Queens Univ Belfast, Sch Math & Phys, Ctr Theoret Atom Mol & Opt Phys, Belfast BT7 1NN, Antrim, North Ireland. [McLaughlin, Brendan M.] Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. RP Ruhl, E (reprint author), Free Univ Berlin, Takustr 3, D-14195 Berlin, Germany. EM ruehl@zedat.fu-berlin.de; b.mclaughlin@qub.ac.uk FU German Research Foundation (DFG) [RU 420/7-1]; U.S. National Science Foundation; Office of Science of the U.S. Department of Energy (DOE) [DE-AC02-05CH11231, DE-AC05-00OR22725] FX Financial support by the German Research Foundation (DFG) is gratefully acknowledged (Grant No. RU 420/7-1). B.M.M. acknowledges support by the U.S. National Science Foundation under the visitors program through a grant to ITAMP at the Harvard-Smithsonian Center for Astrophysics, Queen's University Belfast, through a visiting research fellowship (VRF), and the hospitality of E.R. and the Physikalische Chemie Department of the Freie Universitat of Berlin, during a recent research visit. This research used resources of the National Energy Research Scientific Computing Center, which is supported by the Office of Science of the U.S. Department of Energy (DOE) under Contract No. DE-AC02-05CH11231. The computational work was performed at the National Energy Research Scientific Computing Center in Oakland, CA, and at The High Performance Computing Center Stuttgart (HLRS) of the University of Stuttgart, Stuttgart, Germany. This research also used resources of the Oak Ridge Leadership Computing Facility at the Oak Ridge National Laboratory, which is supported by the Office of Science of the U.S. Department of Energy (DOE) under Contract No. DE-AC05-00OR22725. NR 83 TC 4 Z9 4 U1 2 U2 14 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2469-9926 EI 2469-9934 J9 PHYS REV A JI Phys. Rev. A PD JAN 20 PY 2015 VL 91 IS 1 AR 013406 DI 10.1103/PhysRevA.91.013406 PG 17 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA AZ6JH UT WOS:000348325700012 ER PT J AU Kipping, DM Huang, X Nesvorny, D Torres, G Buchhave, LA Bakos, GA Schmitt, AR AF Kipping, D. M. Huang, X. Nesvorny, D. Torres, G. Buchhave, L. A. Bakos, G. A. . Schmitt, A. R. TI THE POSSIBLE MOON OF KEPLER-90g IS A FALSE POSITIVE SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE planetary systems; planets and satellites: general; stars: individual (Kepler-90); techniques: photometric ID PLANET CANDIDATES; EFFICIENT; EXOMOONS; SYSTEM; HUNT AB The discovery of an exomoon would provide deep insights into planet formation and the habitability of planetary systems, with transiting examples being particularly sought after. Of the hundreds of Kepler planets now discovered, the seven-planet system Kepler-90 is unusual for exhibiting an unidentified transit-like signal in close proximity to one of the transits of the long-period gas-giant Kepler-90g, as noted by Cabrera et al. As part of the "Hunt for Exomoons with Kepler" project, we investigate this possible exomoon signal and find it passes all conventional photometric, dynamical, and centroid diagnostic tests. However, pixel-level light curves indicate that the moon-like signal occurs on nearly all of the target's pixels, which we confirm using a novel way of examining pixel-level data which we dub the "transit centroid." This test reveals that the possible exomoon to Kepler-90g is likely a false positive, perhaps due to a cosmic ray induced sudden pixel sensitivity dropout. This work highlights the extreme care required for seeking non-periodic low-amplitude transit signals, such as exomoons. C1 [Kipping, D. M.; Torres, G.; Buchhave, L. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Huang, X.; Bakos, G. A. .] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 05844 USA. [Nesvorny, D.] SW Res Inst, Dept Space Studies, Boulder, CO 80302 USA. [Buchhave, L. A.] Univ Copenhagen, Ctr Star & Planet Format, Nat Hist Museum Denmark, DK-1350 Copenhagen, Denmark. RP Kipping, DM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM dkipping@cfa.harvard.edu OI Schmitt, Allan/0000-0002-5034-0949; Buchhave, Lars A./0000-0003-1605-5666 FU CfA Menzel Fellowship; NSF [AST-1108686]; NASA [NNX12AH91H] FX This work made use of the Michael Dodds Computing Facility. D.M.K. is funded by the CfA Menzel Fellowship. G.A.B. acknowledges partial support from NSF grant AST-1108686 and NASA grant NNX12AH91H. NR 16 TC 3 Z9 3 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JAN 20 PY 2015 VL 799 IS 1 AR L14 DI 10.1088/2041-8205/799/1/L14 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AZ3RD UT WOS:000348143500014 ER PT J AU Williams, JT Carpenter, KE AF Williams, Jeffrey T. Carpenter, Kent E. TI A new fish species of the subfamily Serraninae (Perciformes, Serranidae) from the Philippines SO ZOOTAXA LA English DT Article DE Chelidoperca santosi; perchlet; Serranidae; Philippines; endemic ID MAXIMUM-LIKELIHOOD AB A new species of serranine fish is described from the Philippine Islands. A single specimen of a new species, Chelidoperca santosi, captured by fishermen working in Palawan waters was discovered in the public fish market in Iloilo City, Panay, Philippines. Two additional specimens of the new species, also from the Philippines, were subsequently discovered in the collections of the Museum Victoria, Australia. The new species is currently known only from the Philippines and is characterized by its distinctive coloration with a row of four small dark spots on the snout (two in front of each eye) and two dark spots on the chin (one on each side of the symphysis of the dentaries), a white anal fin with six large yellow spots separated by broad white interspaces and a narrow yellow distal border, caudal fin with narrow yellow bars and a yellowish distal margin and no dark spots, and a combination of meristic and morphological characters. C1 [Williams, Jeffrey T.] Natl Museum Nat Hist, Smithsonian Inst, Dept Vertebrate Zool, Div Fishes, Suitland, MD 20746 USA. [Carpenter, Kent E.] Old Dominion Univ, Dept Biol Sci, Norfolk, VA 23529 USA. RP Williams, JT (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Dept Vertebrate Zool, Div Fishes, 4210 Silver Hill Rd, Suitland, MD 20746 USA. EM williamsjt@si.edu; kcarpent@odu.edu FU BFAR-NFRDI; National Stock Assessment Program (NSAP); NSF [1257632] FX This study was part of an ongoing (2011 to the present) multi-partnered Memorandum of Agreement between the Department of Agriculture, Bureau of Fisheries and Aquatic Resources-National Fisheries Research and Development Institute (BFAR-NFRDI), Department of Agriculture, Philippines and the National Museum of Natural History of the Smithsonian Institution-Department of Vertebrate Zoology, USA (Title: Collaboration on the Inventory and DNA Barcoding of Commercial Fishes of the Philippines for Food Safety and Biodiversity) designed to obtain specimen-vouchered tissue samples of the commercial fishes found in the Philippines. We thank Jon Deeds, United States Food and Drug Administration, for supporting this food safety project. We are particularly grateful to BFAR-NFRDI for their collaboration and support in all aspects of the project. We thank Carole Baldwin (National Museum of Natural History) for her ongoing support of the project. Jerry Finan, Diane Pitassy, Erika Wilbur, Shirleen Smith, Kris Murphy, David Smith and Sandra Raredon of the Division of Fishes (National Museum of Natural History) assisted with preparations for the trip and processing specimens. Don Dumale of the National Museum of the Philippines and Diane Bray of the Museum Victoria in Australia provided curatorial assistance. Lee Weigt, Amy Driskell and Jeff Hunt of the Laboratories of Analytical Biology (Smithsonian Institution) provided support for and assistance with logistics and molecular analysis of samples throughout the project. Apollo Macro Lizano, Aaron Macaspac and Toby Potenciana worked tirelessly and diligently as our administrative and field assistants. Hilconida Calumpong assisted us in Dumaguete. Cleto 'Ting' Nanola assisted during the sampling at Mindanao and Mia Comeros helped with logistical support in Cebu. We especially thank BFAR Director Asis G. Perez and NFRDI Officer-in-Charge Melchor M. Tayamen for their full support of this project. Through the National Stock Assessment Program (NSAP), numerous BFAR-NFRDI staff at the National and Regional Offices have assisted with this project, facilitated collections of specimens and provided space to conduct lab work in Metro Manila and Provinces of the Philippines, including: Angel Encarnacion and staff of BFAR 2 (Cagayan), Aida Andayog and staff of BFAR 5 (Sorsogon), Drusila Bayate and staff of BFAR 6 (Iloilo), Prudencio Belga and staff of BFAR 7 (Cebu), John Albaladejo and staff of BFAR 8 (Tacloban), Nonita Cabacaba and the staff of NFRDI lab at Guiuan, Myrna Candelario, Elmar Villaflor and staff of BFAR 4B(Palawan), BFAR Fisheries Regulatory and Quarantine Division (Palawan), Glenda Cadigal of PCSDS (Palawan), Ludivina Labe and Edwyn Alesna of BFAR-FRQD (Quezon City) and the lab assistants of the NFRDI-Genetic Fingerprinting Laboratory (Quezon City). NSF project 1257632 provided some travel support for this effort. We thank Carole Baldwin for her constructive review of the manuscript. NR 15 TC 2 Z9 3 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 JAN 19 PY 2015 VL 3911 IS 2 BP 287 EP 293 PG 7 WC Zoology SC Zoology GA AZ1ED UT WOS:000347982100010 PM 25661613 ER PT J AU Gonzalez-Ferez, R Sadeghpour, HR Schmelcher, P AF Gonzalez-Ferez, Rosario Sadeghpour, H. R. Schmelcher, Peter TI Rotational hybridization, and control of alignment and orientation in triatomic ultralong-range Rydberg molecules SO NEW JOURNAL OF PHYSICS LA English DT Article DE Rydberg molecules; electric field; control of alignment and orientation; ultralong-range ID POLAR-MOLECULES; DIMERS; FIELDS; ATOMS AB We explore the electronic structure and rovibrational properties of an ultralong-range triatomic Rydberg molecule formed by a Rydberg atom and a ground state heteronuclear diatomic molecule. We focus here on the interaction of a Rb(n, l >= 3) Rydberg atom with a KRb(N=0) diatomic polar molecule. There is significant electronic hybridization with the Rb(n = 24, l >= 3) degenerate manifold. The polar diatomic molecule is allowed to rotate in the electric fields generated by the Rydberg electron and core as well as an external field. We investigate the metamorphosis of the Born-Oppenheimer potential curves, essential for the binding of the molecule, with varying electric field and analyze the resulting properties such as the vibrational structure and the alignment and orientation of the polar diatomic molecule. C1 [Gonzalez-Ferez, Rosario] Univ Granada, Inst Carlos Fis Teor & Computac 1, E-18071 Granada, Spain. [Gonzalez-Ferez, Rosario] Univ Granada, Dept Fis Atom Mol & Nucl, E-18071 Granada, Spain. [Gonzalez-Ferez, Rosario; Schmelcher, Peter] Hamburg Ctr Ultrafast Imaging, D-22761 Hamburg, Germany. [Sadeghpour, H. R.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. [Schmelcher, Peter] Univ Hamburg, Zentrum Opt Quantentechnol, D-22761 Hamburg, Germany. RP Gonzalez-Ferez, R (reprint author), Univ Granada, Inst Carlos Fis Teor & Computac 1, E-18071 Granada, Spain. EM rogonzal@ugr.es RI Gonzalez-Ferez, Rosario/A-2421-2009; Schmelcher, Peter/D-9592-2014 OI Gonzalez-Ferez, Rosario/0000-0002-8871-116X; Schmelcher, Peter/0000-0002-2637-0937 FU Deutsche Forschungsgemeinschaft; Spanish Ministry of Science (MICINN) [FIS2011-24540]; Andalusian research group [FQM-207]; Initial Training Network COHERENCE of the European Union; Spanish Ministry of Science (Junta de Andalucia) [P11-FQM-7276, FQM-4643] FX RGF gratefully acknowledges a Mildred Dresselhaus award from the excellence cluster 'The Hamburg Center for Ultrafast Imaging Structure, Dynamics and Control of Matter at the Atomic Scale' of the Deutsche Forschungsgemeinschaft and financial support by the Spanish Ministry of Science FIS2011-24540 (MICINN), grants P11-FQM-7276 and FQM-4643 (Junta de Andalucia), and by the Andalusian research group FQM-207. We also acknowledge financial support by the Initial Training Network COHERENCE of the European Union FP7 framework. HRS and PS acknowledge ITAMP at the Harvard-Smithsonian Center for Astrophysics for support. NR 30 TC 2 Z9 2 U1 1 U2 13 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 1367-2630 J9 NEW J PHYS JI New J. Phys. PD JAN 15 PY 2015 VL 17 AR 013021 DI 10.1088/1367-2630/17/1/013021 PG 13 WC Physics, Multidisciplinary SC Physics GA CA2TB UT WOS:000348759300006 ER PT J AU Ishida, Y McCallister, C Nikolaidis, N Tsangaras, K Helgen, KM Greenwood, AD Roca, AL AF Ishida, Yasuko McCallister, Chelsea Nikolaidis, Nikolas Tsangaras, Kyriakos Helgen, Kristofer M. Greenwood, Alex D. Roca, Alfred L. TI Sequence variation of koala retrovirus transmembrane protein p15E among koalas from different geographic regions SO VIROLOGY LA English DT Article DE Endogenous retroviruses; Epitopes; KoRV; Phascolarctos cinereus; Vaccines ID IMMUNODEFICIENCY-VIRUS TYPE-1; PORCINE ENDOGENOUS RETROVIRUS; PROXIMAL EXTERNAL REGION; FELINE LEUKEMIA-VIRUS; PHASCOLARCTOS-CINEREUS; NEUTRALIZING ANTIBODIES; ENVELOPE PROTEIN; REVERSE-TRANSCRIPTASE; CONSERVATION GENETICS; TOPOLOGY PREDICTION AB The koala retrovirus (KoRV), which is transitioning from an exogenous to an endogenous form, has been associated with high mortality in koalas. For other retroviruses, the envelope protein p15E has been considered a candidate for vaccine development. We therefore examined proviral sequence variation of KoRV p15E in a captive Queensland and three wild southern Australian koalas. We generated 163 sequences with intact open reading frames, which grouped into 39 distinct haplotypes. Sixteen distinct haplotypes comprising 139 of the sequences (85%) coded for the same polypeptide. Among the remaining 23 haplotypes, 22 were detected only once among the sequences, and each had 1 or 2 non-synonymous differences from the majority sequence. Several analyses suggested that p15E was under purifying selection. Important epitopes and domains were highly conserved across the p15E sequences and in previously reported exogenous KoRVs. Overall, these results support the potential use of p15E for KoRV vaccine development. (C) 2014 Elsevier Inc. All rights reserved. C1 [Ishida, Yasuko; Roca, Alfred L.] Univ Illinois, Dept Anim Sci, Urbana, IL 61801 USA. [McCallister, Chelsea; Nikolaidis, Nikolas] Calif State Univ Fullerton, Dept Biol Sci, Fullerton, CA 92834 USA. [McCallister, Chelsea; Nikolaidis, Nikolas] Calif State Univ Fullerton, Ctr Appl Biotechnol Studies, Fullerton, CA 92834 USA. [Tsangaras, Kyriakos; Greenwood, Alex D.] Leibniz Inst Zoo & Wildlife Res, D-10315 Berlin, Germany. [Helgen, Kristofer M.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. [Roca, Alfred L.] Univ Illinois, Inst Genom Biol, Urbana, IL 61801 USA. RP Ishida, Y (reprint author), Univ Illinois, Dept Anim Sci, 1207 W Gregory Dr, Urbana, IL 61801 USA. EM yishida@illinois.edu; chelseam@csu.fullerton.edu; nnikolaidis@exchange.fullerton.edu; ktsangaras@gmail.com; helgenk@si.edu; greenwood@izw-berlin.de; roca@illinois.edu FU National Institute of General Medical Sciences (NIGMS) [R01GM092706]; California State University, Fullerton; HHMI; Smithsonian Institution FX The project described was supported by Grant number R01GM092706 from the National Institute of General Medical Sciences (NIGMS). The content is solely the responsibility of the authors and does not necessarily represent the official views of the NIGMS or the National Institutes of Health. NN was supported by start-up funds and a state-mini grant from California State University, Fullerton. CM was supported by an HHMI scholarship. KMH was supported by the Smithsonian Institution. For modern koala samples, we thank M. Malasky, R. Hanson, S. O'Brien, M. Bush, J. Graves, W. Sherwin, N. Murray, and D. Wildt; and the Columbus Zoo and San Diego Zoo. NR 62 TC 6 Z9 6 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 0042-6822 J9 VIROLOGY JI Virology PD JAN 15 PY 2015 VL 475 BP 28 EP 36 DI 10.1016/j.virol.2014.10.036 PG 9 WC Virology SC Virology GA AZ4FE UT WOS:000348176500003 PM 25462343 ER PT J AU Howard, KT Alexander, CMO Schrader, DL Dyl, KA AF Howard, K. T. Alexander, C. M. O'D. Schrader, D. L. Dyl, K. A. TI Classification of hydrous meteorites (CR, CM and C2 ungrouped) by phyllosilicate fraction: PSD-XRD modal mineralogy and planetesimal environments SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article ID X-RAY-DIFFRACTION; PROGRESSIVE AQUEOUS ALTERATION; CARBONACEOUS CHONDRITE GROUP; FINE-GRAINED RIMS; COMPOSITIONAL CLASSIFICATION; MOSSBAUER-SPECTROSCOPY; CI CHONDRITES; PARENT BODIES; SOLAR-SYSTEM; TAGISH LAKE AB The relative differences in the degree of hydration should be reflected in any classification scheme for aqueously altered meteorites. Here we report the bulk mineralogies and degree of hydration in 37 different carbonaceous chondrites: Renazzo-like (CR), Mighei-like (CM), and ungrouped (type 2) samples. This is achieved by quantifying the modal abundances of all major (phases present in abundances >1 wt.%) minerals using Position Sensitive Detector X-ray Diffraction (PSD-XRD). From these modal abundances, a classification scheme is constructed that is based on the normalized fraction of phyllosilicate (total phyllosilicate/total anhydrous silicate + total phyllosilicate). Samples are linearly ranked from type 3.0 - corresponding to a phyllosilicate fraction of <0.05, to type 1.0 - corresponding to a total phyllosilicate fraction of >0.95. Powdered meteorite samples from any hydrated carbonaceous chondrite group can be ranked on this single classification scale. The resulting classifications for CRs exhibit a range from type 2.8 to 1.3, while for CMs the range is 1.7-1.2. The primary manifestation of aqueous alteration is the production of phyllosilicate, which ceased when the fluid supply was exhausted, leading to the preservation of anhydrous silicates in all samples. The variability in hydration indicates that either accretion of ices was heterogeneous or fluid was mobilized. From the bulk mineral abundances of the most hydrated samples, we infer that the initial mass fraction of H2O inside of their parent body(ies) asteroids was <20 wt.%. Bulk carbonaceous chondrite mineralogy evolved towards increasingly oxidizing assemblages as the extent of bulk hydration increased. This is consistent with the escape of reducing H-2 gas that is predicted to have been produced from water during hydration reactions. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Howard, K. T.] CUNY, Kingsborough Community Coll, Brooklyn, NY 11235 USA. [Howard, K. T.] Amer Museum Nat Hist, New York, NY 10024 USA. [Howard, K. T.] Nat Hist Museum, London SW7 5BD, England. [Alexander, C. M. O'D.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA. [Schrader, D. L.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. [Dyl, K. A.] Curtin Univ, Dept Appl Geol, Perth, WA 6845, Australia. RP Howard, KT (reprint author), CUNY, Kingsborough Community Coll, 2001 Oriental Blvd, Brooklyn, NY 11235 USA. EM kieren.howard@kbcc.cuny.edu RI Schrader, Devin/H-6293-2012; OI Schrader, Devin/0000-0001-5282-232X; Alexander, Conel/0000-0002-8558-1427 FU NASA [NNX14AG27G, NNA09DA81A, NNX11AG67G]; Australian Research Council; NSF FX K.T.H. was supported by NASA Cosmochemistry grant NNX14AG27G and thanks Ashley King, Paul Schofield and the UK-Cosmochemical Analysis Network (UK-CAN) at the Natural History Museum, London, for access to the PSD-XRD. C.A. was partially supported by NASA Astrobiology grant NNA09DA81A and by NASA Cosmochemistry grant NNX11AG67G. K.A.D. acknowledges the support of the Australian Research Council via the Australian Laureate Fellowship Program. For supplying the many samples that were necessary for this work, the authors would like to thank: the members of the Meteorite Working Group, Cecilia Satterwhite and Kevin Righter (NASA, Johnson Space Center), Tim McCoy and Linda Welzenbach (Smithsonian Museum for Natural History), Laurence Garvie (Arizona State University), Sara Russell, Caroline Smith and Deborah Cassey (Natural History Museum, London). US Antarctic meteorite samples are recovered by the Antarctic Search for Meteorites (ANSMET) program, which has been funded by NSF and NASA, and characterized and curated by the Department of Mineral Sciences of the Smithsonian Institution and Astromaterials Curation Office at NASA Johnson Space Center. NR 71 TC 20 Z9 20 U1 0 U2 13 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 EI 1872-9533 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JAN 15 PY 2015 VL 149 BP 206 EP 222 DI 10.1016/j.gca.2014.10.025 PG 17 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AX2AC UT WOS:000346744500014 ER PT J AU Cruikshank, DP Grundy, WM DeMeo, FE Buie, MW Binzel, RP Jennings, DE Olkin, CB Parker, JW Reuter, DC Spencer, JR Stern, SA Young, LA Weaver, HA AF Cruikshank, D. P. Grundy, W. M. DeMeo, F. E. Buie, M. W. Binzel, R. P. Jennings, D. E. Olkin, C. B. Parker, J. W. Reuter, D. C. Spencer, J. R. Stern, S. A. Young, L. A. Weaver, H. A. TI The surface compositions of Pluto and Charon SO ICARUS LA English DT Article DE Pluto, surface; Charon; Spectroscopy; Satellites, composition ID KUIPER-BELT OBJECTS; OUTER SOLAR-SYSTEM; NEAR-INFRARED SPECTROSCOPY; DWARF PLANET ERIS; 5 MU-M; OPTICAL-CONSTANTS; ION IRRADIATION; CRYSTALLINE H2O-ICE; NITROGEN ICE; CASSINI-VIMS AB The surface of Pluto as it is understood on the eve of the encounter of the New Horizons spacecraft (mid-2015) consists of a spatially heterogeneous mix of solid N-2, CH4, CO, C2H6, and an additional component that imparts color, and may not be an ice. The known molecular ices are detected by near-infrared spectroscopy. The N-2 ice occurs in the hexagonal crystalline beta-phase, stable at T > 35.6 K. Spectroscopic evidence for wavelength shifts in the CH4 bands attests to the complex mixing of CH4 and N-2 in the solid state, in accordance with the phase diagram for N-2 + CH4. Spectra obtained at several aspects of Pluto's surface as the planet rotates over its 6.4-day period show variability in the distribution of CH4 and N-2 ices, with stronger CH4 absorption bands associated with regions of higher albedo, in correlation with the visible rotational light curve. CO and N-2 ice absorptions are also strongly modulated by the rotation period; the bands are strongest on the anti-Charon hemisphere of Pluto. Longer term changes in the strengths of Pluto's absorption bands occur as the viewing geometry changes on seasonal time-scales, although a complete cycle has not been observed. The non-ice component of Pluto's surface may be a relatively refractory material produced by the UV and cosmic-ray irradiation of the surface ices and gases in the atmosphere, although UV does not generally penetrate the atmospheric CH4 to interact with the surface. Laboratory simulations indicate that a rich chemistry ensues by the irradiation of mixtures of the ices known to occur on Pluto, but specific compounds have not yet been identified in spectra of the planet. Charon's surface is characterized by spectral bands of crystalline H2O ice, and a band attributed to one or more hydrates of NH3. Amorphous H2O ice may also be present; the balance between the amorphization and crystallization processes on Charon remains to be clarified. The albedo of Charon and its generally spatially uniform neutral color indicate that a component, not yet identified, is mixed in some way with the H2O and NH3 center dot nH(2)O ices. Among the many known small bodies in the transneptunian region, several share characteristics with Pluto and Charon, including the presence of CH4, N-2, C2H6, H2O ices, as well as components that yield a wide variety of surface albedo and color. The New Horizons investigation of the Pluto-Charon system will generate new insight into the physical properties of the broader transneptunian population, and eventually to the corresponding bodies expected in the numerous planetary systems currently being discovered elsewhere in the Galaxy. Published by Elsevier Inc. C1 [Cruikshank, D. P.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Grundy, W. M.] Lowell Observ, Flagstaff, AZ 86001 USA. [DeMeo, F. E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Buie, M. W.; Olkin, C. B.; Parker, J. W.; Spencer, J. R.; Stern, S. A.; Young, L. A.] SW Res Inst, Boulder, CO 80302 USA. [Binzel, R. P.] MIT, Cambridge, MA 02139 USA. [Jennings, D. E.; Reuter, D. C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Weaver, H. A.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. RP Cruikshank, DP (reprint author), NASA, Ames Res Ctr, MS 245-6, Moffett Field, CA 94035 USA. EM Dale.P.Cruikshank@nasa.gov RI Weaver, Harold/D-9188-2016 NR 139 TC 19 Z9 19 U1 5 U2 51 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 JAN 15 PY 2015 VL 246 BP 82 EP 92 DI 10.1016/j.icarus.2014.05.023 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AX1FQ UT WOS:000346693800008 ER PT J AU Demeo, FE Dumas, C Cook, JC Carry, B Merlin, F Verbiscer, AJ Binzel, RP AF DeMeo, Francesca E. Dumas, Christophe Cook, Jason C. Carry, Benoit Merlin, Frederic Verbiscer, Anne J. Binzel, Richard P. TI Spectral variability of Charon's 2.21-mu m feature SO ICARUS LA English DT Article DE Charon; Spectroscopy; Ices; Kuiper Belt ID CRYSTALLINE WATER ICE; SOLAR-SYSTEM SURFACES; REFLECTANCE SPECTROSCOPY; H2O; SATELLITES; ORCUS AB The clear angular separation of Pluto and Charon from ground-based telescopes has been enabled by improved technology, particularly adaptive optics systems. Near-infrared spectral data have revealed Charon's surface to be rich in crystalline water ice and ammonia hydrates. In this work, we search for spectral differences across Charon's surface with new near-infrared spectral data taken in the K-band (2.0-2.4 mu m) with SINFONI on the VLT and NIRI on Gemini North as well as with previously published spectral data. The strength of the absorption band of ammonia hydrate is dependent on the state of the ice, concentration in H2O, grain size, temperature and exposure to radiation. We find variability of the band center and band depth among spectra. This could indicate variability of the distribution of ammonia hydrate across Charon's surface. If the spectral variation is due to physical properties of Charon, the New Horizons flyby could find the concentration of ammonia hydrate heterogeneously distributed across the surface. Comparison between this work and New Horizons results will test the limits of ground-based reconnaissance. (C) 2014 Elsevier Inc. All rights reserved. C1 [DeMeo, Francesca E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [DeMeo, Francesca E.; Binzel, Richard P.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. [Dumas, Christophe] European So Observ, Santiago 19, Chile. [Cook, Jason C.] Southwest Res Inst, Boulder, CO 80302 USA. [Carry, Benoit] Observ Paris, UMR8028 CNRS, Inst Mecan Celeste & Calcul Ephemerides, F-75014 Paris, France. [Merlin, Frederic] Observ Paris, LESIA, F-92195 Meudon, France. [Merlin, Frederic] Univ Paris 07, Sorbonne Paris Cite, F-75205 Paris 13, France. [Verbiscer, Anne J.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. RP Demeo, FE (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-16, Cambridge, MA 02138 USA. EM fdemeo@cfa.harvard.edu FU European Southern Observatory (ESO) [075.C-0434, 178.C-0036]; NASA [HST-HF-51319.01-A, NAS 5-26555]; Space Telescope Science Institute; National Aeronautics and Space Administration [NNX12AL26G]; National Science Foundation [0907766] FX We thank Mike Brown, Marc Buie, and Will Grundy for sharing their data. We thank Amanda Zangari for help understanding coordinate systems. We acknowledge Rosario Brunetto for helpful discussions and two anonymous referees for valuable comments. This work is based on observations performed at the European Southern Observatory (ESO) under Programs 075.C-0434 and 178.C-0036. Support for this work was provided by NASA through Hubble Fellowship grant HST-HF-51319.01-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. This material is based upon work supported by the National Aeronautics and Space Administration under Grant No. NNX12AL26G issued through the Planetary Astronomy Program and by the National Science Foundation under Grant 0907766. Any opinions, findings, and conclusions or recommendations expressed in this article are those of the authors and do not necessarily reflect the views of the National Aeronautics and Space Administration or the National Science Foundation. NR 35 TC 4 Z9 4 U1 2 U2 6 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 JAN 15 PY 2015 VL 246 BP 213 EP 219 DI 10.1016/j.icarus.2014.04.010 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AX1FQ UT WOS:000346693800017 ER PT J AU Crichton, EG Pukazhenthi, BS Billah, M Skidmore, JA AF Crichton, Elizabeth G. Pukazhenthi, Budhan S. Billah, M. Skidmore, Julian A. TI Cholesterol addition aids the cryopreservation of dromedary camel (Camelus dromedarius) spermatozoa SO THERIOGENOLOGY LA English DT Article DE Camel; Sperm; CLC; Acrosomal integrity; Capacitation ID CHLORTETRACYCLINE FLUORESCENCE ASSAY; OSMOTIC TOLERANCE LIMITS; LOADED-CYCLODEXTRINS; BULL SPERM; IMPROVES CRYOSURVIVAL; BOAR SPERM; BIOCHEMICAL CHARACTERISTICS; ARTIFICIAL-INSEMINATION; STALLION SPERMATOZOA; FERTILIZING ABILITY AB The cryopreservation of dromedary camel (Camelus dromedarius) sperm has proved challenging with little success reported. The routine application of artificial insemination with frozen semen would assist the flow of valuable genetic material nationally and internationally. The current study sought to examine the effects of cholesterol (cholesterol-loaded cyclodextrin [CLC]) preloading on camel sperm cryosurvival. Ejaculates (n = 3 males; 3 ejaculates per male) were collected using an artificial vagina during the breeding season and extended in HEPES-buffered Tyrode's albumin lactate pyruvate (TALP) and allowed to liquefy in the presence of papain (0.1 mg/mL) before removal of the seminal plasma by centrifugation. Sperm pellets were resuspended (120 million/mL) in fresh TALP and incubated (15 minutes; 37 degrees C) with 0, 1.5, or 4.5 mg CLC/mL Sperm suspensions were then centrifuged and reconstituted in INRA-96 containing 20% (v:v) egg yolk and 2.5% (v:v) methylformamide, loaded in 0.5-mL plastic straws, sealed, and cooled for 20 minutes at 4 degrees C. Straws were frozen over liquid nitrogen (4 cm above liquid; 15 minutes), plunged, and stored. Sperm motility, forward progressive status, and acrosomal integrity were recorded at 0 and 3 hours after thawing and compared with these same parameters before freezing. Aliquots also were stained with chlortetracycline hydrochloride to assess spontaneous sperm capacitation status before freezing and post-thaw. Pretreatment with CLC (1.5 and 4.5 mg/mL) enhanced cryosurvival. Post-thaw sperm motility was highest (P < 0.05) in 1.5 mg CLC/mL immediately after thawing (44%) and after 3 hours incubation at room temperature (34%). Highest post-thaw sperm progressive status was also achieved in the presence of 1.5 CLC. Greater proportions of spermatozoa retained acrosomal membrane integrity when cryopreserved in the presence of CLC, but there was no difference between 1.5 and 4.5 CLC. Although thawed spermatozoa underwent spontaneous capacitation during in vitro incubation, cryopreservation and CLC treatment exerted no effect. In summary, dromedary camel sperm benefit from exposure to CLC before cryopreservation; this may facilitate the routine collection and storage of sperm from this species. (C) 2015 Elsevier Inc. All rights reserved. C1 [Crichton, Elizabeth G.; Billah, M.; Skidmore, Julian A.] Camel Reprod Ctr, Dubai, U Arab Emirates. [Pukazhenthi, Budhan S.] Smithsonian Conservat Biol Inst, Front Royal, VA USA. RP Skidmore, JA (reprint author), Camel Reprod Ctr, Dubai, U Arab Emirates. EM luluskidmore@yahoo.com NR 63 TC 7 Z9 7 U1 0 U2 15 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0093-691X EI 1879-3231 J9 THERIOGENOLOGY JI Theriogenology PD JAN 15 PY 2015 VL 83 IS 2 BP 168 EP 174 DI 10.1016/j.theriogenology.2014.09.005 PG 7 WC Reproductive Biology; Veterinary Sciences SC Reproductive Biology; Veterinary Sciences GA AW3YC UT WOS:000346218000003 PM 25312816 ER PT J AU Zalamea, PC Sarmiento, C Arnold, AE Davis, AS Dalling, JW AF Zalamea, Paul-Camilo Sarmiento, Carolina Arnold, A. Elizabeth Davis, Adam S. Dalling, James W. TI Do soil microbes and abrasion by soil particles influence persistence and loss of physical dormancy in seeds of tropical pioneers? SO FRONTIERS IN PLANT SCIENCE LA English DT Article DE Barro Colorado Island; germination cue; physical dormancy; pioneer plants; seed dormancy loss; seed persistence; soil seed bank ID RAIN-FOREST; RECRUITMENT LIMITATION; SEEDLING SURVIVAL; CLIMATE-CHANGE; GERMINATION; DIVERSITY; LIGHT; TEMPERATURE; DISPERSAL; DYNAMICS AB Germination from the soil seed bank (SSB) is an important determinant of species composition in tropical forest gaps, with seed persistence in the SSB allowing trees to recruit even decades after dispersal. The capacity to form a persistent SSB is often associated with physical dormancy, where seed coats are impermeable at the time of dispersal. Germination literature often speculates, without empirical evidence, that dormancy-break in physically dormant seeds is the result of microbial action and/or abrasion by soil particles. We tested the microbial/soil abrasion hypothesis in four widely distributed neotropical pioneer tree species (Apeiba membranacea, Luehea seemannii, Ochroma pyramidale, and Cochlospermum vitifolium). Seeds were buried in five common gardens in a lowland tropical forest in Panama, and recovered at 1, 3, 6, and 12 months after burial. Seed permeability, microbial infection, seed coat thickness, and germination were measured. Parallel experiments compared the germination fraction of fresh and aged seeds without soil contact, and in seeds as a function of seed permeability. Contrary to the microbial/soil abrasion hypothesis the proportion of permeable seeds, and of seeds infected by cultivable microbes, decreased as a function of burial duration. Furthermore, seeds stored in dark and dry conditions for 2 years showed a higher proportion of seed germination than fresh seeds in identical germination conditions. We determined that permeable seeds of A. membranacea and O. pyramidale had cracks in the chalazal area or lacked the chalazal plug, whereas all surfaces of impermeable seeds were intact. Our results are inconsistent with the microbial/soil abrasion hypothesis of dormancy loss and instead suggest the existence of multiple dormancy phenotypes, where a fraction of each seed cohort is dispersed in a permeable state and germinates immediately, while the impermeable seed fraction accounts for the persistent SSB. Thus, we conclude that fluctuations in the soil temperature in the absence of soil abrasion and microbial infection are sufficient to break physical dormancy on seeds of tropical pioneer trees. C1 [Zalamea, Paul-Camilo; Sarmiento, Carolina; Dalling, James W.] Smithsonian Trop Res Inst, Balboa 084303092, Ancon, Panama. [Arnold, A. Elizabeth] Univ Arizona, Sch Plant Sci, Tucson, AZ USA. [Arnold, A. Elizabeth] Univ Arizona, Dept Ecol & Evolutionary Biol, Tucson, AZ USA. [Davis, Adam S.] USDA ARS, Global Change & Photosynthesis Res Unit, Urbana, IL USA. [Dalling, James W.] Univ Illinois, Dept Plant Biol, Urbana, IL 61801 USA. RP Zalamea, PC (reprint author), Smithsonian Trop Res Inst, Balboa 084303092, Ancon, Panama. EM camilozalamea@gmail.com OI Sarmiento, Carolina/0000-0002-8575-7170 FU NSF [DEB-1120205, DEB-1119758] FX This research was funded by NSF DEB-1120205 to J. W. Dalling and NSF DEB-1119758 to A. Elizabeth Arnold. We thank the Smithsonian Tropical Research Institute for providing facilities, logistical support, and permission to conduct the project. We especially thank Roche and C. Delevich for essential assistance in the field and in the laboratory. In addition, we thank K. Winter and M. Slot for logistical support, and J. Ceballos, M, Vargas, I, Quintero, A. Robison, and J. Shaffer for assistance in the field and in the lab. The manuscript was improved by valuable comments from C. Delevich. NR 60 TC 5 Z9 5 U1 7 U2 45 PU FRONTIERS RESEARCH FOUNDATION PI LAUSANNE PA PO BOX 110, LAUSANNE, 1015, SWITZERLAND SN 1664-462X J9 FRONT PLANT SCI JI Front. Plant Sci. PD JAN 13 PY 2015 VL 5 AR 799 DI 10.3389/fpls.2014.00799 PG 14 WC Plant Sciences SC Plant Sciences GA AZ1XX UT WOS:000348029600001 ER PT J AU Shaheen, R Niles, PB Chong, K Corrigan, CM Thiemens, MH AF Shaheen, Robina Niles, Paul B. Chong, Kenneth Corrigan, Catherine M. Thiemens, Mark H. TI Carbonate formation events in ALH 84001 trace the evolution of the Martian atmosphere SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE Martian meteorite; oxygen isotope anomaly; aqueous interaction; carbon isotope; photochemistry ID METEORITE ALH84001; ISOTOPIC COMPOSITION; CLIMATIC CHANGE; LOW-TEMPERATURE; SNC METEORITES; MARS; OXYGEN; ALLAN-HILLS-84001; CO2; CONSTRAINTS AB Carbonate minerals provide critical information for defining atmosphere-hydrosphere interactions. Carbonate minerals in the Martian meteorite ALH 84001 have been dated to similar to 3.9 Ga, and both C and O-triple isotopes can be used to decipher the planet's climate history. Here we report Delta O-17, delta O-18, and delta C-13 data of ALH 84001 of at least two varieties of carbonates, using a stepped acid dissolution technique paired with ion microprobe analyses to specifically target carbonates from distinct formation events and constrain the Martian atmosphere-hydrosphere-geosphere interactions and surficial aqueous alterations. These results indicate the presence of a Ca-rich carbonate phase enriched in O-18 that formed sometime after the primary aqueous event at 3.9 Ga. The phases showed excess O-17 (0.7 parts per thousand) that captured the atmosphere-regolith chemical reservoir transfer, as well as CO2, O-3, and H2O isotopic interactions at the time of formation of each specific carbonate. The carbon isotopes preserved in the Ca-rich carbonate phase indicate that the Noachian atmosphere of Mars was substantially depleted in C-13 compared with the modern atmosphere. C1 [Shaheen, Robina; Chong, Kenneth; Thiemens, Mark H.] Univ Calif San Diego, Dept Chem & Biochem, La Jolla, CA 92122 USA. [Niles, Paul B.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Chong, Kenneth] Calif State Polytech Univ Pomona, Dept Chem, Pomona, CA 91768 USA. [Corrigan, Catherine M.] Smithsonian Inst, Washington, DC 20004 USA. RP Niles, PB (reprint author), NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. EM paul.b.niles@nasa.gov FU National Aeronautics and Space Administration Mars Fundamental Research; National Science Foundation-Atmospheric Chemistry Division [AGS1259305] FX We thank the reviewers for their critical evaluation, which helped improve the manuscript. H. Bao from Louisiana State University is greatly acknowledged for providing carbonate crust from Antarctic Dry valley. P.B.N. acknowledges funding from National Aeronautics and Space Administration Mars Fundamental Research. M. H. T. and R. S. thank National Science Foundation-Atmospheric Chemistry Division for the partial support Award no. AGS1259305 (to R. S.). C. M. C. would like to thank Zonta International Foundation and the Ohio Space Grant Consortium. NR 35 TC 7 Z9 8 U1 6 U2 26 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 JAN 13 PY 2015 VL 112 IS 2 BP 336 EP 341 DI 10.1073/pnas.1315615112 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AY7HS UT WOS:000347732300032 PM 25535348 ER PT J AU Chirchir, H Kivell, TL Ruff, CB Hublin, JJ Carlson, KJ Zipfel, B Richmond, BG AF Chirchir, Habiba Kivell, Tracy L. Ruff, Christopher B. Hublin, Jean-Jacques Carlson, Kristian J. Zipfel, Bernhard Richmond, Brian G. TI Recent origin of low trabecular bone density in modern humans SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE trabecular bone; human evolution; gracilization; Homo sapiens; sedentism ID POSTCRANIAL ROBUSTICITY; BODY-SIZE; LOWER-LIMB; HOMO; MOBILITY; BIOMECHANICS; ARCHITECTURE; ADAPTATION; AGRICULTURE; PROPORTIONS AB Humans are unique, compared with our closest living relatives (chimpanzees) and early fossil hominins, in having an enlarged body size and lower limb joint surfaces in combination with a relatively gracile skeleton (i.e., lower bone mass for our body size). Some analyses have observed that in at least a few anatomical regions modern humans today appear to have relatively low trabecular density, but little is known about how that density varies throughout the human skeleton and across species or how and when the present trabecular patterns emerged over the course of human evolution. Here, we test the hypotheses that (i) recent modern humans have low trabecular density throughout the upper and lower limbs compared with other primate taxa and (ii) the reduction in trabecular density first occurred in early Homo erectus, consistent with the shift toward a modern human locomotor anatomy, or more recently in concert with diaphyseal gracilization in Holocene humans. We used peripheral quantitative CT and microtomography to measure trabecular bone of limb epiphyses (long bone articular ends) in modern humans and chimpanzees and in fossil hominins attributed to Australopithecus africanus, Paranthropus robustus/ early Homo from Swartkrans, Homo neanderthalensis, and early Homo sapiens. Results show that only recent modern humans have low trabecular density throughout the limb joints. Extinct hominins, including pre-Holocene Homo sapiens, retain the high levels seen in nonhuman primates. Thus, the low trabecular density of the recent modern human skeleton evolved late in our evolutionary history, potentially resulting from increased sedentism and reliance on technological and cultural innovations. C1 [Chirchir, Habiba; Richmond, Brian G.] George Washington Univ, Ctr Adv Study Hominid Paleobiol, Dept Anthropol, Washington, DC 20052 USA. [Chirchir, Habiba; Richmond, Brian G.] Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Human Origins Program, Washington, DC 20560 USA. [Kivell, Tracy L.] Univ Kent, Anim Postcranial Evolut Lab, Sch Anthropol & Conservat, Canterbury CT2 7NR, Kent, England. [Kivell, Tracy L.; Hublin, Jean-Jacques] Max Planck Inst Evolutionary Anthropol, Dept Human Evolut, D-04103 Leipzig, Germany. [Ruff, Christopher B.] Johns Hopkins Univ, Sch Med, Ctr Funct Anat & Evolut, Baltimore, MD 21205 USA. [Carlson, Kristian J.; Zipfel, Bernhard] Univ Witwatersrand, Evolutionary Studies Inst, ZA-2000 Johannesburg, South Africa. [Carlson, Kristian J.] Indiana Univ, Dept Anthropol, Bloomington, IN 47405 USA. [Richmond, Brian G.] Amer Museum Nat Hist, Div Anthropol, New York, NY 10024 USA. RP Chirchir, H (reprint author), George Washington Univ, Ctr Adv Study Hominid Paleobiol, Dept Anthropol, Washington, DC 20052 USA. EM habibachirchir@gmail.com; brichmond@amnh.org FU Wenner-Gren Foundation for Anthropological Research Wadsworth Fellowship; Leakey Foundation Baldwin Fellowship; Smithsonian's Peter Buck Postdoctoral Fellowship; National Science Foundation [BCS-0521835, DGE-0801634] FX We thank Z. Tsegai and D. Plotzki for help with microCT scanning and the curators at the following institutions for providing access to samples in their care: Tel Aviv University, Musee du Perigord Perigueux, Reihnisches Landesmuseum Bonn, University of the Witwatersrand, National Museums of Kenya, Distong National Museum of Natural History, and the National Museum of Natural History, Smithsonian Institution. MicroCT scans of Sterkfontein fossil material were produced through a collaborative project between the University of the Witwatersrand and the Department of Human Evolution, Max Planck Institute for Evolutionary Anthropology. This research was supported by the Wenner-Gren Foundation for Anthropological Research Wadsworth Fellowship (to H.C.), the Leakey Foundation Baldwin Fellowship (to H.C.), Smithsonian's Peter Buck Postdoctoral Fellowship (to H.C.), and National Science Foundation Grants BCS-0521835 and DGE-0801634 (to B.G.R.). NR 54 TC 15 Z9 16 U1 5 U2 23 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD JAN 13 PY 2015 VL 112 IS 2 BP 366 EP 371 DI 10.1073/pnas.1411696112 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AY7HS UT WOS:000347732300037 PM 25535354 ER PT J AU Forister, ML Novotny, V Panorska, AK Baje, L Basset, Y Butterill, PT Cizek, L Coley, PD Dem, F Diniz, IR Drozd, P Fox, M Glassmire, AE Hazen, R Hrcek, J Jahner, JP Kaman, O Kozubowski, TJ Kursar, TA Lewis, OT Lill, J Marquis, RJ Miller, SE Morais, HC Murakami, M Nickel, H Pardikes, NA Ricklefs, RE Singer, MS Smilanich, AM Stireman, JO Villamarin-Cortez, S Vodka, S Volf, M Wagner, DL Walla, T Weiblen, GD Dyer, LA AF Forister, Matthew L. Novotny, Vojtech Panorska, Anna K. Baje, Leontine Basset, Yves Butterill, Philip T. Cizek, Lukas Coley, Phyllis D. Dem, Francesca Diniz, Ivone R. Drozd, Pavel Fox, Mark Glassmire, Andrea E. Hazen, Rebecca Hrcek, Jan Jahner, Joshua P. Kaman, Ondrej Kozubowski, Tomasz J. Kursar, Thomas A. Lewis, Owen T. Lill, John Marquis, Robert J. Miller, Scott E. Morais, Helena C. Murakami, Masashi Nickel, Herbert Pardikes, Nicholas A. Ricklefs, Robert E. Singer, Michael S. Smilanich, Angela M. Stireman, John O. Villamarin-Cortez, Santiago Vodka, Stepan Volf, Martin Wagner, David L. Walla, Thomas Weiblen, George D. Dyer, Lee A. TI The global distribution of diet breadth in insect herbivores SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE host range; latitudinal gradient; niche width; Pareto distribution; specialization ID TRUNCATED PARETO DISTRIBUTION; ECOLOGICAL SPECIALIZATION; HOST SPECIALIZATION; SPECIES RICHNESS; PLANT DIVERSITY; FOOD WEBS; DIVERSIFICATION; EVOLUTION; BUTTERFLIES; FORESTS AB Understanding variation in resource specialization is important for progress on issues that include coevolution, community assembly, ecosystem processes, and the latitudinal gradient of species richness. Herbivorous insects are useful models for studying resource specialization, and the interaction between plants and herbivorous insects is one of the most common and consequential ecological associations on the planet. However, uncertainty persists regarding fundamental features of herbivore diet breadth, including its relationship to latitude and plant species richness. Here, we use a global dataset to investigate host range for over 7,500 insect herbivore species covering a wide taxonomic breadth and interacting with more than 2,000 species of plants in 165 families. We ask whether relatively specialized and generalized herbivores represent a dichotomy rather than a continuum from few to many host families and species attacked and whether diet breadth changes with increasing plant species richness toward the tropics. Across geographic regions and taxonomic subsets of the data, we find that the distribution of diet breadth is fit well by a discrete, truncated Pareto power law characterized by the predominance of specialized herbivores and a long, thin tail of more generalized species. Both the taxonomic and phylogenetic distributions of diet breadth shift globally with latitude, consistent with a higher frequency of specialized insects in tropical regions. We also find that more diverse lineages of plants support assemblages of relatively more specialized herbivores and that the global distribution of plant diversity contributes to but does not fully explain the latitudinal gradient in insect herbivore specialization. C1 [Forister, Matthew L.; Glassmire, Andrea E.; Jahner, Joshua P.; Smilanich, Angela M.; Dyer, Lee A.] Univ Nevada, Dept Biol, Program Ecol Evolut & Conservat Biol, Reno, NV 89557 USA. [Panorska, Anna K.] Univ Nevada, Dept Math & Stat, Reno, NV 89557 USA. [Novotny, Vojtech; Basset, Yves; Butterill, Philip T.; Cizek, Lukas; Hrcek, Jan; Kaman, Ondrej; Vodka, Stepan; Volf, Martin] Univ South Bohemia, Fac Sci, Ceske Budejovice 37005, Czech Republic. [Novotny, Vojtech; Butterill, Philip T.; Cizek, Lukas; Hrcek, Jan; Kaman, Ondrej; Vodka, Stepan; Volf, Martin] Acad Sci Czech Republic, Ctr Biol, Ceske Budejovice 37005, Czech Republic. [Novotny, Vojtech; Baje, Leontine; Dem, Francesca] New Guinea Binatang Res Ctr, Madang, Papua N Guinea. [Baje, Leontine] Univ Papua New Guinea, Dept Biol, Port Moresby, Papua N Guinea. [Basset, Yves; Coley, Phyllis D.; Kursar, Thomas A.] Smithsonian Trop Res Inst, Balboa 084303092, Ancon, Panama. [Coley, Phyllis D.; Kursar, Thomas A.] Univ Utah, Dept Biol, Salt Lake City, UT 84112 USA. [Dem, Francesca] Griffith Univ, Environm Futures Res Inst, Nathan, Qld 4111, Australia. [Diniz, Ivone R.; Morais, Helena C.] Univ Brasilia, Dept Zool, BR-70910900 Brasilia, DF, Brazil. [Drozd, Pavel] Univ Ostrava, Dept Biol, Ostrava 71000, Czech Republic. [Fox, Mark; Hazen, Rebecca] Tulane Univ, Dept Ecol & Evolutionary Biol, New Orleans, LA 70118 USA. [Hrcek, Jan; Lewis, Owen T.] Univ Oxford, Dept Zool, Oxford OX1 3PS, England. [Lill, John] George Washington Univ, Dept Biol Sci, Washington, DC 20052 USA. [Marquis, Robert J.; Ricklefs, Robert E.] Univ Missouri, Dept Biol, St Louis, MO 63121 USA. [Marquis, Robert J.; Ricklefs, Robert E.] Univ Missouri, Whitney R Harris World Ecol Ctr, St Louis, MO 63121 USA. [Miller, Scott E.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. [Murakami, Masashi] Chiba Univ, Dept Biol, Chiba 2638522, Japan. [Nickel, Herbert] Univ Gottingen, JF Blumenbach Inst Zool & Anthropol, D-37073 Gottingen, Germany. [Singer, Michael S.] Wesleyan Univ, Dept Biol, Middletown, CT 06459 USA. [Stireman, John O.] Wright State Univ, Dept Biol Sci, Dayton, OH 45435 USA. [Stireman, John O.; Villamarin-Cortez, Santiago; Walla, Thomas] Museo Nacl Ciencias Nat, Secc Invertebrados, Quito, Ecuador. [Wagner, David L.] Univ Connecticut, Dept Ecol & Evolutionary Biol, Storrs, CT 06269 USA. [Walla, Thomas] Colorado Mesa Univ, Dept Biol, Grand Junction, CO 81507 USA. [Weiblen, George D.] Univ Minnesota, Bell Museum, St Paul, MN 55108 USA. [Weiblen, George D.] Univ Minnesota, Dept Plant Biol, St Paul, MN 55108 USA. RP Forister, ML (reprint author), Univ Nevada, Dept Biol, Program Ecol Evolut & Conservat Biol, Reno, NV 89557 USA. EM mforister@unr.edu; ricklefs@umsl.edu RI Drozd, Pavel/J-3943-2013; Basset, Yves/B-6642-2014; Hrcek, Jan/D-7335-2015; Novotny, Vojtech/G-9434-2014; Cizek, Lukas/K-7111-2015; Kaman, Ondrej/G-5781-2014; Butterill, Philip/L-5916-2016; OI Drozd, Pavel/0000-0002-4602-8856; Hrcek, Jan/0000-0003-0711-6447; Novotny, Vojtech/0000-0001-7918-8023; Kaman, Ondrej/0000-0003-1480-2904; Miller, Scott/0000-0002-4138-1378 FU US National Science Foundation; Earthwatch Institute; Czech Science Foundation; University of Missouri-St. Louis; Wesleyan University; Howard Hughes Medical Institute; Brazilian Council for Scientific and Technological Development; Brazilian Federal District Foundation for Science and Research FX For helpful suggestions on the manuscript, we thank Douglas Futuyma and three anonymous reviewers. We also thank Jonathan Davies for the angiosperm phylogeny. Funding was provided by the US National Science Foundation, the Earthwatch Institute, the Czech Science Foundation, the University of Missouri-St. Louis, Wesleyan University, the Howard Hughes Medical Institute, the Brazilian Council for Scientific and Technological Development, and the Brazilian Federal District Foundation for Science and Research. Additional acknowledgments are SI Appendix, section S6. NR 56 TC 54 Z9 55 U1 35 U2 221 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 JAN 13 PY 2015 VL 112 IS 2 BP 442 EP 447 DI 10.1073/pnas.142304211 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AY7HS UT WOS:000347732300050 PM 25548168 ER PT J AU Leauthaud, A Benson, AJ Civano, F Coil, AL Bundy, K Massey, R Schramm, M Schulze, A Capak, P Elvis, M Kulier, A Rhodes, J AF Leauthaud, Alexie Benson, Andrew J. Civano, Francesca Coil, Alison L. Bundy, Kevin Massey, Richard Schramm, Malte Schulze, Andreas Capak, Peter Elvis, Martin Kulier, Andrea Rhodes, Jason TI The dark matter haloes of moderate luminosity X-ray AGN as determined from weak gravitational lensing and host stellar masses SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: abundances; galaxies: active; galaxies: haloes; galaxies: Seyfert; galaxies: stellar content ID ACTIVE GALACTIC NUCLEI; SUPERMASSIVE BLACK-HOLES; DIGITAL SKY SURVEY; WIDE-FIELD SURVEY; HUBBLE-SPACE-TELESCOPE; SIMILAR-TO 1; COSMOS FIELD; OCCUPATION DISTRIBUTION; GALAXY GROUPS; HIGH-REDSHIFT AB Understanding the relationship between galaxies hosting active galactic nuclei (AGN) and the dark matter haloes in which they reside is key to constraining how black hole fuelling is triggered and regulated. Previous efforts have relied on simple halo mass estimates inferred from clustering, weak gravitational lensing, or halo occupation distribution modelling. In practice, these approaches remain uncertain because AGN, no matter how they are identified, potentially live a wide range of halo masses with an occupation function whose general shape and normalization are poorly known. In this work, we show that better constraints can be achieved through a rigorous comparison of the clustering, lensing, and cross-correlation signals of AGN hosts to the fiducial stellar-to-halo mass relation (SHMR) derived for all galaxies, irrespective of nuclear activity. Our technique exploits the fact that the global SHMR can be measured with much higher accuracy than any statistic derived from AGN samples alone. Using 382 moderate luminosity X-ray AGN at z < 1 from the COSMOS field, we report the first measurements of weak gravitational lensing from an X-ray-selected sample. Comparing this signal to predictions from the global SHMR, we find that, contrary to previous results, most X-ray AGN do not live in medium size groups - nearly half reside in relatively low mass haloes with M-200b similar to 10(12.5) M-circle dot. The AGN occupation function is well described by the same form derived for all galaxies but with a lower normalization - the fraction of haloes with AGN in our sample is a few per cent. The number of AGN satellite galaxies scales as a power law with host halo mass with a power-law index alpha = 1. By highlighting the relatively 'normal' way in which moderate luminosity X-ray AGN hosts occupy haloes, our results suggest that the environmental signature of distinct fuelling modes for luminous quasars compared to moderate luminosity X-ray AGN is less obvious than previously claimed. C1 [Leauthaud, Alexie; Bundy, Kevin; Schramm, Malte; Schulze, Andreas] Univ Tokyo, Kavli IPMU, WPI, Kashiwa, Chiba 2778582, Japan. [Benson, Andrew J.] Carnegie Observ, Pasadena, CA 91101 USA. [Civano, Francesca] Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA. [Coil, Alison L.] Univ Calif San Diego, Ctr Astrophys & Space Sci, Dept Phys, San Diego, CA 92093 USA. [Massey, Richard] Univ Durham, Inst Computat Cosmol, Durham DH1 3LE, England. [Capak, Peter] Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Elvis, Martin] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kulier, Andrea] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Rhodes, Jason] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Rhodes, Jason] CALTECH, Pasadena, CA 91125 USA. RP Leauthaud, A (reprint author), Univ Tokyo, Kavli IPMU, WPI, Kashiwa, Chiba 2778582, Japan. EM alexie.leauthaud@ipmu.jp FU World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan; National Science Foundation Graduate Research Fellowship [DGE-1148900]; NASA [AR1-12012X]; Royal Society University Research Fellowship; JPL; NSF CAREER [AST-1055081] FX We thank Phil Hopkins, Surhud More, and John Silverman for insightful discussions while preparing this paper. We also thank Ed Turner for valuable discussions related to statistical methods. We are grateful to Ian Harnett for editing this manuscript. We also thank Nikos Fanidakis for clarifications regarding halo mass values in Fanidakis et al. (2013). This work was supported by World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan. AK is supported by the National Science Foundation Graduate Research Fellowship, grant no. DGE-1148900. FC acknowledges financial support by the NASA grant AR1-12012X. RM is supported by a Royal Society University Research Fellowship. JR was supported by JPL, which is run by Caltech under a contract for NASA. ALC acknowledge support from NSF CAREER award AST-1055081. NR 87 TC 9 Z9 9 U1 0 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JAN 11 PY 2015 VL 446 IS 2 BP 1874 EP 1888 DI 10.1093/mnras/stu2210 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CC3TF UT WOS:000350272200061 ER PT J AU Munoz, DJ Kratter, K Vogelsberger, M Hernquist, L Springel, V AF Munoz, D. J. Kratter, K. Vogelsberger, M. Hernquist, L. Springel, V. TI Stellar orbit evolution in close circumstellar disc encounters SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE hydrodynamics; methods: numerical; planets and satellites: formation; protoplanetary discs; binaries: general ID SMOOTHED PARTICLE HYDRODYNAMICS; MOVING MESH COSMOLOGY; MULTIPLE STAR SYSTEMS; ORION NEBULA CLUSTER; PROTOSTELLAR ENCOUNTERS; NUMERICAL SIMULATIONS; MOLECULAR CLOUDS; BINARY-SYSTEMS; BROWN DWARF; PLANETARY SYSTEMS AB The formation and early evolution of circumstellar discs often occurs within dense, newborn stellar clusters. For the first time, we apply the moving-mesh code AREPO, to circumstellar discs in 3D, focusing on disc-disc interactions that result from stellar flybys. Although a small fraction of stars are expected to undergo close approaches, the outcomes of the most violent encounters might leave an imprint on the discs and host stars that will influence both their orbits and their ability to form planets. We first construct well-behaved 3D models of self-gravitating discs, and then create a suite of numerical experiments of parabolic encounters, exploring the effects of pericentre separation rp, disc orientation and disc-star mass ratio (M-d/M-*) on the orbital evolution of the host stars. Close encounters (2r(p) less than or similar to disc radius) can truncate discs on very short time-scales. If discs are massive, close encounters facilitate enough orbital angular momentum extraction to induce stellar capture. We find that for realistic primordial disc masses M-d less than or similar to 0.1M(*), non-colliding encounters induce minor orbital changes, which is consistent with analytic calculations of encounters in the linear regime. The same disc masses produce entirely different results for grazing/colliding encounters. In the latter case, rapidly cooling discs lose orbital energy by radiating away the energy excess of the shock-heated gas, thus causing capture of the host stars into a bound orbit. In rare cases, a tight binary with a circumbinary disc forms as a result of this encounter. C1 [Munoz, D. J.; Vogelsberger, M.; Hernquist, L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Munoz, D. J.] Cornell Univ, Dept Astron, Ctr Space Res, Ithaca, NY 14853 USA. [Kratter, K.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Springel, V.] Heidelberg Inst Theoret Studies, D-69118 Heidelberg, Germany. [Springel, V.] Heidelberg Univ, Zentrum Astron, ARI, D-69120 Heidelberg, Germany. RP Munoz, DJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM dmunoz@astro.cornell.edu FU Fulbright-CONICYT graduate fellowship program FX The research presented here was largely carried out as part of DJM's PhD thesis at Harvard University. The simulations in this paper were run on the Odyssey cluster supported by the FAS Science Division Research Computing Group at Harvard University. DJM would like to thank Dimitar Sasselov, Matthew Holman, Ruth Murray-Clay and James Stone for insightful feedback and support throughout the development of this work. DJM acknowledges partial support from the Fulbright-CONICYT graduate fellowship program. NR 89 TC 8 Z9 8 U1 0 U2 2 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JAN 11 PY 2015 VL 446 IS 2 BP 2010 EP 2029 DI 10.1093/mnras/stu2220 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CC3TF UT WOS:000350272200072 ER PT J AU Allen, GE Chow, K DeLaney, T Filipovic, MD Houck, JC Pannuti, TG Stage, MD AF Allen, G. E. Chow, K. DeLaney, T. Filipovic, M. D. Houck, J. C. Pannuti, T. G. Stage, M. D. TI ON THE EXPANSION RATE, AGE, AND DISTANCE OF THE SUPERNOVA REMNANT G266.2-1.2 (Vela Jr.) SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: individual objects (G266.2-1.2); ISM: supernova remnants; shock waves; X-rays: individual (G266.2-1.2) ID ULTRAVIOLET SPECTRAL IMAGES; COMPACT CENTRAL OBJECT; LARGE-AREA TELESCOPE; SNR RX J0852.0-4622; X-RAY SPECTROSCOPY; GALACTIC SUPERNOVA; MOLECULAR CLOUDS; NORTHWESTERN RIM; NEUTRAL HYDROGEN; RADIO-CONTINUUM AB An analysis of Chandra ACIS data for two relatively bright and narrow portions of the northwestern rim of G266.2-1.2 (a. k. a. RX J0852.0-4622 or Vela Jr.) reveal evidence of a radial displacement of 2.40 +/- 0.56 arcsec between 2003 and 2008. The corresponding expansion rate (0.42 +/- 0.10 arcsec yr(-1) or 13.6% +/- 4.2% kyr (1)) is about half the rate reported for an analysis of XMM-Newton data from a similar, but not identical, portion of the rim over a similar, but not identical, time interval (0.84 +/- 0.23 arcsec yr(-1)). If the Chandra rate is representative of the remnant as a whole, then the results of a hydrodynamic analysis suggest that G266.2-1.2 is between 2.4 and 5.1 kyr old if it is expanding into a uniform ambient medium (whether or not it was produced by a Type Ia or Type II event). If the remnant is expanding into the material shed by a steady stellar wind, then the age could be as much as 50% higher. The Chandra expansion rate and a requirement that the shock speed be greater than or equal to 1000 km s(-1) yields a lower limit on the distance of 0.5 kpc. An analysis of previously published distance estimates and constraints suggests G266.2-1.2 is no further than 1.0 kpc. This range of distances is consistent with the distance to the nearer of two groups of material in the Vela Molecular Ridge (0.7 +/- 0.2 kpc) and to the Vel OB1 association (0.8 kpc). C1 [Allen, G. E.] MIT Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Chow, K.] Weston High Sch, Weston, MA 02493 USA. [DeLaney, T.] West Virginia Wesleyan Coll, Dept Phys & Engn, Buckhannon, WV 26201 USA. [Filipovic, M. D.] Univ Western Sydney, Penrith, NSW 1797, Australia. [Houck, J. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Pannuti, T. G.] Morehead State Univ, Dept Earth & Space Sci, Ctr Space Sci, Morehead, KY 40351 USA. [Stage, M. D.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. RP Allen, GE (reprint author), MIT Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave,NE83-557, Cambridge, MA 02139 USA. EM gea@space.mit.edu; kc71135@gmail.com; delaney_t@wvwc.edu; m.filipovic@uws.edu.au; jhouck@cfa.harvard.edu; t.pannuti@moreheadstate.edu; mikstage@astro.umass.edu OI Houck, John/0000-0002-6761-6796 FU MIT [SV3-73016]; Smithsonian Astrophysical Observatory [SV3-73016]; NASA [NAS8-03060] FX We thank the anonymous referee, whose comments helped improve the manuscript. G.E.A. is supported by contract SV3-73016 between MIT and the Smithsonian Astrophysical Observatory. The Smithsonian Astrophysical Observatory is operated on behalf of NASA under contract NAS8-03060. This research has made use of data products from the Chandra Data Archive, the Two Micron All Sky Survey, and the USNO-B1.0 catalog. The analyses described herein were performed using the software package CIAO, provided by the Chandra X-ray Center, the software package ISIS (Houck & Denicola 2000), the scripting language S-Lang, and models of the XSPEC spectral-fitting package. NR 70 TC 9 Z9 9 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 2015 VL 798 IS 2 AR 82 DI 10.1088/0004-637X/798/2/82 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CD1SD UT WOS:000350853700017 ER PT J AU Bai, XN AF Bai, Xue-Ning TI HALL EFFECT CONTROLLED GAS DYNAMICS IN PROTOPLANETARY DISKS. II. FULL 3D SIMULATIONS TOWARD THE OUTER DISK SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; instabilities; magnetohydrodynamics (MHD); methods: numerical; protoplanetary disks; turbulence ID VERTICAL MAGNETIC-FIELD; YOUNG STELLAR OBJECTS; WIND-DRIVEN ACCRETION; MAGNETOROTATIONAL-INSTABILITY; X-RAY; NONLINEAR EVOLUTION; AMBIPOLAR DIFFUSION; PROTOSTELLAR DISKS; LINEAR-ANALYSIS; CHEMICAL-PROCESSES AB We perform three-dimensional stratified shearing-box magnetohydrodynamic (MHD) simulations on the gas dynamics of protoplanetary disks with a net vertical magnetic flux of B-z0. All three nonideal MHD effects, Ohmic resistivity, the Hall effect, and ambipolar diffusion, are included in a self-consistent manner based on equilibrium chemistry. We focus on regions toward outer disk radii, from 5 to 60 AU, where Ohmic resistivity tends to become negligible, ambipolar diffusion dominates over an extended region across the disk height, and the Hall effect largely controls the dynamics near the disk midplane. We find that at around R = 5 AU the system launches a laminar or weakly turbulent magnetocentrifugal wind when the net vertical field B-z0 is not too weak. Moreover, the wind is able to achieve and maintain a configuration with reflection symmetry at the disk midplane. The case with anti-aligned field polarity (Omega . B-z0 < 0) is more susceptible to the magnetorotational instability (MRI) when B-z0 decreases, leading to an outflow oscillating in radial directions and very inefficient angular momentum transport. At the outer disk around and beyond R = 30 AU, the system shows vigorous MRI turbulence in the surface layer due to far-UV ionization, which efficiently drives disk accretion. The Hall effect affects the stability of the midplane region to the MRI, leading to strong/weak Maxwell stress for aligned/anti-aligned field polarities. Nevertheless, the midplane region is only very weakly turbulent in both cases. Overall, the basic picture is analogous to the conventional layered accretion scenario applied to the outer disk. In addition, we find that the vertical magnetic flux is strongly concentrated into thin, azimuthally extended shells in most of our simulations beyond 15 AU, leading to enhanced radial density variations know as zonal flows. Theoretical implications and observational consequences are briefly discussed. C1 Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. RP Bai, XN (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St,MS-51, Cambridge, MA 02138 USA. EM xbai@cfa.harvard.edu FU NASA through Hubble Fellowship - Space Telescope Science Institute [HST-HF2-51301.001-A]; NASA [NAS 5-26555]; Texas Advanced Computing Center through XSEDE [TG-AST140001]; National Institute for Computational Sciences through XSEDE [TG-AST130048] FX I thank Jim Stone for helpful discussions and useful comments to the draft. I also thank the anonymous referee for helpful comments that improve the clarity of this paper. This work is supported by NASA through Hubble Fellowship grant HST-HF2-51301.001-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. Computation for this work was performed on Stampede at the Texas Advanced Computing Center through XSEDE grant TG-AST140001, and on Kraken at the National Institute for Computational Sciences through XSEDE grant TG-AST130048. NR 71 TC 39 Z9 40 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 JAN 10 PY 2015 VL 798 IS 2 AR 84 DI 10.1088/0004-637X/798/2/84 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CD1SD UT WOS:000350853700019 ER PT J AU Bower, GC Deller, A Demorest, P Brunthaler, A Falcke, H Moscibrodzka, M O'Leary, RM Eatough, RP Kramer, M Lee, KJ Spitler, L Desvignes, G Rushton, AP Doeleman, S Reid, MJ AF Bower, Geoffrey C. Deller, Adam Demorest, Paul Brunthaler, Andreas Falcke, Heino Moscibrodzka, Monika O'Leary, Ryan M. Eatough, Ralph P. Kramer, Michael Lee, K. J. Spitler, Laura Desvignes, Gregory Rushton, Anthony P. Doeleman, Sheperd Reid, Mark J. TI THE PROPER MOTION OF THE GALACTIC CENTER PULSAR RELATIVE TO SAGITTARIUS A SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; Galaxy: center; proper motions; pulsars: general; pulsars: individual (J1745-2900) ID SUPERMASSIVE BLACK-HOLE; SCATTER-BROADENED IMAGE; ISOLATED RADIO PULSARS; STAR-FORMATION HISTORY; X-RAY-EMISSION; SGR A-ASTERISK; INTRINSIC SIZE; CENTRAL PARSEC; INTERSTELLAR SCATTERING; GENERAL-RELATIVITY AB We measure the proper motion of the pulsar PSR J1745-2900 relative to the Galactic center massive black hole, Sgr A*, using the Very Long Baseline Array (VLBA). The pulsar has a transverse velocity of 236 +/- 11 km s(-1) at position angle 22 +/- 2 deg east of north at a projected separation of 0.097 pc from Sgr A*. Given the unknown radial velocity, this transverse velocity measurement does not conclusively prove that the pulsar is bound to Sgr A*; however, the probability of chance alignment is very small. We do show that the velocity and position are consistent with a bound orbit originating in the clockwise disk of massive stars orbiting Sgr A* and a natal velocity kick of less than or similar to 500 km s(-1). An origin among the isotropic stellar cluster is possible but less probable. If the pulsar remains radio-bright, multiyear astrometry of PSR J1745-2900 can detect its acceleration and determine the full three-dimensional orbit. We also demonstrate that PSR J1745-2900 exhibits the same angular broadening as Sgr A* over a wavelength range of 3.6 cm to 0.7 cm, further confirming that the two sources share the same interstellar scattering properties. Finally, we place the first limits on the presence of a wavelength-dependent shift in the position of Sgr A*, i.e., the core shift, one of the expected properties of optically thick jet emission. Our results for PSR J1745-2900 support the hypothesis that Galactic center pulsars will originate from the stellar disk and deepen the mystery regarding the small number of detected Galactic center pulsars. C1 [Bower, Geoffrey C.] Acad Sinica, Inst Astron & Astrophys, Hilo, HI 96720 USA. [Deller, Adam; Falcke, Heino] ASTRON, NL-7990 AA Dwingeloo, Netherlands. [Demorest, Paul] NRAO, Charlottesville, VA 22903 USA. [Brunthaler, Andreas; Falcke, Heino; Eatough, Ralph P.; Kramer, Michael; Lee, K. J.; Spitler, Laura; Desvignes, Gregory] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Falcke, Heino; Moscibrodzka, Monika] Radboud Univ Nijmegen, Dept Astrophys, IMAPP, NL-6500 GL Nijmegen, Netherlands. [O'Leary, Ryan M.] Univ Colorado, JILA, Boulder, CO 80309 USA. [O'Leary, Ryan M.] NIST, Boulder, CO 80309 USA. [Kramer, Michael] Univ Manchester, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Rushton, Anthony P.] Univ Oxford, Dept Phys, Astrophys, Oxford OX1 3RH, England. [Rushton, Anthony P.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Doeleman, Sheperd] MIT, Haystack Observ, Westford, MA 01886 USA. [Doeleman, Sheperd; Reid, Mark J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Bower, GC (reprint author), Acad Sinica, Inst Astron & Astrophys, 645 N Aohoku Pl, Hilo, HI 96720 USA. EM gbower@asiaa.sinica.edu.tw OI Deller, Adam/0000-0001-9434-3837 NR 82 TC 12 Z9 12 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 2015 VL 798 IS 2 AR 120 DI 10.1088/0004-637X/798/2/120 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CD1SD UT WOS:000350853700055 ER PT J AU Christian, P Loeb, A AF Christian, Pierre Loeb, Abraham TI PULSAR TIMING CONSTRAINTS ON CUMULATIVE AND INDIVIDUAL MASS OF STARS IN THE GALACTIC CENTER SO ASTROPHYSICAL JOURNAL LA English DT Article DE Galaxy: center; pulsars: general ID SAGITTARIUS-A-ASTERISK; SUPERMASSIVE BLACK-HOLE; PROPER MOTION; MILLISECOND PULSARS; STELLAR ORBITS; SGR J1745-29; DISCOVERY; MAGNETAR; DISTANCE; CATALOG AB We consider the time derivatives of the period P of pulsars at the Galactic Center due to variations in their orbital Doppler shifts. We show that in conjunction with a measurement of a pulsar's proper motion and its projected separation from the supermassive black hole, Sgr A*, measuring two of the three derivatives (P)over dot, (P)double over dot, or (P) triple over dot sets a constraint that allows for the recovery of the complete six phase space coordinates of the pulsar's orbit, as well as the enclosed mass within the orbit. Thus, one can use multiple pulsars at different distances from Sgr A* to determine the radial mass distribution of stars and stellar remnants at the Galactic center. Furthermore, we consider the effect of passing stars on the pulsar's period derivatives and show how it can be exploited to measure the characteristic stellar mass in the Galactic center. C1 [Christian, Pierre; Loeb, Abraham] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Christian, P (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM pchristian@cfa.harvard.edu FU NSF [AST-1312034] FX We thank Vicky Kaspi and Sterl Phinney for helpful comments on the manuscript. This work was supported in part by NSF grant AST-1312034. NR 35 TC 0 Z9 0 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 JAN 10 PY 2015 VL 798 IS 2 AR 78 DI 10.1088/0004-637X/798/2/78 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CD1SD UT WOS:000350853700013 ER PT J AU Dawson, RI Murray-Clay, RA Johnson, JA AF Dawson, Rebekah I. Murray-Clay, Ruth A. Johnson, John Asher TI THE PHOTOECCENTRIC EFFECT AND PROTO-HOT JUPITERS. III. A PAUCITY OF PROTO-HOT JUPITERS ON SUPER-ECCENTRIC ORBITS SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems ID KEPLER PLANET CANDIDATES; CLOSE-IN PLANETS; POTENTIAL TRANSIT SIGNALS; EQUILIBRIUM TIDE THEORY; FALSE-POSITIVE RATE; GIANT PLANETS; PERIOD DISTRIBUTION; EXTRASOLAR PLANETS; LIGHT CURVES; DETERMINISTIC MODEL AB Gas giant planets orbiting within 0.1 AU of their host stars are unlikely to have formed in situ and are evidence for planetary migration. It is debated whether the typical hot Jupiter smoothly migrated inward from its formation location through the proto-planetary disk, or was perturbed by another body onto a highly eccentric orbit, which tidal dissipation subsequently shrank and circularized during close stellar passages. Socrates and collaborators predicted that the latter model should produce a population of super-eccentric proto-hot Jupiters readily observable by Kepler. We find a paucity of such planets in the Kepler sample, which is inconsistent with the theoretical prediction with 96.9% confidence. Observational effects are unlikely to explain this discrepancy. We find that the fraction of hot Jupiters with an orbital period P > 3 days produced by the star-planet Kozai mechanism does not exceed ( at two-sigma) 44%. Our results may indicate that disk migration is the dominant channel for producing hot Jupiters with P > 3 days. Alternatively, the typical hot Jupiter may have been perturbed to a high eccentricity by interactions with a planetary rather than stellar companion, and began tidal circularization much interior to 1 AU after multiple scatterings. A final alternative is that early in the tidal circularization process at high eccentricities tidal circularization occurs much more rapidly than later in the process at low eccentricities, although this is contrary to current tidal theories. C1 [Dawson, Rebekah I.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Dawson, Rebekah I.; Murray-Clay, Ruth A.; Johnson, John Asher] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Murray-Clay, Ruth A.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Johnson, John Asher] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Johnson, John Asher] NASA Exoplanet Sci Inst NExScI, Pasadena, CA 91125 USA. RP Dawson, RI (reprint author), Univ Calif Berkeley, Dept Astron, Hearst Field Annex B-20, Berkeley, CA 94720 USA. EM rdawson@berkeley.edu FU National Science Foundation Graduate Research Fellowship [DGE-1144152]; Alfred P. Sloan foundation; NASA [NAS5-26555]; NASA Office of Space Science [NNX09AF08G]; David & Lucile Packard foundation FX We are thankful to the anonymous referee(s) for an insightful report that improved the paper, and in particular for advocating more conservative assumptions about the completeness of the Kepler pipeline. R.I.D. gratefully acknowledges the National Science Foundation Graduate Research Fellowship under grant DGE-1144152 and the Miller Institute for Basic Research in Science, University of California, Berkeley. J.A.J. is grateful for the generous grant support provided by the Alfred P. Sloan and David & Lucile Packard foundations. We are grateful to Smadar Naoz for many enlightening discussions and comments, including opening our eyes to other possibilities in Section 4, for which we also thank Simon Albrecht and Fred Rasio. Many thanks to Adrian Barker, Rick Greenberg, Renu Malhotra, Francesca Valsecchi, and especially Brad Hansen for tidal insights; to Katherine Deck, Will Farr, Vicky Kalogera, Yoram Lithwick, and Matthew Payne for helpful dynamical discussions; to Will Farr and Moritz Gunther for helpful statistical discussions; to Courtney Dressing and Francois Fressin for Kepler assistance; and to Joel Hartmann for helpful discussions about the ground-based sample. We are grateful to Subo Dong for constructive comments on a manuscript draft. Thanks to Joshua Carter, Boas Katz, Doug Lin, Geoff Marcy, Darin Ragozzine, Kevin Schlaufman, and Aristotle Socrates for helpful comments, and to Thomas Barclay, Christophe Burke, Jon Jenkins, and Jason Rowe for helpful discussions of Kepler's completeness for giant planets. We benefitted from helpful conversations with Thomas Barclay about candidate vetting and Howard Isaacson and Rea Kolb about false positives. We are very grateful to Chelsea Huang for helpful discussions and for providing us with a detrended light curve for KIC 6805414. R.I.D. thanks David Charbonneau, Sean Andrews, Debra Fischer, Matt Holman, and Abraham Loeb for helpful comments on the thesis chapter version of this manuscript. Special thanks to J. Zachary Gazak for helpful modifications to the TAP code. We thank Daithi Stone for making his library of IDL routines available.; This paper includes data collected by the Kepler mission. Funding for the Kepler mission is provided by the NASA Science Mission directorate. We are grateful to Kepler team for their work in making this revolutionizing mission possible and making the rich Kepler data set available. Some of the data presented in this paper were obtained from the Multimission Archive at the Space Telescope Science Institute (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant NNX09AF08G and by other grants and contracts. This research has made use of the Exoplanet Orbit Database, and the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. NR 119 TC 18 Z9 18 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 2015 VL 798 IS 2 AR 66 DI 10.1088/0004-637X/798/2/66 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CD1SD UT WOS:000350853700001 ER PT J AU Jung, YK Udalski, A Sumi, T Han, C Gould, A Skowron, J Kozlowski, S Poleski, R Wyrzykowski, L Szymanski, MK Pietrzynski, G Soszynski, I Ulaczyk, K Pietrukowicz, P Mroz, P Kubiak, M Abe, F Bennett, DP Bond, IA Botzler, CS Freeman, M Fukui, A Fukunaga, D Itow, Y Koshimoto, N Larsen, P Ling, CH Masuda, K Matsubara, Y Muraki, Y Namba, S Ohnishi, K Philpott, L Rattenbury, NJ Saito, T Sullivan, DJ Suzuki, D Tristram, PJ Tsurumi, N Wada, K Yamai, N Yock, PCM Yonehara, A Albrow, M Choi, JY DePoy, DL Gaudi, BS Hwang, KH Lee, CU Park, H Owen, S Pogge, RW Shin, IG Yee, JC AF Jung, Y. K. Udalski, A. Sumi, T. Han, C. Gould, A. Skowron, J. Kozlowski, S. Poleski, R. Wyrzykowski, L. Szymanski, M. K. Pietrzynski, G. Soszynski, I. Ulaczyk, K. Pietrukowicz, P. Mroz, P. Kubiak, M. Abe, F. Bennett, D. P. Bond, I. A. Botzler, C. S. Freeman, M. Fukui, A. Fukunaga, D. Itow, Y. Koshimoto, N. Larsen, P. Ling, C. H. Masuda, K. Matsubara, Y. Muraki, Y. Namba, S. Ohnishi, K. Philpott, L. Rattenbury, N. J. Saito, To. Sullivan, D. J. Suzuki, D. Tristram, P. J. Tsurumi, N. Wada, K. Yamai, N. Yock, P. C. M. Yonehara, A. Albrow, M. Choi, J. -Y. DePoy, D. L. Gaudi, B. S. Hwang, K. -H. Lee, C. -U. Park, H. Owen, S. Pogge, R. W. Shin, I. -G. Yee, J. C. CA OGLE Collaboration MOA Collaboration FUN Collaboration TI OGLE-2013-BLG-0102LA,B: MICROLENSING BINARY WITH COMPONENTS AT STAR/BROWN DWARF AND BROWN DWARF/PLANET BOUNDARIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: general; brown dwarfs; gravitational lensing: micro ID LOW-MASS BINARY; GALACTIC BULGE; CANDIDATE BINARIES; SPEX SPECTROSCOPY; PRESTELLAR CORES; GIANT PLANETS; OGLE-III; PARALLAX; STELLAR; EVENT AB We present an analysis of the gravitational microlensing event OGLE-2013-BLG-0102. The light curve of the event is characterized by a strong short-term anomaly superposed on a smoothly varying lensing curve with a moderate magnification A(max) similar to 1.5. It is found that the event was produced by a binary lens with a mass ratio between the components of q = 0.13 and the anomaly was caused by the passage of the source trajectory over a caustic located away from the barycenter of the binary. Based on the analysis of the effects on the light curve due to the finite size of the source and the parallactic motion of the Earth, we determine the physical parameters of the lens system. The measured masses of the lens components are M-1 = 0.096 +/- 0.013 M-circle dot and M-2 = 0.012 +/- 0.002 M-circle dot, which correspond to near the hydrogen-burning and deuterium-burning mass limits, respectively. The distance to the lens is 3.04 +/- 0.31 kpc and the projected separation between the lens components is 0.80 +/- 0.08 AU. C1 [Jung, Y. K.; Han, C.; Choi, J. -Y.; Hwang, K. -H.; Park, H.; Shin, I. -G.] Chungbuk Natl Univ, Dept Phys, Cheongju 371763, South Korea. [Udalski, A.; Skowron, J.; Kozlowski, S.; Poleski, R.; Wyrzykowski, L.; Szymanski, M. K.; Pietrzynski, G.; Soszynski, I.; Ulaczyk, K.; Pietrukowicz, P.; Mroz, P.; Kubiak, M.] Univ Warsaw Observ, PL-00478 Warsaw, Poland. [Sumi, T.; Koshimoto, N.; Namba, S.; Suzuki, D.; Wada, K.] Osaka Univ, Dept Earth & Space Sci, Osaka 5600043, Japan. [Gould, A.; Poleski, R.; Gaudi, B. S.; Owen, S.; Pogge, R. W.; Yee, J. C.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Wyrzykowski, L.; Larsen, P.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Pietrzynski, G.] Univ Concepcion, Dept Astron, Concepcion, Chile. [Fukunaga, D.; Itow, Y.; Masuda, K.; Matsubara, Y.; Muraki, Y.; Tsurumi, N.] Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan. [Bennett, D. P.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. [Bond, I. A.; Ling, C. H.] Massey Univ, Inst Informat & Math Sci, Auckland, New Zealand. [Botzler, C. S.; Freeman, M.; Rattenbury, N. J.; Yock, P. C. M.] Univ Auckland, Dept Phys, Auckland 1001, New Zealand. [Fukui, A.] Natl Astron Observ Japan, Okayama Astrophys Observ, Asakuchi, Okayama 7190232, Japan. [Ohnishi, K.] Nagano Natl Coll Technol, Nagano 3818550, Japan. [Philpott, L.] Univ British Columbia, Dept Earth Ocean & Atmospher Sci, Vancouver, BC V6T 1Z4, Canada. [Saito, To.] Tokyo Metropolitan Coll Aeronaut, Tokyo 1168523, Japan. [Sullivan, D. J.] Victoria Univ, Sch Chem & Phys Sci, Wellington, New Zealand. [Tristram, P. J.] Mt John Univ Observ, Lake Tekapo 8770, New Zealand. [Yamai, N.; Yonehara, A.] Kyoto Sangyo Univ, Fac Sci, Dept Phys, Kyoto 6038555, Japan. [Albrow, M.] Univ Canterbury, Dept Phys & Astron, Christchurch 1, New Zealand. [DePoy, D. L.] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA. [Lee, C. -U.] Korea Astron & Space Sci Inst, Taejon, South Korea. [Yee, J. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Han, C (reprint author), Chungbuk Natl Univ, Dept Phys, Cheongju 371763, South Korea. EM cheongho@astroph.chungbuk.ac.kr RI Skowron, Jan/M-5186-2014; Kozlowski, Szymon/G-4799-2013; OI Skowron, Jan/0000-0002-2335-1730; Kozlowski, Szymon/0000-0003-4084-880X; Philpott, Lydia/0000-0002-5286-8528 FU Creative Research Initiative Program of National Research Foundation of Korea [2009-0081561]; NSF [AST-1103471]; NASA [NNX12AB99G]; European Research Council under the European Community's Seventh Framework Programme (FP7)/ERC [246678]; JSPS [24253004, JSPS23540339, JSPS19340058]; NASA through the Sagan Fellowship Program; [JSPS23340044] FX Work by C.H. was supported by Creative Research Initiative Program (2009-0081561) of National Research Foundation of Korea. A.G. and B.S.G. acknowledge support from NSF AST-1103471. B.S.G., A.G., and R.W.P. acknowledge support from NASA grant NNX12AB99G. The OGLE project has received funding from the European Research Council under the European Community's Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement No. 246678 to A.U. The MOA experiment was supported by grants JSPS22403003 and JSPS23340064. T.S. acknowledges the support of JSPS 24253004. T.S. is supported by the grant JSPS23340044. Y.M. acknowledges support from JSPS grants JSPS23540339 and JSPS19340058. Work by J.C.Y. was performed in part under contract with the California Institute of Technology (Caltech) funded by NASA through the Sagan Fellowship Program. NR 60 TC 9 Z9 9 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 2015 VL 798 IS 2 AR 123 DI 10.1088/0004-637X/798/2/123 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CD1SD UT WOS:000350853700058 ER PT J AU Lee, JY Raymond, JC Reeves, KK Moon, YJ Kim, KS AF Lee, Jin-Yi Raymond, John C. Reeves, Katharine K. Moon, Yong-Jae Kim, Kap-Sung TI MASS AND ENERGY OF ERUPTING SOLAR PLASMA OBSERVED WITH THE X-RAY TELESCOPE ON HINODE SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: activity; Sun: corona; Sun: coronal mass ejections (CMEs); Sun: X-rays,gamma rays; Sun: UV radiation ID PHYSICAL CONDITIONS; SOHO OBSERVATIONS; A MISSION; EJECTION; FLARE; HOT; SHEET; PROMINENCE; ENERGETICS; DYNAMICS AB We investigate seven eruptive plasma observations by Hinode/ XRT. Their corresponding EUV and/or white light coronal mass ejection features are visible in some events. Five events are observed in several passbands in X-rays, which allows for the determination of the eruptive plasma temperature using a filter ratio method. We find that the isothermal temperatures vary from 1.6 to 10MK. These temperatures are an average weighted toward higher temperature plasma. We determine the mass constraints of eruptive plasmas by assuming simplified geometrical structures of the plasma with isothermal plasma temperatures. This method provides an upper limit to the masses of the observed eruptive plasmas in X-ray passbands since any clumping causes the overestimation of the mass. For the other two events, we assume the temperatures are at the maximum temperature of the X-ray Telescope (XRT) temperature response function, which gives a lower limit of the masses. We find that the masses in XRT, similar to 3x10(13)-5 x 10(14) g, are smaller in their upper limit than the total masses obtained by LASCO, similar to 1 x10(15) g. In addition, we estimate the radiative loss, thermal conduction, thermal, and kinetic energies of the eruptive plasma in X-rays. For four events, we find that the thermal conduction timescales are much shorter than the duration of eruption. This result implies that additional heating during the eruption may be required to explain the plasma observations in X-rays for the four events. C1 [Lee, Jin-Yi; Moon, Yong-Jae; Kim, Kap-Sung] Kyung Hee Univ, Dept Astron & Space Sci, Yongin 446701, Gyeonggi, South Korea. [Raymond, John C.; Reeves, Katharine K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Moon, Yong-Jae; Kim, Kap-Sung] Kyung Hee Univ, Sch Space Res, Yongin 446701, Gyeonggi, South Korea. RP Lee, JY (reprint author), Kyung Hee Univ, Dept Astron & Space Sci, Yongin 446701, Gyeonggi, South Korea. EM jlee@khu.ac.kr RI Moon, Yong-Jae/E-1711-2013; OI Lee, Jin-Yi/0000-0001-6412-5556; Reeves, Katharine/0000-0002-6903-6832 FU NASA [NNM07AA02C, NNX09AB17G]; NSF SHINE [AGS-1156076]; Basic Science Research program [NRF-2013R1A1A2058409, NRF2013R1A1A2012763]; BK21 plus program through the National Research Foundation (NRF) - Ministry of Education of Korea; NRF of Korea Grant funded by the Korean Government [NRF-2013M1A3A3A02042232]; KoreaMeteorological Administration/National Meteorological Satellite Center FX This work was supported by NASA grants NNM07AA02C and NNX09AB17G and NSF SHINE grant AGS-1156076 to the Smithsonian Astrophysical Observatory, Basic Science Research program (NRF-2013R1A1A2058409, NRF2013R1A1A2012763), and the BK21 plus program through the National Research Foundation (NRF) funded by the Ministry of Education of Korea, NRF of Korea Grant funded by the Korean Government (NRF-2013M1A3A3A02042232), and the KoreaMeteorological Administration/National Meteorological Satellite Center. Hinode is a Japanese mission developed and launched by ISAS/JAXA, with NAOJ as a domestic partner and NASA and STFC (UK) as international partners. It is operated by these agencies in co-operation with ESA and the NSC (Norway). The 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. SOHO is a project of international cooperation between ESA and NASA. NR 52 TC 2 Z9 2 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 2015 VL 798 IS 2 AR 106 DI 10.1088/0004-637X/798/2/106 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CD1SD UT WOS:000350853700041 ER PT J AU Meisner, AM Finkbeiner, DP AF Meisner, Aaron M. Finkbeiner, Douglas P. TI MODELING THERMAL DUST EMISSION WITH TWO COMPONENTS: APPLICATION TO THE PLANCK HIGH FREQUENCY INSTRUMENT MAPS SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; infrared: ISM; submillimeter: ISM ID INFRARED-EMISSION; COBE; SKY; GALAXY AB We apply the Finkbeiner et al. two-component thermal dust emission model to the Planck High Frequency Instrument maps. This parameterization of the far-infrared dust spectrum as the sum of two modified blackbodies (MBBs) serves as an important alternative to the commonly adopted single-MBB dust emission model. Analyzing the joint Planck/DIRBE dust spectrum, we show that two-component models provide a better fit to the 100-3000 GHz emission than do single-MBB models, though by a lesser margin than found by Finkbeiner et al. based on FIRAS and DIRBE. We also derive full-sky 6.'1 resolution maps of dust optical depth and temperature by fitting the two-component model to Planck 217-857 GHz along with DIRBE/IRAS 100 mu m data. Because our two-component model matches the dust spectrum near its peak, accounts for the spectrum's flattening at millimeter wavelengths, and specifies dust temperature at 6.'1 FWHM, our model provides reliable, high-resolution thermal dust emission foreground predictions from 100 to 3000 GHz. We find that, in diffuse sky regions, our two-component 100-217 GHz predictions are on average accurate to within 2.2%, while extrapolating the Planck Collaboration et al. single-MBB model systematically underpredicts emission by 18.8% at 100 GHz, 12.6% at 143 GHz, and 7.9% at 217 GHz. We calibrate our two-component optical depth to reddening, and compare with reddening estimates based on stellar spectra. We find the dominant systematic problems in our temperature/reddening maps to be zodiacal light on large angular scales and the cosmic infrared background anisotropy on small angular scales. C1 [Meisner, Aaron M.; Finkbeiner, Douglas P.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Meisner, Aaron M.; Finkbeiner, Douglas P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Meisner, AM (reprint author), Harvard Univ, Dept Phys, 17 Oxford St, Cambridge, MA 02138 USA. EM ameisner@fas.harvard.edu; dfinkbeiner@cfa.harvard.edu OI Meisner, Aaron/0000-0002-1125-7384 FU National Science Foundation Graduate Research Fellowship [DGE1144152]; NASA [NNX12AE08G]; ESA Member States; NASA FX We thank the anonymous referee for helpful suggestions. We gratefully acknowledge support from the National Science Foundation Graduate Research Fellowship under grant No. DGE1144152, and NASA grant NNX12AE08G. Based on observations obtained with Planck, (http://www.esa.int/Planck), an ESA science mission with instruments and contributions directly funded by ESA Member States, NASA, and Canada. This research made use of the NASA Astrophysics Data System (ADS) and the IDL Astronomy User's Library at Goddard (available at http://idlastro.gsfc.nasa.gov). NR 26 TC 11 Z9 11 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 10 PY 2015 VL 798 IS 2 AR 88 DI 10.1088/0004-637X/798/2/88 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CD1SD UT WOS:000350853700023 ER PT J AU Miller, AA Bloom, JS Richards, JW Lee, YS Starr, DL Butler, NR Tokarz, S Smith, N Eisner, JA AF Miller, A. A. Bloom, J. S. Richards, J. W. Lee, Y. S. Starr, D. L. Butler, N. R. Tokarz, S. Smith, N. Eisner, J. A. TI A MACHINE-LEARNING METHOD TO INFER FUNDAMENTAL STELLAR PARAMETERS FROM PHOTOMETRIC LIGHT CURVES SO ASTROPHYSICAL JOURNAL LA English DT Article DE methods: data analysis; methods: statistical; stars: general; stars: statistics; stars: variables: general; surveys ID DIGITAL SKY SURVEY; AUTOMATED SUPERVISED CLASSIFICATION; HIGH-RESOLUTION SPECTROSCOPY; VARIABLE-STARS; RANDOM FORESTS; DATA RELEASE; SPACED DATA; CATALOG; METALLICITY; VARIABILITY AB A fundamental challenge for wide-field imaging surveys is obtaining follow-up spectroscopic observations: there are >10(9) photometrically cataloged sources, yet modern spectroscopic surveys are limited to similar to fewx10(6) targets. As we approach the Large Synoptic Survey Telescope era, new algorithmic solutions are required to cope with the data deluge. Here we report the development of a machine-learning framework capable of inferring fundamental stellar parameters (T-eff, log g, and [Fe/H]) using photometric-brightness variations and color alone. A training set is constructed from a systematic spectroscopic survey of variables with Hectospec/ Multi-Mirror Telescope. In sum, the training set includes similar to 9000 spectra, for which stellar parameters are measured using the SEGUE Stellar Parameters Pipeline (SSPP). We employed the random forest algorithm to perform a non-parametric regression that predicts Teff, log g, and [Fe/H] from photometric time-domain observations. Our final optimized model produces a cross-validated rms error (RMSE) of 165 K, 0.39 dex, and 0.33 dex for T-eff, log g, and [Fe/H], respectively. Examining the subset of sources for which the SSPP measurements are most reliable, the RMSE reduces to 125 K, 0.37 dex, and 0.27 dex, respectively, comparable to what is achievable via low-resolution spectroscopy. For variable stars this represents a approximate to 12%-20% improvement in RMSE relative to models trained with single-epoch photometric colors. As an application of our method, we estimate stellar parameters for similar to 54,000 known variables. We argue that this method may convert photometric time-domain surveys into pseudo-spectrographic engines, enabling the construction of extremely detailed maps of the Milky Way, its structure, and history. C1 [Miller, A. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Miller, A. A.] CALTECH, Pasadena, CA 91125 USA. [Bloom, J. S.; Richards, J. W.; Starr, D. L.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Bloom, J. S.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Phys, Berkeley, CA 94720 USA. [Richards, J. W.; Starr, D. L.] Wise Io, Berkeley, CA 94704 USA. [Lee, Y. S.] Chungnam Natl Univ, Dept Astron & Space Sci, Taejon 305764, South Korea. [Butler, N. R.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85281 USA. [Tokarz, S.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Smith, N.; Eisner, J. A.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. RP Miller, AA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 169-506, Pasadena, CA 91109 USA. EM amiller@astro.caltech.edu FU NASA from a Hubble Fellowship [HST-HF-51325.01]; STScI; NASA [NAS 5-26555]; NSF-CDI [0941742]; Alfred P. Sloan Research Fellowship FX A.A.M. acknowledges support for this work by NASA from a Hubble Fellowship grant: HST-HF-51325.01, awarded by STScI, operated by AURA, Inc., for NASA, under contract NAS 5-26555. J.S.B. acknowledges support from an NSF-CDI grant 0941742. JAE gratefully acknowledges support from an Alfred P. Sloan Research Fellowship. Part of the research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. Observations reported here were obtained at the MMT Observatory, a joint facility of the University of Arizona and the Smithsonian Institution. NR 56 TC 1 Z9 1 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 2015 VL 798 IS 2 AR 122 DI 10.1088/0004-637X/798/2/122 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CD1SD UT WOS:000350853700057 ER PT J AU Ricci, L Carpenter, JM Fu, B Hughes, AM Corder, S Isella, A AF Ricci, L. Carpenter, J. M. Fu, B. Hughes, A. M. Corder, S. Isella, A. TI ALMA OBSERVATIONS OF THE DEBRIS DISK AROUND THE YOUNG SOLAR ANALOG HD 107146 SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; planets and satellites: formation; stars: individual (HD 107146); submillimeter: stars ID GIANT-PLANET FORMATION; MAIN-SEQUENCE STARS; SUN-LIKE STARS; CIRCUMSTELLAR DISKS; MOLECULAR GAS; PROTOPLANETARY DISK; COLLISIONAL CASCADES; SIZE DISTRIBUTIONS; OPTICAL-CONSTANTS; BETA-PICTORIS AB We present the Atacama Large Millimeter/submillimeter Array (ALMA) continuum observations at a wavelength of 1.25 mm of the debris disk surrounding the similar to 100 Myr old solar analog HD 107146. The continuum emission extends from about 30 to 150 AU from the central star with a decrease in the surface brightness at intermediate radii. We analyze the ALMA interferometric visibilities using debris disk models with radial profiles for the dust surface density parameterized as (1) a single power law, (2) a single power law with a gap, and (3) a double power law. We find that models with a gap of radial width similar to 8 AU at a distance of similar to 80 AU from the central star, as well as double power-law models with a dip in the dust surface density at similar to 70 AU provide significantly better fits to the ALMA data than single power-law models. We discuss possible scenarios for the origin of the HD 107146 debris disk using models of planetesimal belts in which the formation of Pluto-sized objects trigger disruptive collisions of large bodies, as well as models that consider the interaction of a planetary system with a planetesimal belt and spatial variation of the dust opacity across the disk. If future observations with higher angular resolution and sensitivity confirm the fully depleted gap structure discussed here, a planet with a mass of approximately a few Earth masses in a nearly circular orbit at similar to 80 AU from the central star would be a possible explanation for the presence of the gap. C1 [Ricci, L.; Carpenter, J. M.; Fu, B.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Ricci, L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hughes, A. M.] Wesleyan Univ, Dept Astron, Midletown, CT 06457 USA. [Corder, S.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Isella, A.] Rice Univ, Dept Phys & Astron, Houston, TX 77521 USA. RP Ricci, L (reprint author), CALTECH, Dept Astron, MC 249-17, Pasadena, CA 91125 USA. EM lricci@astro.caltech.edu FU NSF [AST-1109334] FX This paper makes use of the following ALMA data: ADS/JAO. ALMA#2011.0.00470.S. ALMA is a partnership of ESO (representing its member states), NSF (USA), and NINS (Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. J.M.C. acknowledges support from NSF grant AST-1109334. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. NR 85 TC 20 Z9 20 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 2015 VL 798 IS 2 AR 124 DI 10.1088/0004-637X/798/2/124 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CD1SD UT WOS:000350853700059 ER PT J AU Zapata, LA Lizano, S Rodriguez, LF Ho, PTP Loinard, L Fernandez-Lopez, M Tafoya, D AF Zapata, Luis A. Lizano, Susana Rodriguez, Luis F. Ho, Paul T. P. Loinard, Laurent Fernandez-Lopez, Manuel Tafoya, Daniel TI KINEMATICS OF THE OUTFLOW FROM THE YOUNG STAR DG TAU B: ROTATION IN THE VICINITIES OF AN OPTICAL JET SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: jets and outflows; stars: individual (DG Tau B, Taurus Molecular Cloud); stars: pre-main sequence ID STELLAR OBJECT JETS; CIRCUMSTELLAR DISKS; MOLECULAR OUTFLOWS; PHOTOEVAPORATION; EMISSION; DRIVEN; REGION; SHOCKS; RADIO; CORES AB We present (CO)-C-12(2-1) line and 1300 mu m continuum observations made with the Submillimeter Array of the young star DG Tau B. We find, in the continuum observations, emission arising from the circumstellar disk surrounding DG Tau B. The (CO)-C-12(2-1) line observations, on the other hand, revealed emission associated with the disk and the asymmetric outflow related with this source. Velocity asymmetries about the flow axis are found over the entire length of the flow. The amplitude of the velocity differences is of the order of 1-2 kms(-1) over distances of about 300-400 AU. We interpret them as a result of outflow rotation. The sense of the outflow and disk rotation is the same. Infalling gas from a rotating molecular core cannot explain the observed velocity gradient within the flow. Magneto-centrifugal disk winds or photoevaporated disk winds can produce the observed rotational speeds if they are ejected from a Keplerian disk at radii of several tens of AU. Nevertheless, these slow winds ejected from large radii are not very massive, and cannot account for the observed linear momentum and angular momentum rates of the molecular flow. Thus, the observed flow is probably entrained material from the parent cloud. DG Tau B is a good laboratory to model in detail the entrainment process and see if it can account for the observed angular momentum. C1 [Zapata, Luis A.; Lizano, Susana; Rodriguez, Luis F.; Loinard, Laurent; Tafoya, Daniel] UNAM, Ctr Radioastron & Astrofis, Morelia 58089, Michoacan, Mexico. [Ho, Paul T. P.] Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan. [Ho, Paul T. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Fernandez-Lopez, Manuel] Univ Illinois, Dept Astron, Urbana, IL 61801 USA. [Fernandez-Lopez, Manuel] Consejo Nacl Invest Cient & Tecn, Inst Argentino Radioastron, CCT La Plata, RA-1894 Villa Elisa, Argentina. RP Zapata, LA (reprint author), UNAM, Ctr Radioastron & Astrofis, Apdo Postal 3-72 Xangari, Morelia 58089, Michoacan, Mexico. EM lzapata@crya.unam.mx FU DGAPA; UNAM; CONACyT, Mexico; University of Illinois FX L.A.Z, S.L., L.F.R., L.L., and D.T. acknowledge financial support from DGAPA, UNAM, and CONACyT, Mexico. M.F.L. acknowledges financial support from the University of Illinois and the hospitality of the CRyA (UNAM). We thank the anonymous referee for detailed comments that improved our study. NR 43 TC 6 Z9 6 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 2015 VL 798 IS 2 AR 131 DI 10.1088/0004-637X/798/2/131 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CD1SD UT WOS:000350853700066 ER PT J AU van Dokkum, PG Abraham, R Merritt, A Zhang, JL Geha, M Conroy, C AF van Dokkum, Pieter G. Abraham, Roberto Merritt, Allison Zhang, Jielai Geha, Marla Conroy, Charlie TI FORTY-SEVEN MILKY WAY-SIZED, EXTREMELY DIFFUSE GALAXIES IN THE COMA CLUSTER SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: clusters: individual (Coma); galaxies: evolution; galaxies: structure ID SURFACE-BRIGHTNESS GALAXIES; DRAGONFLY TELEPHOTO ARRAY; DWARF ELLIPTIC GALAXIES; STELLAR POPULATIONS; LOCAL GROUP; EVOLUTION; DYNAMICS; DENSITY; ORIGIN; CORE AB We report the discovery of 47 low surface brightness objects in deep images of a 3 degrees x 3 degrees field centered on the Coma cluster, obtained with the Dragonfly Telephoto Array. The objects have central surface brightness mu(g, 0) ranging from 24-26 mag arcsec(-2) and effective radii r(eff) = 3 ''-10 '', as measured from archival Canada-France-Hawaii Telescope images. From their spatial distribution we infer that most or all of the objects are galaxies in the Coma cluster. This relatively large distance is surprising as it implies that the galaxies are very large: with r(eff) = 1.5-4.6 kpc their sizes are similar to those of L-* galaxies even though their median stellar mass is only similar to 6 x 10(7) M-circle dot. The galaxies are relatively red and round, with < g - i > = 0.8 and < b/a > = 0.74. One of the 47 galaxies is fortuitously covered by a deep Hubble Space Telescope Advanced Camera for Surveys (ACS) observation. The ACS imaging shows a large spheroidal object with a central surface brightness mu(475) = 25.8 mag arcsec(-2), a Sersic index n = 0.6, and an effective radius of 7 '', corresponding to 3.4 kpc at the distance of Coma. The galaxy is not resolved into stars, consistent with expectations for a Coma cluster object. We speculate that these "ultra-diffuse galaxies" may have lost their gas supply at early times, possibly resulting in very high dark matter fractions. C1 [van Dokkum, Pieter G.; Merritt, Allison; Geha, Marla] Yale Univ, Dept Astron, New Haven, CT 06511 USA. [Abraham, Roberto; Zhang, Jielai] Univ Toronto, Dept Astron, Toronto, ON M5S 3H4, Canada. [Conroy, Charlie] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP van Dokkum, PG (reprint author), Yale Univ, Dept Astron, New Haven, CT 06511 USA. FU NSF grant [AST-1312376] FX We thank the anonymous referee for an excellent and constructive report. We also thank the staff at New Mexico Skies for their support and Nelson Caldwell for comments on the manuscript. Support from NSF grant AST-1312376 is gratefully acknowledged. NR 35 TC 37 Z9 37 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JAN 10 PY 2015 VL 798 IS 2 AR L45 DI 10.1088/2041-8205/798/2/L45 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AY3CY UT WOS:000347463300019 ER PT J AU da Fonseca, RR Smith, BD Wales, N Cappellini, E Skoglund, P Fumagalli, M Samaniego, JA Caroe, C Avila-Arcos, MC Hufnagel, DE Korneliussen, TS Vieira, FG Jakobsson, M Arriaza, B Willerslev, E Nielsen, R Hufford, MB Albrechtsen, A Ross-Ibarra, J Gilbert, MTP AF da Fonseca, Rute R. Smith, Bruce D. Wales, Nathan Cappellini, Enrico Skoglund, Pontus Fumagalli, Matteo Samaniego, Jose Alfredo Caroe, Christian Avila-Arcos, Mara C. Hufnagel, David E. Korneliussen, Thorfinn Sand Vieira, Filipe Garrett Jakobsson, Mattias Arriaza, Bernardo Willerslev, Eske Nielsen, Rasmus Hufford, Matthew B. Albrechtsen, Anders Ross-Ibarra, Jeffrey Gilbert, M. Thomas P. TI The origin and evolution of maize in the Southwestern United States SO NATURE PLANTS LA English DT Article ID MAYS SSP PARVIGLUMIS; ANCIENT DNA; DOMESTICATION; SELECTION; ARCHITECTURE; ASSOCIATION; IMPROVEMENT; GENETICS AB The origin of maize (Zea mays mays) in the US Southwest remains contentious, with conflicting archaeological data supporting either coastal(1-4) or highland(5,6) routes of diffusion of maize into the United States. Furthermore, the genetics of adaptation to the new environmental and cultural context of the Southwest is largely uncharacterized(7). To address these issues, we compared nuclear DNA from 32 archaeological maize samples spanning 6,000 years of evolution to modern landraces. We found that the initial diffusion of maize into the Southwest about 4,000 years ago is likely to have occurred along a highland route, followed by gene flow from a lowland coastal maize beginning at least 2,000 years ago. Our population genetic analysis also enabled us to differentiate selection during domestication for adaptation to the climatic and cultural environment of the Southwest, identifying adaptation loci relevant to drought tolerance and sugar content. C1 [da Fonseca, Rute R.; Wales, Nathan; Cappellini, Enrico; Samaniego, Jose Alfredo; Caroe, Christian; Avila-Arcos, Mara C.; Korneliussen, Thorfinn Sand; Vieira, Filipe Garrett; Willerslev, Eske; Nielsen, Rasmus; Gilbert, M. Thomas P.] Univ Copenhagen, Ctr GeoGenet, DK-1350 Copenhagen, Denmark. [da Fonseca, Rute R.; Albrechtsen, Anders] Univ Copenhagen, Bioinformat Ctr, DK-2200 Copenhagen, Denmark. [Smith, Bruce D.] Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Program Human Ecol & Archaeobiol, Washington, DC 20560 USA. [Skoglund, Pontus] Harvard Univ, Sch Med, Dept Genet, Boston, MA 02115 USA. [Fumagalli, Matteo; Vieira, Filipe Garrett] Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. [Avila-Arcos, Mara C.] Stanford Univ, Dept Genet, Sch Med, Stanford, CA 94305 USA. [Hufnagel, David E.; Hufford, Matthew B.] Iowa State Univ, Dept Ecol Evolut & Organismal Biol, Ames, IA 50011 USA. [Jakobsson, Mattias] Uppsala Univ, Dept Evolutionary Biol, S-75236 Uppsala, Sweden. [Jakobsson, Mattias] Uppsala Univ, Sci Life Lab, S-75236 Uppsala, Sweden. [Arriaza, Bernardo] Univ Tarapaca, Inst Alta Invest, Arica 15101, Chile. [Nielsen, Rasmus] Univ Calif Berkeley, Dept Integrat Biol & Stat, Berkeley, CA 94720 USA. [Ross-Ibarra, Jeffrey] Univ Calif Davis, Dept Plant Sci, Ctr Populat Biol, Davis, CA 95616 USA. [Ross-Ibarra, Jeffrey] Univ Calif Davis, Genome Ctr, Davis, CA 95616 USA. [Gilbert, M. Thomas P.] Curtin Univ, Trace & Environm DNA Lab, Dept Environm & Agr, Perth, WA 6102, Australia. RP da Fonseca, RR (reprint author), Univ Copenhagen, Ctr GeoGenet, DK-1350 Copenhagen, Denmark. EM rute.r.da.fonseca@gmail.com; mtpgilbert@gmail.com RI da Fonseca, Rute/F-9143-2013; Albrechtsen, Anders/K-4281-2013; Jakobsson, Mattias/A-6116-2011; Cappellini, Enrico/F-9346-2013; Garrett Vieira, Filipe/B-9464-2015; Korneliussen, Thorfinn Sand/F-6421-2014; Nielsen, Rasmus/D-4405-2009; OI da Fonseca, Rute/0000-0002-2805-4698; Albrechtsen, Anders/0000-0001-7306-031X; Jakobsson, Mattias/0000-0001-7840-7853; Cappellini, Enrico/0000-0001-7885-7811; Garrett Vieira, Filipe/0000-0002-8464-7770; Skoglund, Pontus/0000-0002-3021-5913; Korneliussen, Thorfinn Sand/0000-0001-7576-5380; Nielsen, Rasmus/0000-0003-0513-6591; Avila-Arcos, Maria C./0000-0003-1691-1696; Wales, Nathan/0000-0003-0359-8450 FU Marie Curie Actions [IEF 272927, COFUND DFF-1325-00136]; Danish National Research Foundation [DNRF94]; Danish Council for Independent Research [10-081390, 1325-00136]; Lundbeck Foundation [R52-A5062]; Vand Fondecyt [1130261]; UC Davis Genome Center; NSF [IOS-1238014]; Young Investigator grant from Villum Fonden [VKR023446]; Wenner-Gren foundation FX The authors acknowledge the following grants: Marie Curie Actions IEF 272927 and COFUND DFF-1325-00136, Danish National Research Foundation DNRF94, Danish Council for Independent Research 10-081390 and 1325-00136, Lundbeck Foundation grant R52-A5062, Vand Fondecyt Grant 1130261, a grant from the UC Davis Genome Center for the highland maize sequence and NSF IOS-1238014. R.F. is supported by a Young Investigator grant (VKR023446) from Villum Fonden. P.S. was funded by the Wenner-Gren foundation. The authors thank Angela Ribeiro, Shohei Takuno and Philip Johnson for comments and discussion and staff at the Danish National High-Throughput DNA Sequencing for technical support. NR 38 TC 8 Z9 8 U1 8 U2 24 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 2055-026X EI 2055-0278 J9 NAT PLANTS JI Nat. Plants PD JAN 8 PY 2015 VL 1 IS 1 AR 14003 DI 10.1038/NPLANTS.2014.3 PG 5 WC Plant Sciences SC Plant Sciences GA CV6NS UT WOS:000364387500004 PM 27246050 ER PT J AU Warnock, RCM Parham, JF Joyce, WG Lyson, TR Donoghue, PCJ AF Warnock, Rachel C. M. Parham, James F. Joyce, Walter G. Lyson, Tyler R. Donoghue, Philip C. J. TI Calibration uncertainty in molecular dating analyses: there is no substitute for the prior evaluation of time priors SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE molecular clock; calibration; cross-validation; fossil record; Bayesian; priors ID SPECIES DIVERGENCE TIMES; FOSSIL CALIBRATIONS; BAYESIAN-ESTIMATION; CLOCK; EVOLUTION; POINTS; RECORD; TREE; PERSPECTIVE; LIKELIHOOD AB Calibration is the rate-determining step in every molecular clock analysis and, hence, considerable effort has been expended in the development of approaches to distinguish good from bad calibrations. These can be categorized into a priori evaluation of the intrinsic fossil evidence, and a posteriori evaluation of congruence through cross-validation. We contrasted these competing approaches and explored the impact of different interpretations of the fossil evidence upon Bayesian divergence time estimation. The results demonstrate that a posteriori approaches can lead to the selection of erroneous calibrations. Bayesian posterior estimates are also shown to be extremely sensitive to the probabilistic interpretation of temporal constraints. Furthermore, the effective time priors implemented within an analysis differ for individual calibrations when employed alone and in differing combination with others. This compromises the implicit assumption of all calibration consistency methods, that the impact of an individual calibration is the same when used alone or in unison with others. Thus, the most effective means of establishing the quality of fossil-based calibrations is through a priori evaluation of the intrinsic palaeontological, stratigraphic, geochronological and phylogenetic data. However, effort expended in establishing calibrations will not be rewarded unless they are implemented faithfully in divergence time analyses. C1 [Warnock, Rachel C. M.; Donoghue, Philip C. J.] Univ Bristol, Sch Earth Sci, Bristol, Avon, England. [Warnock, Rachel C. M.] Natl Evolutionary Synth Ctr, Durham, NC USA. [Warnock, Rachel C. M.] Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA. [Parham, James F.] Calif State Univ Fullerton, Dept Geol Sci, John D Cooper Archaeol & Paleontol Ctr, Fullerton, CA 92634 USA. [Joyce, Walter G.] Univ Fribourg, Fribourg, Switzerland. [Lyson, Tyler R.] Denver Museum Nat & Sci, Denver, CO USA. RP Warnock, RCM (reprint author), Univ Bristol, Sch Earth Sci, Bristol, Avon, England. EM warnockr@si.edu; phil.donoghue@bristol.ac.uk RI Donoghue, Philip/A-3873-2008; OI Donoghue, Philip/0000-0003-3116-7463 FU NERC [NE/I528250/1, NE/G009600/1]; BBSRC [BB/G006660/1, BB/J00538X/1]; National Science Foundation [EF-0905606]; NESCent FX This study was supported by NERC studentship NE/I528250/1 to R.C.M.W. and P.C.J.D., NERC grant no. NE/G009600/1 to P.C.J.D. and BBSRC grant nos. BB/G006660/1 and BB/J00538X/1 to Ziheng Yang and P.C.J.D. This work also benefitted from a working group on fossil calibrations (Synthesizing and databasing fossil calibrations: divergence dating and beyond) at the National Evolutionary Synthesis Center (NESCent) (National Science Foundation no. EF-0905606), and an NESCent studentship to R.C.M.W. NR 50 TC 25 Z9 26 U1 4 U2 31 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8452 EI 1471-2954 J9 P ROY SOC B-BIOL SCI JI Proc. R. Soc. B-Biol. Sci. PD JAN 7 PY 2015 VL 282 IS 1798 AR 20141013 DI 10.1098/rspb.2014.1013 PG 10 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA AX8LK UT WOS:000347160800002 PM 25429012 ER PT J AU Ajoy, A Bissbort, U Lukin, MD Walsworth, RL Cappellaro, P AF Ajoy, A. Bissbort, U. Lukin, M. D. Walsworth, R. L. Cappellaro, P. TI Atomic-Scale Nuclear Spin Imaging Using Quantum-Assisted Sensors in Diamond SO PHYSICAL REVIEW X LA English DT Article ID NITROGEN-VACANCY CENTERS; SOLID-STATE SPIN; MAGNETIC-RESONANCE; ELECTRONIC SPIN; RESOLUTION; SPECTROSCOPY; MOLECULE; READOUT; NMR AB Nuclear spin imaging at the atomic level is essential for the understanding of fundamental biological phenomena and for applications such as drug discovery. The advent of novel nanoscale sensors promises to achieve the long-standing goal of single-protein, high spatial-resolution structure determination under ambient conditions. In particular, quantum sensors based on the spin-dependent photoluminescence of nitrogen-vacancy (NV) centers in diamond have recently been used to detect nanoscale ensembles of external nuclear spins. While NV sensitivity is approaching single-spin levels, extracting relevant information from a very complex structure is a further challenge since it requires not only the ability to sense the magnetic field of an isolated nuclear spin but also to achieve atomic-scale spatial resolution. Here, we propose a method that, by exploiting the coupling of the NV center to an intrinsic quantum memory associated with the nitrogen nuclear spin, can reach a tenfold improvement in spatial resolution, down to atomic scales. The spatial resolution enhancement is achieved through coherent control of the sensor spin, which creates a dynamic frequency filter selecting only a few nuclear spins at a time. We propose and analyze a protocol that would allow not only sensing individual spins in a complex biomolecule, but also unraveling couplings among them, thus elucidating local characteristics of the molecule structure. C1 [Ajoy, A.; Bissbort, U.; Cappellaro, P.] MIT, Res Lab Elect, 77 Massachusetts Ave, Cambridge, MA 02139 USA. [Ajoy, A.; Bissbort, U.; Cappellaro, P.] MIT, Dept Nucl Sci & Engn, 77 Massachusetts Ave, Cambridge, MA 02139 USA. [Bissbort, U.] Singapore Univ Technol & Design, Singapore 138682, Singapore. [Lukin, M. D.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Walsworth, R. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Walsworth, R. L.] Ctr Brain Sci, Cambridge, MA 02138 USA. RP Ajoy, A (reprint author), MIT, Res Lab Elect, 77 Massachusetts Ave, Cambridge, MA 02139 USA.; Ajoy, A (reprint author), MIT, Dept Nucl Sci & Engn, 77 Massachusetts Ave, Cambridge, MA 02139 USA. RI Cappellaro, Paola/B-1413-2010 OI Cappellaro, Paola/0000-0003-3207-594X FU U.S. Army Research Office through MURI Grant [W911NF-11-1-0400]; DARPA (QuASAR program) FX We thank F. Jelezko, E. Boyden, C. Belthangady, S. DeVience, I. Lovchinsky, L. Pham, and A. Sushkov for discussions. This work was supported in part by the U.S. Army Research Office through MURI Grant No. W911NF-11-1-0400 and by DARPA (QuASAR program). NR 65 TC 21 Z9 21 U1 4 U2 20 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2160-3308 J9 PHYS REV X JI Phys. Rev. X PD JAN 7 PY 2015 VL 5 IS 1 AR 011001 DI 10.1103/PhysRevX.5.011001 PG 11 WC Physics, Multidisciplinary SC Physics GA DF6JR UT WOS:000371462300001 ER PT J AU Morgan, ME Lewton, KL Kelley, J Otarola-Castillo, E Barry, JC Flynn, LJ Pilbeam, D AF Morgan, Michele E. Lewton, Kristi L. Kelley, Jay Otarola-Castillo, Erik Barry, John C. Flynn, Lawrence J. Pilbeam, David TI A partial hominoid innominate from the Miocene of Pakistan: Description and preliminary analyses SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE Sivapithecus; innominate; Miocene hominoid; torso shape; positional behavior ID MIDDLE MIOCENE; OREOPITHECUS-BAMBOLII; POSTCRANIAL SPECIMENS; CHINJI FORMATION; GREAT-APE; PROCONSUL-NYANZAE; AFRICAN APES; SIVAPITHECUS; MORPHOLOGY; SKELETON AB We describe a partial innominate, YGSP 41216, from a 12.3 Ma locality in the Siwalik Group of the Potwar Plateau in Pakistan, assigned to the Middle Miocene ape species Sivapithecus indicus. We investigate the implications of its morphology for reconstructing positional behavior of this ape. Postcranial anatomy of extant catarrhines falls into two distinct groups, particularly for torso shape. To an extent this reflects different although variable and overlapping positional repertoires: pronograde quadrupedalism for cercopithecoids and orthogrady for hominoids. The YGSP innominate (hipbone) is from a primate with a narrow torso, resembling most extant monkeys and differing from the broader torsos of extant apes. Other postcranial material of S. indicus and its younger and similar congener Sivapithecus sivalensis also supports reconstruction of a hominoid with a positional repertoire more similar to the pronograde quadrupedal patterns of most monkeys than to the orthograde patterns of apes. However, Sivapithecus postcranial morphology differs in many details from any extant species. We reconstruct a slow-moving, deliberate, arboreal animal, primarily traveling above supports but also frequently engaging in antipronograde behaviors. There are no obvious synapomorphic postcranial features shared exclusively with any extant crown hominid, including Pongo. C1 [Morgan, Michele E.; Flynn, Lawrence J.] Harvard Univ, Peabody Museum Archaeol & Ethnol, Cambridge, MA 02138 USA. [Lewton, Kristi L.; Otarola-Castillo, Erik; Barry, John C.; Flynn, Lawrence J.; Pilbeam, David] Harvard Univ, Dept Human Evolutionary Biol, Cambridge, MA 02138 USA. [Lewton, Kristi L.] Boston Univ, Sch Med, Dept Anat & Neurobiol, Boston, MA 02118 USA. [Kelley, Jay] Arizona State Univ, Inst Human Origins, Tempe, AZ 85287 USA. [Kelley, Jay] Arizona State Univ, Sch Human Evolut & Social Change, Tempe, AZ 85287 USA. [Kelley, Jay] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. RP Morgan, ME (reprint author), Harvard Univ, Peabody Museum Archaeol & Ethnol, Cambridge, MA 02138 USA. EM memorgan@fas.harvard.edu; pilbeam@fas.harvard.edu OI Lewton, Kristi/0000-0003-0674-2454 FU National Science Foundation [BCS 0752575, EAR 0958178]; Leakey Foundation; American School for Prehistoric Research, Harvard University FX We thank J. Chupasko and M. Omura for frequent access to primate collections curated at the Museum of Comparative Zoology, Harvard University. C. Ward generously shared data from her comparative sample of extant primates. We supplemented these data and thank the curators and collection managers at the American Museum of Natural History (E. Westwig and D. Lunde), National Museum of Natural History (L. Gordon), Field Museum of Natural History (B. Patterson and W. Stanley), Cleveland Museum of Natural History (Y. Haile-Selassie and L. Jellema), Natural History Museum (P. Jenkins and L. Tomsett), and the Museum National d'Histoire Naturelle (C. Lefevre, J. Lesur-Gebremariam, J. Cuisin, and J. Villemain). Funding was provided by National Science Foundation Grants BCS 0752575 and EAR 0958178, The Leakey Foundation, and the American School for Prehistoric Research, Harvard University. NR 69 TC 7 Z9 7 U1 1 U2 7 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD JAN 6 PY 2015 VL 112 IS 1 BP 82 EP 87 DI 10.1073/pnas.1420275111 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AY2WN UT WOS:000347447100033 PM 25489095 ER PT J AU Bermudez, SE Esser, HJ Miranda, R Moreno, RS AF Bermudez, Sergio E. Esser, Helen J. Miranda C, Roberto Moreno, Ricardo S. TI Wild carnivores (Mammalia) as hosts for ticks (Ixodida) in Panama SO SYSTEMATIC AND APPLIED ACAROLOGY LA English DT Article ID ACARI IXODIDAE; BRAZIL; KOCH; PARK AB This study reports ticks collected from wild carnivores from different habitat types in Panama. We examined 94 individual wild carnivores and we found 87 parasitized by ticks: seven coyotes, six crab-eating foxes, 54 coatis, four raccoons, five ocelots, two pumas, two gray foxes, two skunks, and one each of kinkajou, jaguar, jaguaroundi, greater grison and tayra. We identified 13 species of tick: Ornithodoros puertoricensis, Amblyomma auricularium, A. dissimile, A. mixtum, A. oblongoguttatum, A. ovale, A. parvum, A. pecarium, A. tapirellum, A. varium, Haemaphysalis juxtakochi, Ixodes affinis, Rhipicephalus sanguineus s.l. and immatures of Ixodes and Amblyomma. Amblyomma ovale and A. oblongoguttatum were the most common species, found on nine and six carnivore species respectively. This is the first report of A. oblongoguttatum on Puma yagouaroundi and Procyon lotor; of A. dissimile, A. pecarium, A. tapirellum and A. varium on Nasua narica; and A. auricularium on P. lotor. Our data do not enable us to establish incidence of tick parasitism, but add valuable information to the current knowledge of the tick species that infest wild carnivores in Panama. C1 [Bermudez, Sergio E.; Miranda C, Roberto] Inst Conmemorat Gorgas Estudios Salud, Dept Invest Entomol Med, Panama City, Panama. [Esser, Helen J.] Smithsonian Trop Res Inst, Panama City, Panama. [Esser, Helen J.] Wageningen Univ, Dept Environm Sci, NL-6700 AP Wageningen, Netherlands. [Moreno, Ricardo S.] Soc Panamena Biol, Yaguara Panama, Panama City, Panama. RP Bermudez, SE (reprint author), Inst Conmemorat Gorgas Estudios Salud, Dept Invest Entomol Med, Panama City, Panama. EM sbermudez@gorgas.gob.pa FU Smithsonian Grand Challenges Award; graduate school of Production Ecology and Resource Conservation of Wageningen University FX The authors thank Pedro Mendez-Carvajal (Fundacion Pro-Conservacion de los Primates Panamenos), Nestor Correa (Asociacion Panamericana para la Conservacion), Ben Hirsch, Patrick A. Jansen, Roland Kays (Smithsonian Tropical Research Institution), Rodrigo Chang (Autoridad del Canal de Panama), Nataniel Kadoch (Ministerio de Desarrollo Agropecuario), Daniel Gonzalez and Aydee Cornejo-Remice (ICGES) for providing ticks. We are also grateful to Celestino Aguilar and Matthew Miller for DNA barcoding, to Ninon Meyer (STRI) and Robyn Nadolny (Old Dominion University, Virginia, US) for the English revision, and Alberto Guglielmone (Instituto Nacional de Tecnologia Agropecuaria, Argentina) for his comments on an earlier version of the manuscript. HJE received funds from the Smithsonian Grand Challenges Award and the graduate school of Production Ecology and Resource Conservation of Wageningen University. NR 27 TC 5 Z9 6 U1 2 U2 7 PU SYSTEMATIC & APPLIED ACAROLOGY SOC LONDON, NATURAL HISTORY MUSEUM PI LONDON PA DEPT ENTOMOLOGY, LONDON, SW7 5BD, ENGLAND SN 1362-1971 J9 SYST APPL ACAROL-UK JI Syst. Appl. Acarol. PD JAN 5 PY 2015 VL 20 IS 1 BP 13 EP 19 PG 7 WC Entomology SC Entomology GA CF4WL UT WOS:000352553800002 ER PT J AU Collins, M AF Collins, Martin TI Untitled SO HISTORY AND TECHNOLOGY LA English DT Editorial Material C1 Smithsonian Inst, Washington, DC 20560 USA. RP Collins, M (reprint author), Smithsonian Inst, Washington, DC 20560 USA. EM CollinsM@si.edu NR 0 TC 0 Z9 0 U1 0 U2 0 PU ROUTLEDGE JOURNALS, TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXFORDSHIRE, ENGLAND SN 0734-1512 EI 1477-2620 J9 HIST TECHNOL JI Hist. Technol. PD JAN 2 PY 2015 VL 31 IS 1 BP 1 EP 1 DI 10.1080/07341512.2015.1073885 PG 1 WC History SC History GA CQ0SX UT WOS:000360308400001 ER PT J AU Carrano, MT D'Emic, MD AF Carrano, Matthew T. D'Emic, Michael D. TI OSTEODERMS OF THE TITANOSAUR SAUROPOD DINOSAUR ALAMOSAURUS SANJUANENSIS GILMORE, 1922 SO JOURNAL OF VERTEBRATE PALEONTOLOGY LA English DT Article ID NORTH-AMERICA; EARLY EVOLUTION; SPECIMEN; PHYLOGENY; ARGENTINA; PROVINCE; HIATUS AB SUPPLEMENTAL DATASupplemental materials are available for this article for free at www.tandfonline.com/UJVP; CT data are available as Morphobank project P2093 at http://www.morphobank.org. C1 [Carrano, Matthew T.] Smithsonian Inst, Dept Paleobiol, Washington, DC 20012 USA. [D'Emic, Michael D.] SUNY Stony Brook, Dept Anat Sci, Stony Brook, NY 11794 USA. RP Carrano, MT (reprint author), Smithsonian Inst, Dept Paleobiol, POB 37012,MRC 121, Washington, DC 20012 USA. EM carranom@si.edu; michael.demic@stonybrook.edu RI Carrano, Matthew/C-7601-2011 OI Carrano, Matthew/0000-0003-2129-1612 NR 30 TC 3 Z9 3 U1 0 U2 2 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 530 WALNUT STREET, STE 850, PHILADELPHIA, PA 19106 USA SN 0272-4634 EI 1937-2809 J9 J VERTEBR PALEONTOL JI J. Vertebr. Paleontol. PD JAN 2 PY 2015 VL 35 IS 1 AR e901334 DI 10.1080/02724634.2014.901334 PG 7 WC Paleontology SC Paleontology GA CL4GV UT WOS:000356911500010 ER PT J AU Sues, HD Averianov, A Ridgely, RC Witmer, LM AF Sues, Hans-Dieter Averianov, Alexander Ridgely, Ryan C. Witmer, Lawrence M. TI TITANOSAURIA (DINOSAURIA, SAUROPODA) FROM THE UPPER CRETACEOUS (TURONIAN) BISSEKTY FORMATION OF UZBEKISTAN SO JOURNAL OF VERTEBRATE PALEONTOLOGY LA English DT Article ID PATAGONIA; ARGENTINA; BRAINCASE; PROVINCE; NEUQUEN; ANATOMY; SAURISCHIA; SPECIMEN; FOSSIL; CHINA AB Exposures of the Bissekty Formation (Upper Cretaceous: middle-upper Turonian) at Dzharakuduk in the central Kyzylkum Desert of Uzbekistan have yielded abundant dinosaurian remains. We report here on cranial and postcranial remains that can be attributed to titanosaurian sauropods. This material is of considerable interest in view of the relative scarcity of sauropod fossils from the Upper Cretaceous of Central Asia. An incomplete braincase originally assigned to the ceratopsian Turanoceratops tardabilis actually belongs to a derived titanosaurian. It shares a number of features (including broad basal tubera and presence of wide depression between basal tubera) with braincases of various derived titanosaurian taxa from Asia and South America. Computed tomographic (CT) scanning of the braincase permitted digital reconstruction of a partial endocast. Overall, this endocast resembles those of other sauropods, although the pituitary fossa is considerably swollen. As in other derived titanosaurians, the abducens nerve passed lateral to the pituitary fossa. The inner ear resembles that of some other titanosaurs in having a very short lateral semicircular canal and that the anterior semicircular canal is only slightly longer than the posterior one. Isolated sauropod teeth from Dzharakuduk have slender, pencil-shaped' crowns, which often bear high-angle apical wear facets. The caudal vertebrae are gently opisthocoelous rather than procoelous, as is typically the condition on at least the anterior caudals in many other titanosaurs. An anterior caudal vertebra shows extensive pneumatization of its neural arch. The sauropod remains from the Bissekty Formation establish the presence of titanosaurians in Central Asia during the Turonian. C1 [Sues, Hans-Dieter] Smithsonian Inst, Dept Paleobiol, Natl Museum Nat Hist, Washington, DC 20013 USA. [Averianov, Alexander] Russian Acad Sci, Inst Zool, St Petersburg 199034, Russia. [Averianov, Alexander] St Petersburg State Univ, Geol Fac, Dept Sedimentary Geol, St Petersburg 199178, Russia. [Ridgely, Ryan C.; Witmer, Lawrence M.] Ohio Univ, Dept Biomed Sci, Heritage Coll Osteopath Med, Athens, OH 45701 USA. RP Sues, HD (reprint author), Smithsonian Inst, Dept Paleobiol, Natl Museum Nat Hist, MRC 121,POB 37012, Washington, DC 20013 USA. EM suesh@si.edu; dzharakuduk@mail.ru; ridgely@ohio.edu; witmerL@ohio.edu RI Averianov, Alexander/M-8490-2013 OI Averianov, Alexander/0000-0001-5948-0799 FU National Science Foundation [EAR-9804771, EAR-0207004, IBN-0343744, IOB-0517257, IOS-1050154]; National Geographic Society [5901-97, 6281-98]; Navoi Mining and Metallurgy Combinat; Civilian Research and Development Foundation [RU-G1-2571-ST-04, RUB1-2860-ST-07]; Russian Fund of Basic Research [07-04-91110-AFGIRa]; Russian Scientific Fund [14-14-0015]; Ohio University Heritage College of Osteopathic Medicine; Ohio Supercomputing Center FX H.-D.S. and A. A. thank A. V. Abramov, J. D. Archibald, G. O. Cherepanov, I. G. Danilov, S. Dominguez, C. King, N. Morris, C. M. Redman, A. S. Resvyi, C. Skrabec, P. P. Skutschas, E. V. Syromyatnikova, and D. J. Ward for their efforts in the field, scientific expertise, and camaraderie. The cooperation of the Zoological Institute of the National Academy of Sciences of Uzbekistan is greatly appreciated. I. Morrison carefully prepared USNM 538127. For assistance with CT scanning of CCMGE 628/12457, we thank H. Rockhold, RT, and O'Bleness Memorial Hospital, Athens, Ohio. We are indebted to M. D. D'Emic (Stony Brook University) and A. Paulina Carabajal (Museo Carmen Funes) for constructive reviews of a draft of the manuscript. H.-D.S. and A. A. gratefully acknowledge financial support from the National Science Foundation (EAR-9804771 and EAR-0207004 to J. D. Archibald and H.-D. Sues), the National Geographic Society (5901-97 and 6281-98 to J. D. Archibald and H.-D. Sues), the Navoi Mining and Metallurgy Combinat, the Civilian Research and Development Foundation (RU-G1-2571-ST-04 and RUB1-2860-ST-07), the Russian Fund of Basic Research (07-04-91110-AFGIRa) and the Russian Scientific Fund project 14-14-0015. L.M.W. and R.C.R. acknowledge support from the Ohio University Heritage College of Osteopathic Medicine and the National Science Foundation (IBN-0343744, IOB-0517257, IOS-1050154). The Ohio Supercomputing Center provided additional support. NR 48 TC 8 Z9 8 U1 0 U2 3 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 530 WALNUT STREET, STE 850, PHILADELPHIA, PA 19106 USA SN 0272-4634 EI 1937-2809 J9 J VERTEBR PALEONTOL JI J. Vertebr. Paleontol. PD JAN 2 PY 2015 VL 35 IS 1 AR e889145 DI 10.1080/02724634.2014.889145 PG 14 WC Paleontology SC Paleontology GA CL4GV UT WOS:000356911500019 ER PT J AU Fitzpatrick, SM Rick, TC AF Fitzpatrick, Scott M. Rick, Torben C. TI JICA Celebrates its Tenth Anniversary SO JOURNAL OF ISLAND & COASTAL ARCHAEOLOGY LA English DT Editorial Material C1 [Fitzpatrick, Scott M.] 1218 Univ Oregon, Dept Anthropol, Eugene, OR 97403 USA. [Rick, Torben C.] Smithsonian Inst, Dept Anthropol, Program Human Ecol & Archaeobiol, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Fitzpatrick, SM (reprint author), 1218 Univ Oregon, Dept Anthropol, 308 Condon Hall, Eugene, OR 97403 USA. EM smfitzpa@cas.uoregon.edu; rickt@si.edu NR 0 TC 3 Z9 3 U1 0 U2 2 PU ROUTLEDGE JOURNALS, TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXFORDSHIRE, ENGLAND SN 1556-4894 EI 1556-1828 J9 J ISL COAST ARCHAEOL JI J. Isl. Coast. Archaeol. PD JAN 2 PY 2015 VL 10 IS 1 BP 1 EP 2 DI 10.1080/15564894.2015.1029361 PG 2 WC Archaeology SC Archaeology GA CF1LC UT WOS:000352305800001 ER PT J AU Fitzpatrick, SM Rick, TC Erlandson, JM AF Fitzpatrick, Scott M. Rick, Torben C. Erlandson, Jon M. TI Recent Progress, Trends, and Developments in Island and Coastal Archaeology SO JOURNAL OF ISLAND & COASTAL ARCHAEOLOGY LA English DT Article DE littoral; aquatic adaptations; model systems; maritime prehistory; insularity; seafaring ID CALIFORNIA CHANNEL-ISLANDS; SAN-MIGUEL ISLAND; COMPLEX HUNTER-GATHERERS; DIEPKLOOF ROCK SHELTER; MIDDLE STONE-AGE; SOUTH-AFRICA; HUMAN IMPACTS; LESSER-ANTILLES; WEST-INDIES; BASE-LINE AB In the first issue of the Journal of Island & Coastal Archaeology published 10years ago, Erlandson and Fitzpatrick (2006) outlined eight topics which demonstrated why island and coastal archaeology were relevant to understanding a host of issues related to human cultural and biological evolution across time and space. Here, we evaluate recent trends and developments in island and coastal archaeology and discuss how research over the last decade has changed and continued to illuminate the antiquity of maritime adaptations, human dispersals, historical ecology, and many other issues on a global scale. With rising seas and marine erosion threatening island and coastal archaeological sites around the world, archaeologists face urgent challenges in the coming decades as we continue to promote research and conservation of the global island and coastal archaeological record. C1 [Fitzpatrick, Scott M.; Erlandson, Jon M.] Univ Oregon, Dept Anthropol, Eugene, OR 97403 USA. [Rick, Torben C.] Smithsonian Inst, Dept Anthropol, Washington, DC 20560 USA. [Erlandson, Jon M.] Univ Oregon, Museum Nat & Cultural Hist, Eugene, OR 97403 USA. RP Fitzpatrick, SM (reprint author), Univ Oregon, Dept Anthropol, 308 Condon Hall, Eugene, OR 97403 USA. EM smfitzpa@uoregon.edu OI Erlandson, Jon/0000-0002-4705-4319 NR 194 TC 3 Z9 3 U1 5 U2 12 PU ROUTLEDGE JOURNALS, TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXFORDSHIRE, ENGLAND SN 1556-4894 EI 1556-1828 J9 J ISL COAST ARCHAEOL JI J. Isl. Coast. Archaeol. PD JAN 2 PY 2015 VL 10 IS 1 BP 3 EP 27 DI 10.1080/15564894.2015.1013647 PG 25 WC Archaeology SC Archaeology GA CF1LC UT WOS:000352305800002 ER PT J AU Deutsch, JI AF Deutsch, James I. TI Hollywood exiles in Europe: the blacklist and Cold War film culture SO HISTORICAL JOURNAL OF FILM RADIO AND TELEVISION LA English DT Book Review C1 [Deutsch, James I.] Smithsonian Inst, Washington, DC 20560 USA. RP Deutsch, JI (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 1 PU ROUTLEDGE JOURNALS, TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXFORDSHIRE, ENGLAND SN 0143-9685 EI 1465-3451 J9 HIST J FILM RADIO TV JI Hist. J. Film Radio Telev. PD JAN 2 PY 2015 VL 35 IS 1 BP 199 EP 200 DI 10.1080/01439685.2014.997576 PG 2 WC Film, Radio, Television SC Film, Radio & Television GA CA7KD UT WOS:000349095300010 ER PT S AU Krutak, L AF Krutak, Lars BE Serup, J Kluger, N Baumler, W TI The Cultural Heritage of Tattooing: A Brief History SO TATTOOED SKIN AND HEALTH SE Current Problems in Dermatology LA English DT Article; Book Chapter ID STIMULATION; HORMESIS AB For millennia, peoples around the world have tattooed human skin to communicate various ontological, psychosocial, and sociocultural concepts encompassing beauty, cultural identity, status and position, medicine, and supernatural protection. As a system of knowledge transmission, tattooing has been and continues to be a visual language of the skin whereby culture is inscribed, experienced, and preserved in a myriad of specific ways. If we are to fully comprehend the meanings that tattoos have carried across human history and into the present, then it would be useful to explore some of the ways tattoos, as instruments that transmit culture, have been deployed cross-culturally through time. (C) 2015 S. Karger AG, Basel C1 [Krutak, Lars] Smithsonian Inst, Natl Museum Nat Hist, Repatriat Off, 10th & Constitut Ave NW,MRC 138,POB 37012, Washington, DC 20560 USA. RP Krutak, L (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Repatriat Off, 10th & Constitut Ave NW,MRC 138,POB 37012, Washington, DC 20560 USA. EM larskrutak@gmail.com NR 23 TC 0 Z9 0 U1 0 U2 4 PU KARGER PI BASEL PA POSTFACH, CH-4009 BASEL, SWITZERLAND SN 1421-5721 BN 978-3-318-02777-8; 978-3-318-02776-1 J9 CURR PROBL DERMATOL JI Curr.Probl.Dermatol. PY 2015 VL 48 BP 1 EP 5 DI 10.1159/000369174 D2 10.1159/isbn.978-3-318-02777-8 PG 5 WC Dermatology SC Dermatology GA BG2CP UT WOS:000387252500002 PM 25833618 ER PT B AU Bell, JA West, P Filer, C AF Bell, Joshua A. West, Paige Filer, Colin BE Bell, JA West, P Filer, C TI TROPICAL FORESTS OCEANIA Anthropological Perspectives Introduction SO TROPICAL FORESTS OF OCEANIA: ANTHROPOLOGICAL PERSPECTIVES SE Asia-Pacific Environment Monograph LA English DT Editorial Material; Book Chapter ID PAPUA-NEW-GUINEA; SOLOMON-ISLANDS; OIL PALM; PROPERTY; DEFORESTATION; CONSERVATION; PACIFIC; ECOLOGY; DIVERSITY; INDONESIA C1 [Bell, Joshua A.] Smithsonian Inst, Natl Museum Nat Hist, Globalizat, Washington, DC 20560 USA. [West, Paige] Barnard Coll, Anthropol, New York, NY USA. [West, Paige] Columbia Univ, New York, NY 10027 USA. [Filer, Colin] Australian Natl Univ, Crawford Sch Publ Policy, Canberra, ACT 0200, Australia. RP Bell, JA (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Globalizat, Washington, DC 20560 USA. NR 139 TC 0 Z9 0 U1 1 U2 1 PU AUSTRALIAN NATL UNIV PI CANBERRA ACT PA P O BOX 4, 2600 CANBERRA ACT, AUSTRALIA BN 978-1-925022-72-8; 978-1-925022-73-5 J9 ASIA-PAC ENV MONOGR PY 2015 VL 10 BP 1 EP 21 PG 21 WC Anthropology; Environmental Studies SC Anthropology; Environmental Sciences & Ecology GA BG0QK UT WOS:000386468800001 ER PT B AU Bell, JA AF Bell, Joshua A. BE Bell, JA West, P Filer, C TI The Structural Violence of Resource Extraction in the Purari Delta SO TROPICAL FORESTS OF OCEANIA: ANTHROPOLOGICAL PERSPECTIVES SE Asia-Pacific Environment Monograph LA English DT Article; Book Chapter ID PAPUA-NEW-GUINEA; INDONESIA; RIVER; WEST C1 [Bell, Joshua A.] Smithsonian Inst, Natl Museum Nat Hist, Globalizat, Washington, DC 20560 USA. RP Bell, JA (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Globalizat, Washington, DC 20560 USA. NR 64 TC 1 Z9 1 U1 1 U2 1 PU AUSTRALIAN NATL UNIV PI CANBERRA ACT PA P O BOX 4, 2600 CANBERRA ACT, AUSTRALIA BN 978-1-925022-72-8; 978-1-925022-73-5 J9 ASIA-PAC ENV MONOGR PY 2015 VL 10 BP 127 EP 153 PG 27 WC Anthropology; Environmental Studies SC Anthropology; Environmental Sciences & Ecology GA BG0QK UT WOS:000386468800006 ER PT B AU Ryan, C Brown, KF AF Ryan, Charlotte Brown, Kimberly Freeman BE Hansen, A Cox, R TI TO ACT IN CONCERT Environmental communication from a social movement lens SO ROUTLEDGE HANDBOOK OF ENVIRONMENT AND COMMUNICATION SE Routledge International Handbooks LA English DT Article; Book Chapter ID PUBLIC-HEALTH; CAMPAIGNS; ADVOCACY; POLICY C1 [Ryan, Charlotte] Univ Massachusetts Lowell, Sociol, Lowell, MA 01852 USA. [Ryan, Charlotte] Climate Change Initiat, Lowell, MA USA. [Brown, Kimberly Freeman] Green All, Oakland, CA USA. [Ryan, Charlotte] Smithsonian Inst, Washington, DC 20560 USA. [Brown, Kimberly Freeman] Childrens Def Fund, Washington, DC USA. RP Ryan, C (reprint author), Univ Massachusetts Lowell, Sociol, Lowell, MA 01852 USA. NR 60 TC 0 Z9 0 U1 0 U2 0 PU ROUTLEDGE PI ABINGDON PA 2 PARK SQ, MILTON PARK, ABINGDON OX14 4RN, OXFORD, ENGLAND BN 978-1-315-88758-6; 978-0-415-70435-9 J9 ROUT INT HANDB PY 2015 BP 131 EP 143 PG 13 WC Communication; Environmental Studies SC Communication; Environmental Sciences & Ecology GA BF7AH UT WOS:000383883800011 ER PT J AU Krstovski, K Smith, DA Kurtz, MJ AF Krstovski, Kriste Smith, David A. Kurtz, Michael J. GP ACM TI Evaluating Retrieval Models through Histogram Analysis SO SIGIR 2015: PROCEEDINGS OF THE 38TH INTERNATIONAL ACM SIGIR CONFERENCE ON RESEARCH AND DEVELOPMENT IN INFORMATION RETRIEVAL LA English DT Proceedings Paper CT 38th Annual International ACM SIGIR Conference on Research and Development in Information Retrieval (SIGIR) CY AUG 09-13, 2015 CL Santiago, CHILE SP Assoc Comp Machinery Special Interest Grp Informat Retrieval DE efficient evaluation; retrieval models; topic models AB We present a novel approach for efficiently evaluating the performance of retrieval models and introduce two evaluation metrics: Distributional Overlap (DO), which compares the clustering of scores of relevant and non-relevant documents, and Histogram Slope Analysis (HSA), which examines the log of the empirical distributions of relevant and non-relevant documents. Unlike rank evaluation metrics such as mean average precision (MAP) and normalized discounted cumulative gain (NDCG), DO and HSA only require calculating model scores of queries and a fixed sample of relevant and non-relevant documents rather than scoring the entire collection, even implicitly by means of an inverted index. In experimental meta-evaluations, we find that HSA achieves high correlation with MAP and NDCG on a monolingual and a cross-language document similarity task; on four ad-hoc web retrieval tasks; and on an analysis of ten TREC tasks from the past ten years. In addition, when evaluating latent Dirichlet allocation (LDA) models on document similarity tasks, HSA achieves better correlation with MAP and NCDG than perplexity, an intrinsic metric widely used with topic models. C1 [Krstovski, Kriste] Univ Massachusetts, Coll Informat & Comp Sci, Amherst, MA 01003 USA. [Smith, David A.] Northeastern Univ, Coll Comp & Informat Sci, Boston, MA 02115 USA. [Krstovski, Kriste; Kurtz, Michael J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Krstovski, K (reprint author), Univ Massachusetts, Coll Informat & Comp Sci, Amherst, MA 01003 USA. EM kriste@cs.umass.edu; zdasmith@ccs.neu.edu; kurtz@cfa.harvard.edu NR 10 TC 0 Z9 0 U1 0 U2 0 PU ASSOC COMPUTING MACHINERY PI NEW YORK PA 1515 BROADWAY, NEW YORK, NY 10036-9998 USA BN 978-1-4503-3621-5 PY 2015 BP 859 EP 862 DI 10.1145/2766462.2767821 PG 4 WC Computer Science, Theory & Methods; Engineering, Electrical & Electronic SC Computer Science; Engineering GA BF5NJ UT WOS:000382307300110 ER PT J AU Loi, ST Murphy, T Cairns, IH Trott, CM Bell, ME Hurley-Walker, N Morgan, J Lenc, E Offringa, AR Menk, FW Waters, CL Feng, L Hancock, PJ Kaplan, DL Kudryavtseva, N Lonsdale, CJ Erickson, P Coster, A Ekers, RD Bernardi, G Bowman, JD Briggs, F Cappallo, RJ Deshpande, AA Gaensler, BM Greenhill, LJ Hazelton, BJ Johnston-Hollitt, M McWhirter, SR Mitchell, DA Morales, MF Morgan, E Oberoi, D Ord, SM Prabu, T Shankar, NU Srivani, KS Subrahmanyan, R Tingay, SJ Wayth, RB Webster, RL Williams, A Williams, CL AF Loi, Shyeh Tjing Murphy, Tara Cairns, Iver H. Trott, Cathryn M. Bell, Martin E. Hurley-Walker, Natasha Morgan, John Lenc, Emil Offringa, Andre R. Menk, Frederick W. Waters, Colin L. Feng, Lu Hancock, Paul J. Kaplan, David L. Kudryavtseva, Nadia Lonsdale, Colin J. Erickson, Philip Coster, Anthea Ekers, Ronald D. Bernardi, G. Bowman, J. D. Briggs, F. Cappallo, R. J. Deshpande, A. A. Gaensler, B. M. Greenhill, L. J. Hazelton, B. J. Johnston-Hollitt, M. McWhirter, S. R. Mitchell, D. A. Morales, M. F. Morgan, E. Oberoi, D. Ord, S. M. Prabu, T. Shankar, N. Udaya Srivani, K. S. Subrahmanyan, R. Tingay, S. J. Wayth, R. B. Webster, R. L. Williams, A. Williams, C. L. GP IEEE TI Waves in the sky: Probing the ionosphere with the Murchison Widefield Array SO 2015 1st URSI Atlantic Radio Science Conference (URSI AT-RASC) LA English DT Proceedings Paper CT 1st URSI Atlantic Radio Science Conference (URSI AT-RASC) CY MAY 16-24, 2015 CL Gran Canaria, SPAIN C1 [Loi, Shyeh Tjing; Murphy, Tara; Cairns, Iver H.; Lenc, Emil] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia. [Loi, Shyeh Tjing; Murphy, Tara; Trott, Cathryn M.; Bell, Martin E.; Lenc, Emil; Hancock, Paul J.; Briggs, F.; Gaensler, B. M.; Mitchell, D. A.; Ord, S. M.; Subrahmanyan, R.; Tingay, S. J.; Wayth, R. B.; Webster, R. L.] ARC Ctr All Sky Astrophys CAASTRO, Redfern, NSW, Australia. [Trott, Cathryn M.; Hurley-Walker, Natasha; Morgan, John; Hancock, Paul J.; Kudryavtseva, Nadia; Ord, S. M.; Tingay, S. J.; Wayth, R. B.; Williams, A.] Curtin Univ, Int Ctr Radio Astron Res, Bentley, WA 6102, Australia. [Bell, Martin E.; Ekers, Ronald D.; Mitchell, D. A.] CASS, Epping, NSW 1710, Australia. [Offringa, Andre R.; Briggs, F.] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia. [Menk, Frederick W.; Waters, Colin L.] Univ Newcastle, Sch Math & Phys Sci, Callaghan, NSW 2308, Australia. [Feng, Lu; Morgan, E.; Williams, C. L.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Kaplan, David L.] Univ Wisconsin, Dept Phys, Milwaukee, WI 53201 USA. [Lonsdale, Colin J.; Erickson, Philip; Coster, Anthea; Cappallo, R. J.; McWhirter, S. R.] MIT, Haystack Observ, Westford, MA 01886 USA. [Bernardi, G.] SKA SA, ZA-7405 Cape Town, South Africa. [Bernardi, G.; Greenhill, L. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bowman, J. D.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Deshpande, A. A.; Prabu, T.; Shankar, N. Udaya; Srivani, K. S.; Subrahmanyan, R.] Raman Res Inst, Bangalore 560080, Karnataka, India. [Hazelton, B. J.; Morales, M. F.] Univ Washington, Dept Phys, Seattle, WA 98195 USA. [Johnston-Hollitt, M.] Victoria Univ Wellington, Sch Chem & Phys Sci, Wellington 6140, New Zealand. [Oberoi, D.] Tata Inst Fundamental Res, Natl Ctr Radio Astrophys, Pune 411007, Maharashtra, India. [Webster, R. L.] Univ Melbourne, Sch Phys, Parkville, Vic 3010, Australia. RP Loi, ST (reprint author), Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia. RI Deshpande, Avinash/D-4868-2012; Udayashankar , N/D-4901-2012 NR 0 TC 0 Z9 0 U1 1 U2 1 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA BN 978-9-0900-8628-6 PY 2015 PG 2 WC Engineering, Electrical & Electronic; Remote Sensing SC Engineering; Remote Sensing GA BF3OZ UT WOS:000380563800382 ER PT J AU Vertatschitsch, LE Primiani, R Weintroub, J AF Vertatschitsch, Laura E. Primiani, Rurik Weintroub, Jonathan GP IEEE TI Toward 64 Gbps Wideband Digital Backend Design for the Event Horizon Telescope SO 2015 1st URSI Atlantic Radio Science Conference (URSI AT-RASC) LA English DT Proceedings Paper CT 1st URSI Atlantic Radio Science Conference (URSI AT-RASC) CY MAY 16-24, 2015 CL Gran Canaria, SPAIN C1 [Vertatschitsch, Laura E.; Primiani, Rurik; Weintroub, Jonathan] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RP Vertatschitsch, LE (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA BN 978-9-0900-8628-6 PY 2015 PG 1 WC Engineering, Electrical & Electronic; Remote Sensing SC Engineering; Remote Sensing GA BF3OZ UT WOS:000380563800359 ER PT B AU Odo, F AF Odo, Franklin BA Hoshida, G Hoshida, T BF Hoshida, G Hoshida, T BE Kim, H TI Departure to Hawaii SO TAKEN FROM THE PARADISE ISLE: THE HOSHIDA FAMILY STORY, 1912-1945 SE Nikkei in the Americas LA English DT Article; Book Chapter C1 [Odo, Franklin] Smithsonian Inst, Asian Pacific Amer Ctr, Washington, DC 20560 USA. [Odo, Franklin] Lib Congress, Asian Div, Washington, DC 20540 USA. [Odo, Franklin] Univ Hawaii, Honolulu, HI 96822 USA. [Odo, Franklin] Univ Penn, Philadelphia, PA 19104 USA. [Odo, Franklin] CUNY Hunter Coll, New York, NY 10021 USA. [Odo, Franklin] Princeton Univ, Princeton, NJ 08544 USA. [Odo, Franklin] Columbia Univ, New York, NY 10027 USA. RP Odo, F (reprint author), Smithsonian Inst, Asian Pacific Amer Ctr, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU UNIV PRESS COLORADO PI BOULDER PA 5589 ARAPAHOE AVE, STE 206C, BOULDER, CO 80303 USA BN 978-1-60732-344-0; 978-1-60732-339-6 J9 NIKKEI AMER PY 2015 BP 1 EP 3 DI 10.5876/9781607323440.c001 PG 3 WC History SC History GA BF0CT UT WOS:000378538000004 ER PT B AU Odo, F AF Odo, Franklin BA Hoshida, G Hoshida, T BF Hoshida, G Hoshida, T BE Kim, H TI Hawaii Their Destination (Family Journeys to the Big Island) SO TAKEN FROM THE PARADISE ISLE: THE HOSHIDA FAMILY STORY, 1912-1945 SE Nikkei in the Americas LA English DT Article; Book Chapter C1 [Odo, Franklin] Smithsonian Inst, Asian Pacific Amer Ctr, Washington, DC 20560 USA. [Odo, Franklin] Lib Congress, Asian Div, Washington, DC 20540 USA. [Odo, Franklin] Univ Hawaii, Honolulu, HI 96822 USA. [Odo, Franklin] Univ Penn, Philadelphia, PA 19104 USA. [Odo, Franklin] CUNY Hunter Coll, New York, NY 10021 USA. [Odo, Franklin] Princeton Univ, Princeton, NJ 08544 USA. [Odo, Franklin] Columbia Univ, New York, NY 10027 USA. RP Odo, F (reprint author), Smithsonian Inst, Asian Pacific Amer Ctr, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU UNIV PRESS COLORADO PI BOULDER PA 5589 ARAPAHOE AVE, STE 206C, BOULDER, CO 80303 USA BN 978-1-60732-344-0; 978-1-60732-339-6 J9 NIKKEI AMER PY 2015 BP 5 EP 7 DI 10.5876/9781607323440.c002 PG 3 WC History SC History GA BF0CT UT WOS:000378538000005 ER PT B AU Odo, F AF Odo, Franklin BA Hoshida, G Hoshida, T BF Hoshida, G Hoshida, T BE Kim, H TI Father Becomes a Sugar Cane Planter SO TAKEN FROM THE PARADISE ISLE: THE HOSHIDA FAMILY STORY, 1912-1945 SE Nikkei in the Americas LA English DT Article; Book Chapter C1 [Odo, Franklin] Smithsonian Inst, Asian Pacific Amer Ctr, Washington, DC 20560 USA. [Odo, Franklin] Lib Congress, Asian Div, Washington, DC 20540 USA. [Odo, Franklin] Univ Hawaii, Honolulu, HI 96822 USA. [Odo, Franklin] Univ Penn, Philadelphia, PA 19104 USA. [Odo, Franklin] CUNY Hunter Coll, New York, NY 10021 USA. [Odo, Franklin] Princeton Univ, Princeton, NJ 08544 USA. [Odo, Franklin] Columbia Univ, New York, NY 10027 USA. RP Odo, F (reprint author), Smithsonian Inst, Asian Pacific Amer Ctr, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU UNIV PRESS COLORADO PI BOULDER PA 5589 ARAPAHOE AVE, STE 206C, BOULDER, CO 80303 USA BN 978-1-60732-344-0; 978-1-60732-339-6 J9 NIKKEI AMER PY 2015 BP 9 EP 10 DI 10.5876/9781607323440.c003 PG 2 WC History SC History GA BF0CT UT WOS:000378538000006 ER PT B AU Odo, F AF Odo, Franklin BA Hoshida, G Hoshida, T BF Hoshida, G Hoshida, T BE Kim, H TI Boyhood Days in the Country SO TAKEN FROM THE PARADISE ISLE: THE HOSHIDA FAMILY STORY, 1912-1945 SE Nikkei in the Americas LA English DT Article; Book Chapter C1 [Odo, Franklin] Smithsonian Inst, Asian Pacific Amer Ctr, Washington, DC 20560 USA. [Odo, Franklin] Lib Congress, Asian Div, Washington, DC 20540 USA. [Odo, Franklin] Univ Hawaii, Honolulu, HI 96822 USA. [Odo, Franklin] Univ Penn, Philadelphia, PA 19104 USA. [Odo, Franklin] CUNY Hunter Coll, New York, NY 10021 USA. [Odo, Franklin] Princeton Univ, Princeton, NJ 08544 USA. [Odo, Franklin] Columbia Univ, New York, NY 10027 USA. RP Odo, F (reprint author), Smithsonian Inst, Asian Pacific Amer Ctr, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU UNIV PRESS COLORADO PI BOULDER PA 5589 ARAPAHOE AVE, STE 206C, BOULDER, CO 80303 USA BN 978-1-60732-344-0; 978-1-60732-339-6 J9 NIKKEI AMER PY 2015 BP 11 EP 13 DI 10.5876/9781607323440.c004 PG 3 WC History SC History GA BF0CT UT WOS:000378538000007 ER PT B AU Odo, F AF Odo, Franklin BA Hoshida, G Hoshida, T BF Hoshida, G Hoshida, T BE Kim, H TI End of Schooling and Start of Work SO TAKEN FROM THE PARADISE ISLE: THE HOSHIDA FAMILY STORY, 1912-1945 SE Nikkei in the Americas LA English DT Article; Book Chapter C1 [Odo, Franklin] Smithsonian Inst, Asian Pacific Amer Ctr, Washington, DC 20560 USA. [Odo, Franklin] Lib Congress, Asian Div, Washington, DC 20540 USA. [Odo, Franklin] Univ Hawaii, Honolulu, HI 96822 USA. [Odo, Franklin] Univ Penn, Philadelphia, PA 19104 USA. [Odo, Franklin] CUNY Hunter Coll, New York, NY 10021 USA. [Odo, Franklin] Princeton Univ, Princeton, NJ 08544 USA. [Odo, Franklin] Columbia Univ, New York, NY 10027 USA. RP Odo, F (reprint author), Smithsonian Inst, Asian Pacific Amer Ctr, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU UNIV PRESS COLORADO PI BOULDER PA 5589 ARAPAHOE AVE, STE 206C, BOULDER, CO 80303 USA BN 978-1-60732-344-0; 978-1-60732-339-6 J9 NIKKEI AMER PY 2015 BP 15 EP 17 DI 10.5876/9781607323440.c005 PG 3 WC History SC History GA BF0CT UT WOS:000378538000008 ER PT B AU Odo, F AF Odo, Franklin BA Hoshida, G Hoshida, T BF Hoshida, G Hoshida, T BE Kim, H TI Taken from the Paradise Isle The Hoshida Family Story, 1912-1945 Foreword SO TAKEN FROM THE PARADISE ISLE: THE HOSHIDA FAMILY STORY, 1912-1945 SE Nikkei in the Americas LA English DT Editorial Material; Book Chapter C1 [Odo, Franklin] Smithsonian Inst, Asian Pacific Amer Ctr, Washington, DC 20560 USA. [Odo, Franklin] Lib Congress, Asian Div, Washington, DC 20540 USA. [Odo, Franklin] Univ Hawaii, Honolulu, HI 96822 USA. [Odo, Franklin] Univ Penn, Philadelphia, PA 19104 USA. [Odo, Franklin] CUNY Hunter Coll, New York, NY 10021 USA. [Odo, Franklin] Princeton Univ, Princeton, NJ 08544 USA. [Odo, Franklin] Columbia Univ, New York, NY 10027 USA. RP Odo, F (reprint author), Smithsonian Inst, Asian Pacific Amer Ctr, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU UNIV PRESS COLORADO PI BOULDER PA 5589 ARAPAHOE AVE, STE 206C, BOULDER, CO 80303 USA BN 978-1-60732-344-0; 978-1-60732-339-6 J9 NIKKEI AMER PY 2015 BP XV EP XVIII PG 4 WC History SC History GA BF0CT UT WOS:000378538000001 ER PT B AU Odo, F AF Odo, Franklin BA Hoshida, G Hoshida, T BF Hoshida, G Hoshida, T BE Kim, H TI YBA Convention and Trip to Kauai SO TAKEN FROM THE PARADISE ISLE: THE HOSHIDA FAMILY STORY, 1912-1945 SE Nikkei in the Americas LA English DT Article; Book Chapter C1 [Odo, Franklin] Smithsonian Inst, Asian Pacific Amer Ctr, Washington, DC 20560 USA. [Odo, Franklin] Lib Congress, Asian Div, Washington, DC 20540 USA. [Odo, Franklin] Univ Hawaii, Honolulu, HI 96822 USA. [Odo, Franklin] Univ Penn, Philadelphia, PA 19104 USA. [Odo, Franklin] CUNY Hunter Coll, New York, NY 10021 USA. [Odo, Franklin] Princeton Univ, Princeton, NJ 08544 USA. [Odo, Franklin] Columbia Univ, New York, NY 10027 USA. RP Odo, F (reprint author), Smithsonian Inst, Asian Pacific Amer Ctr, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU UNIV PRESS COLORADO PI BOULDER PA 5589 ARAPAHOE AVE, STE 206C, BOULDER, CO 80303 USA BN 978-1-60732-344-0; 978-1-60732-339-6 J9 NIKKEI AMER PY 2015 BP 19 EP 20 DI 10.5876/9781607323440.c006 PG 2 WC History SC History GA BF0CT UT WOS:000378538000009 ER PT B AU Odo, F AF Odo, Franklin BA Hoshida, G Hoshida, T BF Hoshida, G Hoshida, T BE Kim, H TI Dawn of Romance and Marriage SO TAKEN FROM THE PARADISE ISLE: THE HOSHIDA FAMILY STORY, 1912-1945 SE Nikkei in the Americas LA English DT Article; Book Chapter C1 [Odo, Franklin] Smithsonian Inst, Asian Pacific Amer Ctr, Washington, DC 20560 USA. [Odo, Franklin] Lib Congress, Asian Div, Washington, DC 20540 USA. [Odo, Franklin] Univ Hawaii, Honolulu, HI 96822 USA. [Odo, Franklin] Univ Penn, Philadelphia, PA 19104 USA. [Odo, Franklin] CUNY Hunter Coll, New York, NY 10021 USA. [Odo, Franklin] Princeton Univ, Princeton, NJ 08544 USA. [Odo, Franklin] Columbia Univ, New York, NY 10027 USA. RP Odo, F (reprint author), Smithsonian Inst, Asian Pacific Amer Ctr, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU UNIV PRESS COLORADO PI BOULDER PA 5589 ARAPAHOE AVE, STE 206C, BOULDER, CO 80303 USA BN 978-1-60732-344-0; 978-1-60732-339-6 J9 NIKKEI AMER PY 2015 BP 21 EP 25 DI 10.5876/9781607323440.c007 PG 5 WC History SC History GA BF0CT UT WOS:000378538000010 ER PT B AU Odo, F AF Odo, Franklin BA Hoshida, G Hoshida, T BF Hoshida, G Hoshida, T BE Kim, H TI Taken from the Paradise Isle The Hoshida Family Story, 1912-1945 Introduction SO TAKEN FROM THE PARADISE ISLE: THE HOSHIDA FAMILY STORY, 1912-1945 SE Nikkei in the Americas LA English DT Editorial Material; Book Chapter C1 [Odo, Franklin] Smithsonian Inst, Asian Pacific Amer Ctr, Washington, DC 20560 USA. [Odo, Franklin] Lib Congress, Asian Div, Washington, DC 20540 USA. [Odo, Franklin] Univ Hawaii, Honolulu, HI 96822 USA. [Odo, Franklin] Univ Penn, Philadelphia, PA 19104 USA. [Odo, Franklin] CUNY Hunter Coll, New York, NY 10021 USA. [Odo, Franklin] Princeton Univ, Princeton, NJ 08544 USA. [Odo, Franklin] Columbia Univ, New York, NY 10027 USA. RP Odo, F (reprint author), Smithsonian Inst, Asian Pacific Amer Ctr, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU UNIV PRESS COLORADO PI BOULDER PA 5589 ARAPAHOE AVE, STE 206C, BOULDER, CO 80303 USA BN 978-1-60732-344-0; 978-1-60732-339-6 J9 NIKKEI AMER PY 2015 BP XXI EP XXXII PG 12 WC History SC History GA BF0CT UT WOS:000378538000002 ER PT B AU Odo, F AF Odo, Franklin BA Hoshida, G Hoshida, T BF Hoshida, G Hoshida, T BE Kim, H TI Tragedy and Awakening to Reality SO TAKEN FROM THE PARADISE ISLE: THE HOSHIDA FAMILY STORY, 1912-1945 SE Nikkei in the Americas LA English DT Article; Book Chapter C1 [Odo, Franklin] Smithsonian Inst, Asian Pacific Amer Ctr, Washington, DC 20560 USA. [Odo, Franklin] Lib Congress, Asian Div, Washington, DC 20540 USA. [Odo, Franklin] Univ Hawaii, Honolulu, HI 96822 USA. [Odo, Franklin] Univ Penn, Philadelphia, PA 19104 USA. [Odo, Franklin] CUNY Hunter Coll, New York, NY 10021 USA. [Odo, Franklin] Princeton Univ, Princeton, NJ 08544 USA. [Odo, Franklin] Columbia Univ, New York, NY 10027 USA. RP Odo, F (reprint author), Smithsonian Inst, Asian Pacific Amer Ctr, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU UNIV PRESS COLORADO PI BOULDER PA 5589 ARAPAHOE AVE, STE 206C, BOULDER, CO 80303 USA BN 978-1-60732-344-0; 978-1-60732-339-6 J9 NIKKEI AMER PY 2015 BP 27 EP 29 DI 10.5876/9781607323440.c008 PG 3 WC History SC History GA BF0CT UT WOS:000378538000011 ER PT B AU Odo, F AF Odo, Franklin BA Hoshida, G Hoshida, T BF Hoshida, G Hoshida, T BE Kim, H TI New Life and a New Home SO TAKEN FROM THE PARADISE ISLE: THE HOSHIDA FAMILY STORY, 1912-1945 SE Nikkei in the Americas LA English DT Article; Book Chapter C1 [Odo, Franklin] Smithsonian Inst, Asian Pacific Amer Ctr, Washington, DC 20560 USA. [Odo, Franklin] Lib Congress, Asian Div, Washington, DC 20540 USA. [Odo, Franklin] Univ Hawaii, Honolulu, HI 96822 USA. [Odo, Franklin] Univ Penn, Philadelphia, PA 19104 USA. [Odo, Franklin] CUNY Hunter Coll, New York, NY 10021 USA. [Odo, Franklin] Princeton Univ, Princeton, NJ 08544 USA. [Odo, Franklin] Columbia Univ, New York, NY 10027 USA. RP Odo, F (reprint author), Smithsonian Inst, Asian Pacific Amer Ctr, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU UNIV PRESS COLORADO PI BOULDER PA 5589 ARAPAHOE AVE, STE 206C, BOULDER, CO 80303 USA BN 978-1-60732-344-0; 978-1-60732-339-6 J9 NIKKEI AMER PY 2015 BP 31 EP 32 DI 10.5876/9781607323440.c009 PG 2 WC History SC History GA BF0CT UT WOS:000378538000012 ER PT B AU Odo, F AF Odo, Franklin BA Hoshida, G Hoshida, T BF Hoshida, G Hoshida, T BE Kim, H TI World War II SO TAKEN FROM THE PARADISE ISLE: THE HOSHIDA FAMILY STORY, 1912-1945 SE Nikkei in the Americas LA English DT Article; Book Chapter C1 [Odo, Franklin] Smithsonian Inst, Asian Pacific Amer Ctr, Washington, DC 20560 USA. [Odo, Franklin] Lib Congress, Asian Div, Washington, DC 20540 USA. [Odo, Franklin] Univ Hawaii, Honolulu, HI 96822 USA. [Odo, Franklin] Univ Penn, Philadelphia, PA 19104 USA. [Odo, Franklin] CUNY Hunter Coll, New York, NY 10021 USA. [Odo, Franklin] Princeton Univ, Princeton, NJ 08544 USA. [Odo, Franklin] Columbia Univ, New York, NY 10027 USA. RP Odo, F (reprint author), Smithsonian Inst, Asian Pacific Amer Ctr, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU UNIV PRESS COLORADO PI BOULDER PA 5589 ARAPAHOE AVE, STE 206C, BOULDER, CO 80303 USA BN 978-1-60732-344-0; 978-1-60732-339-6 J9 NIKKEI AMER PY 2015 BP 33 EP 38 DI 10.5876/9781607323440.c010 PG 6 WC History SC History GA BF0CT UT WOS:000378538000013 ER PT B AU Odo, F AF Odo, Franklin BA Hoshida, G Hoshida, T BF Hoshida, G Hoshida, T BE Kim, H TI Taken from the Paradise Isle The Hoshida Family Story, 1912-1945 SO TAKEN FROM THE PARADISE ISLE: THE HOSHIDA FAMILY STORY, 1912-1945 SE Nikkei in the Americas LA English DT Editorial Material; Book Chapter C1 [Odo, Franklin] Smithsonian Inst, Asian Pacific Amer Ctr, Washington, DC 20560 USA. [Odo, Franklin] Lib Congress, Asian Div, Washington, DC 20540 USA. [Odo, Franklin] Univ Hawaii, Honolulu, HI 96822 USA. [Odo, Franklin] Univ Penn, Philadelphia, PA 19104 USA. [Odo, Franklin] CUNY Hunter Coll, New York, NY 10021 USA. [Odo, Franklin] Princeton Univ, Princeton, NJ 08544 USA. [Odo, Franklin] Columbia Univ, New York, NY 10027 USA. RP Odo, F (reprint author), Smithsonian Inst, Asian Pacific Amer Ctr, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU UNIV PRESS COLORADO PI BOULDER PA 5589 ARAPAHOE AVE, STE 206C, BOULDER, CO 80303 USA BN 978-1-60732-344-0; 978-1-60732-339-6 J9 NIKKEI AMER PY 2015 BP XXXIII EP XXXV PG 3 WC History SC History GA BF0CT UT WOS:000378538000003 ER PT B AU Odo, F AF Odo, Franklin BA Hoshida, G Hoshida, T BF Hoshida, G Hoshida, T BE Kim, H TI Detention as Enemy Alien SO TAKEN FROM THE PARADISE ISLE: THE HOSHIDA FAMILY STORY, 1912-1945 SE Nikkei in the Americas LA English DT Article; Book Chapter C1 [Odo, Franklin] Smithsonian Inst, Asian Pacific Amer Ctr, Washington, DC 20560 USA. [Odo, Franklin] Lib Congress, Asian Div, Washington, DC 20540 USA. [Odo, Franklin] Univ Hawaii, Honolulu, HI 96822 USA. [Odo, Franklin] Univ Penn, Philadelphia, PA 19104 USA. [Odo, Franklin] CUNY Hunter Coll, New York, NY 10021 USA. [Odo, Franklin] Princeton Univ, Princeton, NJ 08544 USA. [Odo, Franklin] Columbia Univ, New York, NY 10027 USA. RP Odo, F (reprint author), Smithsonian Inst, Asian Pacific Amer Ctr, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU UNIV PRESS COLORADO PI BOULDER PA 5589 ARAPAHOE AVE, STE 206C, BOULDER, CO 80303 USA BN 978-1-60732-344-0; 978-1-60732-339-6 J9 NIKKEI AMER PY 2015 BP 39 EP 57 DI 10.5876/9781607323440.c011 PG 19 WC History SC History GA BF0CT UT WOS:000378538000014 ER PT B AU Odo, F AF Odo, Franklin BA Hoshida, G Hoshida, T BF Hoshida, G Hoshida, T BE Kim, H TI The Hearing SO TAKEN FROM THE PARADISE ISLE: THE HOSHIDA FAMILY STORY, 1912-1945 SE Nikkei in the Americas LA English DT Article; Book Chapter C1 [Odo, Franklin] Smithsonian Inst, Asian Pacific Amer Ctr, Washington, DC 20560 USA. [Odo, Franklin] Lib Congress, Asian Div, Washington, DC 20540 USA. [Odo, Franklin] Univ Hawaii, Honolulu, HI 96822 USA. [Odo, Franklin] Univ Penn, Philadelphia, PA 19104 USA. [Odo, Franklin] CUNY Hunter Coll, New York, NY 10021 USA. [Odo, Franklin] Princeton Univ, Princeton, NJ 08544 USA. [Odo, Franklin] Columbia Univ, New York, NY 10027 USA. RP Odo, F (reprint author), Smithsonian Inst, Asian Pacific Amer Ctr, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU UNIV PRESS COLORADO PI BOULDER PA 5589 ARAPAHOE AVE, STE 206C, BOULDER, CO 80303 USA BN 978-1-60732-344-0; 978-1-60732-339-6 J9 NIKKEI AMER PY 2015 BP 59 EP 72 DI 10.5876/9781607323440.c012 PG 14 WC History SC History GA BF0CT UT WOS:000378538000015 ER PT B AU Odo, F AF Odo, Franklin BA Hoshida, G Hoshida, T BF Hoshida, G Hoshida, T BE Kim, H TI Internment Camps SO TAKEN FROM THE PARADISE ISLE: THE HOSHIDA FAMILY STORY, 1912-1945 SE Nikkei in the Americas LA English DT Article; Book Chapter C1 [Odo, Franklin] Smithsonian Inst, Asian Pacific Amer Ctr, Washington, DC 20560 USA. [Odo, Franklin] Lib Congress, Asian Div, Washington, DC 20540 USA. [Odo, Franklin] Univ Hawaii, Honolulu, HI 96822 USA. [Odo, Franklin] Univ Penn, Philadelphia, PA 19104 USA. [Odo, Franklin] CUNY Hunter Coll, New York, NY 10021 USA. [Odo, Franklin] Princeton Univ, Princeton, NJ 08544 USA. [Odo, Franklin] Columbia Univ, New York, NY 10027 USA. RP Odo, F (reprint author), Smithsonian Inst, Asian Pacific Amer Ctr, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU UNIV PRESS COLORADO PI BOULDER PA 5589 ARAPAHOE AVE, STE 206C, BOULDER, CO 80303 USA BN 978-1-60732-344-0; 978-1-60732-339-6 J9 NIKKEI AMER PY 2015 BP 73 EP 82 DI 10.5876/9781607323440.c013 PG 10 WC History SC History GA BF0CT UT WOS:000378538000016 ER PT B AU Odo, F AF Odo, Franklin BA Hoshida, G Hoshida, T BF Hoshida, G Hoshida, T BE Kim, H TI Lordsburg Internment Camp SO TAKEN FROM THE PARADISE ISLE: THE HOSHIDA FAMILY STORY, 1912-1945 SE Nikkei in the Americas LA English DT Article; Book Chapter C1 [Odo, Franklin] Smithsonian Inst, Asian Pacific Amer Ctr, Washington, DC 20560 USA. [Odo, Franklin] Lib Congress, Asian Div, Washington, DC 20540 USA. [Odo, Franklin] Univ Hawaii, Honolulu, HI 96822 USA. [Odo, Franklin] Univ Penn, Philadelphia, PA 19104 USA. [Odo, Franklin] CUNY Hunter Coll, New York, NY 10021 USA. [Odo, Franklin] Princeton Univ, Princeton, NJ 08544 USA. [Odo, Franklin] Columbia Univ, New York, NY 10027 USA. RP Odo, F (reprint author), Smithsonian Inst, Asian Pacific Amer Ctr, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU UNIV PRESS COLORADO PI BOULDER PA 5589 ARAPAHOE AVE, STE 206C, BOULDER, CO 80303 USA BN 978-1-60732-344-0; 978-1-60732-339-6 J9 NIKKEI AMER PY 2015 BP 83 EP 131 DI 10.5876/9781607323440.c014 PG 49 WC History SC History GA BF0CT UT WOS:000378538000017 ER PT B AU Odo, F AF Odo, Franklin BA Hoshida, G Hoshida, T BF Hoshida, G Hoshida, T BE Kim, H TI A New Year in the Internment Camp SO TAKEN FROM THE PARADISE ISLE: THE HOSHIDA FAMILY STORY, 1912-1945 SE Nikkei in the Americas LA English DT Article; Book Chapter C1 [Odo, Franklin] Smithsonian Inst, Asian Pacific Amer Ctr, Washington, DC 20560 USA. [Odo, Franklin] Lib Congress, Asian Div, Washington, DC 20540 USA. [Odo, Franklin] Univ Hawaii, Honolulu, HI 96822 USA. [Odo, Franklin] Univ Penn, Philadelphia, PA 19104 USA. [Odo, Franklin] CUNY Hunter Coll, New York, NY 10021 USA. [Odo, Franklin] Princeton Univ, Princeton, NJ 08544 USA. [Odo, Franklin] Columbia Univ, New York, NY 10027 USA. RP Odo, F (reprint author), Smithsonian Inst, Asian Pacific Amer Ctr, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU UNIV PRESS COLORADO PI BOULDER PA 5589 ARAPAHOE AVE, STE 206C, BOULDER, CO 80303 USA BN 978-1-60732-344-0; 978-1-60732-339-6 J9 NIKKEI AMER PY 2015 BP 133 EP 141 DI 10.5876/9781607323440.c015 PG 9 WC History SC History GA BF0CT UT WOS:000378538000018 ER PT B AU Odo, F AF Odo, Franklin BA Hoshida, G Hoshida, T BF Hoshida, G Hoshida, T BE Kim, H TI {Tamae's Journey} SO TAKEN FROM THE PARADISE ISLE: THE HOSHIDA FAMILY STORY, 1912-1945 SE Nikkei in the Americas LA English DT Article; Book Chapter C1 [Odo, Franklin] Smithsonian Inst, Asian Pacific Amer Ctr, Washington, DC 20560 USA. [Odo, Franklin] Lib Congress, Asian Div, Washington, DC 20540 USA. [Odo, Franklin] Univ Hawaii, Honolulu, HI 96822 USA. [Odo, Franklin] Univ Penn, Philadelphia, PA 19104 USA. [Odo, Franklin] CUNY Hunter Coll, New York, NY 10021 USA. [Odo, Franklin] Princeton Univ, Princeton, NJ 08544 USA. [Odo, Franklin] Columbia Univ, New York, NY 10027 USA. RP Odo, F (reprint author), Smithsonian Inst, Asian Pacific Amer Ctr, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU UNIV PRESS COLORADO PI BOULDER PA 5589 ARAPAHOE AVE, STE 206C, BOULDER, CO 80303 USA BN 978-1-60732-344-0; 978-1-60732-339-6 J9 NIKKEI AMER PY 2015 BP 143 EP 156 DI 10.5876/9781607323440.c016 PG 14 WC History SC History GA BF0CT UT WOS:000378538000019 ER PT B AU Odo, F AF Odo, Franklin BA Hoshida, G Hoshida, T BF Hoshida, G Hoshida, T BE Kim, H TI {Waiting for Reunion} SO TAKEN FROM THE PARADISE ISLE: THE HOSHIDA FAMILY STORY, 1912-1945 SE Nikkei in the Americas LA English DT Article; Book Chapter C1 [Odo, Franklin] Smithsonian Inst, Asian Pacific Amer Ctr, Washington, DC 20560 USA. [Odo, Franklin] Lib Congress, Asian Div, Washington, DC 20540 USA. [Odo, Franklin] Univ Hawaii, Honolulu, HI 96822 USA. [Odo, Franklin] Univ Penn, Philadelphia, PA 19104 USA. [Odo, Franklin] CUNY Hunter Coll, New York, NY 10021 USA. [Odo, Franklin] Princeton Univ, Princeton, NJ 08544 USA. [Odo, Franklin] Columbia Univ, New York, NY 10027 USA. RP Odo, F (reprint author), Smithsonian Inst, Asian Pacific Amer Ctr, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU UNIV PRESS COLORADO PI BOULDER PA 5589 ARAPAHOE AVE, STE 206C, BOULDER, CO 80303 USA BN 978-1-60732-344-0; 978-1-60732-339-6 J9 NIKKEI AMER PY 2015 BP 157 EP 186 DI 10.5876/9781607323440.c017 PG 30 WC History SC History GA BF0CT UT WOS:000378538000020 ER PT B AU Odo, F AF Odo, Franklin BA Hoshida, G Hoshida, T BF Hoshida, G Hoshida, T BE Kim, H TI {Tamae and the Children in Jerome} SO TAKEN FROM THE PARADISE ISLE: THE HOSHIDA FAMILY STORY, 1912-1945 SE Nikkei in the Americas LA English DT Article; Book Chapter C1 [Odo, Franklin] Smithsonian Inst, Asian Pacific Amer Ctr, Washington, DC 20560 USA. [Odo, Franklin] Lib Congress, Asian Div, Washington, DC 20540 USA. [Odo, Franklin] Univ Hawaii, Honolulu, HI 96822 USA. [Odo, Franklin] Univ Penn, Philadelphia, PA 19104 USA. [Odo, Franklin] CUNY Hunter Coll, New York, NY 10021 USA. [Odo, Franklin] Princeton Univ, Princeton, NJ 08544 USA. [Odo, Franklin] Columbia Univ, New York, NY 10027 USA. RP Odo, F (reprint author), Smithsonian Inst, Asian Pacific Amer Ctr, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU UNIV PRESS COLORADO PI BOULDER PA 5589 ARAPAHOE AVE, STE 206C, BOULDER, CO 80303 USA BN 978-1-60732-344-0; 978-1-60732-339-6 J9 NIKKEI AMER PY 2015 BP 187 EP 198 DI 10.5876/9781607323440.c018 PG 12 WC History SC History GA BF0CT UT WOS:000378538000021 ER PT B AU Odo, F AF Odo, Franklin BA Hoshida, G Hoshida, T BF Hoshida, G Hoshida, T BE Kim, H TI At Santa Fe Detention Station SO TAKEN FROM THE PARADISE ISLE: THE HOSHIDA FAMILY STORY, 1912-1945 SE Nikkei in the Americas LA English DT Article; Book Chapter C1 [Odo, Franklin] Smithsonian Inst, Asian Pacific Amer Ctr, Washington, DC 20560 USA. [Odo, Franklin] Lib Congress, Asian Div, Washington, DC 20540 USA. [Odo, Franklin] Univ Hawaii, Honolulu, HI 96822 USA. [Odo, Franklin] Univ Penn, Philadelphia, PA 19104 USA. [Odo, Franklin] CUNY Hunter Coll, New York, NY 10021 USA. [Odo, Franklin] Princeton Univ, Princeton, NJ 08544 USA. [Odo, Franklin] Columbia Univ, New York, NY 10027 USA. RP Odo, F (reprint author), Smithsonian Inst, Asian Pacific Amer Ctr, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU UNIV PRESS COLORADO PI BOULDER PA 5589 ARAPAHOE AVE, STE 206C, BOULDER, CO 80303 USA BN 978-1-60732-344-0; 978-1-60732-339-6 J9 NIKKEI AMER PY 2015 BP 199 EP 214 DI 10.5876/9781607323440.c019 PG 16 WC History SC History GA BF0CT UT WOS:000378538000022 ER PT B AU Odo, F AF Odo, Franklin BA Hoshida, G Hoshida, T BF Hoshida, G Hoshida, T BE Kim, H TI Parole and Reunion with Family at Jerome Relocation Center SO TAKEN FROM THE PARADISE ISLE: THE HOSHIDA FAMILY STORY, 1912-1945 SE Nikkei in the Americas LA English DT Article; Book Chapter C1 [Odo, Franklin] Smithsonian Inst, Asian Pacific Amer Ctr, Washington, DC 20560 USA. [Odo, Franklin] Lib Congress, Asian Div, Washington, DC 20540 USA. [Odo, Franklin] Univ Hawaii, Honolulu, HI 96822 USA. [Odo, Franklin] Univ Penn, Philadelphia, PA 19104 USA. [Odo, Franklin] CUNY Hunter Coll, New York, NY 10021 USA. [Odo, Franklin] Princeton Univ, Princeton, NJ 08544 USA. [Odo, Franklin] Columbia Univ, New York, NY 10027 USA. RP Odo, F (reprint author), Smithsonian Inst, Asian Pacific Amer Ctr, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU UNIV PRESS COLORADO PI BOULDER PA 5589 ARAPAHOE AVE, STE 206C, BOULDER, CO 80303 USA BN 978-1-60732-344-0; 978-1-60732-339-6 J9 NIKKEI AMER PY 2015 BP 215 EP 224 DI 10.5876/9781607323440.c020 PG 10 WC History SC History GA BF0CT UT WOS:000378538000023 ER PT B AU Odo, F AF Odo, Franklin BA Hoshida, G Hoshida, T BF Hoshida, G Hoshida, T BE Kim, H TI A New Life in the Relocation Center SO TAKEN FROM THE PARADISE ISLE: THE HOSHIDA FAMILY STORY, 1912-1945 SE Nikkei in the Americas LA English DT Article; Book Chapter C1 [Odo, Franklin] Smithsonian Inst, Asian Pacific Amer Ctr, Washington, DC 20560 USA. [Odo, Franklin] Lib Congress, Asian Div, Washington, DC 20540 USA. [Odo, Franklin] Univ Hawaii, Honolulu, HI 96822 USA. [Odo, Franklin] Univ Penn, Philadelphia, PA 19104 USA. [Odo, Franklin] CUNY Hunter Coll, New York, NY 10021 USA. [Odo, Franklin] Princeton Univ, Princeton, NJ 08544 USA. [Odo, Franklin] Columbia Univ, New York, NY 10027 USA. RP Odo, F (reprint author), Smithsonian Inst, Asian Pacific Amer Ctr, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU UNIV PRESS COLORADO PI BOULDER PA 5589 ARAPAHOE AVE, STE 206C, BOULDER, CO 80303 USA BN 978-1-60732-344-0; 978-1-60732-339-6 J9 NIKKEI AMER PY 2015 BP 225 EP 230 DI 10.5876/9781607323440.c021 PG 6 WC History SC History GA BF0CT UT WOS:000378538000024 ER PT B AU Odo, F AF Odo, Franklin BA Hoshida, G Hoshida, T BF Hoshida, G Hoshida, T BE Kim, H TI Gila Relocation Center SO TAKEN FROM THE PARADISE ISLE: THE HOSHIDA FAMILY STORY, 1912-1945 SE Nikkei in the Americas LA English DT Article; Book Chapter C1 [Odo, Franklin] Smithsonian Inst, Asian Pacific Amer Ctr, Washington, DC 20560 USA. [Odo, Franklin] Lib Congress, Asian Div, Washington, DC 20540 USA. [Odo, Franklin] Univ Hawaii, Honolulu, HI 96822 USA. [Odo, Franklin] Univ Penn, Philadelphia, PA 19104 USA. [Odo, Franklin] CUNY Hunter Coll, New York, NY 10021 USA. [Odo, Franklin] Princeton Univ, Princeton, NJ 08544 USA. [Odo, Franklin] Columbia Univ, New York, NY 10027 USA. RP Odo, F (reprint author), Smithsonian Inst, Asian Pacific Amer Ctr, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU UNIV PRESS COLORADO PI BOULDER PA 5589 ARAPAHOE AVE, STE 206C, BOULDER, CO 80303 USA BN 978-1-60732-344-0; 978-1-60732-339-6 J9 NIKKEI AMER PY 2015 BP 231 EP 235 DI 10.5876/9781607323440.c022 PG 5 WC History SC History GA BF0CT UT WOS:000378538000025 ER PT B AU Odo, F AF Odo, Franklin BA Hoshida, G Hoshida, T BF Hoshida, G Hoshida, T BE Kim, H TI Farewell to the Camps and the Last Lap to Hawaii SO TAKEN FROM THE PARADISE ISLE: THE HOSHIDA FAMILY STORY, 1912-1945 SE Nikkei in the Americas LA English DT Article; Book Chapter C1 [Odo, Franklin] Smithsonian Inst, Asian Pacific Amer Ctr, Washington, DC 20560 USA. [Odo, Franklin] Lib Congress, Asian Div, Washington, DC 20540 USA. [Odo, Franklin] Univ Hawaii, Honolulu, HI 96822 USA. [Odo, Franklin] Univ Penn, Philadelphia, PA 19104 USA. [Odo, Franklin] CUNY Hunter Coll, New York, NY 10021 USA. [Odo, Franklin] Princeton Univ, Princeton, NJ 08544 USA. [Odo, Franklin] Columbia Univ, New York, NY 10027 USA. RP Odo, F (reprint author), Smithsonian Inst, Asian Pacific Amer Ctr, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU UNIV PRESS COLORADO PI BOULDER PA 5589 ARAPAHOE AVE, STE 206C, BOULDER, CO 80303 USA BN 978-1-60732-344-0; 978-1-60732-339-6 J9 NIKKEI AMER PY 2015 BP 237 EP 239 DI 10.5876/9781607323440.c023 PG 3 WC History SC History GA BF0CT UT WOS:000378538000026 ER PT B AU Odo, F AF Odo, Franklin BA Hoshida, G Hoshida, T BF Hoshida, G Hoshida, T BE Kim, H TI Official Transcript of George Hoshida's Hearing SO TAKEN FROM THE PARADISE ISLE: THE HOSHIDA FAMILY STORY, 1912-1945 SE Nikkei in the Americas LA English DT Editorial Material; Book Chapter C1 [Odo, Franklin] Smithsonian Inst, Asian Pacific Amer Ctr, Washington, DC 20560 USA. [Odo, Franklin] Lib Congress, Asian Div, Washington, DC 20540 USA. [Odo, Franklin] Univ Hawaii, Honolulu, HI 96822 USA. [Odo, Franklin] Univ Penn, Philadelphia, PA 19104 USA. [Odo, Franklin] CUNY Hunter Coll, New York, NY 10021 USA. [Odo, Franklin] Princeton Univ, Princeton, NJ 08544 USA. [Odo, Franklin] Columbia Univ, New York, NY 10027 USA. RP Odo, F (reprint author), Smithsonian Inst, Asian Pacific Amer Ctr, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU UNIV PRESS COLORADO PI BOULDER PA 5589 ARAPAHOE AVE, STE 206C, BOULDER, CO 80303 USA BN 978-1-60732-344-0; 978-1-60732-339-6 J9 NIKKEI AMER PY 2015 BP 243 EP 271 DI 10.5876/9781607323440.c025 PG 29 WC History SC History GA BF0CT UT WOS:000378538000027 ER PT J AU Tull, RG Cortes-Rodriguez, MN AF Tull, Renetta G. Cortes-Rodriguez, Maria Nandadevi GP ASEE TI Starting Points for Involving Underrepresented Graduate Students in International Engagement: A Case Study on the Collaborations Between the University of Maryland Baltimore County (UMBC) and Educational Institutions in Latin America SO 2015 ASEE INTERNATIONAL FORUM LA English DT Proceedings Paper CT ASEE Annual Conference and Exposition CY JUN 14-17, 2015 CL Seattle, WA SP ASEE AB Graduate students in engineering and IT do not have many chances to participate in study abroad opportunities, and those who do, may do so as individuals based on their graduate advisor's collaborations. In this globalized world of technological advances, developing international collaborations between scholars within the STEM fields is not only beneficial; it is essential, thus opportunities should not be limited to a select few. The National Academy of Engineering has developed a list of Grand Challenges, and there is growing concern that there won't be an international workforce with enough training to develop solutions for real-world issues. Despite involvement of some graduate students in international research, there remain subsets of graduate students from underrepresented minority (URM) groups who have neither been encouraged nor invited to participate in international projects. The Council of Graduate Schools' 2013 publication, "Graduate Education for Global Career Pathways," included papers that encouraged graduate students to participate in global conferences as means to engage, and serves as the premise for our strategy to broaden participation of URM graduate students in international projects. 1 The Graduate School at UMBC and the National Science Foundation's PROMISE: Maryland's Alliance for Graduate Education and the Professoriate (AGEP) program have started to develop cohorts of students and faculty who travel to international conferences and report on their experiences. Cohort travel models are not unique in undergraduate circles; however, for our group of participants, the model serves as a pathway to broaden the participation of STEM-trained women and minorities in international engagement. The model includes immersing the cohort into a culture through participation in an international conference, presentations at a host university to develop collaborations with faculty and students, scientific excursions, discussion sessions addressing research questions, and plans for building on the short-term experience. This model started in 2012 with a graduate student presentation at the Latin and Caribbean Consortium of Engineering Institutions (LACCEI) conference in Panama. In 2013, participation in LACCEI in Mexico increased to two graduate students, a postdoctoral fellow, and an alumnus who is a member of the faculty at another institution. By 2014, a group of 15 participated in LACCEI in Guayaquil, Ecuador. Plans for 2015 include travel to the Dominican Republic, and affiliations with Tecnologico de Monterrey in Mexico. Given graduate students' 12-month continuous research and laboratory responsibilities, the short-term experience provided a sound introduction. Participants were part of the PROMISE AGEP, Louis Stokes Alliance for Minority Participation Bridges to the Doctorate program, and the UMBC/Puerto Rico ADVANCE Hispanic Women in STEM program. Many of the participants had little to no experience abroad. The 2014 trip included collaborations with the CEDEI - Centro de Estudios Interamericanos in Cuenca, Ecuador for acclimation to the region, graduate student mentoring, and a presentation at the Foro Latinoamericano de Estudiantes sobre Educacion en Ingenieria conference at the Escuela Superior Politecnica del Litoral (ESPOL) for engineering students throughout Ecuador. Students from the U.S. and Latin American universities discussed the academic models of each country, career/life balance, development of cultural competence, and plans to engage in international research collaborations. This paper will present the model and the social science results from questions posed before, during, and after the trip which addressed barriers to entry such as the challenges of family and language, and the rewards associated with international collaborations. C1 [Tull, Renetta G.] Univ Maryland Baltimore Cty, Grad Student Profess Dev & Postdoctoral Affairs, Baltimore, MD 21228 USA. [Cortes-Rodriguez, Maria Nandadevi] Natl Zool Pk, Smithsonian Conservat Biol Inst, Ctr Conservat & Evolutionary Genet, Washington, DC 20013 USA. RP Tull, RG (reprint author), Univ Maryland Baltimore Cty, Grad Student Profess Dev & Postdoctoral Affairs, Baltimore, MD 21228 USA. NR 6 TC 0 Z9 0 U1 3 U2 3 PU AMER SOC ENGINEERING EDUCATION PI WASHINGTON PA 1818 N STREET, NW SUITE 600, WASHINGTON, DC 20036 USA PY 2015 PG 19 WC Education & Educational Research; Education, Scientific Disciplines; Engineering, Multidisciplinary SC Education & Educational Research; Engineering GA BF0XO UT WOS:000379832900021 ER PT J AU Hardesty, V AF Hardesty, Von BA VonHardesty BF VonHardesty TI War and exile SO CAMERA ALOFT: EDWARD STEICHEN IN THE GREAT WAR SE Cambridge Centennial of Flight LA English DT Article; Book Chapter C1 [Hardesty, Von] Smithsonian Natl Air & Space Museum, Washington, DC USA. NR 7 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 BN 978-0-521-82055-4 J9 CAMB CENTEN FLIGHT PY 2015 BP 1 EP 9 D2 10.1017/CBO9781139024433 PG 9 WC History SC History GA BF0AC UT WOS:000378403600002 ER PT J AU Hardesty, V AF Hardesty, Von BA VonHardesty BF VonHardesty TI A new life in the military SO CAMERA ALOFT: EDWARD STEICHEN IN THE GREAT WAR SE Cambridge Centennial of Flight LA English DT Article; Book Chapter C1 [Hardesty, Von] Smithsonian Natl Air & Space Museum, Washington, DC USA. NR 34 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 BN 978-0-521-82055-4 J9 CAMB CENTEN FLIGHT PY 2015 BP 10 EP 34 D2 10.1017/CBO9781139024433 PG 25 WC History SC History GA BF0AC UT WOS:000378403600003 ER PT J AU Hardesty, V AF Hardesty, Von BA VonHardesty BF VonHardesty TI Camera Aloft Edward Steichen in the Great War Foreword SO CAMERA ALOFT: EDWARD STEICHEN IN THE GREAT WAR SE Cambridge Centennial of Flight LA English DT Editorial Material; Book Chapter C1 [Hardesty, Von] Smithsonian Natl Air & Space Museum, Washington, DC USA. NR 0 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 BN 978-0-521-82055-4 J9 CAMB CENTEN FLIGHT PY 2015 BP XIII EP XVI D2 10.1017/CBO9781139024433 PG 4 WC History SC History GA BF0AC UT WOS:000378403600001 ER PT J AU Hardesty, V AF Hardesty, Von BA VonHardesty BF VonHardesty TI Over there SO CAMERA ALOFT: EDWARD STEICHEN IN THE GREAT WAR SE Cambridge Centennial of Flight LA English DT Article; Book Chapter C1 [Hardesty, Von] Smithsonian Natl Air & Space Museum, Washington, DC USA. NR 18 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 BN 978-0-521-82055-4 J9 CAMB CENTEN FLIGHT PY 2015 BP 35 EP 59 D2 10.1017/CBO9781139024433 PG 25 WC History SC History GA BF0AC UT WOS:000378403600004 ER PT J AU Hardesty, V AF Hardesty, Von BA VonHardesty BF VonHardesty TI The world of air observation SO CAMERA ALOFT: EDWARD STEICHEN IN THE GREAT WAR SE Cambridge Centennial of Flight LA English DT Article; Book Chapter C1 [Hardesty, Von] Smithsonian Natl Air & Space Museum, Washington, DC USA. NR 32 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 BN 978-0-521-82055-4 J9 CAMB CENTEN FLIGHT PY 2015 BP 60 EP 84 D2 10.1017/CBO9781139024433 PG 25 WC History SC History GA BF0AC UT WOS:000378403600005 ER PT J AU Hardesty, V AF Hardesty, Von BA VonHardesty BF VonHardesty TI Taking charge SO CAMERA ALOFT: EDWARD STEICHEN IN THE GREAT WAR SE Cambridge Centennial of Flight LA English DT Article; Book Chapter C1 [Hardesty, Von] Smithsonian Natl Air & Space Museum, Washington, DC USA. NR 15 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 BN 978-0-521-82055-4 J9 CAMB CENTEN FLIGHT PY 2015 BP 85 EP 108 D2 10.1017/CBO9781139024433 PG 24 WC History SC History GA BF0AC UT WOS:000378403600006 ER PT J AU Hardesty, V AF Hardesty, Von BA VonHardesty BF VonHardesty TI Over the front SO CAMERA ALOFT: EDWARD STEICHEN IN THE GREAT WAR SE Cambridge Centennial of Flight LA English DT Article; Book Chapter C1 [Hardesty, Von] Smithsonian Natl Air & Space Museum, Washington, DC USA. NR 22 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 BN 978-0-521-82055-4 J9 CAMB CENTEN FLIGHT PY 2015 BP 109 EP 137 D2 10.1017/CBO9781139024433 PG 29 WC History SC History GA BF0AC UT WOS:000378403600007 ER PT J AU Hardesty, V AF Hardesty, Von BA VonHardesty BF VonHardesty TI War and photography SO CAMERA ALOFT: EDWARD STEICHEN IN THE GREAT WAR SE Cambridge Centennial of Flight LA English DT Article; Book Chapter C1 [Hardesty, Von] Smithsonian Natl Air & Space Museum, Washington, DC USA. NR 15 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 BN 978-0-521-82055-4 J9 CAMB CENTEN FLIGHT PY 2015 BP 138 EP 149 D2 10.1017/CBO9781139024433 PG 12 WC History SC History GA BF0AC UT WOS:000378403600008 ER PT J AU Hardesty, V AF Hardesty, Von BA VonHardesty BF VonHardesty TI Life at the cutting edge: The photo sections SO CAMERA ALOFT: EDWARD STEICHEN IN THE GREAT WAR SE Cambridge Centennial of Flight LA English DT Article; Book Chapter C1 [Hardesty, Von] Smithsonian Natl Air & Space Museum, Washington, DC USA. NR 1 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 BN 978-0-521-82055-4 J9 CAMB CENTEN FLIGHT PY 2015 BP 151 EP 153 D2 10.1017/CBO9781139024433 PG 3 WC History SC History GA BF0AC UT WOS:000378403600009 ER PT J AU Hardesty, V AF Hardesty, Von BA VonHardesty BF VonHardesty TI History of Photo Section No. 1, Air Service, 1918 SO CAMERA ALOFT: EDWARD STEICHEN IN THE GREAT WAR SE Cambridge Centennial of Flight LA English DT Article; Book Chapter C1 [Hardesty, Von] Smithsonian Natl Air & Space Museum, Washington, DC USA. NR 0 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 BN 978-0-521-82055-4 J9 CAMB CENTEN FLIGHT PY 2015 BP 154 EP 164 D2 10.1017/CBO9781139024433 PG 11 WC History SC History GA BF0AC UT WOS:000378403600010 ER PT J AU Hardesty, V AF Hardesty, Von BA VonHardesty BF VonHardesty TI History of Photo Section No. 2, Air Service, 1918 SO CAMERA ALOFT: EDWARD STEICHEN IN THE GREAT WAR SE Cambridge Centennial of Flight LA English DT Article; Book Chapter C1 [Hardesty, Von] Smithsonian Natl Air & Space Museum, Washington, DC USA. NR 0 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 BN 978-0-521-82055-4 J9 CAMB CENTEN FLIGHT PY 2015 BP 165 EP 174 D2 10.1017/CBO9781139024433 PG 10 WC History SC History GA BF0AC UT WOS:000378403600011 ER PT J AU Hardesty, V AF Hardesty, Von BA VonHardesty BF VonHardesty TI History Photo Section No. 3, Air Service, 1918 SO CAMERA ALOFT: EDWARD STEICHEN IN THE GREAT WAR SE Cambridge Centennial of Flight LA English DT Article; Book Chapter C1 [Hardesty, Von] Smithsonian Natl Air & Space Museum, Washington, DC USA. NR 0 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 BN 978-0-521-82055-4 J9 CAMB CENTEN FLIGHT PY 2015 BP 175 EP 179 D2 10.1017/CBO9781139024433 PG 5 WC History SC History GA BF0AC UT WOS:000378403600012 ER PT J AU Hardesty, V AF Hardesty, Von BA VonHardesty BF VonHardesty TI History of Photographic Section No. 4, Air Service, USA 1918 SO CAMERA ALOFT: EDWARD STEICHEN IN THE GREAT WAR SE Cambridge Centennial of Flight LA English DT Article; Book Chapter C1 [Hardesty, Von] Smithsonian Natl Air & Space Museum, Washington, DC USA. NR 0 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 BN 978-0-521-82055-4 J9 CAMB CENTEN FLIGHT PY 2015 BP 180 EP 184 D2 10.1017/CBO9781139024433 PG 5 WC History SC History GA BF0AC UT WOS:000378403600013 ER PT J AU Hardesty, V AF Hardesty, Von BA VonHardesty BF VonHardesty TI Camera Aloft Edward Steichen in the Great War SO CAMERA ALOFT: EDWARD STEICHEN IN THE GREAT WAR SE Cambridge Centennial of Flight LA English DT Article; Book Chapter C1 [Hardesty, Von] Smithsonian Natl Air & Space Museum, Washington, DC USA. NR 0 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 BN 978-0-521-82055-4 J9 CAMB CENTEN FLIGHT PY 2015 BP 185 EP 187 D2 10.1017/CBO9781139024433 PG 3 WC History SC History GA BF0AC UT WOS:000378403600014 ER PT J AU Wegener, C AF Wegener, Corine TI Museums in Crisis:: Helping our Colleagues and their Museums in Need SO MUSEUM INTERNATIONAL LA English DT Article C1 [Wegener, Corine] Smithsonian Inst, Off Secretary Hist Art & Culture, Washington, DC 20560 USA. [Wegener, Corine] US Comm Blue Shield, Washington, DC USA. RP Wegener, C (reprint author), Smithsonian Inst, Off Secretary Hist Art & Culture, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1350-0775 EI 1468-0033 J9 MUSEUM INT JI Mus. Int. PY 2015 VL 67 IS 1-4 SI SI BP 132 EP 137 DI 10.1111/muse.12082 PG 6 WC Art SC Art GA DQ9FG UT WOS:000379515200012 ER PT B AU Gibb, JG AF Gibb, James G. BE VanDyke, RM Bernbeck, R TI Constructive Imagination and the Elusive Past Playwriting as Method SO SUBJECTS AND NARRATIVES IN ARCHAEOLOGY LA English DT Article; Book Chapter C1 [Gibb, James G.] Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. [Gibb, James G.] Stevenson Univ, Pikesville, MD USA. [Gibb, James G.] Anne Arundel Community Coll, Arnold, MD USA. RP Gibb, JG (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. NR 30 TC 0 Z9 0 U1 0 U2 0 PU UNIV PRESS COLORADO PI BOULDER PA 5589 ARAPAHOE AVE, STE 206C, BOULDER, CO 80303 USA BN 978-1-60732-387-7; 978-1-60732-381-5 PY 2015 BP 145 EP 167 DI 10.5876/9781607323815.c007 D2 10.5876/9781607323815 PG 23 WC Archaeology SC Archaeology GA BF0BR UT WOS:000378484500007 ER PT B AU Diaz, V AF Diaz, Vanessa BE Cobb, S Ewen, N TI 'Brad & Angelina: And Now ... Brangelina!': A Sociocultural Analysis of Blended Celebrity Couple Names SO FIRST COMES LOVE: POWER COUPLES, CELEBRITY KINSHIP AND CULTURAL POLITICS LA English DT Article; Book Chapter C1 [Diaz, Vanessa] Univ Michigan, Anthropol, Ann Arbor, MI 48109 USA. [Diaz, Vanessa] Ford Fdn, New York, NY USA. [Diaz, Vanessa] Smithsonian Inst, Washington, DC 20560 USA. RP Diaz, V (reprint author), Univ Michigan, Anthropol, Ann Arbor, MI 48109 USA. NR 50 TC 0 Z9 0 U1 0 U2 0 PU BLOOMSBURY PUBL INC PI NEW YORK PA 1385 BROADWAY, FIFTH FLOOR, NEW YORK, NY 10018 USA BN 978-1-6289-2122-9; 978-1-6289-2119-9; 978-1-6289-2121-2 PY 2015 BP 275 EP 294 PG 20 WC Cultural Studies; Film, Radio, Television SC Cultural Studies; Film, Radio & Television GA BE7WD UT WOS:000375953600019 ER PT S AU Tong, CYE Zeng, LZ Grimes, PK Blundell, R AF Tong, Cheuk-yu Edward Zeng, Lingzhen Grimes, Paul K. Blundell, Raymond GP IEEE TI Wideband SIS Receiver Development for the Submillimeter Array SO 2015 40TH INTERNATIONAL CONFERENCE ON INFRARED, MILLIMETER AND TERAHERTZ WAVES (IRMMW-THZ) SE International Conference on Infrared Millimeter and Terahertz Waves LA English DT Proceedings Paper CT 40th International Conference on Infrared, Millimeter, and Terahertz Waves (IRMMW-THz) CY AUG 23-28, 2015 CL Chinese Univ Hong Kong, Hong Kong, PEOPLES R CHINA SP IEEE, IEEE Microwave Theory & Tech Soc, Virginal Diodes Inc, TeraView, Microtech Instruments Inc, Hong Kong Univ Sci & Technol, Dept Elect & Comp Engn, Croucher Fdn, Capital Normal Univ, K C Wong Educ Fdn, Meetings & Exhibit Hong Kong, Army Res Off, NSF HO Chinese Univ Hong Kong AB We report on the development of wideband receivers for the Submillimeter Array (SMA). The current generation of SMA receiver offers an intermediate frequency (IF) of 4 - 14 GHz. We have further pushed the frontier of wideband SIS mixing, by developing a low noise receiver with an IF of 4 18 GHz. C1 [Tong, Cheuk-yu Edward; Zeng, Lingzhen; Grimes, Paul K.; Blundell, Raymond] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RP Tong, CYE (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM etong@cfa.harvard.edu NR 7 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 2162-2027 BN 978-1-4799-8272-1 J9 INT CONF INFRA MILLI PY 2015 PG 2 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA BE8OY UT WOS:000376674000304 ER PT S AU Yao, QJ Liu, D Lin, ZH Duan, WY Li, J Lou, Z Shi, SC Maezawa, H Paine, S AF Yao, Qijun Liu, Dong Lin, Zhenhui Duan, Wenying Li, Jing Lou, Zheng Shi, Shengcai Maezawa, Hiroyuki Paine, Scott GP IEEE TI Atmospheric Profiling Synthetic Observation System at THz Wave Band SO 2015 40TH INTERNATIONAL CONFERENCE ON INFRARED, MILLIMETER AND TERAHERTZ WAVES (IRMMW-THZ) SE International Conference on Infrared Millimeter and Terahertz Waves LA English DT Proceedings Paper CT 40th International Conference on Infrared, Millimeter, and Terahertz Waves (IRMMW-THz) CY AUG 23-28, 2015 CL Chinese Univ Hong Kong, Hong Kong, PEOPLES R CHINA SP IEEE, IEEE Microwave Theory & Tech Soc, Virginal Diodes Inc, TeraView, Microtech Instruments Inc, Hong Kong Univ Sci & Technol, Dept Elect & Comp Engn, Croucher Fdn, Capital Normal Univ, K C Wong Educ Fdn, Meetings & Exhibit Hong Kong, Army Res Off, NSF HO Chinese Univ Hong Kong AB We introduced a dual-THz-band SIS (Superconductor-Insulator-Superconductor) heterodyne radiometer system which is under developing for the atmospheric profiling synthetic observation system project (APSOS). This THz system is intended to have a durable and compact design to meet the challenging requirements of remote operation at Tibetan Plateau. The system as well as its major components such as antenna tipping, quasi-optics, cryogenics, SIS mixers and FFTS backend will be discussed thoroughly. Some scientific simulation focusing on the atmospheric profiling components at THz bands will also be investigated. C1 [Yao, Qijun; Liu, Dong; Lin, Zhenhui; Duan, Wenying; Li, Jing; Lou, Zheng; Shi, Shengcai] Chinese Acad Sci, Purple Mt Observ, Beijing, Peoples R China. [Yao, Qijun; Liu, Dong; Lin, Zhenhui; Duan, Wenying; Li, Jing; Lou, Zheng; Shi, Shengcai] Chinese Acad Sci, Key Lab Radio Astron, Beijing, Peoples R China. [Maezawa, Hiroyuki] Osaka Prefectural Univ, Osaka, Japan. [Paine, Scott] Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA. RP Yao, QJ (reprint author), Chinese Acad Sci, Purple Mt Observ, Beijing, Peoples R China. NR 8 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 2162-2027 BN 978-1-4799-8272-1 J9 INT CONF INFRA MILLI PY 2015 PG 2 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA BE8OY UT WOS:000376674000540 ER PT S AU Zeng, LZ Tong, CYE Wollack, EJ Chuss, DT AF Zeng, Lingzhen Tong, Cheuk-yu Edward Wollack, Edward J. Chuss, David T. GP IEEE TI A wideband profiled corrugated horn for multichroic applications SO 2015 40TH INTERNATIONAL CONFERENCE ON INFRARED, MILLIMETER AND TERAHERTZ WAVES (IRMMW-THZ) SE International Conference on Infrared Millimeter and Terahertz Waves LA English DT Proceedings Paper CT 40th International Conference on Infrared, Millimeter, and Terahertz Waves (IRMMW-THz) CY AUG 23-28, 2015 CL Chinese Univ Hong Kong, Hong Kong, PEOPLES R CHINA SP IEEE, IEEE Microwave Theory & Tech Soc, Virginal Diodes Inc, TeraView, Microtech Instruments Inc, Hong Kong Univ Sci & Technol, Dept Elect & Comp Engn, Croucher Fdn, Capital Normal Univ, K C Wong Educ Fdn, Meetings & Exhibit Hong Kong, Army Res Off, NSF HO Chinese Univ Hong Kong ID CROSS-POLARIZATION AB A wideband profiled corrugated feedhorn was developed for multichroic applications. This feedhorn features a return loss of better than -25 dB and cross polarization peaks below -30 dB, over a fractional bandwidth of > 50%. Its performance is close to that of the ring-loaded corrugated feedhorn; however, the design presented is much easier to fabricate at millimeter wavelengths. C1 [Zeng, Lingzhen; Tong, Cheuk-yu Edward] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Wollack, Edward J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Chuss, David T.] Villanova Univ, Villanova, PA 19085 USA. RP Zeng, LZ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Wollack, Edward/D-4467-2012 OI Wollack, Edward/0000-0002-7567-4451 NR 8 TC 0 Z9 0 U1 0 U2 2 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 2162-2027 BN 978-1-4799-8272-1 J9 INT CONF INFRA MILLI PY 2015 PG 2 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA BE8OY UT WOS:000376674000444 ER PT B AU Goddard, I AF Goddard, Ives BE Costa, DJ TI Three Nineteenth-Century Munsee Texts: Archaisms, Dialect Variation, and Problems of Textual Criticism SO NEW VOICES FOR OLD WORDS: ALGONQUIAN ORAL LITERATURES SE Studies in the Anthropology of North American Indians LA English DT Proceedings Paper CT Conference on Problems and Strategies in the Analysis, Redaction, and Presentation of Native Texts CY OCT 25-26, 2008 CL Minneapolis, MN C1 [Goddard, Ives] Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20560 USA. RP Goddard, I (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20560 USA. NR 79 TC 0 Z9 0 U1 0 U2 0 PU UNIV NEBRASKA PRESS PI LINCOLN PA 1111 LINCOLN MALL, LINCOLN, NE 68588-0630 USA BN 978-0-8032-7890-5; 978-0-8032-6548-6 J9 STUD ANTHR N AM IND PY 2015 BP 198 EP 314 PG 117 WC Anthropology SC Anthropology GA BE8WB UT WOS:000377082100006 ER PT B AU Thomason, L AF Thomason, Lucy BE Costa, DJ TI On Editing Bill Leaf's Meskwaki Texts SO NEW VOICES FOR OLD WORDS: ALGONQUIAN ORAL LITERATURES SE Studies in the Anthropology of North American Indians LA English DT Proceedings Paper CT Conference on Problems and Strategies in the Analysis, Redaction, and Presentation of Native Texts CY OCT 25-26, 2008 CL Minneapolis, MN C1 [Thomason, Lucy] Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20560 USA. RP Thomason, L (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20560 USA. NR 6 TC 0 Z9 0 U1 0 U2 0 PU UNIV NEBRASKA PRESS PI LINCOLN PA 1111 LINCOLN MALL, LINCOLN, NE 68588-0630 USA BN 978-0-8032-7890-5; 978-0-8032-6548-6 J9 STUD ANTHR N AM IND PY 2015 BP 315 EP 452 PG 138 WC Anthropology SC Anthropology GA BE8WB UT WOS:000377082100007 ER PT S AU Schnitzer, SA AF Schnitzer, Stefan A. BE Parthasarathy, N TI The Contribution of Lianas to Forest Ecology, Diversity, and Dynamics SO BIODIVERSITY OF LIANAS SE Sustainable Development and Biodiversity LA English DT Article; Book Chapter ID BARRO-COLORADO ISLAND; TROPICAL FOREST; TREE GROWTH; GAPS; REGENERATION; PATTERNS; BIOMASS; CANOPY; PANAMA; ABUNDANCE AB Lianas are a common component of forests worldwide and they contribute to forest ecology, diversity, and dynamics. Lianas can have both positive and negative effects in forests. Lianas can be an important resource for animals, as food (in the form of nectar, pollen, fruits, leaves, or sap), providing nesting sites, shelter and, by climbing among many tree crowns, lianas can provide aerial highways for many animal species. By contrast, lianas also compete intensively with trees, reducing tree recruitment, growth, reproduction, and survival, as well as tree diversity and forest-level carbon sequestration. While the inclusion of lianas in ecological studies have lagged behind that of trees, over the past three decades, the study of liana ecology has grown significantly, revealing many important contributions of lianas to forest ecology. In this chapter, I review the state of knowledge about the ecology of lianas and their contribution to forest ecology, diversity, and dynamics. C1 [Schnitzer, Stefan A.] Marquette Univ, Dept Biol Sci, POB 1881, Milwaukee, WI 53201 USA. [Schnitzer, Stefan A.] Smithsonian Trop Res Inst, Balboa 2072, Panama. RP Schnitzer, SA (reprint author), Marquette Univ, Dept Biol Sci, POB 1881, Milwaukee, WI 53201 USA. EM S1@uwm.edu NR 50 TC 0 Z9 0 U1 2 U2 2 PU SPRINGER INT PUBLISHING AG PI CHAM PA GEWERBESTRASSE 11, CHAM, CH-6330, SWITZERLAND SN 2352-474X BN 978-3-319-14592-1; 978-3-319-14591-4 J9 SUSTAIN DEV BIODIVER PY 2015 VL 5 BP 149 EP 160 DI 10.1007/978-3-319-14592-1_9 D2 10.1007/978-3-319-14592-1 PG 12 WC Biodiversity Conservation; Plant Sciences SC Biodiversity & Conservation; Plant Sciences GA BE8NE UT WOS:000376612700010 ER PT B AU Fariello, MA AF Fariello, M. Anna BE Gillespie, M McMillen, SG TI Olive Dame Campbell Among the Folk: Education, Experimentation, and Rural Life SO NORTH CAROLINA WOMEN: THEIR LIVES AND TIMES, VOL 2 SE Southern Women-Their Lives and Times LA English DT Article; Book Chapter C1 [Fariello, M. Anna] Western Carolina Univ, Hunter Lib, Project Reg Heritage, Cullowhee, NC 28723 USA. [Fariello, M. Anna] Smithsonian Amer Art Museum, Cullowhee, NC 28723 USA. [Fariello, M. Anna] Smithsonian Folklife Ctr, Cullowhee, NC 28723 USA. RP Fariello, MA (reprint author), Western Carolina Univ, Hunter Lib, Special Collect, Cullowhee, NC 28723 USA. NR 40 TC 0 Z9 0 U1 0 U2 0 PU UNIV GEORGIA PRESS PI ATHENS PA ATHENS, GA 30602 USA BN 978-0-8203-4002-9; 978-0-8203-4756-1; 978-0-8203-4001-2 J9 SOUTH WOMEN PY 2015 VL 1 BP 32 EP 51 PG 20 WC History; Women's Studies SC History; Women's Studies GA BE6KB UT WOS:000374258000003 ER PT J AU Bourg, NA Gill, DE McShea, WJ AF Bourg, Norman A. Gill, Douglas E. McShea, William J. TI Fire and Canopy Removal Effects on Demography and Reproduction in Turkeybeard (Xerophyllum asphodeloides), a Fire-Dependent Temperate Forest Herb SO JOURNAL OF SUSTAINABLE FORESTRY LA English DT Article; Proceedings Paper CT Conference on Fire Ecology of the Northeast - Restoring Native and Cultural Ecosystems CY FEB 20-22, 2014 CL Yale Univ, Sch Forestry & Environm Studies, New Haven, CT SP Tall Timbers Res Stn & Land Conservancy HO Yale Univ, Sch Forestry & Environm Studies DE Appalachians; disturbance ecology; fire adaptation; fire ecology; forest herbs; mass-flowering; plant reproduction; rare plants; Xerophyllum asphodeloides ID SOUTHERN APPALACHIAN MOUNTAINS; POPULATION VIABILITY ANALYSIS; PLANT-POLLINATOR INTERACTIONS; INDUCED SEED-GERMINATION; PINUS-PUNGENS; POLLEN LIMITATION; FLORIDA SCRUB; HYPERICUM-CUMULICOLA; PRESCRIBED FIRE; NATIONAL-PARK AB We examined the effects of fire and canopy disturbance on turkeybeard (Xerophyllum asphodeloides [L.] Nutt.), a rare temperate forest herb. We used long-term data and a fire and canopy alteration experiment with controls to address our hypothesis that turkeybeard is fire-adapted. Analyses of a primary study population demonstrated that turkeybeard is a long-lived, infrequently flowering perennial with high survival and rapid postfire resprouting ability. Experimental responses showed that population-level flowering and inflorescence production increased 60-280% across treatments compared to controls in two posttreatment seasons. Seed production/inflorescence was significantly higher in treated plants. Fire and canopy removal treatments had a positive and additive effect on seed set compared to controls. Additional population surveys and pollination experiments showed that turkeybeard exhibited low flowering levels in undisturbed forest and required outcrossing for good seed set. Burning released plants from these limiting factors by inducing mass-flowering and altering the forest habitat to attract insect pollinators. Our research demonstrates that turkeybeard is one of the few known definitively fire-adapted montane forest understory herbs in the eastern United States, such that fire management including prescribed burning is recommended for its conservation and management. It also adds new impetus for studying fire's ecological role in these lands. C1 [Bourg, Norman A.; Gill, Douglas E.] Univ Maryland, Dept Biol, College Pk, MD 20742 USA. [Bourg, Norman A.; McShea, William J.] Natl Zool Pk, Smithsonian Conservat Biol Inst, Conservat Ecol Ctr, 1500 Remount Rd, Front Royal, VA 22630 USA. RP Bourg, NA (reprint author), Natl Zool Pk, Smithsonian Conservat Biol Inst, Conservat Ecol Ctr, 1500 Remount Rd, Front Royal, VA 22630 USA. EM bourgn@si.edu OI Bourg, Norman/0000-0002-7443-1992 FU National Fish & Wildlife Foundation General Conservation Challenge Grant; Smithsonian Institution (SI) Predoctoral Fellowship; National Science Foundation (NSF) Research Training Grant in the Biology of Small Populations at the University of Maryland-College Park (UMCP); UMCP Graduate School; U.S. Department of Agriculture, Forest Service [08-97-08-11] FX Funding was provided by a National Fish & Wildlife Foundation General Conservation Challenge Grant to William J. McShea, Norman A. Bourg, and Douglas E. Gill; a Smithsonian Institution (SI) Predoctoral Fellowship to Norman A. Bourg; the National Science Foundation (NSF) Research Training Grant in the Biology of Small Populations at the University of Maryland-College Park (UMCP), the UMCP Graduate School, and U.S. Department of Agriculture, Forest Service cost-share agreement #08-97-08-11 for the Orchid Hill Ecosystem Management Project. NR 126 TC 1 Z9 2 U1 5 U2 9 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 530 WALNUT STREET, STE 850, PHILADELPHIA, PA 19106 USA SN 1054-9811 EI 1540-756X J9 J SUSTAIN FOREST JI J. Sustain. For. PY 2015 VL 34 IS 1-2 SI SI BP 71 EP 104 DI 10.1080/10549811.2014.973609 PG 34 WC Forestry SC Forestry GA DI5VL UT WOS:000373568500005 ER PT S AU Fraser, M Altavilla, G Blagorodnova, N Campbell, HC Clementini, G de Miguel, E Gilmore, G Hodgkin, ST Jonker, PG Koposov, S Rixon, G Rybicki, K Torres, MAP van Leeuwen, F van Velzen, S Walton, NA Wevers, T Wielgorski, P Wyrzykowski, L AF Fraser, M. Altavilla, G. Blagorodnova, N. Campbell, H. C. Clementini, G. de Miguel, E. Gilmore, G. Hodgkin, S. T. Jonker, P. G. Koposov, S. Rixon, G. Rybicki, K. Torres, M. A. P. van Leeuwen, F. van Velzen, S. Walton, N. A. Wevers, T. Wielgorski, P. Wyrzykowski, L. BE Walton, NA Figueras, F BalaguerNunez, L Soubiran, C TI GROUND BASED FOLLOW-UP FOR GAIA SCIENCE ALERTS: FIRST RESULTS SO MILKY WAY UNRAVELLED BY GAIA: GREAT SCIENCE FROM THE GAIA DATA RELEASES SE EAS Publications Series LA English DT Proceedings Paper CT Conference on the Milky Way Unravelled by Gaia: GREAT Science from the Gaia Data Releases CY DEC 01-05, 2014 CL Barcelona, SPAIN SP European Union's Seventh Framework Programme, Minist Econ y Competitividad, Fundacion Espanola Ciencia Tecnologia, MINECO FEDER, Univ Barcelona, Fac Phys, Univ Barcelona, Inst Cosmos, Inst Estudis Espacials Catalunya AB The Gaia Science Alerts project (GSA) aims to augment a precision survey of the Milky Way with a controlled, precision survey of all classes of transient phenomena. While onboard BP/RP spectra from Gaia will ultimately allow us to classify many Gaia Alerts based on Gaia data alone, in the initial phases of the GSA project it is necessary to verify and classify discoveries with ground-based spectroscopic followup. In this article, we describe a subset of the ongoing Gaia Alerts followup programmes, and some of the initial science results from this work. C1 [Fraser, M.; Blagorodnova, N.; Campbell, H. C.; Gilmore, G.; Hodgkin, S. T.; Koposov, S.; Rixon, G.; van Leeuwen, F.; Walton, N. A.; Wyrzykowski, L.] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. [Altavilla, G.; Clementini, G.] Osservatorio Astron Bologna, INAF, I-40127 Bologna, Italy. [de Miguel, E.] Observ CIECEM, CBA Huelva, Almonte 21076, Huelva, Spain. [de Miguel, E.] Univ Huelva, Dept Fis Aplicada, Huelva 21071, Spain. [Jonker, P. G.; Torres, M. A. P.] SRON Netherlands Inst Space Res, SRON, NL-3584 CA Utrecht, Netherlands. [Jonker, P. G.; Torres, M. A. P.; Wevers, T.] Radboud Univ Nijmegen, IMAPP, Dept Astrophys, NL-6525 AJ Nijmegen, Netherlands. [Jonker, P. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Rybicki, K.; Wielgorski, P.; Wyrzykowski, L.] Univ Warsaw Observ, PL-00478 Warsaw, Poland. [van Velzen, S.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6500 GL Nijmegen, Netherlands. [van Velzen, S.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. RP Fraser, M (reprint author), Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. RI Koposov, Sergey/F-2754-2012; Balaguer-Nunez, Lola/C-9094-2011; OI Koposov, Sergey/0000-0003-2644-135X; Altavilla, Giuseppe/0000-0002-9934-1352; Balaguer-Nunez, Lola/0000-0001-9789-7069; Fraser, Morgan/0000-0003-2191-1674 NR 8 TC 0 Z9 0 U1 0 U2 0 PU E D P SCIENCES PI CEDEX A PA 17 AVE DU HOGGAR PARC D ACTIVITES COUTABOEUF BP 112, F-91944 CEDEX A, FRANCE SN 1633-4760 BN 978-2-7598-1826-6 J9 EAS PUBLICATIONS PY 2015 VL 67-68 BP 295 EP 298 DI 10.1051/eas/1567054 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE4ZE UT WOS:000372372700053 ER PT S AU Wen, J Egan, AN Dikow, RB Zimmer, EA AF Wen, Jun Egan, Ashley N. Dikow, Rebecca B. Zimmer, Elizabeth A. BE Horandl, E Appelhans, MS TI Utility of transcriptome sequencing for phylogenetic inference and character evolution SO NEXT GENERATION SEQUENCING IN PLANT SYSTEMATICS SE Regnum Vegetabile LA English DT Article; Book Chapter DE RNA-Seq; RNA-Seq phylogenetics; systematics; transcriptome; transcriptomics ID RNA-SEQ DATA; MULTI-TISSUE TRANSCRIPTOMICS; ESTIMATING SPECIES TREES; UNROOTED GENE TREES; HIDDEN MARKOV MODEL; CANDIDATE GENES; NUCLEAR GENES; LAND PLANTS; COMPARATIVE GENOMICS; ORTHOLOGY INFERENCE AB Transcriptome sequencing or RNA-Seq is one of the most efficient and cost-effective methods currently available for gene discovery in non-model organisms. Recent studies have demonstrated the utility of these data for resolving the relationships of diverse lineages of organisms, by extracting sequences of a large number of single-copy nuclear genes from transcriptomes of the taxa under study (i.e., RNA-Seq phylogenetics). Comparative transcriptomics has also been applied in several other areas in systematic biology, especially concerning polyploidy, introgression, hybridization, and horizontal gene transfer, as well as character evolution, including the identification of likely key innovations. This review focuses on the utility of transcriptomics in phylogenetic inferences and character evolution, and discusses the analytical framework, challenges, and prospects of transcriptome data in plant systematics, especially in phylogenetics. The main limitations are related to the high RNA-grade tissue quality requirement, the comparisons among expressed genes at a particular time point or developmental stage, orthology determination, and sequencing that arises from coding regions only, as well as several bioinformatics and analytical challenges. Comparative transcriptomics offers a rich set of genic sources for phylogenetic inference and single- or low-copy nuclear marker development. As whole genomes and genomic data become less costly and more prevalent, comparisons among transcriptomes will increase. With transcriptome- and genome-scale bioinformatics continuing to develop, we expect that the utility of transcriptomics will only increase in systematic biology, and that the RNA-Seq approach will offer tremendous insights into the understanding of the ontogeny and evolution of characters in the next decade. C1 [Wen, Jun; Egan, Ashley N.; Zimmer, Elizabeth A.] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, MRC 166, Washington, DC 20013 USA. [Dikow, Rebecca B.] Smithsonian Inst, Ctr Conservat & Evolutionary Genet, Washington, DC 20013 USA. [Dikow, Rebecca B.] Smithsonian Inst, Div Mammals, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Wen, J (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, MRC 166, Washington, DC 20013 USA. EM wenj@si.edu NR 217 TC 1 Z9 1 U1 5 U2 8 PU A R G GANTNER VERLAG K G PI KOENIGSTEIN PA C/O KOELTZ SCIENTIFIC BOOKS, PO BOX 1360, KOENIGSTEIN, D-61453, GERMANY SN 0080-0694 BN 978-3-87429-492-8 J9 REGNUM VEG JI Regnum Veg. PY 2015 VL 158 BP 51 EP 91 PG 41 WC Plant Sciences SC Plant Sciences GA BE3US UT WOS:000371282700003 ER PT S AU Bonomo, AS Sozzetti, A Lovis, C Malavolta, L Rice, K Dumusque, X Cameron, AC Latham, DW Molinari, E Pepe, F Udry, S AF Bonomo, A. S. Sozzetti, A. Lovis, C. Malavolta, L. Rice, K. Dumusque, X. Cameron, A. C. Latham, D. W. Molinari, E. Pepe, F. Udry, S. CA HARPS-N Team BE Garcia, RA Ballot, J TI Characterization of small planets with Kepler and HARPS-N SO SPACE PHOTOMETRY REVOLUTION - COROT SYMPOSIUM 3, KEPLER KASC-7 JOINT MEETING SE EPJ Web of Conferences LA English DT Proceedings Paper CT Symposium 3 on Space Photometry Revolution - CoRoT / Kepler KASC-7 Joint Meeting CY JUL 06-11, 2014 CL Toulouse, FRANCE ID EARTH-SIZED PLANET; EXOPLANETS AB The high-accuracy and high-precision HARPS-N spectrograph has been installed at the italian Telescopio Nazionale Galileo in La Palma approximately two years and a half ago. Eighty nights per year of Guaranteed Time of Observation are mostly dedicated to the radial-velocity (RV) follow up of Kepler small-size planetary candidates to establish their nature and to determine accurately their masses. We report on recent results of this ongoing RV campaign, including the recent characterization of the planetary system Kepler-101. C1 [Bonomo, A. S.; Sozzetti, A.] INAF Osservatorio Astrofis Torino, Via Osservatorio 20, I-10025 Pino Torinese, Italy. [Lovis, C.; Pepe, F.; Udry, S.] Univ Geneva, Observ Astron, CH-1290 Versoix, Switzerland. [Malavolta, L.] Univ Padua, Dipartimento Fis & Astron Galileo Galilei, I-35122 Padua, Italy. [Malavolta, L.] INAF Osservatorio Astron Padova, I-35122 Padua, Italy. [Rice, K.] Univ Edinburgh, Royal Observ, Inst Astron, SUPA, Edinburgh EH9 3HJ, Midlothian, Scotland. [Dumusque, X.; Latham, D. W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Cameron, A. C.] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland. [Molinari, E.] INAF Fdn Galileo Galilei, Brea Baja 38712, Spain. [Molinari, E.] INAF IASF Milano, I-20133 Milan, Italy. RP Bonomo, AS (reprint author), INAF Osservatorio Astrofis Torino, Via Osservatorio 20, I-10025 Pino Torinese, Italy. EM bonomo@oato.inaf.it OI Molinari, Emilio/0000-0002-1742-7735; Sozzetti, Alessandro/0000-0002-7504-365X; Cameron, Andrew/0000-0002-8863-7828 NR 8 TC 0 Z9 0 U1 0 U2 0 PU E D P SCIENCES PI CEDEX A PA 17 AVE DU HOGGAR PARC D ACTIVITES COUTABOEUF BP 112, F-91944 CEDEX A, FRANCE SN 2100-014X J9 EPJ WEB CONF PY 2015 VL 101 AR 06011 DI 10.1051/epjconf/201510106011 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE5BE UT WOS:000372491300050 ER PT S AU Guenther, EW Cusano, F Deeg, H Gandolfi, D Geier, S Grziwa, S Heber, U Tal-Or, L Sebastian, D Rodle, F AF Guenther, E. W. Cusano, F. Deeg, H. Gandolfi, D. Geier, S. Grziwa, S. Heber, U. Tal-Or, L. Sebastian, D. Rodle, F. CA CoRoT-team BE Garcia, RA Ballot, J TI A planet in a polar orbit of 1.4 solar-mass star SO SPACE PHOTOMETRY REVOLUTION - COROT SYMPOSIUM 3, KEPLER KASC-7 JOINT MEETING SE EPJ Web of Conferences LA English DT Proceedings Paper CT Symposium 3 on Space Photometry Revolution - CoRoT / Kepler KASC-7 Joint Meeting CY JUL 06-11, 2014 CL Toulouse, FRANCE ID COROT-FIELDS IRA01; MULTIOBJECT SPECTROSCOPY; II.; EXOPLANETS; LRA02; DISKS; GAS AB Although more than a thousand transiting extrasolar planets have been discovered, only very few of them orbit stars that are more massive than the Sun. The discovery of such planets is interesting, because they have formed in disks that are more massive but had a shorter life time than those of solar-like stars. Studies of planets more massive than the Sun thus tell us how the properties of the proto-planetary disks effect the formation of planets. Another aspect that makes these planets interesting is that they have kept their original orbital inclinations. By studying them we can thus find out whether the orbital axes planets are initially aligned to the stars rotational axes, or not. Here we report on the discovery of a planet of a 1.4 solar-mass star with a period of 5.6 days in a polar orbit made by CoRoT. This new planet thus is one of the few known close-in planets orbiting a star that is substantially more massive than the Sun. C1 [Guenther, E. W.; Sebastian, D.] Thuringer Landessternwarte Tautenburg, Sternwarte 5, D-07778 Tautenburg, Germany. [Cusano, F.] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy. [Deeg, H.] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain. [Deeg, H.] Inst Astrofis Canarias, E-38205 Tenerife, Spain. [Gandolfi, D.] Zentrum Astron Heidelberg, D-69117 Heidelberg, Germany. [Geier, S.] European So Observ, D-85748 Garching, Germany. [Grziwa, S.] Univ Cologne, Rhein Inst Umweltforsch, D-50931 Cologne, Germany. [Heber, U.] Univ Erlangen Nurnberg, Astron Inst, Dr Karl Remeis Observ, D-96049 Bamberg, Germany. [Heber, U.] Univ Erlangen Nurnberg, Astron Inst, ECAP, D-96049 Bamberg, Germany. [Tal-Or, L.] Tel Aviv Univ, Raymond & Beverly Sackler Fac Exact Sci, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. [Rodle, F.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Rodle, F.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Guenther, EW (reprint author), Thuringer Landessternwarte Tautenburg, Sternwarte 5, D-07778 Tautenburg, Germany. EM guenther@tls-tautenburg.de OI Cusano, Felice/0000-0003-2910-6565; Gandolfi, Davide/0000-0001-8627-9628 NR 23 TC 0 Z9 0 U1 0 U2 0 PU E D P SCIENCES PI CEDEX A PA 17 AVE DU HOGGAR PARC D ACTIVITES COUTABOEUF BP 112, F-91944 CEDEX A, FRANCE SN 2100-014X J9 EPJ WEB CONF PY 2015 VL 101 AR 02001 DI 10.1051/epjconf/201510102001 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE5BE UT WOS:000372491300017 ER PT S AU Oshagh, M Santos, NC Boisse, I Boue, G Ehrenreich, D Haghighipour, N Figueira, P Santerne, A Dumusque, X AF Oshagh, M. Santos, N. C. Boisse, I Boue, G. Ehrenreich, D. Haghighipour, N. Figueira, P. Santerne, A. Dumusque, X. BE Garcia, RA Ballot, J TI Effect of stellar activity on the high precision transit light curve SO SPACE PHOTOMETRY REVOLUTION - COROT SYMPOSIUM 3, KEPLER KASC-7 JOINT MEETING SE EPJ Web of Conferences LA English DT Proceedings Paper CT Symposium 3 on Space Photometry Revolution - CoRoT / Kepler KASC-7 Joint Meeting CY JUL 06-11, 2014 CL Toulouse, FRANCE ID TRANSMISSION SPECTRA AB Stellar activity features such as spots and plages can create difficulties in determining planetary parameters through spectroscopic and photometric observations. The overlap of a transiting planet and a stellar spot, for instance, can produce anomalies in the transit light curve that may lead to inaccurate estimation of the transit duration, depth, and timing. Such inaccuracies can affect the precise derivation of the planet's radius. In this talk we will present the results of a quantitative study on the effects of stellar spots on high precision transit light curves. We show that spot anomalies can lead to the estimate of a planet radius that is 4% smaller than the real value. The effects on the transit duration can also be of the order of 4%, longer or shorter. Depending on the size and distribution of spots, anomalies can also produce transit timing variations with significant amplitudes. For instance, TTVs with signal amplitudes of 200 seconds can be produced by spots as large as the largest sunspot. Finally, we examine the impact of active regions on the transit depth measurements in different wavelengths, in order to probe the impact of this effect on transmission spectroscopy measurements. We show that significant (up to 10%) underestimation/overestimation of the planet-to-star radius ratio can be measured, especially in the short wavelength regime. C1 [Oshagh, M.; Santos, N. C.; Figueira, P.; Santerne, A.] Univ Porto, Ctr Astrofis, Rua Estrelas, P-4150762 Oporto, Portugal. [Oshagh, M.; Santos, N. C.; Figueira, P.; Santerne, A.] Univ Porto, CAUP, Inst Astrofis & Ciencias Espaco, P-4150762 Oporto, Portugal. [Oshagh, M.; Santos, N. C.] Univ Porto, Fac Ciencias, Dept Fis & Astron, P-4169007 Oporto, Portugal. [Boisse, I] Aix Marseille Univ, CNRS, LAM, UMR 7326, F-13388 Marseille 13, France. [Boue, G.] UPMC, Observ Paris, Astron & Syst Dynam, IMCCE,CNRS,UMR 8028, F-75014 Paris, France. [Ehrenreich, D.] Univ Geneva, Observ Geneve, CH-1290 Sauverny, Switzerland. [Haghighipour, N.] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. [Haghighipour, N.] Univ Hawaii Manoa, Astrobiol Inst, NASA, Honolulu, HI 96822 USA. [Dumusque, X.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Oshagh, M (reprint author), Univ Porto, Ctr Astrofis, Rua Estrelas, P-4150762 Oporto, Portugal. EM moshagh@astro.up.pt RI Figueira, Pedro/J-4916-2013 OI Figueira, Pedro/0000-0001-8504-283X NR 9 TC 2 Z9 2 U1 0 U2 1 PU E D P SCIENCES PI CEDEX A PA 17 AVE DU HOGGAR PARC D ACTIVITES COUTABOEUF BP 112, F-91944 CEDEX A, FRANCE SN 2100-014X J9 EPJ WEB CONF PY 2015 VL 101 AR UNSP 05003 DI 10.1051/epjconf/201510105003 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE5BE UT WOS:000372491300034 ER PT S AU Poppenhaeger, K AF Poppenhaeger, K. BE Garcia, RA Ballot, J TI Stellar magnetic activity - Star-Planet Interactions SO SPACE PHOTOMETRY REVOLUTION - COROT SYMPOSIUM 3, KEPLER KASC-7 JOINT MEETING SE EPJ Web of Conferences LA English DT Proceedings Paper CT Symposium 3 on Space Photometry Revolution - CoRoT / Kepler KASC-7 Joint Meeting CY JUL 06-11, 2014 CL Toulouse, FRANCE ID X-RAY-EMISSION; EXTRASOLAR GIANT PLANETS; EARTH-LIKE EXOPLANETS; EJECTION CME ACTIVITY; MAIN-SEQUENCE STARS; IN HABITABLE ZONES; MASS M-STARS; HOT JUPITERS; HOST STARS; ATMOSPHERIC ESCAPE AB Stellar magnetic activity is an important factor in the formation and evolution of exoplanets. Magnetic phenomena like stellar flares, coronal mass ejections, and high-energy emission affect the exoplanetary atmosphere and its mass loss over time. One major question is whether the magnetic evolution of exoplanet host stars is the same as for stars without planets; tidal and magnetic interactions of a star and its close-in planets may play a role in this. Stellar magnetic activity also shapes our ability to detect exoplanets with different methods in the first place, and therefore we need to understand it properly to derive an accurate estimate of the existing exoplanet population. I will review recent theoretical and observational results, as well as outline some avenues for future progress. C1 [Poppenhaeger, K.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambrigde, MA 02138 USA. [Poppenhaeger, K.] NASA, New York, NY USA. RP Poppenhaeger, K (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambrigde, MA 02138 USA. EM kpoppenhaeger@cfa.harvard.edu OI Poppenhaeger, Katja/0000-0003-1231-2194 NR 66 TC 1 Z9 1 U1 0 U2 0 PU E D P SCIENCES PI CEDEX A PA 17 AVE DU HOGGAR PARC D ACTIVITES COUTABOEUF BP 112, F-91944 CEDEX A, FRANCE SN 2100-014X J9 EPJ WEB CONF PY 2015 VL 101 AR 05002 DI 10.1051/epjconf/201510105002 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE5BE UT WOS:000372491300033 ER PT S AU Szabo, R Benko, JM Paparo, M Chapellier, E Poretti, E Baglin, A Weiss, WW Kolenberg, K Guggenberger, E Le Borgne, JF AF Szabo, R. Benko, J. M. Paparo, M. Chapellier, E. Poretti, E. Baglin, A. Weiss, W. W. Kolenberg, K. Guggenberger, E. Le Borgne, J. -F. BE Garcia, RA Ballot, J TI The space photometry revolution and our understanding of RR Lyrae stars SO SPACE PHOTOMETRY REVOLUTION - COROT SYMPOSIUM 3, KEPLER KASC-7 JOINT MEETING SE EPJ Web of Conferences LA English DT Proceedings Paper CT Symposium 3 on Space Photometry Revolution - CoRoT / Kepler KASC-7 Joint Meeting CY JUL 06-11, 2014 CL Toulouse, FRANCE ID BLAZHKO MODULATION; NONRADIAL MODE; KEPLER; MISSION; ASTEROSEISMOLOGY AB The study of RRLyrae stars has recently been invigorated thanks to the long, uninterrupted, ultra-precise time series data provided by the Kepler and CoRoT space telescopes. We give a brief overview of the new observational findings concentrating on the connection between period doubling and the Blazhko modulation, and the omnipresence of additional periodicities in all RR Lyrae subtypes, except for non-modulated RRab stars. Recent theoretical results demonstrate that if more than two modes are present in a nonlinear dynamical system such as a high-amplitude RR Lyrae star, the outcome is often an extremely intricate dynamical state. Thus, based on these discoveries, an underlying picture of complex dynamical interactions between modes is emerging which sheds new light on the century-old Blazhko-phenomenon, as well. New directions of theoretical efforts, like multidimensional hydrodynamical simulations, future space photometric missions and detailed spectroscopic investigations will pave the way towards a more complete understanding of the atmospheric and pulsation dynamics of these enigmatic touchstone objects. C1 [Szabo, R.; Benko, J. M.; Paparo, M.] Konkoly Observ Budapest, MTA CSFK, Konkoly Thege Miklos Ut 15-17, H-1121 Budapest, Hungary. [Chapellier, E.] Univ Nice Sophia Antipolis, Lab Lagrange, UMR 7293, Observ Cote Azur, F-06300 Nice, France. [Poretti, E.] Osserv Astron Brera, INAF, I-23807 Merate, LC, Italy. [Baglin, A.] Univ Paris 07, Univ Paris 06, Observ Paris, LESIA, F-92195 Meudon, France. [Weiss, W. W.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria. [Kolenberg, K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kolenberg, K.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Heverlee, Belgium. [Guggenberger, E.] Max Planck Inst Solar Syst Res, D-37077 Gottingen, Germany. [Guggenberger, E.] Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, DK-8000 Aarhus C, Denmark. [Le Borgne, J. -F.] Univ Toulouse, IRAP, UPS OMP, Toulouse, France. [Le Borgne, J. -F.] CNRS, IRAP, F-31400 Toulouse, France. RP Szabo, R (reprint author), Konkoly Observ Budapest, MTA CSFK, Konkoly Thege Miklos Ut 15-17, H-1121 Budapest, Hungary. EM rszabo@konkoly.hu NR 27 TC 0 Z9 0 U1 0 U2 0 PU E D P SCIENCES PI CEDEX A PA 17 AVE DU HOGGAR PARC D ACTIVITES COUTABOEUF BP 112, F-91944 CEDEX A, FRANCE SN 2100-014X J9 EPJ WEB CONF PY 2015 VL 101 AR 01003 DI 10.1051/epjconf/201510101003 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE5BE UT WOS:000372491300004 ER PT S AU Bruzzone, L Plaut, JJ Alberti, G Blankenship, DD Bovolo, F Campbell, BA Castelletti, D Gim, Y Ilisei, AM Kofman, W Komatsu, G McKinnon, W Mitri, G Moussessian, A Notarnicola, C Orosei, R Patterson, GW Pettinelli, E Plettemeier, D AF Bruzzone, L. Plaut, J. J. Alberti, G. Blankenship, D. D. Bovolo, F. Campbell, B. A. Castelletti, D. Gim, Y. Ilisei, A. M. Kofman, W. Komatsu, G. McKinnon, W. Mitri, G. Moussessian, A. Notarnicola, C. Orosei, R. Patterson, G. W. Pettinelli, E. Plettemeier, D. GP IEEE TI JUPITER ICY MOON EXPLORER (JUICE): ADVANCES IN THE DESIGN OF THE RADAR FOR ICY MOONS (RIME) SO 2015 IEEE INTERNATIONAL GEOSCIENCE AND REMOTE SENSING SYMPOSIUM (IGARSS) SE IEEE International Symposium on Geoscience and Remote Sensing IGARSS LA English DT Proceedings Paper CT IEEE International Geoscience and Remote Sensing Symposium (IGARSS) CY JUL 26-31, 2015 CL Milan, ITALY SP IEEE DE radar sounder; ice penetrating radar; radar design; RIME; JUICE; icy moons; Jovian system; planetary exploration AB This paper presents the Radar for Icy Moon Exploration (RIME) that is a fundamental payload in the Jupiter Icy Moon Explorer (JUICE) mission of the European Space Agency (ESA). RIME is a radar sounder aimed to study the subsurface of Jupiter's icy moons Ganymede, Europa and Callisto. The paper illustrates the main goals of RIME, its architecture and parameters and some recent advances in its design. C1 [Bruzzone, L.; Castelletti, D.; Ilisei, A. M.] Univ Trento, Dept Informat Engn & Comp Sci, Trento, Trento, Italy. [Plaut, J. J.; Gim, Y.; Moussessian, A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Alberti, G.] CORISTA, Naples, Italy. [Blankenship, D. D.; Pettinelli, E.] Univ Texas Austin, Inst Geophys, Austin, TX 78712 USA. [Bovolo, F.] Fdn Bruno Kessler, Ctr Informat & Commun Technol, Trento, Trento, Italy. [Campbell, B. A.] Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. [Kofman, W.] Inst Planetol & Astrophys Grenoble IPAG CNRS UJF, Grenoble, France. [Komatsu, G.] Univ G dAnnunzio, Int Res Sch Planetary Sci, Pescara, Italy. [McKinnon, W.] Washington Univ, St Louis, MO USA. [Mitri, G.] Univ Nantes, Lab Planetol & Geodynam, Nantes, France. [Notarnicola, C.] EURAC, Bolzano, Italy. [Orosei, R.] INAF IRA, Bologna, Italy. [Patterson, G. W.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA. Univ Roma Tre, Rome, Italy. [Plettemeier, D.] Tech Univ Dresden, D-01062 Dresden, Germany. RP Bruzzone, L (reprint author), Univ Trento, Dept Informat Engn & Comp Sci, Trento, Trento, Italy. EM lorenzo.bruzzone@ing.unitn.it RI Komatsu, Goro/I-7822-2012; Patterson, Gerald/E-7699-2015 OI Komatsu, Goro/0000-0003-4155-108X; NR 4 TC 1 Z9 1 U1 0 U2 2 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 2153-6996 BN 978-1-4799-7929-5 J9 INT GEOSCI REMOTE SE PY 2015 BP 1257 EP 1260 PG 4 WC Engineering, Electrical & Electronic; Geosciences, Multidisciplinary; Remote Sensing SC Engineering; Geology; Remote Sensing GA BE4GM UT WOS:000371696701094 ER PT S AU Godwin, A Scott, TD Potvin, G Sonnert, G Sadler, PM AF Godwin, Allison Scott, Tyler D. Potvin, Geoff Sonnert, Gerhard Sadler, Phillip M. GP IEEE TI The Academic Performance Index: Creating a More Robust and Less Biased Measure of Student Academic Performance SO FRONTIERS IN EDUCATION CONFERENCE (FIE), 2015 SE Frontiers in Education Conference LA English DT Proceedings Paper CT 45th Annual Frontiers in Education Conference (FIE) CY OCT 21-24, 2015 CL El Paso, TX SP IEEE Educ Soc, IEEE Comp Soc, ASEE Educ Res & Methods Div, New Mexico State Univ, Univ Texas El Paso, Hewlett Packard, VentureWell, Markkula Ctr Appl Eth, IEEE DE API; academic performance; measurements; controls AB This paper introduces an alternative to singular performance measures through the creation of a scaled index incorporating a variety of performance factors indicating overall student success as well as the creation of similar sub-indices for performances in the particular areas of math, English, and science. These indices have been used in two studies based on nationally representative college student data: the Sustainability and Gender in Engineering (SaGE) and the Outreach Programs and Science Career Intentions (OPSCI) projects. The Academic Performance Index (API) is a scale constructed out of students' weighted high school GPA, available standardized test scores (ACT/SAT), AP test scores (if any), highest levels of various high school coursework taken, and college credit hours earned prior to enrolling in college. Importantly, the API uses any and all available data in these domains, which can be up to 42 different indicators for an individual student in the case of the SaGE project. This index shows less bias regarding race and gender, when compared with commonly-used standardized tests scores. Additionally, this item is psychometrically better at indicating variation across students' performance. C1 [Godwin, Allison] Purdue Univ, Sch Engn Educ, W Lafayette, IN 47907 USA. [Scott, Tyler D.] Northwestern Coll, Dept Phys, Orange City, IA USA. [Potvin, Geoff] Florida Int Univ, Dept Phys, Miami, FL 33199 USA. [Potvin, Geoff] Florida Int Univ, STEM Transformat Inst, Miami, FL 33199 USA. [Sonnert, Gerhard; Sadler, Phillip M.] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Godwin, A (reprint author), Purdue Univ, Sch Engn Educ, W Lafayette, IN 47907 USA. EM godwina@purdue.edu; tyler.scott@nwciowa.edu; gpotvin@fiu.edu; gsonnert@cfa.harvard.edu; psadler@cfa.harvard.edu NR 25 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 0190-5848 BN 978-1-4799-8454-1 J9 PROC FRONT EDUC CONF PY 2015 BP 1573 EP 1580 PG 8 WC Education, Scientific Disciplines; Engineering, Electrical & Electronic SC Education & Educational Research; Engineering GA BE4GO UT WOS:000371705200267 ER PT J AU Ricker, GR Winn, JN Vanderspek, R Latham, DW Bakos, GA Bean, JL Berta-Thompson, ZK Brown, TM Buchhave, L Butler, NR Butler, RP Chaplin, WJ Charbonneau, D Christensen-Dalsgaard, J Clampin, M Deming, D Doty, J De Lee, N Dressing, C Dunham, EW Endl, M Fressin, F Ge, J Henning, T Holman, MJ Howard, AW Ida, S Jenkins, JM Jernigan, G Johnson, JA Kaltenegger, L Kawai, N Kjeldsen, H Laughlin, G Levine, AM Lin, D Lissauer, JJ MacQueen, P Marcy, G McCullough, PR Morton, TD Narita, N Paegert, M Palle, E Pepe, F Pepper, J Quirrenbach, A Rinehart, SA Sasselov, D Sato, B Seager, S Sozzetti, A Stassun, KG Sullivan, P Szentgyorgyi, A Torres, G Udry, S Villasenor, J AF Ricker, George R. Winn, Joshua N. Vanderspek, Roland Latham, David W. Bakos, Gaspar A. Bean, Jacob L. Berta-Thompson, Zachory K. Brown, Timothy M. Buchhave, Lars Butler, Nathaniel R. Butler, R. Paul Chaplin, William J. Charbonneau, David Christensen-Dalsgaard, Jorgen Clampin, Mark Deming, Drake Doty, John De Lee, Nathan Dressing, Courtney Dunham, Edward W. Endl, Michael Fressin, Francois Ge, Jian Henning, Thomas Holman, Matthew J. Howard, Andrew W. Ida, Shigeru Jenkins, Jon M. Jernigan, Garrett Johnson, John Asher Kaltenegger, Lisa Kawai, Nobuyuki Kjeldsen, Hans Laughlin, Gregory Levine, Alan M. Lin, Douglas Lissauer, Jack J. MacQueen, Phillip Marcy, Geoffrey McCullough, Peter R. Morton, Timothy D. Narita, Norio Paegert, Martin Palle, Enric Pepe, Francesco Pepper, Joshua Quirrenbach, Andreas Rinehart, Stephen A. Sasselov, Dimitar Sato, Bun'ei Seager, Sara Sozzetti, Alessandro Stassun, Keivan G. Sullivan, Peter Szentgyorgyi, Andrew Torres, Guillermo Udry, Stephane Villasenor, Joel TI Transiting Exoplanet Survey Satellite SO JOURNAL OF ASTRONOMICAL TELESCOPES INSTRUMENTS AND SYSTEMS LA English DT Article DE exoplanet; extrasolar planet; photometry; satellite; transits ID KEPLER; PLANETS; STARS; MISSION; SYSTEMS; CATALOG AB The Transiting Exoplanet Survey Satellite (TESS) will search for planets transiting bright and nearby stars. TESS has been selected by NASA for launch in 2017 as an Astrophysics Explorer mission. The spacecraft will be placed into a highly elliptical 13.7-day orbit around the Earth. During its 2-year mission, TESS will employ four wide-field optical charge-coupled device cameras to monitor at least 200,000 main-sequence dwarf stars with I-C approximate to 4-13 for temporary drops in brightness caused by planetary transits. Each star will be observed for an interval ranging from 1 month to 1 year, depending mainly on the star's ecliptic latitude. The longest observing intervals will be for stars near the ecliptic poles, which are the optimal locations for follow-up observations with the James Webb Space Telescope. Brightness measurements of preselected target stars will be recorded every 2 min, and full frame images will be recorded every 30 min. TESS stars will be 10 to 100 times brighter than those surveyed by the pioneering Kepler mission. This will make TESS planets easier to characterize with follow-up observations. TESS is expected to find more than a thousand planets smaller than Neptune, including dozens that are comparable in size to the Earth. Public data releases will occur every 4 months, inviting immediate community-wide efforts to study the new planets. The TESS legacy will be a catalog of the nearest and brightest stars hosting transiting planets, which will endure as highly favorable targets for detailed investigations. (C) The Authors. Published by SPIE under a Creative Commons Attribution 3.0 Unported License. Distribution or reproduction of this work in whole or in part requires full attribution of the original publication, including its DOI. C1 [Ricker, George R.; Winn, Joshua N.; Vanderspek, Roland; Berta-Thompson, Zachory K.; Levine, Alan M.; Seager, Sara; Sullivan, Peter; Villasenor, Joel] MIT, 77 Massachusetts Ave, Cambridge, MA 02139 USA. [Latham, David W.; Buchhave, Lars; Charbonneau, David; Dressing, Courtney; Fressin, Francois; Holman, Matthew J.; Johnson, John Asher; Sasselov, Dimitar; Szentgyorgyi, Andrew; Torres, Guillermo] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bakos, Gaspar A.; Morton, Timothy D.] Princeton Univ, Princeton, NJ 08540 USA. [Bean, Jacob L.] Univ Chicago, Chicago, IL 60611 USA. [Brown, Timothy M.] Las Cumbres Observ Global Telescope, Goleta, CA 93117 USA. [Buchhave, Lars] Univ Copenhagen, DK-1165 Copenhagen, Denmark. [Butler, Nathaniel R.] Arizona State Univ, Tempe, AZ 85004 USA. [Butler, R. Paul] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA. [Chaplin, William J.] Univ Birmingham, Birmingham B15 2TT, W Midlands, England. [Chaplin, William J.; Christensen-Dalsgaard, Jorgen; Kjeldsen, Hans] Univ Aarhus, Stellar Astrophys Ctr, DK-8000 Aarhus, Denmark. [Clampin, Mark; Rinehart, Stephen A.] NASA, Goddard Space Flight Ctr, Green Belt, MD 20771 USA. [Deming, Drake] Univ Maryland, College Pk, MD 20742 USA. [Doty, John] Noqsi Aerosp Ltd, Pine, CO 80470 USA. [De Lee, Nathan] No Kentucky Univ, Highland Hts, KY 41099 USA. [De Lee, Nathan; Paegert, Martin; Pepper, Joshua; Stassun, Keivan G.] Vanderbilt Univ, Nashville, TN 37235 USA. [Dunham, Edward W.] Lowell Observ, Flagstaff, AZ 86001 USA. [Endl, Michael; MacQueen, Phillip] McDonald Observ, Austin, TX 78712 USA. [Ge, Jian] Univ Florida, Gainesville, FL 32611 USA. [Henning, Thomas; Kaltenegger, Lisa] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Howard, Andrew W.] Univ Hawaii, Manoa, HI 96822 USA. [Ida, Shigeru; Kawai, Nobuyuki; Sato, Bun'ei] Tokyo Inst Technol, Tokyo 1528851, Japan. [Jenkins, Jon M.; Lissauer, Jack J.] NASA, Ames Res Ctr, Mountain View, CA 94035 USA. [Jernigan, Garrett] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Laughlin, Gregory; Lin, Douglas] UCO, Lick Observ, Santa Cruz, CA 95064 USA. [Marcy, Geoffrey] Univ Calif Berkeley, Berkeley, CA 94720 USA. [McCullough, Peter R.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [McCullough, Peter R.] Johns Hopkins Univ, Baltimore, MD 21218 USA. [Narita, Norio] Natl Astron Observ Japan, Tokyo 1818588, Japan. [Palle, Enric] Inst Astrofis Canarias, E-38205 San Cristobal la Laguna, Tenerife, Spain. [Pepe, Francesco; Udry, Stephane] Observ Geneva, CH-1290 Versoix, Switzerland. [Pepper, Joshua] Lehigh Univ, Bethlehem, PA 18015 USA. [Quirrenbach, Andreas] Heidelberg Univ, Zentrum Astron, Landessternwarte, D-69117 Heidelberg, Germany. [Sozzetti, Alessandro] INAF, Osservatorio Astrofis Torino, I-10025 Turin, Italy. [Stassun, Keivan G.] Fisk Univ, Nashville, TN 37208 USA. RP Ricker, GR (reprint author), MIT, 77 Massachusetts Ave, Cambridge, MA 02139 USA. EM grr@space.mit.edu NR 33 TC 93 Z9 93 U1 6 U2 12 PU SPIE-SOC PHOTO-OPTICAL INSTRUMENTATION ENGINEERS PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA SN 2329-4124 EI 2329-4221 J9 J ASTRON TELESC INST JI J. Astron. Telesc. Instrum. Syst. PD JAN-MAR PY 2015 VL 1 IS 1 AR 014003 DI 10.1117/1.JATIS.1.1.014003 PG 10 WC Engineering, Aerospace; Instruments & Instrumentation; Optics SC Engineering; Instruments & Instrumentation; Optics GA DG2EP UT WOS:000371879500004 ER PT S AU Zaninoni, E Bernardini, MG Margutti, R Amati, L AF Zaninoni, Elena Bernardini, Maria Grazia Margutti, Raffaella Amati, Lorenzo BE DeAlmeida, UB Chardonnet, P Negreiros, RP Rueda, J Ruffini, R Vereshchagin, G Vasconcellos, CZ TI Ten Years of Swift: a Universal Scaling for Short and Long Gamma-Ray Bursts (E-X,E-iso - E-gamma,E-iso - E-pk) SO SECOND ICRANET CESAR LATTES MEETING: SUPERNOVAE, NEUTRON STARS AND BLACK HOLES SE AIP Conference Proceedings LA English DT Proceedings Paper CT 2nd ICRANet Cesar Lattes Meeting - Supernovae, Neutron Stars and Black Holes CY APR 13-22, 2015 CL Rio De Janeiro, BRAZIL SP Cent Brasileiro Pesquisas Fisicas, Coordenacao Aperfeicoamento Pessoal Nivel Super, European Union, Educ Audiovisual & Culture Execut Agcy, Espaco Ciencia Recife, Estacao Ciencias Auditorium Joao Pessoa, Fundacao Carlos Chagas Filho Amparo Pesquisa Estado Rio De Janeiro, Fundacao Planetario Cidade Rio De Janeiro, Inst Fed Educacao Ciencia Tecnologia Ceara, Int Ctr Relativist Astrophys Network, Univ Fed Paraiba, Univ Fed Pernambuco, Univ Fed Fluminense, ICTP, Ceara, ITA, IHEP, UNS, Univ Sapienza Rome, UNAM, INPE, UIS, Univ Nice Sophia Antipolis, State Comm Sci RA, NAS Armenia, FAPERJ, Consortium GARR, BSU, IHES, NASB, ASI, UNIFEI, Al Farabi Kazhak Natl Univ, Univ Fed Rio Grande Sul, Inst Fisica, Univ Estado Rio De Janeiro, UFF, UAM, CNR, UFSC, UFPE, INFN, IFCE, LeCosPA, UnB ID PHOTOSPHERIC EMISSION; LIGHT CURVES; PEAK ENERGY; GRB 101225A; PROMPT; AFTERGLOW; SPECTRA; EFFICIENCY; REDSHIFT; MERGERS AB From the comprehensive statistical analysis of Swift X-ray light-curves collected from the launch of the Swift satellite until the end of 2010, we found a three-parameter correlation between the isotropic energy emitted in the rest frame 1-10(4) keV energy band during the prompt emission (E-gamma,E-iso), the rest frame peak of the prompt emission energy spectrum (E-pk), and the X-ray energy emitted in the rest frame 0.3-30 keV observed energy band (E-X,E-iso), computed excluding the contribution of the flares. The importance of this scaling law is that it is followed by both long and short GRBs, and, at the same time, involves prompt and afterglow emission quantities. Therefore there are some properties which are shared by long and short GRBs as a whole. We updated this correlation considering all GRBs observed until June 2014, confirming the existence of this scaling law, and examining some particular GRBs, as 090426 and 100816A. We also discuss the physics that is driving this correlation. C1 [Zaninoni, Elena] ICRANet Rio, Ctr Brasileiro Pesquisas Fis, Rua Dr Xavier Sigaud 150, BR-22290180 Rio De Janeiro, Brazil. [Bernardini, Maria Grazia] Osserv Astron Brera, INAF, I-23807 Merate, Italy. [Margutti, Raffaella] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Amati, Lorenzo] INAF, Ist Astrofis Spaziale & Fis Cosm, I-40129 Bologna, Italy. RP Zaninoni, E (reprint author), ICRANet Rio, Ctr Brasileiro Pesquisas Fis, Rua Dr Xavier Sigaud 150, BR-22290180 Rio De Janeiro, Brazil. EM elena.zaninoni@gmail.com NR 38 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 978-0-7354-1340-5 J9 AIP CONF PROC PY 2015 VL 1693 AR 050008 DI 10.1063/1.4937201 PG 7 WC Astronomy & Astrophysics; Physics, Applied SC Astronomy & Astrophysics; Physics GA BE4DR UT WOS:000371596000023 ER PT B AU Mink, J Mann, RG Hanisch, R Rots, A Seaman, R Jenness, T Thomas, B O'Mullane, W AF Mink, Jessica Mann, Robert G. Hanisch, Robert Rots, Arnold Seaman, Rob Jenness, Tim Thomas, Brian O'Mullane, William BE Taylor, AR Rosolowsky, E TI The Past, Present, and Future of Astronomical Data Formats SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS: XXIV SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 24th International Conference on Astronomical Data Analysis Software and Systems, ADASS XXIV CY OCT 05-09, 2014 CL Univ Calgary, Calgary, CANADA SP Anglo-Australian Observ, Cybera Inc, Univ Calgary, European Space Agcy, European So Observ, Infrared Process & Anal Ctr, Natl Opt Astron Observ, Smithsonian Astrophys Observ, Space Telescope Sci Inst HO Univ Calgary ID COMPRESSION AB The future of astronomy is inextricably entwined with the care and feeding of astronomical data products. Community standards such as FITS and NDF have been instrumental in the success of numerous astronomy projects. Their very success challenges us to entertain pragmatic strategies to adapt and evolve the standards to meet the aggressive data-handling requirements of facilities now being designed and built. We discuss characteristics that have made standards successful in the past, as well as desirable features for the future, and an open discussion follows. C1 [Mink, Jessica; Rots, Arnold] Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. [Mann, Robert G.] Univ Edinburgh, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. [Hanisch, Robert] NIST, Off Data & Informat, Mat Measurement Lab, Gaithersburg, MD USA. [Seaman, Rob; Thomas, Brian] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Jenness, Tim] Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA. [O'Mullane, William] European Space Agcy, Sci Operat Dept, European Space Astron Ctr, Madrid, Spain. RP Mink, J (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. NR 18 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 978-1-58381-875-6; 978-1-58381-874-9 J9 ASTR SOC P PY 2015 VL 495 BP 11 EP 18 PG 8 WC Astronomy & Astrophysics; Computer Science, Information Systems; Computer Science, Interdisciplinary Applications SC Astronomy & Astrophysics; Computer Science GA BE3OY UT WOS:000371098000003 ER PT B AU Beaumont, C Goodman, A Greenfield, P AF Beaumont, Christopher Goodman, Alyssa Greenfield, Perry BE Taylor, AR Rosolowsky, E TI Hackable User Interfaces In Astronomy with Glue SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS: XXIV SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 24th International Conference on Astronomical Data Analysis Software and Systems, ADASS XXIV CY OCT 05-09, 2014 CL Univ Calgary, Calgary, CANADA SP Anglo-Australian Observ, Cybera Inc, Univ Calgary, European Space Agcy, European So Observ, Infrared Process & Anal Ctr, Natl Opt Astron Observ, Smithsonian Astrophys Observ, Space Telescope Sci Inst HO Univ Calgary AB Astronomers typically choose between Graphical User Interfaces and custom-written computer code when exploring and analyzing data. Few tools are designed to encourage both of these workflows, despite their complementary strengths. We believe that such hybrid hackable user interfaces could enable more agile data exploration, combining the fluidity that comes from a GUI with the precision and reproducibility that comes from writing code. In this article we articulate the different strengths and weaknesses of both workflows and discuss how to enable both in a single tool. We focus on Glue (http://glue-viz.org) as a case study and examine how the goal of creating a hackable user interface has influenced the design of Glue. C1 [Beaumont, Christopher; Goodman, Alyssa] Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 42, Cambridge, MA 02138 USA. [Greenfield, Perry] Space Telescope Sci Inst, Baltimore, MD 21218 USA. RP Beaumont, C (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 42, Cambridge, MA 02138 USA. NR 12 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 978-1-58381-875-6; 978-1-58381-874-9 J9 ASTR SOC P PY 2015 VL 495 BP 101 EP 109 PG 9 WC Astronomy & Astrophysics; Computer Science, Information Systems; Computer Science, Interdisciplinary Applications SC Astronomy & Astrophysics; Computer Science GA BE3OY UT WOS:000371098000019 ER PT B AU Miller, J Burke, DJ Evans, IN Evans, JD McLaughlin, W AF Miller, Joseph Burke, Douglas J. Evans, Ian N. Evans, Janet D. McLaughlin, Warren BE Taylor, AR Rosolowsky, E TI Reviewing ChIPS, The Chandra Imaging and Plotting System SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS: XXIV SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 24th International Conference on Astronomical Data Analysis Software and Systems, ADASS XXIV CY OCT 05-09, 2014 CL Univ Calgary, Calgary, CANADA SP Anglo-Australian Observ, Cybera Inc, Univ Calgary, European Space Agcy, European So Observ, Infrared Process & Anal Ctr, Natl Opt Astron Observ, Smithsonian Astrophys Observ, Space Telescope Sci Inst HO Univ Calgary AB The Chandra Imaging and Plotting System (ChIPS) is a 2D plotting system designed to allow users to easily create, manipulate, and produce publication quality visualizations. ChIPS has a simple but very powerful interactive interface that allows users to dynamically modify the contents and layout of their plots quickly and efficiently, with the results of any changes being immediately visible. ChIPS allows users to construct their plots fully interactively, and then save the final plot commands as a Python script. This bypasses the need to iteratively edit and rerun the script when developing the plot. Features such as undo and redo commands allow users to easily step backwards and forwards through previous commands, while the ability so save ChIPS sessions in a platform-independent state file allows the session to be restored at any time, even on another machine. Because ChIPS offers a Python interface, users can analyze their data using the broad array of modules offered in Python, and visualize the information in ChIPS at the same time. In this paper we explore the design decisions behind the development of ChIPS and some of the lessons learned along the way. C1 [Miller, Joseph; Burke, Douglas J.; Evans, Ian N.; Evans, Janet D.; McLaughlin, Warren] Smithsonian Astrophys Observ, 60 Garden St,MS-81, Cambridge, MA 02138 USA. RP Miller, J (reprint author), Smithsonian Astrophys Observ, 60 Garden St,MS-81, Cambridge, MA 02138 USA. 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 978-1-58381-875-6; 978-1-58381-874-9 J9 ASTR SOC P PY 2015 VL 495 BP 111 EP 119 PG 9 WC Astronomy & Astrophysics; Computer Science, Information Systems; Computer Science, Interdisciplinary Applications SC Astronomy & Astrophysics; Computer Science GA BE3OY UT WOS:000371098000020 ER PT B AU Mink, J Moran, S AF Mink, Jessica Moran, Sean BE Taylor, AR Rosolowsky, E TI Thirty Years, One Million Spectra: Public Access to the SAO Spectral Archives SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS: XXIV SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 24th International Conference on Astronomical Data Analysis Software and Systems, ADASS XXIV CY OCT 05-09, 2014 CL Univ Calgary, Calgary, CANADA SP Anglo-Australian Observ, Cybera Inc, Univ Calgary, European Space Agcy, European So Observ, Infrared Process & Anal Ctr, Natl Opt Astron Observ, Smithsonian Astrophys Observ, Space Telescope Sci Inst HO Univ Calgary ID REDUCTION AB Over the last 30 years, the SAO Telescope Data Center has reduced and archived over 1,000,000 spectra, consisting of 287,000 spectra from five high dispersion Echelle spectrographs and 717,000 spectra from four low dispersion spectrographs, across three telescopes. 151,000 spectra from six instruments are currently online and publicly available, covering many interesting objects in the northern sky, including most of the galaxies in the Updated Zwicky Catalog which are reachable through NED or Simbad. A majority of the high dispersion spectra will soon be made public, as will more data from the MMT multi-fiber spectrographs. Many objects in the archive have multiple spectra over time, which make them a valuable resource for archival time domain studies. We are now developing a system to make all of the public spectra more easily searchable and viewable through the Virtual Observatory. C1 [Mink, Jessica; Moran, Sean] Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. RP Mink, J (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. 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 978-1-58381-875-6; 978-1-58381-874-9 J9 ASTR SOC P PY 2015 VL 495 BP 153 EP 156 PG 4 WC Astronomy & Astrophysics; Computer Science, Information Systems; Computer Science, Interdisciplinary Applications SC Astronomy & Astrophysics; Computer Science GA BE3OY UT WOS:000371098000029 ER PT B AU Evans, I AF Evans, Ian CA Chandra Source Catalog Project Tea BE Taylor, AR Rosolowsky, E TI Building Release 2 of the Chandra Source Catalog SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS: XXIV SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 24th International Conference on Astronomical Data Analysis Software and Systems, ADASS XXIV CY OCT 05-09, 2014 CL Univ Calgary, Calgary, CANADA SP Anglo-Australian Observ, Cybera Inc, Univ Calgary, European Space Agcy, European So Observ, Infrared Process & Anal Ctr, Natl Opt Astron Observ, Smithsonian Astrophys Observ, Space Telescope Sci Inst HO Univ Calgary AB The second major release of the Chandra Source Catalog builds on the first catalog release by stacking subsets of overlapping observations, using a permissive source detection approach to identify source candidates and enable point detections down to similar to 5 net counts on-axis, and evaluating the reality of the candidate detections by applying a Sherpa-based maximum-likelihood estimatorlThe catalog provides a detailed set of properties for each X-ray source, including source position, extent, multi band aperture photometry, spectral fits and hardness ratios, and temporal variability measures. In addition, the catalog provides per-field and per-source data products such as images, photon event lists, spectra, light curves, and extended source polygons. We highlight the differences between the first and second catalog releases, and discuss the decisions that drove the changes. We present the newly developed techniques that were required to build release 2 of the catalog, and identify algorithms that have been updated. Finally, we briefly discuss lessons learned. C1 [Evans, Ian] Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. [Chandra Source Catalog Project Tea] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. RP Evans, I (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. 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 978-1-58381-875-6; 978-1-58381-874-9 J9 ASTR SOC P PY 2015 VL 495 BP 297 EP 300 PG 4 WC Astronomy & Astrophysics; Computer Science, Information Systems; Computer Science, Interdisciplinary Applications SC Astronomy & Astrophysics; Computer Science GA BE3OY UT WOS:000371098000061 ER PT B AU Laurino, O Siemiginowska, A Evans, J Aldcroft, T Burke, DJ McDowell, J McLaughlin, W Nguyen, D AF Laurino, Omar Siemiginowska, Aneta Evans, Janet Aldcroft, Thomas Burke, Douglas J. McDowell, Jonathan McLaughlin, Warren Dan Nguyen BE Taylor, AR Rosolowsky, E TI Sherpa. On the Move to Open Collaborative, Development SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS: XXIV SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 24th International Conference on Astronomical Data Analysis Software and Systems, ADASS XXIV CY OCT 05-09, 2014 CL Univ Calgary, Calgary, CANADA SP Anglo-Australian Observ, Cybera Inc, Univ Calgary, European Space Agcy, European So Observ, Infrared Process & Anal Ctr, Natl Opt Astron Observ, Smithsonian Astrophys Observ, Space Telescope Sci Inst HO Univ Calgary AB Sherpa is the Chandra Interactive Analysis of Observations (CIAO) modeling and fitting application. Written in Python, with efficient C, C++, and Fortran extensions, Sherpa enables the user to construct complex models from simple definitions and fit those models to data, using a variety of statistics and optimization methods. Sherpa is a general-purpose fitting engine with advanced capabilities, and has been used as a backend for the development of new applications like Iris, the Virtual Astronomical Observatory spectral energy distribution builder and analyzer. However, building and installing Sherpa as a standalone Python package was problematic, and such a build would not maintain all of the Sherpa capabilities. For version 4.7 (December 2014) Sherpa's build scripts have been completely rewritten, standardized, and made independent of CIAO, so that Sherpa can now be built as a fully functional standalone Python package, and yet allow users the flexibility they need in order to build Sherpa in customized environments. C1 [Laurino, Omar; Siemiginowska, Aneta; Evans, Janet; Aldcroft, Thomas; Burke, Douglas J.; McDowell, Jonathan; McLaughlin, Warren; Dan Nguyen] Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02474 USA. RP Laurino, O (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02474 USA. NR 5 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 978-1-58381-875-6; 978-1-58381-874-9 J9 ASTR SOC P PY 2015 VL 495 BP 313 EP 317 PG 5 WC Astronomy & Astrophysics; Computer Science, Information Systems; Computer Science, Interdisciplinary Applications SC Astronomy & Astrophysics; Computer Science GA BE3OY UT WOS:000371098000065 ER PT B AU Chyla, R Accomazzi, A Holachek, A Grant, CS Elliott, J Henneken, EA Thompson, DM Kurtz, MJ Murray, SS Sudilovsky, V AF Chyla, Roman Accomazzi, Alberto Holachek, Alexandra Grant, Carolyn S. Elliott, Jonathan Henneken, Edwin A. Thompson, Donna M. Kurtz, Michael J. Murray, Stephen S. Sudilovsky, Vladimir BE Taylor, AR Rosolowsky, E TI ADS 2.0: New Architecture, API and Services SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS: XXIV SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 24th International Conference on Astronomical Data Analysis Software and Systems, ADASS XXIV CY OCT 05-09, 2014 CL Univ Calgary, Calgary, CANADA SP Anglo-Australian Observ, Cybera Inc, Univ Calgary, European Space Agcy, European So Observ, Infrared Process & Anal Ctr, Natl Opt Astron Observ, Smithsonian Astrophys Observ, Space Telescope Sci Inst HO Univ Calgary AB The ADS platform is undergoing the biggest rewrite of its 20-year history. While several components have been added to its architecture over the past couple of years, this talk will concentrate on the underpinnings of ADS's search layer and its API. To illustrate the design of the components in the new system, we will show how the new ADS user interface is built exclusively on top of the API using RESTful web services. Taking one step further, we will discuss how we plan to expose the treasure trove of information hosted by ADS (10 million records and fulltext for much of the Astronomy and Physics refereed literature) to partners interested in using this API. This will provide you (and your intelligent applications) with access to ADS's underlying data to enable the extraction of new knowledge and the ingestion of these results back into the ADS. Using this framework, researchers could run controlled experiments with content extraction, machine learning, natural language processing, etc. In this talk, we will discuss what is already implemented, what will be available soon, and where we are going next. C1 [Chyla, Roman; Accomazzi, Alberto; Holachek, Alexandra; Grant, Carolyn S.; Elliott, Jonathan; Henneken, Edwin A.; Thompson, Donna M.; Kurtz, Michael J.; Murray, Stephen S.; Sudilovsky, Vladimir] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RP Chyla, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Henneken, Edwin/0000-0003-4264-2450 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 978-1-58381-875-6; 978-1-58381-874-9 J9 ASTR SOC P PY 2015 VL 495 BP 401 EP 407 PG 7 WC Astronomy & Astrophysics; Computer Science, Information Systems; Computer Science, Interdisciplinary Applications SC Astronomy & Astrophysics; Computer Science GA BE3OY UT WOS:000371098000086 ER PT B AU Hanisch, RJ Allen, A Berriman, GB DuPrie, K Mink, J Nemiroff, RJ Schmidt, J Shamir, L Shortridge, K Taylor, M Teuben, PJ Wallin, J AF Hanisch, Robert J. Allen, Alice Berriman, G. Bruce DuPrie, Kimberly Mink, Jessica Nemiroff, Robert J. Schmidt, Judy Shamir, Lior Shortridge, Keith Taylor, Mark Teuben, Peter J. Wallin, John BE Taylor, AR Rosolowsky, E TI Astrophysics Source Code Library Enhancements SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS: XXIV SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 24th International Conference on Astronomical Data Analysis Software and Systems, ADASS XXIV CY OCT 05-09, 2014 CL Univ Calgary, Calgary, CANADA SP Anglo-Australian Observ, Cybera Inc, Univ Calgary, European Space Agcy, European So Observ, Infrared Process & Anal Ctr, Natl Opt Astron Observ, Smithsonian Astrophys Observ, Space Telescope Sci Inst HO Univ Calgary AB The Astrophysics Source Code Library (ASCL)(1) is a free online registry of codes used in astronomy research; it currently contains over 900 codes and is indexed by ADS. The ASCL has recently moved a new infrastructure into production. The new site provides a true database for the code entries and integrates the WordPress news and information pages and the discussion forum into one site. Previous capabilities are retained and permalinks to ascl.net continue to work. This improvement offers more functionality and flexibility than the previous site, is easier to maintain, and offers new possibilities for collaboration. This paper covers these recent changes to the ASCL. C1 [Hanisch, Robert J.] NIST, Espoo, Finland. [Allen, Alice; DuPrie, Kimberly; Schmidt, Judy] Astrophys Source Code Lib, Baner, Maharashtra, India. [Berriman, G. Bruce] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [DuPrie, Kimberly] Space Telescope Sci Inst, Baltimore, MD USA. [Mink, Jessica] Smithsonian Astrophys Observ, Cambridge, MA USA. [Nemiroff, Robert J.] Michigan Technol Univ, Houghton, MI 49931 USA. [Shamir, Lior] Lawrence Technol Univ, Southfield, MI USA. [Shortridge, Keith] Australian Astron Observ, Coonabarabran, NSW, Australia. [Taylor, Mark] Univ Bristol, Bristol BS8 1TH, Avon, England. [Teuben, Peter J.] Univ Maryland, Bethesda, MD USA. [Wallin, John] Middle Tennessee State Univ, Murfreesboro, TN USA. RP Hanisch, RJ (reprint author), NIST, Espoo, Finland. NR 1 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 978-1-58381-875-6; 978-1-58381-874-9 J9 ASTR SOC P PY 2015 VL 495 BP 453 EP 456 PG 4 WC Astronomy & Astrophysics; Computer Science, Information Systems; Computer Science, Interdisciplinary Applications SC Astronomy & Astrophysics; Computer Science GA BE3OY UT WOS:000371098000098 ER PT B AU Lemson, G Laurino, O AF Lemson, Gerard Laurino, Omar BE Taylor, AR Rosolowsky, E TI Astronomical Data Integration Beyond the Virtual Observatory SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS: XXIV SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 24th International Conference on Astronomical Data Analysis Software and Systems, ADASS XXIV CY OCT 05-09, 2014 CL Univ Calgary, Calgary, CANADA SP Anglo-Australian Observ, Cybera Inc, Univ Calgary, European Space Agcy, European So Observ, Infrared Process & Anal Ctr, Natl Opt Astron Observ, Smithsonian Astrophys Observ, Space Telescope Sci Inst HO Univ Calgary AB "Data integration" generally refers to the process of combining data from different source data bases into a unified view. Much work has been devoted in this area by the International Virtual Observatory Alliance (IVOA), allowing users to discover and access databases through standard protocols. However, different archives present their data through their own schemas and users must still select, filter, and combine data for each archive individually. An important reason for this is that the creation of common data models that satisfy all sub-disciplines is fraught with difficulties. Furthermore it requires a substantial amount of work for data providers to present their data according to some standard representation. We will argue that existing standards allow us to build a data integration framework that works around these problems. The particular framework requires the implementation of the IVOA Table Access Protocol (TAP) only. It uses the newly developed VO data modelling language (VO-DML) specification, which allows one to define extensible object-oriented data models using a subset of UML concepts through a simple XML serialization language. A rich mapping language allows one to describe how instances of VO-DML data models are represented by the TAP service, bridging the possible mismatch between a local archive's schema and some agreed-upon representation of the astronomical domain. In this so called local-as-view approach to data integration, "mediators" use the mapping prescriptions to translate queries phrased in terms of the common schema to the underlying TAP service. This mapping language has a graphical representation, which we expose through a web based graphical "drag-and-drop-and-connect" interface. This service allows any user to map the holdings of any TAP service to the data model(s) of choice. The mappings are defined and stored outside of the data sources themselves, which allows the interface to be used in a kind of crowd-sourcing effort to annotate any remote database of interest. This reduces the burden of publishing one's data and allows a great flexibility in the definition of the views through which particular communities might wish to access remote archives. At the same time, the framework easies the user's effort to select, filter, and combine data from many different archives, so as to build knowledge bases for their analysis. We will present the framework and demonstrate a prototype implementation. We will discuss ideas for producing the missing elements, in particular the query language and the implementation of mediator tools to translate object queries to ADQL C1 [Lemson, Gerard] Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85748 Garching, Germany. [Lemson, Gerard] Johns Hopkins Univ, Baltimore, MD USA. [Laurino, Omar] Smithsonian Astrophys Observ, Cambridge, MA USA. RP Lemson, G (reprint author), Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85748 Garching, Germany. 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 978-1-58381-875-6; 978-1-58381-874-9 J9 ASTR SOC P PY 2015 VL 495 BP 513 EP 522 PG 10 WC Astronomy & Astrophysics; Computer Science, Information Systems; Computer Science, Interdisciplinary Applications SC Astronomy & Astrophysics; Computer Science GA BE3OY UT WOS:000371098000112 ER PT B AU Price, DC Barsdell, BR Greenhill, LJ AF Price, Danny C. Barsdell, Benjamin R. Greenhill, Lincoln J. BE Taylor, AR Rosolowsky, E TI Is HDF5 a Good Format to Replace UVFITS? SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS: XXIV SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 24th International Conference on Astronomical Data Analysis Software and Systems, ADASS XXIV CY OCT 05-09, 2014 CL Univ Calgary, Calgary, CANADA SP Anglo-Australian Observ, Cybera Inc, Univ Calgary, European Space Agcy, European So Observ, Infrared Process & Anal Ctr, Natl Opt Astron Observ, Smithsonian Astrophys Observ, Space Telescope Sci Inst HO Univ Calgary ID FITS; EXTENSION AB The FITS (Flexible Image Transport System) data format was developed in the late 1970s for storage and exchange of astronomy-related image data. Since then, it has become a standard file format not only for images, but also for radio interferometer data (e.g. UVFITS, FITS-IDI). But is FITS the right format for next-generation telescopes to adopt? The newer Hierarchical Data Format (HDF5) file format offers considerable advantages over FITS, but has yet to gain widespread adoption within the radio astronomy. One of the major holdbacks is that HDF5 is not well supported by data reduction software packages. Here, we present a comparison of FITS, HDF5, and the MeasurementSet (MS) format for storage of interferometric data. In addition, we present a tool for converting between formats. We show that the underlying data model of FITS can be ported to HDF5, a first step toward achieving wider HDF5 support. C1 [Price, Danny C.; Barsdell, Benjamin R.; Greenhill, Lincoln J.] Harvard Smithsonian Ctr Astrophys, MS 42 60 Garden St, Cambridge, MA 02143 USA. RP Price, DC (reprint author), Harvard Smithsonian Ctr Astrophys, MS 42 60 Garden St, Cambridge, MA 02143 USA. NR 20 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 978-1-58381-875-6; 978-1-58381-874-9 J9 ASTR SOC P PY 2015 VL 495 BP 531 EP 534 PG 4 WC Astronomy & Astrophysics; Computer Science, Information Systems; Computer Science, Interdisciplinary Applications SC Astronomy & Astrophysics; Computer Science GA BE3OY UT WOS:000371098000115 ER PT S AU Ferreira, PSF Henry, TJ Coelho, LA AF Ferreira, Paulo S. F. Henry, Thomas J. Coelho, Livia A. BE Panizzi, AR Grazia, J TI Plant Bugs (Miridae) SO TRUE BUGS (HETEROPTERA) OF THE NEOTROPICS SE Entomology in Focus LA English DT Article; Book Chapter ID HEMIPTERA HETEROPTERA MIRIDAE; GENUS PREPOPS REUTER; INSECT ORDER HETEROPTERA; NEOTROPICAL MIRIDAE; PHYLOGENETIC ANALYSIS; SPECIES HEMIPTERA; PILOPHORINI HETEROPTERA; RESTHENINI REUTER; STAL HETEROPTERA; GENERA HEMIPTERA AB The Miridae, or plant bugs, with more than 1,300 genera and 11,130 described species, represent the largest and most diverse family of Heteroptera. Although many plant bugs are phytophagous and may cause serious damage to crops, a great many are predatory and may be important in biological control programs. In the Neotropics, about 561 genera and more than 3,400 species are included in seven of the world's eight recognized subfamilies. In this chapter, we give an overview of the classification, general life history, and economic importance and provide identification keys to the Neotropical subfamilies and tribes. For each subfamily, we present a brief diagnosis, an overview of the respective tribes and subtribes, and key literature. C1 [Ferreira, Paulo S. F.] Univ Fed Vicosa, Dept Entomol, Ave Peter Henry Rolfs S-N, BR-36570900 Vicosa, MG, Brazil. [Henry, Thomas J.] Natl Museum Nat Hist, ARS, USDA, Systemat Entomol Lab,Smithsonian Inst, Washington, DC 20013 USA. [Coelho, Livia A.] Univ Fed Vicosa, Museu Reg Entomol, BR-36570900 Vicosa, MG, Brazil. RP Ferreira, PSF (reprint author), Univ Fed Vicosa, Dept Entomol, Ave Peter Henry Rolfs S-N, BR-36570900 Vicosa, MG, Brazil. EM pfiuza@ufv.br; thomas.henry@ars.usda.gov; liviaguiar04@gmail.com NR 300 TC 2 Z9 2 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 2405-8548 BN 978-94-017-9861-7; 978-94-017-9860-0 J9 ENTOMOL FOCUS PY 2015 VL 2 BP 237 EP 286 DI 10.1007/978-94-017-9861-7_10 D2 10.1007/978-94-017-9861-7 PG 50 WC Entomology SC Entomology GA BE3WN UT WOS:000371323900012 ER PT S AU Henry, TJ Dellape, PM de Paula, AS AF Henry, Thomas J. Dellape, Pablo M. de Paula, Alexandre S. BE Panizzi, AR Grazia, J TI The Big-Eyed Bugs, Chinch Bugs, and Seed Bugs (Lygaeoidea) SO TRUE BUGS (HETEROPTERA) OF THE NEOTROPICS SE Entomology in Focus LA English DT Article; Book Chapter ID HEMIPTERA HETEROPTERA LYGAEOIDEA; CLERADA-APICICORNIS HEMIPTERA; GENUS TOONGLASA HEMIPTERA; BICRUCIS SAY HETEROPTERA; NEW-SPECIES HEMIPTERA; NORTH-AMERICA; STILT BUG; WESTERN-HEMISPHERE; PENTATOMOMORPHA HEMIPTERA; RHYPAROCHROMINAE HETEROPTERA AB The Lygaeoidea, representing the second largest superfamily in the infraorder Pentatomomorpha, are one of the most diverse groups of Heteroptera with about 700 genera and more than 4,200 species in the world. In the Neotropics, about 184 genera and 836 species are included in 12 of the world's 16 families. For each family, we provide a diagnosis; an overview of the classification; information on the general life history, ecology, and economic importance; and comprehensive keys to subfamilies, tribes, and genera for the Neotropical Region, including Mexico, Central and South America, and the West Indies. C1 [Henry, Thomas J.] Natl Museum Nat Hist, ARS, USDA, Systemat Entomol Lab,Smithsonian Inst, MRC 168 ,POB 37012, Washington, DC 20013 USA. [Dellape, Pablo M.] Museo La Plata, Div Entomol, Buenos Aires, DF, Argentina. [de Paula, Alexandre S.] Univ Fed Ouro Preto, Inst Ciencias Exatas & Biol, Dept Ciencias Biol, BR-35400000 Ouro Preto, MG, Brazil. RP Henry, TJ (reprint author), Natl Museum Nat Hist, ARS, USDA, Systemat Entomol Lab,Smithsonian Inst, MRC 168 ,POB 37012, Washington, DC 20013 USA. EM thomas.henry@ars.usda.gov; pdellape@gmail.com; hetalex@terra.com.br OI Dellape, Pablo M./0000-0002-6914-1026 NR 197 TC 7 Z9 7 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 2405-8548 BN 978-94-017-9861-7; 978-94-017-9860-0 J9 ENTOMOL FOCUS PY 2015 VL 2 BP 459 EP 514 DI 10.1007/978-94-017-9861-7_16 D2 10.1007/978-94-017-9861-7 PG 56 WC Entomology SC Entomology GA BE3WN UT WOS:000371323900018 ER PT B AU De Beck, E Kaminski, T Menten, KM Patel, NA Young, KH Gottlieb, CA AF De Beck, Elvire Kaminski, Tomasz Menten, Karl M. Patel, Nimesh A. Young, Ken H. Gottlieb, Carl A. BE Kerschbaum, F Wing, RF Hron, J TI SMA Spectral Line Imaging Survey at 279-355 GHz of the Oxygen-rich AGB Star IK Tau SO WHY GALAXIES CARE ABOUT AGB STARS III: A CLOSER LOOK IN SPACE AND TIME SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT Conference on Why Galaxies Care About AGB Stars III: A Closer Look in Space and Time CY JUL 28-AUG 01, 2014 CL Univ Vienna, Vienna, AUSTRIA SP Univ Vienna, Ohio State Univ, Robert Wing Support Fund, Austrian Sci Fund, Vienna Convent Bur HO Univ Vienna ID CIRCUMSTELLAR ENVELOPES; MOLECULAR ABUNDANCES; INNER WIND; IRC+10216; CHEMISTRY; PHOSPHORUS; SILICON; BAND AB Dedicated, unbiased spectral scans of asymptotic giant branch stars have so far been published only for a few carbon-rich stars, with a strong focus on the nearby and bright IRC +10216. We present results from a spectral survey of the circumstellar envelope of the oxygen-rich AGB star IK Tau obtained with the Submillimeter Array (SMA) at similar to 0 ''.9 angular resolution in the frequency range 279 - 355 GHz, expanding the molecular inventory for M-type evolved stars and filling an observational gap. The survey shows over 140 emission lines, belonging to more than 30 species. The emission of AlO and of several vibrationally excited species traces the acceleration of the wind. Isotopic ratios for carbon, silicon, and sulfur will be derived from the observed emission of isotopologues of CO, SiO, SiS, HCN, SO, and SO2. This will allow us to constrain the AGB nucleosynthesis of IK Tau. We highlight the first detection of PO and PN around an oxygen-rich AGB star, detected at unexpectedly high abundances, and emphasise the importance of unbiased spectral surveys of AGB stars and the need for updated chemical models. C1 [De Beck, Elvire; Kaminski, Tomasz; Menten, Karl M.] Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. [De Beck, Elvire] Chalmers, Onsala Space Observ, Dept Earth & Space Sci, S-43900 Onsala, Sweden. [Patel, Nimesh A.; Young, Ken H.; Gottlieb, Carl A.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RP De Beck, E (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. EM edebeck@mpifr-bonn.mpg.de NR 19 TC 1 Z9 1 U1 1 U2 1 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-879-4; 978-1-58381-878-7 J9 ASTR SOC P PY 2015 VL 497 BP 73 EP 78 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE3OZ UT WOS:000371098100009 ER PT B AU Matthews, LD Reid, MJ Menten, KM AF Matthews, L. D. Reid, M. J. Menten, K. M. BE Kerschbaum, F Wing, RF Hron, J TI Imaging Radio Photospheres with the Jansky Very Large Array SO WHY GALAXIES CARE ABOUT AGB STARS III: A CLOSER LOOK IN SPACE AND TIME SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT Conference on Why Galaxies Care About AGB Stars III: A Closer Look in Space and Time CY JUL 28-AUG 01, 2014 CL Univ Vienna, Vienna, AUSTRIA SP Univ Vienna, Ohio State Univ, Robert Wing Support Fund, Austrian Sci Fund, Vienna Convent Bur HO Univ Vienna ID ENVELOPES AB Using the Jansky Very Large Array (JVLA), we have imaged the radio photosphere of the long-period variable star W Hya at 45 GHz (similar to 7 mm) with a resolution of similar to 40 mas. Our data reveal a non-spherical photospheric shape, consistent with earlier measurements. We also find evidence for an elongation along PA approximate to -5 angstrom, the orientation of which is consistent with the previously measured projected magnetic field direction and an extension in the 18 mu m dust emission, both at larger scales. C1 [Matthews, L. D.] MIT, Haystack Observ, Westford, MA 01886 USA. [Reid, M. J.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Menten, K. M.] Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. RP Matthews, LD (reprint author), MIT, Haystack Observ, Westford, MA 01886 USA. EM lmatthew@haystack.mit.edu 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 978-1-58381-879-4; 978-1-58381-878-7 J9 ASTR SOC P PY 2015 VL 497 BP 131 EP 132 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE3OZ UT WOS:000371098100025 ER PT S AU Tong, CYE Grimes, PK Weintroub, J Blundell, R AF Tong, Cheuk-yu Edward Grimes, Paul K. Weintroub, Jonathan Blundell, Raymond GP IEEE TI Ultra-wide IF Bandwidth - The Next Frontier for SIS Receivers SO 2015 IEEE MTT-S INTERNATIONAL MICROWAVE SYMPOSIUM (IMS) SE IEEE MTT-S International Microwave Symposium LA English DT Proceedings Paper CT IEEE MTT-S International Microwave Symposium (IMS) CY MAY 17-22, 2015 CL Phoenix, AZ SP IEEE MTT S DE Superconductor-Insulator-Superconductor (SIS) mixer; distributed mixer; ultra-wide band technology AB Tucker's theory of quantum mixing can be extended to model distributed series connected SIS mixers, which offer a lower capacitance and a higher dynamic range. These mixers have wider IF bandwidth than single junction mixer. Coupled with the emerging ultra-wide band technologies in low noise amplifier and fast digital signal processing, they open a new frontier of ultra-wide band receivers. We report on the development of the wideband SIS receivers for the Submillimeter Array, designed with Tucker's theory. C1 [Tong, Cheuk-yu Edward; Grimes, Paul K.; Weintroub, Jonathan; Blundell, Raymond] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RP Tong, CYE (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 14 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 0149-645X BN 978-1-4799-8275-2 J9 IEEE MTT S INT MICR PY 2015 PG 3 WC Computer Science, Theory & Methods; Engineering, Electrical & Electronic; Physics, Applied SC Computer Science; Engineering; Physics GA BE3HO UT WOS:000370722900101 ER PT S AU Singh, S Chu, YW Lukin, M Yelin, S AF Singh, Swati Chu, Yiwen Lukin, Mikhail Yelin, Susanne BE Arimondo, E Lin, CC Yelin, SF TI Coherent Population Trapping, Nuclear Spin Cooling, and Levy Flights in Solid-State Atom-Like Systems SO ADVANCES IN ATOMIC, MOLECULAR, AND OPTICAL PHYSICS, VOL 64 SE Advances In Atomic Molecular and Optical Physics LA English DT Review; Book Chapter ID ELECTROMAGNETICALLY INDUCED TRANSPARENCY; PHOTON RECOIL ENERGY; DIAMOND; MAGNETOMETRY; ENTANGLEMENT; SPECTROSCOPY; DEFECTS; OPTICS; QUBITS; MEDIA AB We describe and analyze a method for controlling nuclear spin environment of atomlike quantum emitters in the solid state. The method makes use of laser manipulation of an electronic spin transition via coherent population trapping. Specifically, we present a detailed description of the nuclear spin dynamics and its interplay with the optical excitation of the electronic spin of nitrogen-vacancy color centers in diamond. We introduce a simple model of this process that allows us to study both optimal cooling parameters for nuclear spins and optimal information transfer between the optical measurement of the electron and the nuclear bath dynamics. This allows us to investigate the statistical properties of the nuclear spin bath. Potential applications to quantum information processing and quantum metrology are possible. C1 [Singh, Swati] Harvard Smithsonian Ctr Astrophys, ITAMP, 60 Garden St, Cambridge, MA 02138 USA. [Singh, Swati; Yelin, Susanne] Univ Connecticut, Dept Phys, Storrs, CT USA. [Chu, Yiwen] Yale Univ, Dept Appl Phys, New Haven, CT 06520 USA. [Lukin, Mikhail; Yelin, Susanne] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. RP Yelin, S (reprint author), Univ Connecticut, Dept Phys, Storrs, CT USA. EM syelin@physics.harvard.edu NR 57 TC 1 Z9 1 U1 1 U2 6 PU ELSEVIER ACADEMIC PRESS INC PI SAN DIEGO PA 525 B STREET, SUITE 1900, SAN DIEGO, CA 92101-4495 USA SN 1049-250X BN 978-0-12-802127-9 J9 ADV ATOM MOL OPT PHY JI Adv. Atom. Mol. Opt. Phys. PY 2015 VL 64 BP 273 EP 327 DI 10.1016/bs.aamop.2015.05.001 PG 55 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA BE3BX UT WOS:000370490900012 ER PT J AU Alvarado, JJ Cortes, J Guzman, H Reyes-Bonilla, H AF Jose Alvarado, Juan Cortes, Jorge Guzman, Hector Reyes-Bonilla, Hector TI Density, size, and biomass of Diadema mexicanum (Echinoidea) in Eastern Tropical Pacific coral reefs SO AQUATIC BIOLOGY LA English DT Article DE Marine protected area; Biomass; Organic matter; Overfishing; Shelter ID SEA-URCHIN DIADEMA; FISH COMMUNITY STRUCTURE; ANTILLARUM PHILIPPI ECHINODERMATA; GULF-OF-CALIFORNIA; 1982-1983 EL-NINO; MARINE RESERVES; COSTA-RICA; PARACENTROTUS-LIVIDUS; CARBONATE BUDGETS; MASS MORTALITIES AB Diadema is among the most abundant, widely dispersed, and ecologically important genera of sea urchin in tropical shallow waters. D. mexicanum is distributed from the Gulf of California to northern Peru, including the oceanic islands of Revillagigedo, Clipperton, Coco, Malpelo, and Galapagos, and it is one of the most important sea urchin species in Eastern Tropical Pacific (ETP) coral reefs. In the 1980s, El Nino caused high coral mortality, resulting in an increase in macroalgal cover. This resulted in higher sea urchin bioerosion activity, which weakened the reef frameworks. Considering the high vulnerability of the ETP coral reefs, the aim of this study was to determine regional differences in the density, size (test diameter), and biomass of D. mexicanum at 12 localities in 4 countries between 2009 and 2010, and to determine possible causes of these differences. The average density, size, and biomass of D. mexicanum were 0.47 +/- 0.15 ind. m(-2), 4.38 +/- 1.50 cm, and 0.26 +/- 0.33 g m(-2). The test size frequency that predominated was 2 to 3 cm. Predation by macrophagous fishes seems to be one of the most important factors that explains the presence of low densities and small size of sea urchins throughout the region. The increase in D. mexicanum predators is probably a result of overfishing of top predators. C1 [Jose Alvarado, Juan; Cortes, Jorge] Univ Costa Rica, Ctr Invest Ciencias Mar & Limnol CIMAR, San Jose 115012060, Costa Rica. [Jose Alvarado, Juan; Cortes, Jorge] Univ Costa Rica, Escuela Biol, San Jose 115012060, Costa Rica. [Guzman, Hector] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Reyes-Bonilla, Hector] Univ Autonoma Baja California Sur, Dept Biol Marina, La Paz, Bolivia. RP Alvarado, JJ (reprint author), Univ Costa Rica, Ctr Invest Ciencias Mar & Limnol CIMAR, San Jose 115012060, Costa Rica. EM juan.alvarado@ucr.ac.cr FU Vicerrectoria de Investigacion-Universidad de Costa Rica; Ministerio de Ciencia y Tecnologia de Costa Rica (MICIT); Consejo Nacional para Investigaciones Cientificas y Tecnologicas de Costa Rica (CONICIT); Consejo Nacional de Ciencia y Tecnologia de Mexico (CONACYT); Fonds Francais pour l'Environnement Mondial (FFEM); Ecodesarrollo Papagayo; Grupo Adelante FX We thank the following individuals who collaborated during the development of this work: C. Fernandez, O. Breedy, C. Sanchez, S. Martinez, E. Gomez, A. Planas, V. Flores, O. Norzagaray, L.E. Calderon-Aguilera, A. Ayala, J. Carrion, L. Hernandez, G. Ramirez, V. Vargas, J. Ramirez, and the Bezy, Sanchez-Camacho, and Garcia-Zuniga families. We also thank the following institutions, organizations, and companies: Centro de Investigacion en Ciencias del Mar y Limnologia (CIMAR, Universidad de Costa Rica), Universidad Autonoma de Baja California Sur (UABCS), Laboratorio de Sistemas Arrecifales (LSA), Centro de Investigaciones en Ciencias Marinas (CICIMAR), Universidad de Guadalajara, Centro de Investigacion Cientifica y Educacion Superior de Ensenada (CICESE), Universidad del Mar, Ministerios del Ambiente y Recursos Naturales-El Salvador, Universidad de El Salvador, Smithsonian Tropical Research Institute, Liquid Jungle Lab, Charles Darwin Foundation, Hotel Pacifica, Mero Divers, Vallartec, Fundarrecife, and Reserva Biologica Isla del Cano, Parque Nacional Isla del Coco, and Parque Nacional Los Cobanos park rangers, MY Adventure crew, Instituto Costarricense de Turismo, Sistema Nacional de Areas de Conservacion-Costa Rica (SINAC), Autoridad Nacional del Ambiente-Panama (ANAM), Hotel Punta Marenco Lodge, and Aguila de Osa Inn. We acknowledge financial support from the Vicerrectoria de Investigacion-Universidad de Costa Rica, Ministerio de Ciencia y Tecnologia de Costa Rica (MICIT), Consejo Nacional para Investigaciones Cientificas y Tecnologicas de Costa Rica (CONICIT), Consejo Nacional de Ciencia y Tecnologia de Mexico (CONACYT), Fonds Francais pour l'Environnement Mondial (FFEM), Ecodesarrollo Papagayo, and Grupo Adelante. Finally, we are grateful to M. Chavez for help with the graphs and to P. Hanson and J. Lawrence for their English review and comments. We appreciate the comments of 3 anonymous reviewers who greatly improved this paper. NR 81 TC 1 Z9 1 U1 2 U2 7 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 2015 VL 24 IS 3 BP 151 EP 161 DI 10.3354/ab00645 PG 11 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA DE1YM UT WOS:000370422900002 ER PT J AU Kelley, NP Motani, R AF Kelley, Neil P. Motani, Ryosuke TI Trophic convergence drives morphological convergence in marine tetrapods SO BIOLOGY LETTERS LA English DT Article DE marine mammal; marine reptile; convergent evolution; feeding adaptation; functional morphology ID FEEDING KINEMATICS; SUCTION; EVOLUTION; MAMMALS; WHALES AB Marine tetrapod clades (e.g. seals, whales) independently adapted to marine life through the Mesozoic and Caenozoic, and provide iconic examples of convergent evolution. Apparent morphological convergence is often explained as the result of adaptation to similar ecological niches. However, quantitative tests of this hypothesis are uncommon. We use dietary data to classify the feeding ecology of extant marine tetrapods and identify patterns in skull and tooth morphology that discriminate trophic groups across clades. Mapping these patterns onto phylogeny reveals coordinated evolutionary shifts in diet and morphology in different marine tetrapod lineages. Similarities in morphology between species with similar diets-even across large phylogenetic distances-are consistent with previous hypotheses that shared functional constraints drive convergent evolution in marine tetrapods. C1 [Kelley, Neil P.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, POB 37012, Washington, DC 20013 USA. [Kelley, Neil P.; Motani, Ryosuke] Univ Calif Davis, Dept Earth & Planetary Sci, 1 Shields Ave, Davis, CA 95616 USA. RP Kelley, NP (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, POB 37012, Washington, DC 20013 USA. EM kelleynp@si.edu RI Motani, Ryosuke/K-2607-2015 OI Motani, Ryosuke/0000-0001-5022-1053 FU Geological Society of America; UC Davis Department of Earth and Planetary Sciences Cordell Durrell Fund; NMNH Peter Buck postdoctoral fellowship FX The Geological Society of America and the UC Davis Department of Earth and Planetary Sciences Cordell Durrell Fund provided research support to N.P.K., additional postdoctoral support provided by NMNH Peter Buck postdoctoral fellowship. NR 20 TC 8 Z9 8 U1 9 U2 14 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 1744-9561 EI 1744-957X J9 BIOL LETTERS JI Biol. Lett. PD JAN 1 PY 2015 VL 11 IS 1 AR 20140709 DI 10.1098/rsbl.2014.0709 PG 5 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA DE5KF UT WOS:000370669200003 PM 25631228 ER PT B AU Ladd, EF Gingrich, EC Nottis, KEK Udomprasert, P Goodman, AA AF Ladd, E. F. Gingrich, E. C. Nottis, K. E. K. Udomprasert, P. Goodman, A. A. BE Schultz, G Buxner, S Shore, L Barnes, J TI Combining Real World Experiences with WorldWide Telescope Visualization to Build a Better Parallax Lab SO CELEBRATING SCIENCE: PUTTING EDUCATION BEST PRACTICES TO WORK SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 126th Astronomical-Society-of-the-Pacific Annual Meeting on Celebrating Science: Putting Education Best Practices to Work CY AUG 02-06, 2014 CL Burlingame, CA SP Astron Soc Pacif, NRAO, Sky Skan, E&S, Ball Aerosp & Technol Corp, Stratospher Observ Infrared Astron, CELESTRON, AAS, EXPLORE Sci AB We present a lab activity designed to help students understand the concept of parallax in both astronomical and non-astronomical contexts. In an outdoor setting, students learn the methodology of distance determination via parallax. They identify a distant landmark to establish a reference of direction, and then measure the change in apparent direction for more nearby objects as they change position in a 2 meter radius "orbit" around the "Sun." This hands-on activity involves large, visually-discernable angles so that students can internalize the concept of parallax from everyday experience. However, students often have difficulty transferring this experience to the astronomical realm, so we pair this hands-on activity with a more explicitly astronomically based activity using the WorldWide Telescope visualization environment. Students apply the same methodology in this environment and learn how the apparent motion of stars is related to their distance from Earth. The combination of hands-on activity and computer-aided visualization is designed to produce a deeper understanding of parallax in the astronomical environment, and an improved understanding of the inherently three-dimensional distribution of objects in our universe. More formal assessment is underway. C1 [Ladd, E. F.; Gingrich, E. C.; Nottis, K. E. K.] Bucknell Univ, Lewisburg, PA 17837 USA. [Udomprasert, P.; Goodman, A. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Ladd, EF (reprint author), Bucknell Univ, Lewisburg, PA 17837 USA. EM ladd@bucknell.edu NR 1 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 978-1-58381-884-8 J9 ASTR SOC P PY 2015 VL 500 BP 191 EP 194 PG 4 WC Astronomy & Astrophysics; Education, Scientific Disciplines SC Astronomy & Astrophysics; Education & Educational Research GA BE2YJ UT WOS:000370302600032 ER PT B AU Gingrich, EC Ladd, EF Nottis, KEK Udomprasert, P Goodman, AA AF Gingrich, E. C. Ladd, E. F. Nottis, K. E. K. Udomprasert, P. Goodman, A. A. BE Schultz, G Buxner, S Shore, L Barnes, J TI The Size, Scale, and Structure Concept Inventory (S3CI) for Astronomy SO CELEBRATING SCIENCE: PUTTING EDUCATION BEST PRACTICES TO WORK SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 126th Astronomical-Society-of-the-Pacific Annual Meeting on Celebrating Science: Putting Education Best Practices to Work CY AUG 02-06, 2014 CL Burlingame, CA SP Astron Soc Pacif, NRAO, Sky Skan, E&S, Ball Aerosp & Technol Corp, Stratospher Observ Infrared Astron, CELESTRON, AAS, EXPLORE Sci AB We present a concept inventory to evaluate student understanding of size, scale, and structure concepts in the astronomical context. Students harbor misconceptions regarding these concepts, and these misconceptions often persist even after instruction. Evaluation of these concepts prior to as well as after instruction can ensure misconceptions are addressed. Currently, no concept inventories focus exclusively on these geometrical ideas, so we have developed the Size, Scale and Structure Concept Inventory (SKI). In fall 2013, we piloted a 24-item version of the S3CI in an introductory astronomy course at a small private university. We performed an item analysis and estimated the internal consistency reliability for the instrument. Based on these analyses, problematic questions were revised for a second version. We discuss the results from the pilot phase and preview our updated test in this work. A valid and reliable concept inventory has the potential to accurately evaluate undergraduates' understanding of size, scale, and structure concepts in the astronomical context, as well as assess conceptual change after targeted instruction. Lessons learned in the evaluation of the initial version of the S3CI can guide future development of this and other astronomical concept inventories. Instructors interested in participating in the ongoing development of the S3CI should contact the authors. C1 [Gingrich, E. C.; Ladd, E. F.; Nottis, K. E. K.] Bucknell Univ, Lewisburg, PA 17837 USA. [Udomprasert, P.; Goodman, A. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Gingrich, EC (reprint author), Bucknell Univ, Lewisburg, PA 17837 USA. EM ladd@bucknell.edu 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 978-1-58381-884-8 J9 ASTR SOC P PY 2015 VL 500 BP 269 EP 274 PG 6 WC Astronomy & Astrophysics; Education, Scientific Disciplines SC Astronomy & Astrophysics; Education & Educational Research GA BE2YJ UT WOS:000370302600047 ER PT S AU Mikolajewska, J Shara, MM Caldwell, N Drozd, K Ilkiewicz, K Zurek, D AF Mikolajewska, J. Shara, M. M. Caldwell, N. Drozd, K. Ilkiewicz, K. Zurek, D. BA Lanz, T BF Lanz, T BE Lagadec, E Millour, F TI SYMBIOTIC STARS IN THE LOCAL GROUP OF GALAXIES SO PHYSICS OF EVOLVED STARS: A CONFERENCE DEDICATED TO THE MEMORY OF OLIVIER CHESNEAU SE EAS Publications Series LA English DT Proceedings Paper CT Physics of Evolved Stars: A Conference Dedicated to the Memory of Olivier Chesneau CY JUN 08, 2015 CL Nice, FRANCE SP Observ Cote Azur, Lab Joseph Louis Lagrange Lagrange UMR 7293, INSU, Programme Natl Phys Stellaire, INSU, Act Specif Haute Resolut Angulaire, Univ Nice Sophia Antipolis, CNRS, Ville Nice ID M33; DISCOVERY AB Preliminary results of the ongoing search for symbiotic binary stars in the Local Group of Galaxies are presented and discussed. C1 [Mikolajewska, J.; Drozd, K.; Ilkiewicz, K.] Nicolaus Copernicus Astron Ctr, Warsaw, Poland. [Shara, M. M.; Zurek, D.] Amer Museum Nat Hist, Dept Astrophys, New York, NY 10024 USA. [Caldwell, N.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA. RP Mikolajewska, J (reprint author), Nicolaus Copernicus Astron Ctr, Warsaw, Poland. NR 13 TC 1 Z9 1 U1 0 U2 0 PU E D P SCIENCES PI CEDEX A PA 17 AVE DU HOGGAR PARC D ACTIVITES COUTABOEUF BP 112, F-91944 CEDEX A, FRANCE SN 1633-4760 BN 978-2-7598-1907-2 J9 EAS PUBLICATIONS PY 2015 VL 71-72 BP 199 EP 204 DI 10.1051/eas/1571046 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE2YK UT WOS:000370302700045 ER PT J AU Rincon, AF Bloch, JI Macfadden, BJ Jaramillo, CA AF Rincon, Aldo F. Bloch, Jonathan I. Macfadden, Bruce J. Jaramillo, Carlos A. TI NEW EARLY MIOCENE PROTOCERATIDS (MAMMALIA, ARTIODACTYLA) FROM PANAMA SO JOURNAL OF VERTEBRATE PALEONTOLOGY LA English DT Article ID NEOTROPICAL PALEOBOTANY; NORTH-AMERICA; MIDDLE MIOCENE; LATE EOCENE; COMMUNITIES; CALIBRATION; HYPSODONTY; EVOLUTION; PENINSULA; TERTIARY AB Although Cenozoic protoceratid artiodactyls are known from throughout North America, species referred to the Miocene protoceratine Paratoceras are restricted to subtropical areas of the Gulf Coast and southern Mexico and tropical areas of Panama. Newly discovered fossils from the late Arikareean Lirio Norte Local Fauna, Panama Canal basin, include partial dentitions of a protoceratid remarkably similar to those of Paratoceras tedfordi from Mexico, suggesting a rapid early Miocene colonization of recently emerged tropical volcanic terrains (Las Cascadas Formation). Partial lower dentitions from the overlying shallow marine to transitional Culebra Formation (early Centenario Fauna) are here referred to Paratoceras orarius, sp. nov., based on relatively small size, shallow mandible anterior to p3, and narrow cheek teeth. New early Hemingfordian protoceratine fossils from the upper part of the Cucaracha Formation (late Centenario Fauna) include a partial male skull and several dentitions that, together with specimens previously referred to P. wardi (only known from the Barstovian of Texas), are here referred to Paratoceras coatesi, sp. nov., based on distinctly more gracile cranial ornamentation, relatively longer nasals, a smaller and wider lower p4 (relative to m1), and more bulbous lower premolars. Results from a cladistic analysis of 15 craniodental characters coded for 11 protoceratine species suggests that Paratoceras is a monophyletic clade with its origin in subtropical areas of Central America, spreading into the tropics of Panama during the early Miocene (Arikareean through Hemingfordian North American Land Mammal Ages [NALMAs]), and later inhabiting subtropical areas of the Gulf Coast during the middle-late Miocene (Barstovian through Clarendonian NALMAs). C1 [Rincon, Aldo F.; Bloch, Jonathan I.; Macfadden, Bruce J.] Univ Florida, Florida Museum Nat Hist, Gainesville, FL 32611 USA. [Rincon, Aldo F.] Univ Florida, Dept Geol Sci, Gainesville, FL 32611 USA. [Jaramillo, Carlos A.] Smithsonian Trop Res Inst, Balboa, Panama. RP Rincon, AF (reprint author), Univ Florida, Florida Museum Nat Hist, Gainesville, FL 32611 USA. EM arincon@ufl.edu; jbloch@flmnh.ufl.edu; bmacfadd@flmnh.ufl.edu; jaramilloc@si.edu OI Bloch, Jonathan/0000-0003-1484-6931 FU UF Research Opportunity Grant; U.S. National Science Foundation Partnerships in International Research and Education [0966884, EAR 0824299, EAR 0418042]; National Science Foundation's Advancing Digitization of Biodiversity Collections Program (iDigBio) NSF [EF 1115210]; STRI-Tupper Paleontological Fund; STRI-Panama Canal Authority Fund; Ricardo Perez Toyota, Panama FX We thank J. Bourque and D. Byerley at the FLMNH who prepared fossil specimens in the laboratory, and C. Montes, S. Suarez, M. Vallejo, and F. Moreno (STRI) and G. S. Morgan, A. Wood, J. Carr, S. Lukowski, D. Jones, J. Velez-Juarbe, and B. Newstead (PCP-PIRE) who helped collect the specimens. Special thanks to R. Hulbert Jr. (FLMNH) for help with anatomical terminology and taxonomic nomenclature. Thanks also to the AMNH staff for access to relevant fossil specimens, and K. Cummings, J. Pardo, and C. Byrd who edited an earlier version of the manuscript and made helpful comments for its improvement. Thanks to R. Emry and one anonymous reviewer for helpful reviews and comments that improved the quality of the manuscript. We also thank the Panama Canal Authority (ACP) and the Ministerio de Comercio e Industria (MICI) for access to relevant fossil sites and the UF Department of Geological Sciences for its support. This research was supported by UF Research Opportunity Grant; the U.S. National Science Foundation Partnerships in International Research and Education grant 0966884 (OISE, EAR, DRL), EAR 0824299, and EAR 0418042; National Science Foundation's Advancing Digitization of Biodiversity Collections Program (iDigBio) NSF EF 1115210; STRI-Tupper Paleontological Fund; STRI-Panama Canal Authority Fund; and Ricardo Perez Toyota, Panama. This is UF Contribution to Paleobiology number 660. NR 80 TC 3 Z9 3 U1 0 U2 0 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 530 WALNUT STREET, STE 850, PHILADELPHIA, PA 19106 USA SN 0272-4634 EI 1937-2809 J9 J VERTEBR PALEONTOL JI J. Vertebr. Paleontol. PY 2015 VL 35 IS 5 AR e970688 DI 10.1080/02724634.2015.970688 PG 22 WC Paleontology SC Paleontology GA DD3JJ UT WOS:000369818100007 ER PT J AU Mawdsley, JR AF Mawdsley, Jonathan R. TI An annotated checklist of the large carpenter bees, genus Xylocopa Latreille (Hymenoptera: Apidae), from the Philippine Islands SO ORIENTAL INSECTS LA English DT Article DE Apidae; Xylocopa; bee; carpenter bee; large carpenter bee; Philippines AB An annotated checklist is presented for the 37 valid species-level taxa of the genus Xylocopa Latreille (Hymenoptera: Apidae) recorded from the Philippine Islands. A key is provided to the four subgenera of Xylocopa represented in the Philippine fauna: Xylocopa subgenus Biluna Maa, Xylocopa subgenus Koptortosoma Gribodo, Xylocopa subgenus Platynopoda Westwood and Xylocopa subgenus Zonohirsuta Maa. For each species and subspecies, the following information is provided: original combination, type locality, available information about primary types, a list of synonyms described from the Philippines, a brief synopsis of the principal external diagnostic features and a summary of the known geographic distribution of the species in the Philippine Islands. C1 [Mawdsley, Jonathan R.] Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Mawdsley, JR (reprint author), Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, MRC 187, Washington, DC 20560 USA. EM mawdsleyj@si.edu NR 50 TC 0 Z9 0 U1 0 U2 1 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 0030-5316 EI 2157-8745 J9 ORIENT INSECTS JI Orient. Insects PY 2015 VL 49 IS 1-2 BP 47 EP 67 DI 10.1080/00305316.2015.1081423 PG 21 WC Entomology SC Entomology GA DD4HX UT WOS:000369884200007 ER PT B AU Kepler, SO Pelisoli, I Koester, D Ourique, G Kleinman, SJ Romero, AD Nitta, A Eisenstein, DJ Costa, JES Kulebi, B Jordan, S Dufour, P Giommi, P Rebassa-Mansergas, A AF Kepler, S. O. Pelisoli, I. Koester, D. Ourique, G. Kleinman, S. J. Romero, A. D. Nitta, A. Eisenstein, D. J. Costa, J. E. S. Kuelebi, B. Jordan, S. Dufour, P. Giommi, Paolo Rebassa-Mansergas, Alberto BE Dufour, P Bergeron, P Fontaine, G TI New White Dwarfs in the SDSS DR10 SO 19TH EUROPEAN WORKSHOP ON WHITE DWARFS SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 19th European Workshop on White Dwarfs CY AUG 11-15, 2014 CL Univ Montreal, Montreal, CANADA SP Univ Montreal HO Univ Montreal ID DIGITAL SKY SURVEY; OSCILLATION SPECTROSCOPIC SURVEY; DATA RELEASE; STARS; PROGENITORS; EVOLUTION; ATMOSPHERES; SUPERNOVAE; SEQUENCES; CATALOG AB We report the discovery of 8 991 new spectroscopically confirmed white dwarfs and subdwarfs in the Sloan Digital Sky Survey Data Release 10. We obtain T-eff,, log g and mass for hydrogen atmosphere white dwarf stars (DAs) and helium atmosphere white dwarf stars (DBs), and estimate the calcium/helium abundances for the white dwarf stars with metallic lines (DZs) and carbon/helium for cool carbon dominated spectra DQs. We found 2 new oxygen dominated spectra white dwarfs, 69 DQs, 42 hot DO/PG1159s, 175 white dwarf+main sequence star binaries, 206 magnetic DAHs, 325 continuum dominated DCs, 397 metal polluted white dwarfs, 450 helium dominated white dwarfs, 636 subdwarfs and 6796 new hydrogen dominated white dwarf stars. C1 [Kepler, S. O.; Pelisoli, I.; Ourique, G.; Romero, A. D.; Costa, J. E. S.] Univ Fed Rio Grande do Sul, Inst Fis, BR-91501900 Porto Alegre, RS, Brazil. [Koester, D.] Univ Kiel, Inst Theoret Phys & Astrophys, Olshaussenstr 40, D-24098 Kiel, Germany. [Kleinman, S. J.; Nitta, A.] Gemini Observ, Hilo, HI 96720 USA. [Eisenstein, D. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kuelebi, B.] Univ Autonoma Barcelona, Inst Ciencies Espai, Bellaterra 08193, Spain. [Kuelebi, B.] Inst Space Studies Catalonia, Barcelona 08034, Spain. [Dufour, P.] Heidelberg Univ, Astron Rechen Inst, Zentrum Astron, D-69120 Heidelberg, Germany. [Dufour, P.] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada. [Giommi, Paolo] ASDC Agenzia Spaziale Italiana, Rome, Italy. [Rebassa-Mansergas, Alberto] Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China. RP Kepler, SO (reprint author), Univ Fed Rio Grande do Sul, Inst Fis, BR-91501900 Porto Alegre, RS, Brazil. EM kepler@if.ufrgs.br RI Romero, Alejandra/G-1644-2016; Kepler, S. O. /H-5901-2012 OI Kepler, S. O. /0000-0002-7470-5703 NR 30 TC 1 Z9 1 U1 0 U2 1 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-871-8; 978-1-58381-870-1 J9 ASTR SOC P PY 2015 VL 493 BP 449 EP 454 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE2LS UT WOS:000369565800086 ER PT B AU Gianninas, A Kilic, M Brown, WR Canton, P Hermes, JJ Bell, KJ Harrold, ST AF Gianninas, A. Kilic, M. Brown, W. R. Canton, P. Hermes, J. J. Bell, K. J. Harrold, S. T. BE Dufour, P Bergeron, P Fontaine, G TI The Search for the Shortest Period Binary White Dwarfs: The Latest Results from the ELM Survey SO 19TH EUROPEAN WORKSHOP ON WHITE DWARFS SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 19th European Workshop on White Dwarfs CY AUG 11-15, 2014 CL Univ Montreal, Montreal, CANADA SP Univ Montreal HO Univ Montreal ID EXTREMELY LOW-MASS; METAL-RICH AB We present the latest results from the ongoing ELM Survey, our targeted search for short-period (P < 1 d), extremely low mass white dwarf binaries. This includes the exciting discovery of a new 20 min system which constitutes a new verification binary for gravitational wave detectors operating in the mHz range. We also discuss the puzzling presence of metals in many ELM WDs. Finally, we present an updated view of the extremely low-mass white dwarf instability strip. C1 [Gianninas, A.; Kilic, M.; Canton, P.] Univ Oklahoma, Homer L Dodge Dept Phys & Astron, 440 W Brooks St, Norman, OK 73019 USA. [Brown, W. R.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Hermes, J. J.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Bell, K. J.; Harrold, S. T.] Univ Texas Austin, Dept Astron, RLM 15308, Austin, TX 78712 USA. RP Gianninas, A (reprint author), Univ Oklahoma, Homer L Dodge Dept Phys & Astron, 440 W Brooks St, Norman, OK 73019 USA. EM alexg@nhn.ouedu OI Gianninas, Alexandros/0000-0002-8655-4308 NR 12 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 978-1-58381-871-8; 978-1-58381-870-1 J9 ASTR SOC P PY 2015 VL 493 BP 481 EP 486 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE2LS UT WOS:000369565800092 ER PT J AU Thompson, FC Hauser, M AF Thompson, F. Christian Hauser, Martin TI In honor of Brian Stuckenberg: Two new Spheginobaccha species of flower flies (Diptera: Syrphidae) from the Afrotropics SO AFRICAN INVERTEBRATES LA English DT Article DE Afrotropical Region; Madagascar; Spheginobaccha; taxonomy; new species ID MORPHOLOGICAL CHARACTERS; MADAGASCAR DIPTERA; GENUS; PHYLOGENY; GENERA AB The Afrotropical species of genus Spheginobaccha are reviewed and a new identification key is provided. Two new species are described: S. stuckenbergi from Madagascar and S. pamela from South Africa. C1 [Thompson, F. Christian] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20560 USA. [Hauser, Martin] Calif Dept Food & Agr, Plant Pest Diagnost Branch, 3294 Meadowview Rd, Sacramento, CA 95832 USA. RP Thompson, FC (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20560 USA. EM thompsonf@si.edu; Phycus@gmail.com FU Schlinger Foundation; US National Science Foundation [DEB-0072713] FX This paper was developed and written by the senior author. The junior author joined the effort during the review process when he added additional material and significant enhancements. This report represents the first contribution to a comprehensive understanding of the Madagascan flower fly fauna based on the new and enriched collections made through the support of the Schlinger Foundation.; We acknowledge the Schlinger Foundation for establishing the entomological survey of Madagascar and the US National Science Foundation (grant DEB-0072713) for their continued support of the survey. Mike E. Irwin (Vail, AZ) and Harin' Hala (Rin'ha) Rasolondalao (Antananarivo, Madagascar) are thanked for all the organizing and the field work, collecting, and sorting of the material. We thank all the curators of the various collections listed above for their help and loan of material. Brian Fisher, Charles Griswold and Norman Penny of the California Academy of Sciences, were critical in making material available to us. We thank Taina Litwak, Department of Entomology, Smithsonian Institution, Washington, for the male genitalia figures. Naturally, we thank our colleagues for their review and critical comments on the manuscript: Norman Woodley, Systematic Entomology Laboratory, ARS, US Department of Agriculture, Washington and Jeffrey Skevington, Canada Agriculture and Agri-Food Canada, Ottawa. NR 43 TC 0 Z9 0 U1 0 U2 0 PU COUNCIL NATAL MUSEUM PI PIETERMARITZBURG PA PRIVATE BAG 9070, PIETERMARITZBURG, KWAZULU-NATAL 00000, SOUTH AFRICA SN 1681-5556 EI 2305-2562 J9 AFR INVERTEBR JI Afr. Invertebr. PY 2015 VL 56 IS 3 BP 769 EP 777 PG 9 WC Entomology; Paleontology; Zoology SC Entomology; Paleontology; Zoology GA DC9FS UT WOS:000369527100017 ER PT B AU Britt, CT Hynes, RI Jonker, PG Maccarone, T Torres, MAP Steeghs, D Nelemans, G Johnson, C Greiss, S AF Britt, C. T. Hynes, R. I. Jonker, P. G. Maccarone, T. Torres, M. A. P. Steeghs, D. Nelemans, G. Johnson, C. Greiss, S. BE Points, S Kunder, A TI The Chandra Galactic Bulge Survey SO FIFTY YEARS OF WIDE FIELD STUDIES IN THE SOUTHERN HEMISPHERE: RESOLVED STELLAR POPULATIONS OF THE GALACTIC BULGE AND MAGELLANIC CLOUDS SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT Conference celebrating Cerro Tololo Inter-American Observatory 50th anniversary CY MAY 06-09, 2013 CL La Serena, CHILE ID X-RAY BINARIES; BLACK-HOLE; LOW-MASS; GALAXY; IDENTIFICATION; COUNTERPARTS; CANDIDATES; STARS; LONG AB The Chandra Galactic Bulge Survey (GBS) is a multi-wavelength survey of two 6 x 1 degree strips above and below the Galactic plane, including deep r' and i' imaging and time domain photometry from CTIO and shallow, wide-field X-ray imaging with Chandra. Targeting fields above vertical bar b vertical bar = 1 avoids most of the copious extinction along the Galactic plane while maintaining high source density. This results in targets that are accessible to follow up in optical and NIR wavelengths. The X-ray observations are shallow to maximize the number of quiescent Low Mass X-ray Binaries (LMXBs) relative to Cataclysmic Variables (CVs). The goals of the GBS are to conduct a census of Low Mass X-ray Binaries in the Milky Way in order to constrain models of binary evolution, the common envelope phase in particular, and to expand the number of known LMXBs for optical follow up. Mass measurements in particular will help constrain the black hole (BH) mass distribution and the equation of state for neutron stars (NS). Constraining the BH mass distribution will constrain models of their formation in supernovae. The current population of Galactic BHs suffers from selection effects, which the GBS avoids by finding new objects while still in quiescence. We expect to find qLMXBs, magnetic CVs, RS CVn stars, and smaller numbers of other types of sources. After removing duplicates, there are 1640 unique X-ray sources in the 12 square degree survey area, which closely matches the predicted number of 1648. We are currently matching X-ray sources to counterparts in other wavelengths using new photometric and spectroscopic observations as well as in archival data where it exists, and searching for variability and periodicity in the counterparts in photometric data. So far, we have spectroscopically identified 27 interacting binaries including promising candidates for quiescent black holes. C1 [Britt, C. T.; Hynes, R. I.; Johnson, C.] Louisiana State Univ, Dept Phys & Astron, Baton Rouge, LA 70803 USA. [Jonker, P. G.; Torres, M. A. P.] SRON Netherlands Inst Space Res, SRON, NL-3584 CA Utrecht, Netherlands. [Jonker, P. G.; Torres, M. A. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Maccarone, T.] Texas Tech Univ, Dept Phys, Lubbock, TX 79409 USA. [Steeghs, D.; Greiss, S.] Univ Warwick, Dept Phys, Astron & Astrophys, Coventry CV4 7AL, W Midlands, England. [Nelemans, G.] Radboud Univ Nijmegen, Dept Astrophys, IMAPP, NL-6500 GL Nijmegen, Netherlands. RP Britt, CT (reprint author), Louisiana State Univ, Dept Phys & Astron, Baton Rouge, LA 70803 USA. NR 26 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 978-1-58381-867-1; 978-1-58381-866-4 J9 ASTR SOC P PY 2015 VL 491 BP 77 EP 82 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE2LR UT WOS:000369565000009 ER PT B AU Dront, MR Massey, P AF Dront, M. R. Massey, P. BE Points, S Kunder, A TI Evolved Massive Stars in the Local Group SO FIFTY YEARS OF WIDE FIELD STUDIES IN THE SOUTHERN HEMISPHERE: RESOLVED STELLAR POPULATIONS OF THE GALACTIC BULGE AND MAGELLANIC CLOUDS SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT Conference celebrating Cerro Tololo Inter-American Observatory 50th anniversary CY MAY 06-09, 2013 CL La Serena, CHILE ID ANDROMEDA GALAXY M31; WOLF-RAYET CONTENT; RED SUPERGIANTS; YELLOW SUPERGIANTS; STELLAR EVOLUTION; MAGELLANIC-CLOUD; SOLAR METALLICITY; SPECTRAL TYPES; MILKY-WAY; O-STARS AB In this manuscript we describe a number of recent advances in the study of evolved massive stars in the Local Group, with an emphasis on how representative populations of these stars can be used to test models of massive star evolution. In honor of the 50th anniversary of the Cerro Tololo Inter-American Observatory (CTIO) we attempt to put these finding in some historical context by discussing how our understanding of the various stages in the lives of massive stars has evolved since Cerro Tololo was first selected as the site for the observatory which would become CTIO. C1 [Dront, M. R.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Massey, P.] Lowell Observ, Flagstaff, AZ 86001 USA. RP Dront, MR (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Massey, Philip/0000-0001-6563-7828 NR 34 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 978-1-58381-867-1; 978-1-58381-866-4 J9 ASTR SOC P PY 2015 VL 491 BP 307 EP 316 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE2LR UT WOS:000369565000039 ER PT B AU Pessev, P Meyer, S Goudfrooij, P Puzia, T Chandar, R AF Pessev, P. Meyer, S. Goudfrooij, P. Puzia, T. Chandar, R. BE Points, S Kunder, A TI Near-Infrared Integrated-Light Photometry of Magellanic Clouds Star Clusters SO FIFTY YEARS OF WIDE FIELD STUDIES IN THE SOUTHERN HEMISPHERE: RESOLVED STELLAR POPULATIONS OF THE GALACTIC BULGE AND MAGELLANIC CLOUDS SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT Conference celebrating Cerro Tololo Inter-American Observatory 50th anniversary CY MAY 06-09, 2013 CL La Serena, CHILE ID POPULATION SYNTHESIS; COLORS; MODELS; 2MASS AB We present the results of several consecutive studies of the near-infrared (NIR) integrated-light properties of star clusters in the Large and Small Magellanic Clouds based on 2MASS archival imaging. The sample covers a wide range in the age/metallicity parameter space and the ages and metallicities for the majority of the clusters are derived based on deep CMDs and spectroscopy of individual cluster members. It is a valuable new resource to study the evolution of the NIR integrated-light properties as a function of the properties of the underlying stellar populations. Some future projects are briefly outlined in terms of further development of the integrated light database and its applications. C1 [Pessev, P.] Gemini Observ, Southern Operat Ctr, Casilla 603, La Serena, Chile. [Meyer, S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Goudfrooij, P.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Puzia, T.] Pontificia Univ Catolica Chile, Dept Astron & Astrophys, Santiago 7820436, Chile. [Chandar, R.] Univ Toledo, RO106, Toledo, OH 43606 USA. RP Pessev, P (reprint author), Gemini Observ, Southern Operat Ctr, Casilla 603, La Serena, Chile. NR 13 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 978-1-58381-867-1; 978-1-58381-866-4 J9 ASTR SOC P PY 2015 VL 491 BP 334 EP 337 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE2LR UT WOS:000369565000043 ER PT J AU Davis, JL Alford, RA Schwarzkopf, L AF Davis, Jennifer L. Alford, Ross A. Schwarzkopf, Lin TI Some lights repel amphibians: implications for improving trap lures for invasive species SO INTERNATIONAL JOURNAL OF PEST MANAGEMENT LA English DT Article DE Rhinella marina; cane toad; invasive; pest management; trap; light attractant ID TOADS BUFO-MARINUS; CANE TOADS; DIENCEPHALON; ATTRACTION; AUSTRALIA AB Traps with baits or other lures are often used to reduce densities of vertebrate pests. Invasive amphibians often feed on insects at lights in urban settings, but it is unclear whether they are attracted to the light itself, the insect food source (which is attracted to the light), or both. Here we examine the attractiveness of four types of lights (incandescent, white fluorescent, yellow fluorescent and ultraviolet) to cane toads (Rhinella marina) in controlled Y-maze experiments, in the absence of insects. In the Y-maze, more cane toads selected darkness over incandescent and white fluorescent lights, indicating these light types repelled toads. In comparison, toads did not distinguish between ultraviolet or yellow fluorescent lights and darkness. We then used field trapping trials to determine the effectiveness of white fluorescent and ultraviolet light for attracting amphibians to traps in the presence of insects. In the field, traps equipped with ultraviolet light trapped significantly more toads than those with white fluorescent lights. Our research indicates that trapping success for amphibians can be significantly improved by using ultraviolet lights as insect attractants. Traps equipped with these lights could help reduce the impact of invasive cane toads, and possibly other invasive amphibians. C1 [Davis, Jennifer L.; Alford, Ross A.; Schwarzkopf, Lin] James Cook Univ, Sch Marine & Trop Biol, Townsville, Qld 4811, Australia. [Davis, Jennifer L.] Smithsonian Conservat Biol Inst, Front Royal, VA USA. RP Davis, JL (reprint author), James Cook Univ, Sch Marine & Trop Biol, Townsville, Qld 4811, Australia. EM jldavis2690@yahoo.com RI Schwarzkopf, Lin/C-1242-2012 OI Schwarzkopf, Lin/0000-0002-1009-670X NR 33 TC 0 Z9 0 U1 1 U2 7 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 0967-0874 EI 1366-5863 J9 INT J PEST MANAGE JI Int. J. Pest Manage. PY 2015 VL 61 IS 4 BP 305 EP 311 DI 10.1080/09670874.2015.1058991 PG 7 WC Entomology SC Entomology GA DD3IH UT WOS:000369814900005 ER PT B AU Torres, G Lacy, CHS Pavlovski, K Feiden, GA Sabby, JA Bruntt, H Clausen, JV AF Torres, Guillermo Lacy, Claud H. Sandberg Pavlovski, Kresimir Feiden, Gregory A. Sabby, Jeffrey A. Bruntt, Hans Clausen, Jens Viggo BE Rucinski, SM Torres, G Zejda, M TI The Benchmark Eclipsing Binary V530 Ori: A Critical Test of Magnetic Evolution Models for Low-Mass Stars SO LIVING TOGETHER: PLANETS, HOST STARS, AND BINARIES SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT Conference on Living Together: Planets, Host Stars and Binaries CY SEP 08-12, 2014 CL Litomysl, CZECH REPUBLIC SP Sci Org Comm ID Y-2 ISOCHRONES; CORE AB We report accurate measurements of the physical properties (mass, radius, temperature) of components of the G+M eclipsing binary V530 On. The M-type secondary shows a larger radius and a cooler temperature than predicted by standard stellar evolution models, as has been found for many other low-mass stars and ascribed to the effects of magnetic activity and/or spots. We show that models from the Dartmouth series that incorporate magnetic fields are able to match the observations with plausible field strengths of 1-2 kG, consistent with a rough estimate we derive for that star. C1 [Torres, Guillermo] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Lacy, Claud H. Sandberg] Univ Arkansas, Dept Phys, Fayetteville, AR 72701 USA. [Pavlovski, Kresimir] Univ Zagreb, Fac Sci, Dept Phys, Zagreb 10000, Croatia. [Feiden, Gregory A.] Uppsala Univ, Dept Phys & Astron, SE-75120 Uppsala, Sweden. [Sabby, Jeffrey A.] So Illinois Univ, Dept Phys, Edwardsville, IL 62026 USA. [Bruntt, Hans] Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, DK-8000 Aarhus C, Denmark. [Bruntt, Hans] Aarhus Katedralskole, DK-8000 Aarhus C, Denmark. [Clausen, Jens Viggo] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen O, Denmark. RP Torres, G (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM gtorres@cfa.harvard.edu NR 21 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 978-1-58381-877-0; 978-1-58381-876-3 J9 ASTR SOC P PY 2015 VL 496 BP 169 EP 173 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE2JW UT WOS:000369467900024 ER PT B AU Vanko, M Torres, G Pribulla, T Parimucha, S Krushevska, V Neuhauser, R Shugarov, SY Hambalek, L Kundra, E Nedoroscik, J Garai, Z AF Vanko, M. Torres, G. Pribulla, T. Parimucha, S. Krushevska, V. Neuhaeuser, R. Shugarov, S. Yu. Hambalek, L' Kundra, E. Nedoroscik, J. Garai, Z. BE Rucinski, SM Torres, G Zejda, M TI Long-Term Photometric and Spectroscopic Variability of V501 Aur SO LIVING TOGETHER: PLANETS, HOST STARS, AND BINARIES SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT Conference on Living Together: Planets, Host Stars and Binaries CY SEP 08-12, 2014 CL Litomysl, CZECH REPUBLIC SP Sci Org Comm ID T-TAURI STARS AB We present new VRI photometry of V501 Aur obtained between 2007 and 2013 at the Grossschwabhausen (Germany) and Stara Lesna (Slovakia) observatories, as well as spectroscopic obervations from the Harvard-Smithsonian Center for Astrophysics (USA). The spectroscopic observations show it to be a single-lined binary, with a different period (68.8 days) than the one indicated by the photometry (similar to 55 days). We discuss the possible nature of the system. C1 [Vanko, M.; Pribulla, T.; Shugarov, S. Yu.; Hambalek, L'; Kundra, E.; Nedoroscik, J.; Garai, Z.] Slovak Acad Sci, Astron Inst, Tatranska Lomnica 05960, Slovakia. [Torres, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Parimucha, S.] Univ PJ Safarik, Fac Sci, Inst Phys, Kosice 04001, Slovakia. [Krushevska, V.] Natl Acad Sci Ukraine, Main Astron Observ, UA-03680 Kiev, Ukraine. [Neuhaeuser, R.] Univ Jena, Astrophys Inst, D-07745 Jena, Germany. RP Vanko, M (reprint author), Slovak Acad Sci, Astron Inst, Tatranska Lomnica 05960, Slovakia. EM vanko@astro.sk NR 2 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 978-1-58381-877-0; 978-1-58381-876-3 J9 ASTR SOC P PY 2015 VL 496 BP 262 EP 263 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE2JW UT WOS:000369467900052 ER PT B AU Girart, JM Zhang, Q Frau, P Qiu, K Liu, HB Tang, YW Koch, P AF Girart, J. M. Zhang, Q. Frau, P. Qiu, K. Liu, H-B. Tang, Y-W. Koch, P. BE Iono, D Tatematsu, K Wootten, A Testi, L TI Magnetic Fields in Star-Forming Regions in the pre-ALMA Era: The SMA View SO REVOLUTION IN ASTRONOMY WITH ALMA: THE THIRD YEAR SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 4th ALMA Science Conference on Revolution in Astronomy with ALMA: The Third Year CY DEC 08-11, 2014 CL Tokyo Int Forum, Tokyo, JAPAN HO Tokyo Int Forum ID DENSE CORE AB We present results from an SMA Legacy project based on the observations of a total of 14 molecular clumps with embedded massive stars. The high resolution observations allow to trace the magnetic field in less than or similar to 0.1 pc cores embedded in the massive clumps. We found that the magnetic fields threading the massive clumps are in general relatively uniform. The magnetic fields appear, in most cases, to be perpendicular to the major axis of the filaments where the cores are embedded, and parallel to the large scale magnetic field. However, there is no correlation between the axis of molecular outflows associated with these dense cores and the magnetic field direction in the cores. Our findings suggest that magnetic fields play an important role during collapse of massive molecular clumps and the formation of dense cores at spatial scales of less than or similar to 0.1 pc. At the scale of an accretion disk, gravity and dynamic interactions in close binary or multiple systems dominate over magnetic fields. Therefore, outflows emanating from the disk do not maintain the magnetic direction in the 0.1pc core. C1 [Girart, J. M.] Inst Ciencies Espai CSIC IEEC, Cerdanyola Del Valles, Catalonia, Spain. [Zhang, Q.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Frau, P.] Observ Astron Nacl, Madrid, Spain. [Frau, P.] ICMM CSIC, Madrid, Spain. [Qiu, K.] Nanjing Univ, Sch Astron & Space Sci, Nanjing 210008, Jiangsu, Peoples R China. [Liu, H-B.; Tang, Y-W.; Koch, P.] Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan. RP Girart, JM (reprint author), Inst Ciencies Espai CSIC IEEC, Cerdanyola Del Valles, Catalonia, Spain. EM girart@ice.cat NR 16 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 978-1-58381-883-1; 978-1-58381-882-4 J9 ASTR SOC P PY 2015 VL 499 BP 197 EP 198 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE2JX UT WOS:000369469500066 ER PT B AU Plunkett, AL Gallardo, J Arce, HG Corder, SA Dunham, MM Fernandez-Lopez, M Mardoness, D AF Plunkett, Adele L. Gallardo, Jose Arce, Hector G. Corder, Stuartt A. Dunham, Michael M. Fernandez-Lopez, Manuel Mardoness, Diego BE Iono, D Tatematsu, K Wootten, A Testi, L TI ALMA's High-Resolution View of the Protostellar Cluster Serpens South: Outflow Activity and Continuum Sources SO REVOLUTION IN ASTRONOMY WITH ALMA: THE THIRD YEAR SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 4th ALMA Science Conference on Revolution in Astronomy with ALMA: The Third Year CY DEC 08-11, 2014 CL Tokyo Int Forum, Tokyo, JAPAN HO Tokyo Int Forum ID AQUILA RIFT AB The study of embedded protostellar clusters is critical to understanding the complex environments where stars are most likely to form. During the star formation process, molecular outflows are generally understood to be necessary and ubiquitous, but quantifying their impact on the nearby protostars and the surrounding cloud remains a challenge. ALMA probes protostellar clusters on the scales of cores to clouds, and our ALMA Cycle I observations (using the 12 m and 7 m arrays) targeted the active protocluster Serpens South. Our previous findings for this region show that in this very young, low-mass star-forming cluster the outflows impart energy that sustains turbulence, and the outflows do not yet contribute enough energy to cause total disruption. ALMA Band 6 (230 GHz) observations of CO and continuum provide an unprecedented sub-arcsecond resolution and high-sensitivity view of outflow activity in the innermost regions of the cluster environment, characterizing outflows and their driving sources. C1 [Plunkett, Adele L.; Arce, Hector G.] Yale Univ, Dept Astron, New Haven, CT 06511 USA. [Gallardo, Jose; Corder, Stuartt A.] Joint ALMA Observ, Santiago, Chile. [Dunham, Michael M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Fernandez-Lopez, Manuel] CCT La Plata CONICET, Inst Argentino Radioastron, Buenos Aires, DF, Argentina. [Mardoness, Diego] Univ Chile, Dept Astron, Santiago, Chile. RP Plunkett, AL (reprint author), Yale Univ, Dept Astron, New Haven, CT 06511 USA. EM adele.plunkett@yale.edu; hector.arce@yale.edu NR 6 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 978-1-58381-883-1; 978-1-58381-882-4 J9 ASTR SOC P PY 2015 VL 499 BP 241 EP 242 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE2JX UT WOS:000369469500082 ER PT B AU Zhang, YC Arce, HG Mardones, D Dunham, MM Garay, G Noriega-Crespo, A Corder, S Offner, S AF Zhang, Yichen Arce, Hector G. Mardones, Diego Dunham, Michael M. Garay, Guido Noriega-Crespo, Alberto Corder, Stuartt Offner, Stella BE Iono, D Tatematsu, K Wootten, A Testi, L TI Studying the Outflow-Core Interaction with ALMA Cycle 1 Observations of the HH46/47 Molecular Outflow SO REVOLUTION IN ASTRONOMY WITH ALMA: THE THIRD YEAR SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 4th ALMA Science Conference on Revolution in Astronomy with ALMA: The Third Year CY DEC 08-11, 2014 CL Tokyo Int Forum, Tokyo, JAPAN HO Tokyo Int Forum AB We present preliminary analysis of ALMA cycle 1 12m array (CO)-C-12/(CO)-C-13/(CO)-O-18 data of the HH 46/47 molecular outflow. (CO)-C-13 and (CO)-O-18 trace relatively denser outflow material than (CO)-C-12 and allow us to trace the outflow to lower velocities than what it possible using only the (CO)-C-12 emission. Interestingly, the cavity wall of the red lobe can be seen at velocity as low as 0.2 km/s. Using (CO)-O-18, we are now able to estimate the optical depth of CO, and then use the corrected (CO)-C-13 emission to further and better correct the (CO)-C-12 emission and estimate the mass, momentum, and kinetic energy of the outflow. Moreover, (CO)-O-18 reveals a flattened rotational structure at the center, likely to be a rotational envelope infalling onto an inner Keplerian disk. C1 [Zhang, Yichen; Mardones, Diego; Garay, Guido] Univ Chile, Santiago, Chile. [Zhang, Yichen; Arce, Hector G.] Yale Univ, New Haven, CT USA. [Dunham, Michael M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Noriega-Crespo, Alberto] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Corder, Stuartt] Joint ALMA Observ, Santiago, Chile. [Offner, Stella] Univ Massachusetts, Amherst, MA 01003 USA. RP Zhang, YC (reprint author), Univ Chile, Santiago, Chile. EM yzhang@das.uchile.cl NR 1 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 978-1-58381-883-1; 978-1-58381-882-4 J9 ASTR SOC P PY 2015 VL 499 BP 243 EP 244 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE2JX UT WOS:000369469500083 ER PT B AU Sanhueza, P Jackson, JM Zhang, Q Foster, J Guzman, A AF Sanhueza, P. Jackson, J. M. Zhang, Q. Foster, J. Guzman, A. BE Iono, D Tatematsu, K Wootten, A Testi, L TI A Massive, Prestellar Clump Hosting no High-Mass Cores SO REVOLUTION IN ASTRONOMY WITH ALMA: THE THIRD YEAR SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 4th ALMA Science Conference on Revolution in Astronomy with ALMA: The Third Year CY DEC 08-11, 2014 CL Tokyo Int Forum, Tokyo, JAPAN HO Tokyo Int Forum ID STAR-FORMATION AB We observed a high-mass, prestellar clump in dust continuum with SMA (3.5 '') and in NH3 line emission with JVLA (2 ''). We find no core with sufficient mass to form high-mass stars at the current evolutionary stage. In order to form high mass stars, the embedded cores need to accrete a significant amount of mass over time which is consistent with some models of high-mass star formation. We also find that the gas in the cores is transonic or mildly supersonic. The embedded cores are sub-virialized, which is inconsistent with some models of high-mass star formation unless strong magnetic fields of similar to 1 mG are present. C1 [Sanhueza, P.] Natl Inst Nat Sci, Natl Astron Observ Japan, 2-21-1 Osawa, Mitaka, Tokyo, Japan. [Sanhueza, P.; Jackson, J. M.] Boston Univ, Dept Astron, Boston, MA 02215 USA. [Zhang, Q.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Foster, J.] Yale Univ, Ctr Astron & Astrophys, New Haven, CT USA. [Guzman, A.] Univ Chile, Dept Astron, Santiago, Chile. RP Sanhueza, P (reprint author), Natl Inst Nat Sci, Natl Astron Observ Japan, 2-21-1 Osawa, Mitaka, Tokyo, Japan. EM patricio.sanhueza@naoac.jp NR 10 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 978-1-58381-883-1; 978-1-58381-882-4 J9 ASTR SOC P PY 2015 VL 499 BP 245 EP 246 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE2JX UT WOS:000369469500084 ER PT B AU Ricci, L Carpenter, J Fu, B Hughes, M Corder, S Isella, A AF Ricci, Luca Carpenter, John Fu, Betsy Hughes, Meredith Corder, Stuartt Isella, Andrea BE Iono, D Tatematsu, K Wootten, A Testi, L TI Highlighting the Dynamical Interaction Between Planets and Planetesimal Belts with ALMA SO REVOLUTION IN ASTRONOMY WITH ALMA: THE THIRD YEAR SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 4th ALMA Science Conference on Revolution in Astronomy with ALMA: The Third Year CY DEC 08-11, 2014 CL Tokyo Int Forum, Tokyo, JAPAN HO Tokyo Int Forum ID MAIN-SEQUENCE STARS; DEBRIS DISKS; HD 107146 AB We observed the debris disk surrounding the young Solar analog BD 107146 using ALMA at 1.25 mm. The continuum emission extends from about 30 to 150 AU from the central star, with a depletion region at intermediate radii (similar to 80 AU). The dust density in the outer regions appears similar or larger than in the inner regions, which can be interpreted by models of formation and evolution of planetesimal belts which involve the disruptive collisions of planetesimals triggered by the recent formation of Pluto-sized bodies. If the region with lower dust density at intermediate radii in the disk is a fully depleted gap, then this structure could be carved by a planet with a mass of similar to 1 to few Earth masses at 80 AU from the star. C1 [Ricci, Luca] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Carpenter, John; Fu, Betsy] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Hughes, Meredith] Wesleyan Univ, Van Vleck Observ, Dept Astron, Midletown, CT 06457 USA. [Corder, Stuartt] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Isella, Andrea] Rice Univ, Dept Phys & Astron, Houston, TX 77521 USA. RP Ricci, L (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM luca.ricci@cfa.harvard.edu; jmc@astro.caltech.edu; bfu@caltech.edu; amhughes@wesleyan.edu; scorder@nrao.edu; isella@rice.edu NR 11 TC 0 Z9 0 U1 0 U2 1 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-883-1; 978-1-58381-882-4 J9 ASTR SOC P PY 2015 VL 499 BP 269 EP 272 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE2JX UT WOS:000369469500093 ER PT J AU Curler, GR Priyadarsanan, DR AF Curler, Gregory R. Priyadarsanan, Dharma Rajan TI Descriptions of Psychodidae (Diptera) from the Western Ghats of India SO ACTA ENTOMOLOGICA MUSEI NATIONALIS PRAGAE LA English DT Article DE Diptera; Psychodidae; moth flies; new species; new records; biodiversity; taxonomy; India; Oriental Region ID GENUS GONDWANOSCURUS AB Three new species of Psychodidae from the Western Ghats of India are described and illustrated. Specimens are from a single Malaise trap sample taken in 2007. Horaiella pectinata sp. nov. represents the first record of Horaiellinae from southern India; Gondwanoscurus jezeki sp. nov. and Saximormia gladiator sp. nov. represent new genus records for India and range extensions for both genera. Telmatoscopus arcuatus Vaillant, 1965 is transferred to Gondwanoscurus Jezek, 2002. A research prospectus for Indian Psychodidae is given. C1 [Curler, Gregory R.] Mississippi State Univ, Mississippi Entomol Museum, 100 Old Highway 12,PO Drawer 9775, Mississippi State, MS 39762 USA. [Curler, Gregory R.] Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20560 USA. [Priyadarsanan, Dharma Rajan] ATREE, Bengaluru 560064, India. RP Curler, GR (reprint author), Mississippi State Univ, Mississippi Entomol Museum, 100 Old Highway 12,PO Drawer 9775, Mississippi State, MS 39762 USA. EM gcurler@gmail.com FU Samuel W. Williston Dipterology Fund, Smithsonian Institution, Washington, D.C.; Schlinger Foundation, USA FX Best wishes to Jan Jezek on his 70th birthday. We are grateful to M. E. Irwin and E. Schlinger for collecting and sorting the specimens, respectively. A. J. Jacobson kindly assisted with recording measurements. This work was supported in part by the Samuel W. Williston Dipterology Fund, Smithsonian Institution, Washington, D.C. (award to GRC).; We are grateful to the Kerala Forests and Wild life Department for permits, and the Schlinger Foundation, USA, for funding in support of fieldwork. Thorough reviews from Gunnar Mikalsen Kvifte and Danilo Pacheco Cordeiro helped to improve the manuscript. NR 20 TC 1 Z9 1 U1 1 U2 3 PU NARODNI MUZEUM - PRIRODOVEDECKE MUZEUM PI PRAHA PA KUNRATICE, PRAHA, CZ-148 00, CZECH REPUBLIC SN 0374-1036 EI 1804-6487 J9 ACTA ENT MUS NAT PRA JI Acta Entomol. Mus. Natl. Pragae PY 2015 VL 55 IS 2 BP 473 EP 483 PG 11 WC Entomology SC Entomology GA DB3TN UT WOS:000368434800003 ER PT S AU Helz, RT Clague, DA Mastin, LG Rose, TR AF Helz, Rosalind T. Clague, David A. Mastin, Larry G. Rose, Timothy R. BE Carey, R Cayol, V Poland, M Weis, D TI Evidence for Large Compositional Ranges in Coeval Melts Erupted from Kilauea's Summit Reservoir SO HAWAIIAN VOLCANOES: FROM SOURCE TO SURFACE SE Geophysical Monograph Book Series LA English DT Proceedings Paper CT American Geophysical Union Chapman Conference on Hawaiian Volcanoes - From Source to Surface CY AUG 20-24, 2012 CL HI SP Amer Geophys Union ID IKI LAVA LAKE; EXPLOSIVE ERUPTIONS; ASH MEMBER; HAWAII; VOLCANO; MAGMA; DIFFERENTIATION; MECHANICS; GLASSES; STORAGE AB Petrologic observations on Kilauea's lavas include abundant microprobe analyses of glasses, which show the range of melts available in Kilauea's summit reservoir over time. During the past two centuries, compositions of melts erupted within the caldera have been limited to MgO = 6.3-7.5 wt%. Extracaldera lavas of the 1959, 1971, and 1974 eruptions contain melts with up to 10.2, 8.9, and 9.2 wt% MgO, respectively, and the 1924 tephra contains juvenile Pele's tears with up to 9.1 wt% MgO. Melt compositions from explosive deposits at Kilauea, including the Keanakako'i (A.D. 1500-1800), Kulanaokuaiki (A.D. 400-1000), and Pahala (10-25 ka) tephra units, show large ranges of MgO contents. The range of melt MgO is 6.5-11.0 wt% for the Keanakako'i; the Kulanaokuaiki extends to 12.5% MgO and the Pahala Ash includes rare shards with 13-14.5% MgO. The frequency distributions for MgO in the Keanakako'i and Kulanaokuaiki glasses are bimodal, suggesting preferential magma storage at two different depths. Kilauea's summit reservoir contains melts ranging from 6.5 to at least 11.0 wt% MgO, and such melts were available for sampling near instantaneously and repeatedly over centuries. More magnesian melts are inferred to have risen directly from greater depth. C1 [Helz, Rosalind T.] US Geol Survey, Reston, VA 22092 USA. [Clague, David A.] Monterey Bay Aquarium Res Inst, Moss Landing, CA USA. [Mastin, Larry G.] US Geol Survey, Cascades Volcano Observ, Vancouver, WA USA. [Rose, Timothy R.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Helz, RT (reprint author), US Geol Survey, 959 Natl Ctr, Reston, VA 22092 USA. NR 51 TC 0 Z9 0 U1 1 U2 1 PU JOHN WILEY & SONS INC PI HOBOKEN PA 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 0065-8448 BN 978-1-118-87207-9; 978-1-118-87204-8 J9 GEOPHYS MONOGR SER PY 2015 VL 208 BP 125 EP 145 PG 21 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA BE1RH UT WOS:000368412500007 ER PT B AU Erdmann, C AF Erdmann, Christopher BE Holl, A Lesteven, S Dietrich, D Gasperini, A TI Data Scientist Training for Librarians SO LIBRARY AND INFORMATION SERVICES IN ASTRONOMY VII: OPEN SCIENCE AT THE FRONTIERS OF LIBRARIANSHIP SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 7th Library and Information Service in Astronomy Conference: Open Science at the Frontiers of Librarianship CY JUN 17-20, 2014 CL Astron Observ Capodimonte, Naples, ITALY SP Springer, Amer Astron Soc, Amer Inst Phys Publish, Inst Phys, EDP Sci, Altmetr, APS Phys, European So Observ, Elsevier, Figshare, PTFS Europe, STANDARDS AND MORE, SPIE Digital Lib, Parthenope Univ, Dept Sci & Technol, Certosa & Museum San Martino, Assoc Amici Capodimonte, Italian Lib Assoc, Municipal Naples, Regione Campania HO Astron Observ Capodimonte AB Recent studies suggest that there will be a shortfall in the near future of skilled talent available to help take advantage of big data in organizations. Meanwhile, government initiatives have encouraged the research community to share their data more openly, raising new challenges for researchers. Librarians can assist in this new data-driven environment. Data Scientist Training for Librarians (or Data Savvy Librarians) is an experimental course being offered by the Harvard Library to train librarians to respond to the growing data needs of their communities. In the course, librarians familiarize themselves with the research data lifecycle, working hands-on with the latest tools for extracting, wrangling, storing, analyzing, and visualizing data. By experiencing the research data lifecycle themselves, and becoming data savvy and embracing the data science culture, librarians can begin to imagine how their services might be transformed. C1 [Erdmann, Christopher] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Erdmann, C (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 10 TC 0 Z9 0 U1 3 U2 6 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-868-8 J9 ASTR SOC P PY 2015 VL 492 BP 31 EP 37 PG 7 WC Astronomy & Astrophysics; Computer Science, Information Systems; Information Science & Library Science SC Astronomy & Astrophysics; Computer Science; Information Science & Library Science GA BE1QL UT WOS:000368385000005 ER PT B AU Rots, AH Winkelman, SL AF Rots, Arnold H. Winkelman, Sherry L. BE Holl, A Lesteven, S Dietrich, D Gasperini, A TI Observatory Bibliographies: Toward Multi-usage and Better Metrics SO LIBRARY AND INFORMATION SERVICES IN ASTRONOMY VII: OPEN SCIENCE AT THE FRONTIERS OF LIBRARIANSHIP SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 7th Library and Information Service in Astronomy Conference: Open Science at the Frontiers of Librarianship CY JUN 17-20, 2014 CL Astron Observ Capodimonte, Naples, ITALY SP Springer, Amer Astron Soc, Amer Inst Phys Publish, Inst Phys, EDP Sci, Altmetr, APS Phys, European So Observ, Elsevier, Figshare, PTFS Europe, STANDARDS AND MORE, SPIE Digital Lib, Parthenope Univ, Dept Sci & Technol, Certosa & Museum San Martino, Assoc Amici Capodimonte, Italian Lib Assoc, Municipal Naples, Regione Campania HO Astron Observ Capodimonte AB There are typically two areas of motivation for the establishment of observatory bibliographies. One area of motivation is to provide a management-oriented tool that facilitates the compilation of metrics that yield some measure of the performance of the observatory. The second area of motivation is to produce a research tool that allows the science community to integrate the mining of published works in their research. It is important to keep in mind that these two objectives impose different requirements on the metadata that are collected in a bibliography. We submit that there are good reasons to integrate the two objectives in the formulation of requirements and in the design of observatory bibliographies: they benefit from each other and the yield from the sum of the metadata collections is greater than the sum of their individual yields. Further integration of the bibliography with the observatory's databases offers an additional important benefit for metrics regarding the performance of the observatory. We propose a suite of metrics, enabled by the extended metadata and database linking, that provides better insight into how well the observatory functions and is being used. These include measuring the delay between observation and publication, the percentage of data that gets published, and the re-use of the data and their archival value. C1 [Rots, Arnold H.; Winkelman, Sherry L.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Rots, AH (reprint author), Smithsonian Astrophys Observ, 60 Garden St MS 67, 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 978-1-58381-868-8 J9 ASTR SOC P PY 2015 VL 492 BP 71 EP 79 PG 9 WC Astronomy & Astrophysics; Computer Science, Information Systems; Information Science & Library Science SC Astronomy & Astrophysics; Computer Science; Information Science & Library Science GA BE1QL UT WOS:000368385000011 ER PT B AU Henneken, EA Accomazzi, A Kurtz, MJ Grant, CS Thompson, D Luker, J Chyla, R Holachek, A Murray, SS AF Henneken, Edwin A. Accomazzi, Alberto Kurtz, Michael J. Grant, Carolyn S. Thompson, Donna Luker, Jay Chyla, Roman Holachek, Alexandra Murray, Stephen S. BE Holl, A Lesteven, S Dietrich, D Gasperini, A TI Computing and Using Metrics in the ADS SO LIBRARY AND INFORMATION SERVICES IN ASTRONOMY VII: OPEN SCIENCE AT THE FRONTIERS OF LIBRARIANSHIP SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 7th Library and Information Service in Astronomy Conference: Open Science at the Frontiers of Librarianship CY JUN 17-20, 2014 CL Astron Observ Capodimonte, Naples, ITALY SP Springer, Amer Astron Soc, Amer Inst Phys Publish, Inst Phys, EDP Sci, Altmetr, APS Phys, European So Observ, Elsevier, Figshare, PTFS Europe, STANDARDS AND MORE, SPIE Digital Lib, Parthenope Univ, Dept Sci & Technol, Certosa & Museum San Martino, Assoc Amici Capodimonte, Italian Lib Assoc, Municipal Naples, Regione Campania HO Astron Observ Capodimonte AB Finding measures for research impact, be it for individuals, institutions, instruments, or projects, has gained a lot of popularity. There are more papers written than ever on new impact measures, and problems with existing measures are being pointed out on a regular basis. Funding agencies require impact statistics in their reports, job candidates incorporate them in their resumes, and publication metrics have even been used in at least one recent court case. To support this need for research impact indicators, the SAO/NASA Astrophysics Data System (ADS) has developed a service that provides a broad overview of various impact measures. In this paper we discuss how the ADS can be used to quench the thirst for impact measures. We will also discuss a couple of the lesser-known indicators in the metrics overview and the main issues to be aware of when compiling publication-based metrics in the ADS, namely author name ambiguity and citation incompleteness. C1 [Henneken, Edwin A.; Accomazzi, Alberto; Kurtz, Michael J.; Grant, Carolyn S.; Thompson, Donna; Luker, Jay; Chyla, Roman; Holachek, Alexandra] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Murray, Stephen S.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. RP Henneken, EA (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. OI Henneken, Edwin/0000-0003-4264-2450 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 978-1-58381-868-8 J9 ASTR SOC P PY 2015 VL 492 BP 80 EP 84 PG 5 WC Astronomy & Astrophysics; Computer Science, Information Systems; Information Science & Library Science SC Astronomy & Astrophysics; Computer Science; Information Science & Library Science GA BE1QL UT WOS:000368385000012 ER PT B AU Egret, D Laurenceau, A Accomazzi, A AF Egret, Daniel Laurenceau, Amelia Accomazzi, Alberto BE Holl, A Lesteven, S Dietrich, D Gasperini, A TI Using ADS for Creating Bibliographies of Research Institutions SO LIBRARY AND INFORMATION SERVICES IN ASTRONOMY VII: OPEN SCIENCE AT THE FRONTIERS OF LIBRARIANSHIP SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 7th Library and Information Service in Astronomy Conference: Open Science at the Frontiers of Librarianship CY JUN 17-20, 2014 CL Astron Observ Capodimonte, Naples, ITALY SP Springer, Amer Astron Soc, Amer Inst Phys Publish, Inst Phys, EDP Sci, Altmetr, APS Phys, European So Observ, Elsevier, Figshare, PTFS Europe, STANDARDS AND MORE, SPIE Digital Lib, Parthenope Univ, Dept Sci & Technol, Certosa & Museum San Martino, Assoc Amici Capodimonte, Italian Lib Assoc, Municipal Naples, Regione Campania HO Astron Observ Capodimonte AB Institutions often have a need for maintaining "institutional bibliographies," a list of all papers published by individuals affiliated with the institution. Using the Observatoire de Paris (France) as an example, we show how this can be done, using the services of the ADS and other bibliographic databases. In this specific case, we are able to quantify the success rate in creating the extensive list of the scientific output of the institution by each source database. Our analysis helps identify the current limitations and ambiguities in the contents and format of the affiliation/address field, as produced by the authors and modified by journal editors and database managers. We advocate for the development of an authoritative list of astronomical institutions that can be used by the ADS and publishers as a controlled field in order to significantly improve the efficiency of affiliation queries. C1 [Egret, Daniel] PSL Res Univ, LUTH, Observ Paris, F-92190 Meudon, France. [Egret, Daniel] Univ Paris Diderot, CNRS, UMR 8102, F-92190 Meudon, France. [Laurenceau, Amelia] PSL Res Univ, Observ Paris, UMS 2201, CNRS,INSU, F-75014 Paris, France. [Accomazzi, Alberto] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Egret, D (reprint author), PSL Res Univ, LUTH, Observ Paris, F-92190 Meudon, France. NR 5 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 978-1-58381-868-8 J9 ASTR SOC P PY 2015 VL 492 BP 85 EP 89 PG 5 WC Astronomy & Astrophysics; Computer Science, Information Systems; Information Science & Library Science SC Astronomy & Astrophysics; Computer Science; Information Science & Library Science GA BE1QL UT WOS:000368385000013 ER PT B AU Thompson, DM Henneken, EA Grant, CS Holachek, A Accomazzi, A Kurtz, MJ Chyla, R Luker, J Murray, SS AF Thompson, Donna M. Henneken, Edwin A. Grant, Carolyn S. Holachek, Alexandra Accomazzi, Alberto Kurtz, Michael J. Chyla, Roman Luker, James Murray, Stephen S. BE Holl, A Lesteven, S Dietrich, D Gasperini, A TI Saving the Orphaned Astronomical Literature SO LIBRARY AND INFORMATION SERVICES IN ASTRONOMY VII: OPEN SCIENCE AT THE FRONTIERS OF LIBRARIANSHIP SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 7th Library and Information Service in Astronomy Conference: Open Science at the Frontiers of Librarianship CY JUN 17-20, 2014 CL Astron Observ Capodimonte, Naples, ITALY SP Springer, Amer Astron Soc, Amer Inst Phys Publish, Inst Phys, EDP Sci, Altmetr, APS Phys, European So Observ, Elsevier, Figshare, PTFS Europe, STANDARDS AND MORE, SPIE Digital Lib, Parthenope Univ, Dept Sci & Technol, Certosa & Museum San Martino, Assoc Amici Capodimonte, Italian Lib Assoc, Municipal Naples, Regione Campania HO Astron Observ Capodimonte AB A large portion of the astronomical research of the 19th and early 20th centuries was reported in publications written and distributed by individual observatories. Many of these collections were not widely distributed and complete sets of these volumes are now difficult to locate. The ADS has taken on the effort to put these publications online and make them searchable. In this paper I will outline the project and discuss some of the highlights and challenges the ADS has encountered over the duration of the project. C1 [Thompson, Donna M.; Henneken, Edwin A.; Grant, Carolyn S.; Holachek, Alexandra; Accomazzi, Alberto; Kurtz, Michael J.; Chyla, Roman; Luker, James] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Murray, Stephen S.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. RP Thompson, DM (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. OI Henneken, Edwin/0000-0003-4264-2450 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 978-1-58381-868-8 J9 ASTR SOC P PY 2015 VL 492 BP 150 EP 154 PG 5 WC Astronomy & Astrophysics; Computer Science, Information Systems; Information Science & Library Science SC Astronomy & Astrophysics; Computer Science; Information Science & Library Science GA BE1QL UT WOS:000368385000024 ER PT B AU Accomazzi, A Kurtz, MJ Henneken, EA Chyla, R Luker, J Grant, CS Thompson, DM Holachek, A Dave, R Murray, SS AF Accomazzi, Alberto Kurtz, Michael J. Henneken, Edwin A. Chyla, Roman Luker, James Grant, Carolyn S. Thompson, Donna M. Holachek, Alexandra Dave, Rahul Murray, Stephen S. BE Holl, A Lesteven, S Dietrich, D Gasperini, A TI ADS: The Next Generation Search Platform SO LIBRARY AND INFORMATION SERVICES IN ASTRONOMY VII: OPEN SCIENCE AT THE FRONTIERS OF LIBRARIANSHIP SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 7th Library and Information Service in Astronomy Conference: Open Science at the Frontiers of Librarianship CY JUN 17-20, 2014 CL Astron Observ Capodimonte, Naples, ITALY SP Springer, Amer Astron Soc, Amer Inst Phys Publish, Inst Phys, EDP Sci, Altmetr, APS Phys, European So Observ, Elsevier, Figshare, PTFS Europe, STANDARDS AND MORE, SPIE Digital Lib, Parthenope Univ, Dept Sci & Technol, Certosa & Museum San Martino, Assoc Amici Capodimonte, Italian Lib Assoc, Municipal Naples, Regione Campania HO Astron Observ Capodimonte ID ASTROPHYSICS DATA SYSTEM AB Four years after the last LISA meeting, the NASA Astrophysics Data System (ADS) finds itself in the middle of major changes to the infrastructure and contents of its database. In this paper we highlight a number of features of great importance to librarians and discuss the additional functionality that we are currently developing. Our citation coverage has doubled since 2010 and now consists of over 10 million citations. We are normalizing the affiliation information in our records and we have started collecting and linking funding sources with papers in our system. At the same time, we are undergoing major technology changes in the ADS platform. We have rolled out and are now enhancing a new high-performance search engine capable of performing full-text as well as metadata searches using an intuitive query language. We are currently able to index acknowledgments, affiliations, citations, and funding sources. While this effort is still ongoing, some of its benefits are already available through the ADS Labs user interface and API at http://adslabs.org/adsabs/. C1 [Accomazzi, Alberto; Kurtz, Michael J.; Henneken, Edwin A.; Chyla, Roman; Luker, James; Grant, Carolyn S.; Thompson, Donna M.; Holachek, Alexandra; Dave, Rahul; Murray, Stephen S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Accomazzi, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Henneken, Edwin/0000-0003-4264-2450 NR 10 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 978-1-58381-868-8 J9 ASTR SOC P PY 2015 VL 492 BP 189 EP 197 PG 9 WC Astronomy & Astrophysics; Computer Science, Information Systems; Information Science & Library Science SC Astronomy & Astrophysics; Computer Science; Information Science & Library Science GA BE1QL UT WOS:000368385000031 ER PT B AU Frey, K Erdmann, C Accomazzi, A Rubin, L Biemesderfer, C Gray, N Soles, J AF Frey, Katie Erdmann, Christopher Accomazzi, Alberto Rubin, Louise Biemesderfer, Chris Gray, Norman Soles, Justin BE Holl, A Lesteven, S Dietrich, D Gasperini, A TI Management of the Unified Astronomy Thesaurus SO LIBRARY AND INFORMATION SERVICES IN ASTRONOMY VII: OPEN SCIENCE AT THE FRONTIERS OF LIBRARIANSHIP SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 7th Library and Information Service in Astronomy Conference: Open Science at the Frontiers of Librarianship CY JUN 17-20, 2014 CL Astron Observ Capodimonte, Naples, ITALY SP Springer, Amer Astron Soc, Amer Inst Phys Publish, Inst Phys, EDP Sci, Altmetr, APS Phys, European So Observ, Elsevier, Figshare, PTFS Europe, STANDARDS AND MORE, SPIE Digital Lib, Parthenope Univ, Dept Sci & Technol, Certosa & Museum San Martino, Assoc Amici Capodimonte, Italian Lib Assoc, Municipal Naples, Regione Campania HO Astron Observ Capodimonte AB The Unified Astronomy Thesaurus (UAT) is an open, interoperable, and community-supported thesaurus of astronomical and astrophysical concepts and their relationships. Management of the UAT is based on a community-supported approach. This will ensure that the thesaurus stays current by allowing users to suggest an addition or revision. These suggestions will then be subjected to a thorough expert review process before being accepted for addition to the UAT or rejected. Many leading astronomical institutions, professional associations, journal publishers, learned societies, and data repositories support the UAT as a standard astronomical terminology. C1 [Frey, Katie; Erdmann, Christopher; Rubin, Louise] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Accomazzi, Alberto] SAO NASA Astrophys Data Syst, New York, NY USA. [Biemesderfer, Chris] Amer Astron Soc, Washington, DC USA. [Gray, Norman] Univ Glasgow, Glasgow G12 8QQ, Lanark, Scotland. [Soles, Justin] McGill Univ, Montreal, PQ H3A 2T5, Canada. RP Frey, K (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. NR 2 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 978-1-58381-868-8 J9 ASTR SOC P PY 2015 VL 492 BP 204 EP 207 PG 4 WC Astronomy & Astrophysics; Computer Science, Information Systems; Information Science & Library Science SC Astronomy & Astrophysics; Computer Science; Information Science & Library Science GA BE1QL UT WOS:000368385000033 ER PT B AU Grant, CS Thompson, DM Chyla, R Holachek, A Accomazzi, A Henneken, EA Kurtz, MJ Luker, J Murray, SS AF Grant, Carolyn S. Thompson, Donna M. Chyla, Roman Holachek, Alexandra Accomazzi, Alberto Henneken, Edwin A. Kurtz, Michael J. Luker, James Murray, Stephen S. BE Holl, A Lesteven, S Dietrich, D Gasperini, A TI Enabling Meaningful Affiliation Searches in the ADS SO LIBRARY AND INFORMATION SERVICES IN ASTRONOMY VII: OPEN SCIENCE AT THE FRONTIERS OF LIBRARIANSHIP SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 7th Library and Information Service in Astronomy Conference: Open Science at the Frontiers of Librarianship CY JUN 17-20, 2014 CL Astron Observ Capodimonte, Naples, ITALY SP Springer, Amer Astron Soc, Amer Inst Phys Publish, Inst Phys, EDP Sci, Altmetr, APS Phys, European So Observ, Elsevier, Figshare, PTFS Europe, STANDARDS AND MORE, SPIE Digital Lib, Parthenope Univ, Dept Sci & Technol, Certosa & Museum San Martino, Assoc Amici Capodimonte, Italian Lib Assoc, Municipal Naples, Regione Campania HO Astron Observ Capodimonte AB For many years, users have wanted to search affiliations in the ADS in order to build institutional databases and to help with author disambiguation. Although we currently provide this capability upon request, we have yet to incorporate it as part of the operational Abstract Service. This is because it cannot be used reliably, primarily because of the lack of uniform representation of the affiliation data. In an effort to make affiliation searches more meaningful, we have designed a two-tiered hierarchy of standard institutional names based on Ringgold identifiers, with the expectation that this will enable us to implement a search by institution, which will work for the vast majority of institutions. It is our intention to provide the capability of searching the ADS both by standard affiliation name and original affiliation string, as well as to enable autosuggest of affiliations as a means of helping to disambiguate author identification. Some institutions are likely to require manual work, and we encourage interested librarians to assist us in standardizing the representation of their institutions in the affiliation field. C1 [Grant, Carolyn S.; Thompson, Donna M.; Chyla, Roman; Holachek, Alexandra; Accomazzi, Alberto; Henneken, Edwin A.; Kurtz, Michael J.; Luker, James; Murray, Stephen S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Grant, CS (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. OI Henneken, Edwin/0000-0003-4264-2450 NR 0 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 978-1-58381-868-8 J9 ASTR SOC P PY 2015 VL 492 BP 208 EP 211 PG 4 WC Astronomy & Astrophysics; Computer Science, Information Systems; Information Science & Library Science SC Astronomy & Astrophysics; Computer Science; Information Science & Library Science GA BE1QL UT WOS:000368385000034 ER PT B AU Holmquist, J Erdmann, C Damon, J AF Holmquist, Jane Erdmann, Christopher Damon, James BE Holl, A Lesteven, S Dietrich, D Gasperini, A TI 416492 ORCID IDs and Counting: Uptake by the Astronomical Community SO LIBRARY AND INFORMATION SERVICES IN ASTRONOMY VII: OPEN SCIENCE AT THE FRONTIERS OF LIBRARIANSHIP SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 7th Library and Information Service in Astronomy Conference: Open Science at the Frontiers of Librarianship CY JUN 17-20, 2014 CL Astron Observ Capodimonte, Naples, ITALY SP Springer, Amer Astron Soc, Amer Inst Phys Publish, Inst Phys, EDP Sci, Altmetr, APS Phys, European So Observ, Elsevier, Figshare, PTFS Europe, STANDARDS AND MORE, SPIE Digital Lib, Parthenope Univ, Dept Sci & Technol, Certosa & Museum San Martino, Assoc Amici Capodimonte, Italian Lib Assoc, Municipal Naples, Regione Campania HO Astron Observ Capodimonte AB ORCID - an acronym short for Open Researcher and Contributor ID - is an international, interdisciplinary and community-driven effort to create and maintain a registry of persistent, unique identifiers for researchers and scholars. ORCID IDs are extremely important in the disambiguation of non-unique author names. They can also be embedded in key workflows, such as research profile maintenance, manuscript submissions and grant applications. Using several approaches to reach out to our users, we will report on ORCID ID uptake by the astronomical community. C1 [Holmquist, Jane] Princeton Univ Lib, Princeton, NJ 08544 USA. [Erdmann, Christopher; Damon, James] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Holmquist, J (reprint author), Princeton Univ Lib, Princeton, NJ 08544 USA. EM jane@princeton.edu NR 3 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 978-1-58381-868-8 J9 ASTR SOC P PY 2015 VL 492 BP 323 EP 330 PG 8 WC Astronomy & Astrophysics; Computer Science, Information Systems; Information Science & Library Science SC Astronomy & Astrophysics; Computer Science; Information Science & Library Science GA BE1QL UT WOS:000368385000053 ER PT J AU Braje, TJ Rick, TC AF Braje, Todd J. Rick, Torben C. TI IDENTIFYING SPECIALIZED 19TH CENTURY FISHING CAMPS ON CALIFORNIA'S NORTHERN CHANNEL ISLANDS: APPLYING AMS RADIOCARBON DATING TO HISTORICAL SITES SO RADIOCARBON LA English DT Article ID SAN-MIGUEL ISLAND; ROSA ISLAND; SOUTHERN CALIFORNIA; RESERVOIR AGES; SHELL MIDDEN; COASTAL; ARCHAEOLOGY; ABALONE; CHINESE; SUBSISTENCE AB California's Northern Channel Islands have long been an epicenter of specialized fishing economies dating from 13,000 yr ago to the mid-19th century. With thousands of well-preserved shell middens, some dominated by single shellfish species and little to no material culture, it can be difficult to distinguish between specialized prehistoric and historical deposits at some site types. Beginning at least in the Early Holocene and continuing into the Historic period, California mussels, turban snails, and abalone were targeted for specialized collection and processing by Native Americans and later Chinese and Euro-American fishers. Here, we demonstrate how selective accelerator mass spectrometry (AMS) radiocarbon dating of specialized abalone processing camps can help distinguish between prehistoric and historical sites. While unconventional, our case study demonstrates the utility of C-14 dating at sites less than 300 yr old. C1 [Braje, Todd J.] San Diego State Univ, Dept Anthropol, San Diego, CA 92182 USA. [Rick, Torben C.] Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Program Human Ecol & Archaeobiol, Washington, DC 20560 USA. RP Braje, TJ (reprint author), San Diego State Univ, Dept Anthropol, San Diego, CA 92182 USA. FU Channel Islands National Park (CINP); Nature Conservancy (TNC); Smithsonian Institution; TNC FX Our field and analytical research was supported by Channel Islands National Park (CINP), the Nature Conservancy (TNC), and our home institutions. Our CINP fieldwork was completed under Cooperative Agreement No. P11AC91045. Our work for the TNC was supported by a cooperative agreement between the Smithsonian Institution and the TNC. We are grateful to Ann Huston, Kelly Minas, Mark Senning, Ian Williams, and Don Morris at CINP and Christina Boser, Jennifer Baker, David Dewey, Scott Morrison, and John Randall from the TNC for their time and support. Thanks to Linda Bentz, Breana Campbell, Charles Dickerson, Jon Erlandson, Kristina Gill, Courtney Hofman, Don Morris, and Leslie Reeder-Myers for sharing their expertise and assisting in fieldwork. Finally, we thank Jon Erlandson and the editors for their assistance in the review, revision, and production of our manuscript. NR 38 TC 0 Z9 0 U1 0 U2 0 PU UNIV ARIZONA DEPT GEOSCIENCES PI TUCSON PA RADIOCARBON 4717 E FORT LOWELL RD, TUCSON, AZ 85712 USA SN 0033-8222 EI 1945-5755 J9 RADIOCARBON JI Radiocarbon PY 2015 VL 57 IS 5 BP 909 EP 916 DI 10.2458/azu_rc.57.18397 PG 8 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA DB1WF UT WOS:000368299000013 ER PT S AU Cook-Patton, SC AF Cook-Patton, Susan C. BE Sutton, RK TI Plant Biodiversity on Green Roofs SO GREEN ROOF ECOSYSTEMS SE Ecological Studies-Analysis and Synthesis LA English DT Article; Book Chapter DE Genotypic richness; Species richness; Functional group diversity; Functional trait diversity; Phylogenetic diversity; Habitat; Ecosystem stability; Plant-animal interactions ID SPECIES-DIVERSITY; POSITIVE INTERACTIONS; GRASSLAND ECOSYSTEMS; SUBSTRATE DEPTH; FUNCTIONAL-ROLE; PRODUCTIVITY; URBAN; RICHNESS; COMMUNITIES; VEGETATION AB Experimentation in grasslands and other ecosystems suggest that diverse plant communities grow more vigorously than simple communities, support a more robust animal community, and better resist stressors like disease, herbivory, and invasion. Despite the potential advantages of plant diversity on green roofs, many green roof communities consist of a few hardy species that are known to tolerate the harsh conditions on green roofs. Moreover, experimental tests of diversity on green roofs are infrequent. I therefore review the ecological literature in the context of green roof design to suggest ways to increase plant diversity on green roofs and hypothesize how increasing diversity might improve green roof function. Although it is unlikely that the complex, ecological dynamics of natural ecosystems will map directly onto the simplified, highly engineered ecosystem of a green roof, I argue that the lessons learned from decades of ecological experimentation can be adapted to green roof design to improve long-term plant performance and enhance the services provided by green roofs to urban communities. Ultimately, diversity experiments on green roofs will be required to prove whether similar ecological dynamics can exist in natural ecosystems and on rooftops, and whether or not the parallels I draw are justified. Therefore I end this chapter with a research agenda for the future, suggesting experiments that would greatly enhance our understanding of green roofs as ecosystems. C1 [Cook-Patton, Susan C.] Smithsonian Environm Res Ctr, Forest Ecol Lab, Edgewater, MD 21037 USA. RP Cook-Patton, SC (reprint author), Smithsonian Environm Res Ctr, Forest Ecol Lab, POB 28, Edgewater, MD 21037 USA. EM cookpatton@gmail.com NR 93 TC 1 Z9 1 U1 2 U2 7 PU SPRINGER INT PUBLISHING AG PI CHAM PA GEWERBESTRASSE 11, CHAM, CH-6330, SWITZERLAND SN 0070-8356 BN 978-3-319-14983-7; 978-3-319-14982-0 J9 ECOL STUD-ANAL SYNTH JI Ecol. Stud. PY 2015 VL 223 BP 193 EP 209 DI 10.1007/978-3-319-14983-7_8 D2 10.1007/978-3-319-14983-7 PG 17 WC Ecology; Horticulture SC Environmental Sciences & Ecology; Agriculture GA BE1LW UT WOS:000368109000009 ER PT J AU Agrain, FA Buffington, ML Chaboo, CS Chamorro, ML Scholler, M AF Agrain, Federico A. Buffington, Matthew L. Chaboo, Caroline S. Chamorro, Maria L. Schoeller, Matthias TI Leaf beetles are ant-nest beetles: the curious life of the juvenile stages of case-bearers (Coleoptera, Chrysomelidae, Cryptocephalinae) SO ZOOKEYS LA English DT Review DE Myrmecophily; Camptosomata; Larvae; Biology; Clytrini; Cryptocephalini ID HYMENOPTERA-FORMICIDAE; EARLY EVOLUTION; PHYLOGENY; DIVERSIFICATION; BIOLOGY; AMBER; ASSOCIATIONS; ARCHITECTURE; ANGIOSPERMS; DOMINICAN AB Although some species of Cryptocephalinae (Coleoptera: Chrysomelidae) have been documented with ants (Hymenoptera: Formicidae) for almost 200 years, information on this association is fragmentary. This contribution synthesizes extant literature and analysizes the data for biological patterns. Myrmecophily is more common in the tribe Clytrini than in Cryptocephalini, but not documented for Fulcidacini or the closely-related Lamprosomatinae. Myrmecophilous cryptocephalines (34 species in 14 genera) primarily live among formicine and myrmecines ants as hosts. These two ant lineages are putative sister-groups, with their root-node dated to between 77-90 mya. In the New World tropics, the relatively recent radiation of ants from moist forests to more xeric ecosystems might have propelled the association of cryptocephalines and ant nests. Literature records suggest that the defensive behavioral profile or chemical profile (or both) of these ants has been exploited by cryptocephalines. Another pattern appears to be that specialized natural enemies, especially parasitoid Hymenoptera, exploit cryptocephaline beetles inside the ant nests. With the extant data at hand, based on the minimum age of a fossil larva dated to 45 mya, we can infer that the origin of cryptocephaline myrmecophily could have arisen within the Upper Cretaceous or later. It remains unknown how many times myrmecophily has appeared, or how old is the behavior. This uncertainty is compounded by incongruent hypotheses about the origins of Chrysomelidae and angiosperm-associated lineages of cryptocephalines. Living with ants offers multiple advantages that might have aided the colonization of xeric environments by some cryptocephaline species. C1 [Agrain, Federico A.] CCT CONICET, IADIZA, Entomol Lab, Mendoza, Argentina. [Buffington, Matthew L.; Chamorro, Maria L.] USDA ARS, Systemat Entomol Lab, Natl Museum Nat Hist, MRC 168,Smithsonian Inst, Washington, DC 20013 USA. [Chaboo, Caroline S.] Univ Kansas, Dept Entomol, Lawrence, KS 66045 USA. [Schoeller, Matthias] Univ Humberside, Fac Life Sci, D-14195 Berlin, Germany. RP Agrain, FA (reprint author), CCT CONICET, IADIZA, Entomol Lab, CC507,5500,Ave A Ruiz Leal S-N, Mendoza, Argentina. EM fagrain@mendoza-conicet.gov.ar FU Agencia Nacional de Promocion Cientifica y Tecnica, Argentina (ANPCyT) [2013-2211, 2011-2573]; University of Kansas; Systematic Entomology Laboratory, ARS-USDA FX This research was supported by the authors' respective institutions. Agrain is grateful to CONICET for continued research support and Agencia Nacional de Promocion Cientifica y Tecnica, Argentina (ANPCyT) for additional support to compete this work by PICT#2013-2211, and PICT#2011-2573. Chaboo is supported by the University of Kansas. Buffington and Chamorro are supported by the Systematic Entomology Laboratory, ARS-USDA. We are pleased to dedicate this paper to our esteemed colleague and chrysomelid researcher, Dr Pierre Jolivet, who has spent his professional career promoting knowledge of leaf beetles, including the relations of leaf beetles and ants. Mention of trade names or commercial products in this publication is solely for the purpose of providing specific information and does not imply recommendation or endorsement by the USDA. USDA is an equal opportunity provider and employer. NR 140 TC 1 Z9 1 U1 3 U2 8 PU PENSOFT PUBL PI SOFIA PA 12 PROF GEORGI ZLATARSKI ST, SOFIA, 1700, BULGARIA SN 1313-2989 EI 1313-2970 J9 ZOOKEYS JI ZooKeys PY 2015 IS 547 SI SI BP 133 EP 164 DI 10.3897/zookeys.547.6098 PG 32 WC Zoology SC Zoology GA DA5YG UT WOS:000367877900008 PM 26798319 ER PT J AU Schindel, DE Bubela, T Rosenthal, J Castle, D du Plessis, P Bye, R AF Schindel, David E. Bubela, Tania Rosenthal, Joshua Castle, David du Plessis, Pierre Bye, Robert CA PMCW TI The New Age of the Nagoya Protocol SO NATURE CONSERVATION-BULGARIA LA English DT Article DE Nagoya Protocol; Access and Benefit Sharing; DNA barcoding; medicinal plants; Convention on Biological Diversity; international agreements ID DNA BARCODE; IDENTIFICATION; PRODUCTS AB The entry into force of the Nagoya Protocol of the Convention on Biological Diversity will lead to new legislation and regulations that could change international collaborative research in biology. This article suggests a new approach that researchers can use in negotiating international Access and Benefit Sharing agreements under the Protocol. Research on medicinal plants is used as a case study because it is a domain with many competing stakeholders involving non-commercial and commercial research, as well as national and international commercial markets. We propose a decision-based framework to aid all participants as they negotiate ABS agreements for non-commercial biodiversity research. Our proposed approach promotes transparency and builds trust, reflects the principles in the Convention on Biological Diversity, and respects and protects the interests of biodiversity rich developing countries. This approach is an alternative to often-used adversarial approaches. C1 [Schindel, David E.] Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20560 USA. [Bubela, Tania] Univ Alberta, Sch Publ Hlth, Edmonton, AB, Canada. [Rosenthal, Joshua] Fogarty Int Ctr, Div Epidemiol & Populat Studies, Washington, DC USA. [Castle, David] Univ Victoria, Victoria, BC V8W 2Y2, Canada. [du Plessis, Pierre] CRIAA SA DC, Windhoek, Namibia. [Bye, Robert] Univ Nacl Autonoma Mexico, Inst Biol, Mexico City 04510, DF, Mexico. [PMCW] Mexico City Workshop, Med Plant Barcoding & Nat Hlth Prod Res Moving De, Mexico City, DF, Mexico. RP Schindel, DE (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20560 USA. EM schindeld@si.edu OI Bubela, Tania/0000-0002-0807-2899 NR 24 TC 2 Z9 2 U1 1 U2 6 PU PENSOFT PUBL PI SOFIA PA 12 PROF GEORGI ZLATARSKI ST, SOFIA, 1700, BULGARIA SN 1314-6947 EI 1314-3301 J9 NAT CONSERV-BULGARIA JI Nat. Conserv.-Bulgaria PY 2015 IS 12 BP 43 EP 56 DI 10.3897/natureconservation.12.5412 PG 14 WC Biodiversity Conservation SC Biodiversity & Conservation GA CR5SU UT WOS:000361405100003 ER PT J AU Sharma, D Vergara-Asenjo, G Cunampio, M Cunampio, RB Cunampio, MB Potvin, C AF Sharma, Divya Vergara-Asenjo, Gerardo Cunampio, Mitzy Cunampio, Raquel B. Cunampio, Mara B. Potvin, Catherine TI Genesis of an indigenous social-ecological landscape in eastern Panama SO ECOLOGY AND SOCIETY LA English DT Article DE eastern Panama; deforestation; forest cover; indigenous migration; land-cover mapping; land-use change; land-use decisions; livelihood strategies; local knowledge; reforestation; social-ecological landscape ID LAND-COVER CHANGE; SHIFTING CULTIVATION; TROPICAL DEFORESTATION; USE INTENSIFICATION; ECUADORIAN AMAZON; BIOSPHERE RESERVE; SOUTHERN YUCATAN; SOUTHWEST CHINA; FOREST; LIVELIHOODS AB Knowledge of the interplay between ecological and social influences in the context of land-use decision-making is sparse. To help fill this gap, we conducted participatory land-cover mapping in an indigenous territory of eastern Panama to identify factors that influenced household land-use decisions. The map illustrated a mosaic of land cover dominated by pasture. Primary discourse on influences from 35 semistructured interviews with landowners, women, and youth emphasized economic concerns, such as subsistence, and social-cultural factors, such as reticence to abandon traditional agriculture. Multivariate analysis showed that timing of family settlement helped determine proportion of forest cover, and place of origin helped determine proportion of short fallow for agriculture. Cultural norms and economic opportunities inform gendered perspectives; women perceived internal social-cultural influences and men perceived external and ecological influences on the land. Giving consideration to subsistence, traditional land uses, social organization, and women's perspectives could inform future communal reforestation. C1 [Sharma, Divya; Vergara-Asenjo, Gerardo; Potvin, Catherine] McGill Univ, Dept Biol, Montreal, PQ H3A 2T5, Canada. [Vergara-Asenjo, Gerardo] Inst Forestal Chile, Concepcion, Chile. [Cunampio, Mitzy; Cunampio, Raquel B.; Cunampio, Mara B.] Community Piriati Embera, Panama City, Panama. [Potvin, Catherine] Smithsonian Trop Res Inst, Panama City, Panama. RP Sharma, D (reprint author), McGill Univ, Dept Biol, Montreal, PQ H3A 2T5, Canada. FU Natural Sciences and Engineering Resource Council of Canada; Margaret A. Cargill Foundation; Fonds de recherche du Quebec - Natures et technologies; McGill University; Ford Foundation International Fellowship Program; Global Environmental and Climate Change Centre FX We thank Rodolfo Cunampio for his continued support and guidance throughout the research process, and the community members of Piriati-Embera for their participation and interest. We also thank Ignacia Holmes, Jeanine Rhemtulla, and Ana Spalding for their guidance on methodology and with the manuscript. We acknowledge a Discovery Grant (to C. Potvin) and scholarship (to D. Sharma) from the Natural Sciences and Engineering Resource Council of Canada, the Margaret A. Cargill Foundation project grant (to C. Potvin), a scholarship of the Fonds de recherche du Quebec - Natures et technologies (to D. Sharma), a travel grant from McGill University (to D. Sharma), and fellowships from the Ford Foundation International Fellowship Program and the Global Environmental and Climate Change Centre (to G. Vergara-Asenjo). NR 80 TC 1 Z9 1 U1 3 U2 7 PU RESILIENCE ALLIANCE PI WOLFVILLE PA ACADIA UNIV, BIOLOGY DEPT, WOLFVILLE, NS B0P 1X0, CANADA SN 1708-3087 J9 ECOL SOC JI Ecol. Soc. PY 2015 VL 20 IS 4 AR 37 DI 10.5751/ES-07897-200437 PG 18 WC Ecology; Environmental Studies SC Environmental Sciences & Ecology GA DA2MM UT WOS:000367628900013 ER PT S AU Loss, SR Will, T Marra, P AF Loss, Scott R. Will, Tom Marra, Peter BE Futuyma, DJ TI Direct Mortality of Birds from Anthropogenic Causes SO ANNUAL REVIEW OF ECOLOGY, EVOLUTION, AND SYSTEMATICS, VOL 46 SE Annual Review of Ecology Evolution and Systematics LA English DT Review; Book Chapter DE anthropogenic mortality; avian ecology; conservation biology; incidental take; population ecology ID WIND ENERGY DEVELOPMENT; COMMUNICATION TOWERS; UNITED-STATES; POWER-LINES; FERAL CATS; AVIAN COLLISIONS; RAPTOR ELECTROCUTION; UTILITY STRUCTURES; DECISION-MAKING; INSECTICIDE USE AB Understanding and reversing the widespread population declines of birds require estimating the magnitude of all mortality sources. Numerous anthropogenic mortality sources directly kill birds. Cause-specific annual mortality in the United States varies from billions (cat predation) to hundreds of millions (building and automobile collisions), tens of millions (power line collisions), millions (power line electrocutions, communication tower collisions), and hundreds of thousands (wind turbine collisions). However, great uncertainty exists about the independent and cumulative impacts of this mortality on avian populations. To facilitate this understanding, additional research is needed to estimate mortality for individual bird species and affected populations, to sample mortality throughout the annual cycle to inform full life-cycle population models, and to develop models that clarify the degree to which multiple mortality sources are additive or compensatory. We review sources of direct anthropogenic mortality in relation to the fundamental ecological objective of disentangling how mortality sources affect animal populations. C1 [Loss, Scott R.] Oklahoma State Univ, Dept Nat Resource Ecol & Management, Stillwater, OK 74078 USA. [Will, Tom] US Fish & Wildlife Serv, Div Migratory Birds, Midwest Reg Off, Bloomington, MN 55437 USA. [Marra, Peter] Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Washington, DC 20013 USA. RP Loss, SR (reprint author), Oklahoma State Univ, Dept Nat Resource Ecol & Management, Stillwater, OK 74078 USA. EM scott.loss@okstate.edu; tom_will@fws.gov; marrap@si.edu NR 115 TC 16 Z9 16 U1 21 U2 65 PU ANNUAL REVIEWS PI PALO ALTO PA 4139 EL CAMINO WAY, PO BOX 10139, PALO ALTO, CA 94303-0897 USA SN 1543-592X BN 978-0-8243-1446-0 J9 ANNU REV ECOL EVOL S JI Annu. Rev. Ecol. Evol. Syst. PY 2015 VL 46 BP 99 EP 120 DI 10.1146/annurev-ecolsys-112414-054133 PG 22 WC Ecology; Evolutionary Biology SC Environmental Sciences & Ecology; Evolutionary Biology GA BE0XG UT WOS:000367292700005 ER PT J AU Sakchoowong, W Hasin, S Pachey, N Amornsak, W Bunyavejchewin, S Kongnoo, P Basset, Y AF Sakchoowong, Watana Hasin, Sasitorn Pachey, Nongphanga Amornsak, Weerawan Bunyavejchewin, Sarayudh Kongnoo, Pitoon Basset, Yves TI Influence of leaf litter composition on ant assemblages in a lowland tropical rainforest in Thailand SO ASIAN MYRMECOLOGY LA English DT Article DE ant assemblages; indicator species; leaf litter; microhabitat; southern Thailand; spatial ecology; tropical rainforest ID ARTHROPOD ABUNDANCE; DWELLING ARTHROPODS; SOIL; INVERTEBRATES; DIVERSITY; COMMUNITY; DYNAMICS; BEETLES AB In tropical rainforests, variability in the distribution of soil and litter arthropods is usually explained at regional scales by altitude, soil nutrients, and disturbance regimes. However, the influence of these factors on insect assemblages at the micro-habitat scale has rarely been studied. We investigated whether the species identity of decomposing leaves in tropical forest affected the composition of ant assemblages around them. Ants were extracted from litter below three common tree species, Parashorea stellata (Dipterocarpaceae), Intsia palembanica (Fabaceae) and Shorea gratissima (Dipterocarpaceae) in a 24 ha lowland rainforest plot in southern Thailand. A total of 2,257 individual ants, representing 71 species in 38 genera of 6 subfamilies were collected in the dry and wet seasons during 2010. Ant species richness was never significantly different among litter samples under the crown cover of three tree species. Ant species richness was higher in the wet season than the dry season. Our results demonstrate that ant assemblages are seasonally heterogeneous. Leaf mass and litter mass did not relate to the presence of ant diversity. Soil humidity was the only important factor influencing ant diversity in this study. Future studies should consider the importance of soil moisture related to litter ant diversity. C1 [Sakchoowong, Watana; Pachey, Nongphanga; Bunyavejchewin, Sarayudh] Dept Natl Pk Wildlife & Plant Conservat, Forest & Plant Conservat Res Off, Bangkok 10900, Thailand. [Hasin, Sasitorn] Kasetsart Univ, Dept Forest Biol, Fac Forestry, Bangkok 10900, Thailand. [Hasin, Sasitorn] Kasetsart Univ, Ctr Adv Studies Trop Nat Resources, NRU KU, Bangkok 10900, Thailand. [Amornsak, Weerawan] Kasetsart Univ, Dept Entomol, Fac Agr, Bangkok 10900, Thailand. [Kongnoo, Pitoon] Khao Chong Bot Garden, Ctr Trop Forest Sci, Trang 92170, Thailand. [Basset, Yves] Smithsonian Trop Res Inst, Panama City, Panama. RP Sakchoowong, W (reprint author), Dept Natl Pk Wildlife & Plant Conservat, Forest & Plant Conservat Res Off, 61 Phaholyothin Rd, Bangkok 10900, Thailand. EM wat_sak@yahoo.com RI Basset, Yves/B-6642-2014 FU CTFS; Arnold Arboretum of Harvard University FX We thank CTFS and the Arnold Arboretum of Harvard University for funding the project. We also would like to thank David J. Lohman and Gordon Gordh for comments on earlier drafts of the manuscript. We thank the staff of Khao Chong Forest Insect Ecological Research Laboratory for helping with fieldwork and the Department of National Parks, Wildlife and Plant Conservation for granting the permission to collect the samples for this study project. NR 34 TC 1 Z9 2 U1 4 U2 7 PU UNIV MALAYSIA SABAH PI KOTA KINABALU PA JALAN UMS, 88400, KOTA KINABALU, SABAH 00000, MALAYSIA SN 1985-1944 J9 ASIAN MYRMECOL JI Asian Myrmecol. PY 2015 VL 7 BP 57 EP 72 PG 16 WC Entomology SC Entomology GA CZ8PD UT WOS:000367360700007 ER PT J AU Talamas, EJ Buffington, ML AF Talamas, Elijah J. Buffington, Matthew L. TI Fossil Platygastroidea in the National Museum of Natural History, Smithsonian Institution SO JOURNAL OF HYMENOPTERA RESEARCH LA English DT Article DE Platygastroidea; Platygastrinae; Scelioninae; Telenominae; Sceliotrachelinae; amber; Miocene; Eocene; taxonomy ID HYMENOPTERA; SCELIONIDAE; EVOLUTION; PARASITOIDS; PHYLOGENY; REVISION AB Platygastroid wasps preserved in Dominican amber and oil shale from the Kishenehn formation (Montana, USA) in the National Museum of Natural History are catalogued. Compression fossils in Kishenehn oil shale yield a specimen of Fidiobia, a specimen of Telenominae, and a specimen with a Scelio-type ovipositor system. Twenty-five described genera are documented from Dominican amber, all of which are known from the extant fauna: Allostemma Masner & Huggert, Aradophagus Ashmead, Calliscelio Ashmead, Calotelea Westwood, Duta Nixon, Embidobia Ashmead, Embioctonus Masner, Fidiobia Ashmead, Gryon Haliday, Idris Forster, Inostemma Haliday, Leptacis Forster, Leptoteleia Kieffer, Macroteleia Kieffer, Odontacolus Kieffer, Opisthacantha Ashmead, Parabaeus Kieffer, Paridris Kieffer, Platygaster Latreille, Plaumannion Masner & Johnson, Probaryconus Kieffer, Psilanteris Kieffer, Spiniteleia Masner, Telenomus Haliday, and Triteleia Kieffer. Fourteen of these genera do not have previously published fossil records and are here documented for the first time. Plaumannion fistulosum Talamas, sp. n., and Paridris yumai Talamas, sp. n. are described as new species. A phylogenetic analysis of Paridris including P. yumai is presented. A male specimen belonging to an undescribed scelionine genus is documented and illustrated, but not described, as the best features for circumscribing this taxon are found in the female, and monographic work on this group is currently underway by other workers. Four specimens from Baltic amber, belonging to Leptacis, Platygaster, and Sembilanocera Brues are presented for comparison to extant specimens and inclusions in Dominican amber. C1 [Talamas, Elijah J.; Buffington, Matthew L.] ARS, Systemat Entomol Lab, USDA, NMNH,Smithsonian Inst, Washington, DC 20250 USA. RP Talamas, EJ (reprint author), ARS, Systemat Entomol Lab, USDA, NMNH,Smithsonian Inst, Washington, DC 20250 USA. EM elijah.talamas@ars.usda.gov FU Systematic Entomology Laboratory, USDA-ARS FX We extend our thanks to: Mark Florence, Jonathan Wingerath, Dale Greenwalt, Alan Rulis, Conrad Labandeira and Jorge Santiago-Blay (USNM) for making fossil specimens available; Norman Johnson (The Ohio State University) for taxonomic input and identification of Sembilanocera; Joe Cora (The Ohio State University) for continual database support and creating the IPT; Lubomir Masner (Canadian National Collection of Insects) for taxonomic input; Andrew Austin (University of Adelaide) for commentary on the systematics of Idris and Ceratobaeus; Elizabeth Alvarez, Pei Luo, Ashton Smith, Annika Salzberg, and Samantha Fitzsimmons-Schoenberger for photographic contributions; and Laetitia Plaisance (USNM) for translation. This work was made possible by funding from the Systematic Entomology Laboratory, USDA-ARS. The USDA does not endorse any commercial product mentioned in this research. USDA is an equal opportunity provider and employer. NR 41 TC 2 Z9 2 U1 1 U2 1 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. PY 2015 VL 47 BP 1 EP 52 DI 10.3897/JHR.47.5730 PG 52 WC Entomology SC Entomology GA CZ4WY UT WOS:000367104700001 ER PT J AU Tull, RG Cortes-Rodriguez, MN AF Tull, Renetta G. Cortes-Rodriguez, Maria Nandadevi GP ASEE TI Starting Points for Involving Underrepresented Graduate Students in International Engagement: A Case Study on the Collaborations Between the University of Maryland Baltimore County (UMBC) and Educational Institutions in Latin America SO 2015 ASEE ANNUAL CONFERENCE AND EXPOSITION LA English DT Proceedings Paper CT ASEE International Forum CY JUN 14, 2015 CL Seattle, WA SP ASEE AB Graduate students in engineering and IT do not have many chances to participate in study abroad opportunities, and those who do, may do so as individuals based on their graduate advisor's collaborations. In this globalized world of technological advances, developing international collaborations between scholars within the STEM fields is not only beneficial; it is essential, thus opportunities should not be limited to a select few. The National Academy of Engineering has developed a list of Grand Challenges, and there is growing concern that there won't be an international workforce with enough training to develop solutions for real-world issues. Despite involvement of some graduate students in international research, there remain subsets of graduate students from underrepresented minority (URM) groups who have neither been encouraged nor invited to participate in international projects. The Council of Graduate Schools' 2013 publication, "Graduate Education for Global Career Pathways," included papers that encouraged graduate students to participate in global conferences as means to engage, and serves as the premise for our strategy to broaden participation of URM graduate students in international projects. 1 The Graduate School at UMBC and the National Science Foundation's PROMISE: Maryland's Alliance for Graduate Education and the Professoriate (AGEP) program have started to develop cohorts of students and faculty who travel to international conferences and report on their experiences. Cohort travel models are not unique in undergraduate circles; however, for our group of participants, the model serves as a pathway to broaden the participation of STEM-trained women and minorities in international engagement. The model includes immersing the cohort into a culture through participation in an international conference, presentations at a host university to develop collaborations with faculty and students, scientific excursions, discussion sessions addressing research questions, and plans for building on the short-term experience. This model started in 2012 with a graduate student presentation at the Latin and Caribbean Consortium of Engineering Institutions (LACCEI) conference in Panama. In 2013, participation in LACCEI in Mexico increased to two graduate students, a postdoctoral fellow, and an alumnus who is a member of the faculty at another institution. By 2014, a group of 15 participated in LACCEI in Guayaquil, Ecuador. Plans for 2015 include travel to the Dominican Republic, and affiliations with Tecnologico de Monterrey in Mexico. Given graduate students' 12-month continuous research and laboratory responsibilities, the short-term experience provided a sound introduction. Participants were part of the PROMISE AGEP, Louis Stokes Alliance for Minority Participation Bridges to the Doctorate program, and the UMBC/Puerto Rico ADVANCE Hispanic Women in STEM program. Many of the participants had little to no experience abroad. The 2014 trip included collaborations with the CEDEI - Centro de Estudios Interamericanos in Cuenca, Ecuador for acclimation to the region, graduate student mentoring, and a presentation at the Foro Latinoamericano de Estudiantes sobre Educacion en Ingenieria conference at the Escuela Superior Politecnica del Litoral (ESPOL) for engineering students throughout Ecuador. Students from the U.S. and Latin American universities discussed the academic models of each country, career/life balance, development of cultural competence, and plans to engage in international research collaborations. This paper will present the model and the social science results from questions posed before, during, and after the trip which addressed barriers to entry such as the challenges of family and language, and the rewards associated with international collaborations. C1 [Tull, Renetta G.] Univ Maryland Baltimore Cty, Grad Student Profess Dev & Postdoctoral Affairs, Baltimore, MD 21228 USA. [Cortes-Rodriguez, Maria Nandadevi] Smithsonian Conservat Biol Inst, Ctr Conservat & Evolutionary Genet, Front Royal, VA 22630 USA. RP Tull, RG (reprint author), Univ Maryland Baltimore Cty, Grad Student Profess Dev & Postdoctoral Affairs, Baltimore, MD 21228 USA. NR 6 TC 0 Z9 0 U1 3 U2 7 PU AMER SOC ENGINEERING EDUCATION PI WASHINGTON PA 1818 N STREET, NW SUITE 600, WASHINGTON, DC 20036 USA PY 2015 PG 19 WC Education & Educational Research; Education, Scientific Disciplines; Engineering, Multidisciplinary SC Education & Educational Research; Engineering GA BE0KB UT WOS:000366178800021 ER PT J AU Mendieta-Leiva, G Zotz, G AF Mendieta-Leiva, Glenda Zotz, Gerhard TI A conceptual framework for the analysis of vascular epiphyte assemblages SO PERSPECTIVES IN PLANT ECOLOGY EVOLUTION AND SYSTEMATICS LA English DT Review DE Assemblage; Ecological scales; Host individual; Environmental heterogeneity; Diversity; Vascular epiphytes ID PALM SOCRATEA-EXORRHIZA; HOST TREE UTILIZATION; MONTANE RAIN-FORESTS; LAND-USE INTENSITIES; TROPICAL DRY FOREST; LONG-TERM CHANGES; SPECIES-RICHNESS; POPULATION-DYNAMICS; LOWLAND FOREST; FLORISTIC COMPOSITION AB Despite their ecological importance, particularly in tropical rainforests, vascular epiphytes are among the least studied plant groups. Theoretical knowledge about the composition, structure and dynamics of epiphyte assemblages is strikingly scarce: in contrast to soil-rooted plants for which major insights have been gained in the last decades. These insights cannot be simply transferred to epiphytes, because structurally-dependent vascular epiphytes are fundamentally different in several aspects from non-structurally-dependent plants, as well as from other epiphyte types (e.g. mosses). Apart from the difficulty Of accessing the canopy, we largely attribute the lack of-development in the field to terminological issues and the lack of standardized sampling, both of which stem from the lack of a conceptual framework. We develop such a framework for future studies and illustrate the potential of this suggested approach. Our analysis is based on a review of studies of vascular epiphyte assemblages that have data on abundance, since diversity comprises two aspects: species richness and relative abundance. We found 62 studies of very idiosyncratic character over the last 30 years, of which 18% included a temporal component ranging from 4 months to 8 years. Surprisingly, over 80% of the studies collected data at the tree level, but few analyzed the data at that level (34%) and none has made their data available for meta-analyses. We argue that this represents a problem in the development of the field and we urge researchers to make this wealth of data available. We suggest explicitly using the host individual as the sampling unit when studying vascular epiphyte assemblages. Moreover, the ecological scales (zone, tree and stand scales) i.e. relating to the three-dimensional nature of vascular epiphytes assemblages (VEAs), can be used to scale up or down from the host individual. The importance of scaling, and availability of data at the tree level, was assessed by comparing diversity patterns of vascular epiphytes at the tree and stand scales, which revealed clear and consistently different patterns. More general questions on the diversity patterns of vascular epiphytes could be answered if the wealth of data already collected were made accessible and if future sampling were to be standardized. (C) 2015 Geobotanisches Institut ETH, Stiftung Ruebel. Published by Elsevier GmbH. All rights reserved. C1 [Mendieta-Leiva, Glenda; Zotz, Gerhard] Carl von Ossietzky Univ Oldenburg, Inst Biol & Umweltwissensch, AG Funkt Okol, D-26111 Oldenburg, Germany. [Zotz, Gerhard] Smithsonian Trop Res Inst, Panama City, Panama. RP Mendieta-Leiva, G (reprint author), Carl von Ossietzky Univ Oldenburg, Inst Biol & Umweltwissensch, AG Funkt Okol, Postfach 2503, D-26111 Oldenburg, Germany. EM glendamendieta@gmail.com; gerhard.zotz@uni-oldenburg.de OI Zotz, Gerhard/0000-0002-6823-2268; Mendieta-Leiva, Glenda/0000-0002-0156-4153 FU Deutsche Forschungsgemeinschaft (DFG) [ZO 94/5-1] FX We are thankful to Florian Werner who kindly provided his dataset and for comments on an earlier version of the manuscript. The manuscript profited through valuable comments by Lou Jost and two anonymous reviewers. Funding was provided by Deutsche Forschungsgemeinschaft (DFG ZO 94/5-1). NR 128 TC 4 Z9 5 U1 4 U2 14 PU ELSEVIER GMBH, URBAN & FISCHER VERLAG PI JENA PA OFFICE JENA, P O BOX 100537, 07705 JENA, GERMANY SN 1433-8319 J9 PERSPECT PLANT ECOL JI Perspect. Plant Ecol. Evol. Syst. PY 2015 VL 17 IS 6 BP 510 EP 521 DI 10.1016/j.ppees.2015.09.003 PG 12 WC Plant Sciences; Ecology SC Plant Sciences; Environmental Sciences & Ecology GA CY6RD UT WOS:000366535600009 ER PT S AU Aguilera-Fernandez, J Sadeghpour, HR Schmelcher, P Gonzalez-Ferez, R AF Aguilera-Fernandez, Javier Sadeghpour, H. R. Schmelcher, Peter Gonzalez-Ferez, Rosario BE Diaz, C Rabadan, I Garcia, G Mendez, L Martin, F TI Ultralong-Range Rb-KRb Rydberg Molecules: Selected Aspects of Electronic Structure, Orientation and Alignment SO XXIX INTERNATIONAL CONFERENCE ON PHOTONIC, ELECTRONIC, AND ATOMIC COLLISIONS (ICPEAC2015), PTS 1-12 SE Journal of Physics Conference Series LA English DT Proceedings Paper CT 29th International Conference on Photonic, Electronic, and Atomic Collisions (ICPEAC) CY JUL 22-28, 2015 CL Toledo, SPAIN SP Univ Autonoma Madrid, Consejo Super Investigaciones Cient ID POLAR-MOLECULES; DIMERS AB We investigate the structure and features of an ultralong-range triatomic Rydberg molecule formed by a Rb Rydberg atom and a KRb diatomic molecule. In our numerical description, we perform a realistic treatment of the internal rotational motion of the diatomic molecule, and take into account the Rb(n, l >= 3) Rydberg degenerate manifold and the energetically closest neighboring levels with principal quantum numbers n' > n and orbital quantum number l <= 2. We focus here on the adiabatic electronic potentials evolving from the Rb(n, l >= 3) and Rb(n = 26, l = 2) manifolds. The directional properties of the KRb diatomic molecule within the Rb-KRb triatomic Rydberg molecule are also analyzed in detail. C1 [Aguilera-Fernandez, Javier; Gonzalez-Ferez, Rosario] Univ Granada, Inst Carlos I Fis Tear & Computac, E-18071 Granada, Spain. [Aguilera-Fernandez, Javier; Gonzalez-Ferez, Rosario] Univ Granada, Dept Fis Atom Mol & Nucl, E-18071 Granada, Spain. [Sadeghpour, H. R.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. [Schmelcher, Peter] Hamburg Ctr Ultrafast Imaging, D-22761 Hamburg, Germany. [Schmelcher, Peter] Univ Hamburg, Zentrum Opt Quantentechnol, D-22761 Hamburg, Germany. RP Aguilera-Fernandez, J (reprint author), Univ Granada, Inst Carlos I Fis Tear & Computac, E-18071 Granada, Spain. NR 11 TC 0 Z9 0 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 1742-6588 J9 J PHYS CONF SER PY 2015 VL 635 AR 012023 DI 10.1088/1742-6596/635/1/012023 PG 9 WC Engineering, Electrical & Electronic; Optics; Physics, Multidisciplinary SC Engineering; Optics; Physics GA BE0NP UT WOS:000366407000023 ER PT S AU Bartschat, K Sadeghpour, HR AF Bartschat, Klaus Sadeghpour, H. R. BE Diaz, C Rabadan, I Garcia, G Mendez, L Martin, F TI Hyperfine-changing transitions in He-3 II and other one-electron ions by electron scattering SO XXIX INTERNATIONAL CONFERENCE ON PHOTONIC, ELECTRONIC, AND ATOMIC COLLISIONS (ICPEAC2015), PTS 1-12 SE Journal of Physics Conference Series LA English DT Proceedings Paper CT 29th International Conference on Photonic, Electronic, and Atomic Collisions (ICPEAC) CY JUL 22-28, 2015 CL Toledo, SPAIN SP Univ Autonoma Madrid, Consejo Super Investigaciones Cient AB We present short-range phase shifts and spin-exchange cross sections for elastic electron scattering from selected one-electron ions from He+ to Fe25+. The results are explained in a simple physical picture based on quantum defect theory. C1 [Bartschat, Klaus] Drake Univ, Dept Phys & Astron, Des Moines, IA 50311 USA. [Bartschat, Klaus; Sadeghpour, H. R.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. RP Bartschat, K (reprint author), Drake Univ, Dept Phys & Astron, Des Moines, IA 50311 USA. EM klaus.bartschat@drake.edu; hrs@cfa.harvard.edu NR 6 TC 0 Z9 0 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 1742-6588 J9 J PHYS CONF SER PY 2015 VL 635 AR 052016 DI 10.1088/1742-6596/635/5/052016 PG 1 WC Engineering, Electrical & Electronic; Optics; Physics, Multidisciplinary SC Engineering; Optics; Physics GA BE0NP UT WOS:000366407000267 ER PT S AU DeSalvo, BJ Aman, J Dunning, FB Killian, TC Sadeghpour, HR Yoshida, S Burgdorfer, J AF DeSalvo, B. J. Aman, J. Dunning, F. B. Killian, T. C. Sadeghpour, H. R. Yoshida, S. Burgdoerfer, J. BE Diaz, C Rabadan, I Garcia, G Mendez, L Martin, F TI Production of ultra-long-range Rydberg molecules in a divalent atomic system SO XXIX INTERNATIONAL CONFERENCE ON PHOTONIC, ELECTRONIC, AND ATOMIC COLLISIONS (ICPEAC2015), PTS 1-12 SE Journal of Physics Conference Series LA English DT Proceedings Paper CT 29th International Conference on Photonic, Electronic, and Atomic Collisions (ICPEAC) CY JUL 22-28, 2015 CL Toledo, SPAIN SP Univ Autonoma Madrid, Consejo Super Investigaciones Cient AB Sr-2 Rydberg molecules are created through two-photon excitation in an ultracold strontium gas contained in an optical dipole trap and are detected through atom loss from the trap. First order perturbation theory employing the Fermi pseudopotential and effective s-wave and p-wave scattering lengths is used to evaluate the binding energies of the molecular levels. C1 [DeSalvo, B. J.; Aman, J.; Dunning, F. B.; Killian, T. C.] Rice Univ, Dept Phys & Astron MS61, Houston, TX 77005 USA. [Sadeghpour, H. R.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. [Yoshida, S.; Burgdoerfer, J.] Vienna Univ Technol, Inst Theoret Phys, A-1040 Vienna, Austria. RP DeSalvo, BJ (reprint author), Rice Univ, Dept Phys & Astron MS61, Houston, TX 77005 USA. EM jim.aman@rice.edu NR 2 TC 2 Z9 2 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 1742-6588 J9 J PHYS CONF SER PY 2015 VL 635 AR 092023 DI 10.1088/1742-6596/635/9/092023 PG 1 WC Engineering, Electrical & Electronic; Optics; Physics, Multidisciplinary SC Engineering; Optics; Physics GA BE0NP UT WOS:000366407000459 ER PT S AU Gharaibeh, MF Bizau, JM Cubaynes, D Guilbaud, S Al Shorman, MM Ababneh, IQ Sakho, I Blancard, C McLaughlin, BM AF Gharaibeh, M. F. Bizau, J. M. Cubaynes, D. Guilbaud, S. Al Shorman, M. M. Ababneh, I. Q. Sakho, I. Blancard, C. McLaughlin, B. M. BE Diaz, C Rabadan, I Garcia, G Mendez, L Martin, F TI K-Shell Photoionization of the Oxygen Isonuclear Sequence SO XXIX INTERNATIONAL CONFERENCE ON PHOTONIC, ELECTRONIC, AND ATOMIC COLLISIONS (ICPEAC2015), PTS 1-12 SE Journal of Physics Conference Series LA English DT Proceedings Paper CT 29th International Conference on Photonic, Electronic, and Atomic Collisions (ICPEAC) CY JUL 22-28, 2015 CL Toledo, SPAIN SP Univ Autonoma Madrid, Consejo Super Investigaciones Cient ID XMM-NEWTON AB K-shell photoionization cross-section measurements for the oxygen isonuclear sequence from N-like to Li-like made at the SOLEIL Light Source are compared with SUNC, MCDF and R-matrix calculations. C1 [Gharaibeh, M. F.] Qatar Univ, Dept Math Stat & Phys, Doha, Qatar. [Gharaibeh, M. F.; Ababneh, I. Q.] Jordan Univ Sci & Technol, Dept Phys, Irbid 22110, Jordan. [Bizau, J. M.; Cubaynes, D.; Guilbaud, S.; Al Shorman, M. M.] Univ Paris 11, CNRS UMR 8214, ISMO, F-91405 Orsay, France. [Sakho, I.] Univ Assane Seek Ziguinchor, Dept Phys, UFR Sci & Technol, Ziguinchor, Senegal. [Blancard, C.] CEA DAM DIF, F-91297 Arpajon, France. [McLaughlin, B. M.] Queens Univ Belfast, Sch Math & Phys, Ctr Theoret Atom & Mol Phys CTAMOP, Belfast BT7 1NN, Antrim, North Ireland. [McLaughlin, B. M.] Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys ITAMP, Cambridge, MA 02138 USA. RP Gharaibeh, MF (reprint author), Qatar Univ, Dept Math Stat & Phys, POB 2713, Doha, Qatar. EM mgharaibeh@qu.edu.qa; b.mclaughlin@qub.ac.uk NR 4 TC 0 Z9 0 U1 1 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 1742-6588 J9 J PHYS CONF SER PY 2015 VL 635 AR 092074 DI 10.1088/1742-6596/635/9/092074 PG 1 WC Engineering, Electrical & Electronic; Optics; Physics, Multidisciplinary SC Engineering; Optics; Physics GA BE0NP UT WOS:000366407000502 ER PT S AU Huppert, M Jordan, I Pabst, S Worner, HJ AF Huppert, M. Jordan, I. Pabst, S. Woerner, H. J. BE Diaz, C Rabadan, I Garcia, G Mendez, L Martin, F TI Relativistic photoionization delays and the role of auto-ionizing resonances SO XXIX INTERNATIONAL CONFERENCE ON PHOTONIC, ELECTRONIC, AND ATOMIC COLLISIONS (ICPEAC2015), PTS 1-12 SE Journal of Physics Conference Series LA English DT Proceedings Paper CT 29th International Conference on Photonic, Electronic, and Atomic Collisions (ICPEAC) CY JUL 22-28, 2015 CL Toledo, SPAIN SP Univ Autonoma Madrid, Consejo Super Investigaciones Cient ID PULSES AB We measured the relative ionization delays into the two spin-orbit components of the electronic ground states of Xe+ and Kr+ under the influence of auto-ionizing intermediate and final states. The results are in good agreement with state-of-the-art calculations based on the time-dependent configuration-interaction singles (TDCIS) approach. C1 [Huppert, M.; Jordan, I.; Woerner, H. J.] Swiss Fed Inst Technol, Phys Chem Lab, CH-8093 Zurich, Switzerland. [Pabst, S.] DESY, Ctr Free Elect Laser Sci, D-22607 Hamburg, Germany. [Pabst, S.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. RP Huppert, M (reprint author), Swiss Fed Inst Technol, Phys Chem Lab, Vladimir Prelog Weg 2, CH-8093 Zurich, Switzerland. EM martin.huppert@phys.chem.ethz.ch; hansjakob.woerner@phys.chem.ethz.ch RI Pabst, Stefan/J-6541-2013; Worner, Hans Jakob/B-1802-2013 OI Pabst, Stefan/0000-0003-1134-4629; NR 4 TC 1 Z9 1 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 1742-6588 J9 J PHYS CONF SER PY 2015 VL 635 AR 092135 DI 10.1088/1742-6596/635/9/092135 PG 1 WC Engineering, Electrical & Electronic; Optics; Physics, Multidisciplinary SC Engineering; Optics; Physics GA BE0NP UT WOS:000366407000559 ER PT S AU Pabst, S Worner, HJ AF Pabst, Stefan Woerner, Hans Jakob BE Diaz, C Rabadan, I Garcia, G Mendez, L Martin, F TI Creating coherent hole wave packets with strong-field pulses SO XXIX INTERNATIONAL CONFERENCE ON PHOTONIC, ELECTRONIC, AND ATOMIC COLLISIONS (ICPEAC2015), PTS 1-12 SE Journal of Physics Conference Series LA English DT Proceedings Paper CT 29th International Conference on Photonic, Electronic, and Atomic Collisions (ICPEAC) CY JUL 22-28, 2015 CL Toledo, SPAIN SP Univ Autonoma Madrid, Consejo Super Investigaciones Cient AB A new approach is identified that can generate highly coherent hole wave packets with multi-cycle strong-field pulses and stands in contrast, to the usual idea of making the ionizing pulse as short as possible. "I he effect is demonstrated in atomic xenon with a spin orbit wave packet involving the 5p1, and 5p1 ionic states. Tuning the driving frequency to an even fraction of the hole oscillation frequency ensures the creation of highly coherent holes. C1 [Pabst, Stefan] DESY, Ctr Free Electron Laser Sci, D-22607 Hamburg, Germany. [Pabst, Stefan] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. [Woerner, Hans Jakob] Swiss Fed Inst Technol, Lab Phys Chem, CH-8093 Zurich, Switzerland. RP Pabst, S (reprint author), DESY, Ctr Free Electron Laser Sci, Notkestr 85, D-22607 Hamburg, Germany. EM stefan.pabst@cfa.harvard.edu; woerner@phys.chem.ethz.ch RI Pabst, Stefan/J-6541-2013; Worner, Hans Jakob/B-1802-2013 OI Pabst, Stefan/0000-0003-1134-4629; NR 4 TC 0 Z9 0 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 1742-6588 J9 J PHYS CONF SER PY 2015 VL 635 AR 092096 DI 10.1088/1742-6596/635/9/092096 PG 1 WC Engineering, Electrical & Electronic; Optics; Physics, Multidisciplinary SC Engineering; Optics; Physics GA BE0NP UT WOS:000366407000524 ER PT S AU Eisenstein, DJ AF Eisenstein, Daniel J. BE Kearns, E Feldman, G TI Neutrinos and Large-Scale Structure SO XXVI INTERNATIONAL CONFERENCE ON NEUTRINO PHYSICS AND ASTROPHYSICS (NEUTRINO 2014) SE AIP Conference Proceedings LA English DT Proceedings Paper CT 26th International Conference on Neutrino Physics and Astrophysics (Neutrino) CY JAN 02-07, 2014 CL Boston Univ, Boston, MA SP M I T, Harward Univ, Tufts Univ HO Boston Univ DE cosmology: observations; cosmological parameters; large scale structure of Universe ID OSCILLATION SPECTROSCOPIC SURVEY; BARYON ACOUSTIC-OSCILLATIONS; PROBE WMAP OBSERVATIONS; SDSS-III; COSMOLOGICAL PARAMETERS; GALAXY CLUSTERS; HUBBLE CONSTANT; UNIVERSE; CALIBRATION; MASS AB I review the use of cosmological large-scale structure to measure properties of neutrinos and other relic populations of light relativistic particles. With experiments to measure the anisotropies of the cosmic microwave anisotropies and the clustering of matter at low redshift, we now have securely measured a relativistic background with density appropriate to the cosmic neutrino background. Our limits on the mass of the neutrino continue to shrink. Experiments coming in the next decade will greatly improve the available precision on searches for the energy density of novel relativistic backgrounds and the mass of neutrinos. C1 [Eisenstein, Daniel J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Eisenstein, DJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 20, Cambridge, MA 02138 USA. NR 31 TC 0 Z9 0 U1 0 U2 1 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 978-0-7354-1313-9 J9 AIP CONF PROC PY 2015 VL 1666 AR UNSP 140002 DI 10.1063/1.4915586 PG 6 WC Astronomy & Astrophysics; Physics, Applied SC Astronomy & Astrophysics; Physics GA BE0NM UT WOS:000366402800038 ER PT J AU Greenwalt, DE Rose, TR Siljestrom, SM Goreva, YS Constenius, KN Wingerath, JG AF Greenwalt, Dale E. Rose, Tim R. Siljestrom, Sandra M. Goreva, Yulia S. Constenius, Kurt N. Wingerath, Jonathan G. TI Taphonomy of the fossil insects of the middle Eocene Kishenehn Formation SO ACTA PALAEONTOLOGICA POLONICA LA English DT Article DE Diptera; Hemiptera; taphonomy; varve; depositional environment; Eocene; USA; Montana ID EXCEPTIONAL PRESERVATION; LACUSTRINE ENVIRONMENTS; FLORISSANT FORMATION; LAKE ENVIRONMENTS; BRITISH-COLUMBIA; MICROBIAL MATS; CRUDE OILS; TOF-SIMS; OLIGOCENE; COLORADO AB The lacustrine oil shales of the Coal Creek Member of the Kishenehn Formation in northwestern Montana comprise a relatively unstudied middle Eocene fossil insect locality. Herein, we detail the stratigraphic position of the fossiliferous unit, describe the insect fauna of the Coal Creek locality and document its bias towards very small but remarkably preserved insects. In addition, the depositional environment is examined and the mineral constituents of the laminations that comprise the varves of the Kishenehn oil shale are defined. Fifteen orders of insects have been recorded with the majority of all insects identified as aquatic with the families Chironomidae (Diptera) and Corixidae (Hemiptera) dominant. The presence of small aquatic insects, many of which are immature, the intact nature of >90% of the fossil insects and the presence of Daphnia ephippia, all indicate that the depositional environment was the shallow margin of a large freshwater lake. The fossil insects occur within fossilized microbial mat layers that comprise the bedding planes of the oil shale. Unlike the fossiliferous shales of the Florissant and Okanagan Highlands, the mats are not a product of diatomaceous algae nor are diatom frustules a component of the sediments or the varve structure. Instead, the varves are composed of very fine eolian siliciclastic silt grains overlaid with non-diatomaceous, possibly cyanobacteria-derived microbial mats which contain distinct traces of polyaromatic hydrocarbons. A distinct third layer composed of essentially pure calcite is present in the shale of some exposures and is presumably derived from the seasonal warming-induced precipitation of carbonate from the lake's waters. The Coal Creek locality presents a unique opportunity to study both very small middle Eocene insects not often preserved as compression fossils in most Konservat-Lagerstatte and the processes that led to their preservation. C1 [Greenwalt, Dale E.; Wingerath, Jonathan G.] Smithsonian Inst, NMNH, Dept Paleobiol, Washington, DC 20013 USA. [Rose, Tim R.; Goreva, Yulia S.] Smithsonian Inst, NMNH, Dept Mineral Sci, Washington, DC 20013 USA. [Siljestrom, Sandra M.] SP Tech Res Inst Sweden, Dept Chem Mat & Surfaces, S-50111 Boras, Sweden. [Siljestrom, Sandra M.] Smithsonian Inst, NMNH, Dept Mineral Sci, Washington, DC 20013 USA. [Constenius, Kurt N.] Carnegie Museum Nat Hist, Sect Vertebrate Fossils, Tucson, AZ 85704 USA. RP Greenwalt, DE (reprint author), Smithsonian Inst, NMNH, Dept Paleobiol, POB 37012 MRC 121, Washington, DC 20013 USA. EM GreenwaltD@si.edu; roset@si.edu; SiljestromS@si.edu; gorevay@si.edu; kconstenius@comcast.net; wingerat@si.edu FU Deep Carbon Observatory; Geophysical Laboratory (Carnegie Institution of Washington, Washington, D.C., USA); Swedish National Space Board [121/11] FX We thank Conrad Labandeira and Finnegan Marsh (both National Museum of Natural History, Washington, D.C., USA) for administrative support and Sonja Wedmann (Senckenberg Forschungsinstitut und Naturmuseum, Messel, Germany) and an anonymous reviewer for suggestions that significantly improved the manuscript. We thank Kay Van Damme (University of Ghent, Belgium) for the identification of fossil ephippia to the subgenus Daphnia (Ctenodaphnia) and Marie Huizing, editor of Rocks & Minerals (Philadelphia, USA), for granting permission to reproduce the photograph in Fig. 13C. This work was funded in part by the Deep Carbon Observatory (Andrew Steele, PI) and the Postdoctoral fellowship program of the Geophysical Laboratory (Carnegie Institution of Washington, Washington, D.C., USA) and the Swedish National Space Board (Contract No. 121/11). This is contribution number 284 of the Evolution of Terrestrial Ecosystems Consortium of the USNM. NR 107 TC 7 Z9 7 U1 4 U2 11 PU INST PALEOBIOLOGII PAN PI WARSAW PA UL TWARDA 51/55, 00-818 WARSAW, POLAND SN 0567-7920 EI 1732-2421 J9 ACTA PALAEONTOL POL JI Acta Palaeontol. Pol. PY 2015 VL 60 IS 4 BP 931 EP 947 DI 10.4202/app.00071.2014 PG 17 WC Paleontology SC Paleontology GA CY1AQ UT WOS:000366138900015 ER PT J AU Xu, JW Martin, RV van Donkelaar, A Kim, J Choi, M Zhang, Q Geng, G Liu, Y Ma, Z Huang, L Wang, Y Chen, H Che, H Lin, P Lin, N AF Xu, J. -W. Martin, R. V. van Donkelaar, A. Kim, J. Choi, M. Zhang, Q. Geng, G. Liu, Y. Ma, Z. Huang, L. Wang, Y. Chen, H. Che, H. Lin, P. Lin, N. TI Estimating ground-level PM2.5 in eastern China using aerosol optical depth determined from the GOCI satellite instrument SO ATMOSPHERIC CHEMISTRY AND PHYSICS LA English DT Article ID FINE PARTICULATE MATTER; UNITED-STATES; AMMONIUM AEROSOLS; AIR-QUALITY; MODEL; EMISSIONS; AERONET; HYDROCARBONS; SIMULATION; REGRESSION AB We determine and interpret fine particulate matter (PM2.5) concentrations in eastern China for January to December 2013 at a horizontal resolution of 6 km from aerosol optical depth (AOD) retrieved from the Korean geostationary ocean color imager (GOCI) satellite instrument. We implement a set of filters to minimize cloud contamination in GOCI AOD. Evaluation of filtered GOCI AOD with AOD from the Aerosol Robotic Network (AERONET) indicates significant agreement with mean fractional bias (MFB) in Beijing of 6.7 % and northern Taiwan of -1.2 %. We use a global chemical transport model (GEOS-Chem) to relate the total column AOD to the near-surface PM2.5. The simulated PM2.5 / AOD ratio exhibits high consistency with ground-based measurements in Taiwan (MFB = -0.52 %) and Beijing (MFB = 8.0 %). We evaluate the satellite-derived PM2.5 versus the ground-level PM2.5 in 2013 measured by the China Environmental Monitoring Center. Significant agreement is found between GOCI-derived PM2.5 and in situ observations in both annual averages (r(2) = 0.66, N = 494) and monthly averages (relative RMSE = 18.3 %), indicating GOCI provides valuable data for air quality studies in Northeast Asia. The GEOS-Chem simulated chemical composition of GOCI-derived PM2.5 reveals that secondary inorganics (SO42-, NO3-, NH4+) and organic matter are the most significant components. Biofuel emissions in northern China for heating increase the concentration of organic matter in winter. The population-weighted GOCI-derived PM2.5 over eastern China for 2013 is 53.8 mu g m(-3), with 400 million residents in regions that exceed the Interim Target-1 of the World Health Organization. C1 [Xu, J. -W.; Martin, R. V.; van Donkelaar, A.] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS, Canada. [Martin, R. V.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kim, J.; Choi, M.] Yonsei Univ, Dept Phys & Atmospher Sci, Seoul 120749, South Korea. [Zhang, Q.; Geng, G.; Wang, Y.] Tsinghua Univ, Ctr Earth Syst Sci, Inst Global Change Studies, Key Lab Earth Syst Modeling,Minist Educ, Beijing 100084, Peoples R China. [Zhang, Q.; Geng, G.] Tsinghua Univ, Sch Environm, State Key Joint Lab Environm Simulat & Pollut Con, Beijing 100084, Peoples R China. [Liu, Y.; Ma, Z.] Emory Univ, Rollins Sch Publ Hlth, Dept Environm Hlth, Atlanta, GA 30322 USA. [Ma, Z.; Huang, L.] Nanjing Univ, Sch Environm, State Key Lab Pollut Control & Resource Reuse, Nanjing 210008, Jiangsu, Peoples R China. [Wang, Y.] Texas A&M Univ, Dept Marine Biol, Galveston, TX 77553 USA. [Wang, Y.] Texas A&M Univ, Dept Atmospher Sci, College Stn, TX USA. [Chen, H.] Chinese Acad Sci, Inst Atmospher Phys, Beijing, Peoples R China. [Che, H.] Chinese Acad Meteorol Sci, Inst Atmospher Composit, Beijing, Peoples R China. [Lin, P.] Natl Taiwan Univ, Dept Atmospher Sci, Taipei 10764, Taiwan. [Lin, N.] Natl Cent Univ, Dept Atmospher Sci, Taoyan, Taiwan. RP Xu, JW (reprint author), Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS, Canada. EM junwei.xu@.dal.ca RI Zhang, Qiang/D-9034-2012; Martin, Randall/C-1205-2014; Chem, GEOS/C-5595-2014; Wang, Yuxuan/C-6902-2014; che, Huizheng/B-1354-2014 OI Martin, Randall/0000-0003-2632-8402; Wang, Yuxuan/0000-0002-1649-6974; che, Huizheng/0000-0002-9458-3387 FU NSERC (Natural Sciences and Engineering Research Council of Canada); Izaak Walton Killiam Memorial Scholarship FX We are grateful to the GOCI, AERONET, CEMC, TEPA and SPARTAN for providing available data used in this study. Funding for this work was provided by NSERC (Natural Sciences and Engineering Research Council of Canada) and by an Izaak Walton Killiam Memorial Scholarship for J.-W. Xu. Computational facilities are partially provided by ACEnet, the regional high performance computing consortium for universities in Atlantic Canada. NR 65 TC 6 Z9 6 U1 13 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 2015 VL 15 IS 22 BP 13133 EP 13144 DI 10.5194/acp-15-13133-2015 PG 12 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CX8TM UT WOS:000365977100026 ER PT J AU Avva, J Kovac, JM Miki, C Saltzberg, D Vieregg, AG AF Avva, Jessica Kovac, John M. Miki, Christian Saltzberg, David Vieregg, Abigail G. TI An in situ measurement of the radio-frequency attenuation in ice at Summit Station, Greenland SO JOURNAL OF GLACIOLOGY LA English DT Article DE radio-echo sounding ID COSMIC NEUTRINOS; DETECTOR; TEMPERATURE; PERFORMANCE; ANTARCTICA; EMISSION; CHARGE; SHELF; ARRAY AB We report an in situ measurement of the electric field attenuation length L-alpha at radio frequencies for the bulk ice at Summit Station, Greenland, made by broadcasting radio-frequency signals vertically through the ice and measuring the relative power in the return ground bounce signal. We find the depth-averaged field attenuation length to be < L-alpha > = 947(-85)(+92) m at 75 MHz. While this measurement has clear radioglaciological applications, the radio clarity of the ice also has implications for the detection of ultra-high energy (UHE) astrophysical particles via their radio emission in dielectric media such as ice. Assuming a reliable extrapolation to higher frequencies, the measured attenuation length at Summit Station is comparable to previously measured radio-frequency attenuation lengths at candidate particle detector sites around the world, and strengthens the case for Summit Station as a promising northern site for UHE neutrino detection. C1 [Avva, Jessica; Vieregg, Abigail G.] Univ Chicago, Dept Phys, Kavli Inst Cosmol Phys, Enrico Fermi Inst, Chicago, IL 60637 USA. [Kovac, John M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Miki, Christian] Univ Hawaii Manoa, Dept Phys, Honolulu, HI 96822 USA. [Saltzberg, David] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA USA. RP Vieregg, AG (reprint author), Univ Chicago, Dept Phys, Kavli Inst Cosmol Phys, Enrico Fermi Inst, Chicago, IL 60637 USA. EM avieregg@kicp.uchicago.edu FU NSF's Office of Polar Programs [PLR-1103553]; US Department of Energy; Kavli Institute for Cosmological Physics at the University of Chicago; University of California, Los Angeles; Illinois Space Grant Consortium FX We thank CH2M HILL Polar Services and the US National Science Foundation (NSF) for dedicated, knowledgeable and extremely helpful logistical support. We particularly thank K. Gorham. We are deeply indebted to those who dedicate their careers to help make our science possible in such remote environments. This work was supported by the NSF's Office of Polar Programs (PLR-1103553), the US Department of Energy, the Kavli Institute for Cosmological Physics at the University of Chicago, the University of California, Los Angeles, and the Illinois Space Grant Consortium. We thank P. Gorham for support of C. Miki. We also thank Warner Brothers Studios, who lent us parkas for the expedition. NR 22 TC 3 Z9 3 U1 0 U2 3 PU INT GLACIOL SOC PI CAMBRIDGE PA LENSFIELD RD, CAMBRIDGE CB2 1ER, ENGLAND SN 0022-1430 EI 1727-5652 J9 J GLACIOL JI J. Glaciol. PY 2015 VL 61 IS 229 BP 1005 EP 1011 DI 10.3189/2015JoG15J057 PG 7 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA CY3YE UT WOS:000366345000015 ER PT S AU Allured, R Ben-Ami, S Cotroneo, V Marquez, V McMuldroch, S Reid, PB Schwartz, DA Trolier-McKinstry, S Vikhlinin, AA Wallace, ML AF Allured, Ryan Ben-Ami, Sagi Cotroneo, Vincenzo Marquez, Vanessa McMuldroch, Stuart Reid, Paul B. Schwartz, Daniel A. Trolier-McKinstry, Susan Vikhlinin, Alexey A. Wallace, Margeaux L. BE ODell, ST Pareschi, G TI Improved Control and Characterization of Adjustable X-ray Optics SO OPTICS FOR EUV, X-RAY, AND GAMMA-RAY ASTRONOMY VII SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on Optics for EUV, X-Ray, and Gamma-Ray Astronomy VII as part of the SPIE Optics + Photonics International Symposium on Optical Engineering + Applications CY AUG 10-13, 2015 CL San Diego, CA SP SPIE AB We report on improvements in our efforts to control and characterize piezoelectrically adjustable, thin glass optics. In the past, an optical profilometer and a Shack-Hartmann wavefront sensor have been used to measure influence functions for a flat adjustable mirror. An electronics system has since been developed to control > 100 actuator cells and has been used in a full calibration of a high-yield flat adjustable mirror. The calibrated influence functions have been used to induce a pre-determined figure change to the mirror, representing our first attempt at figure control of a full mirror. Furthermore, we have adapted our metrology systems for cylindrical optics, allowing characterization of Wolter-type mirrors. We plan to use this metrology to perform the first piezoelectric figure correction of a cylindrical mirror over the next year. C1 [Allured, Ryan; Ben-Ami, Sagi; Cotroneo, Vincenzo; Marquez, Vanessa; McMuldroch, Stuart; Reid, Paul B.; Schwartz, Daniel A.; Vikhlinin, Alexey A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Trolier-McKinstry, Susan; Wallace, Margeaux L.] Penn State Univ, University Pk, PA 16802 USA. RP Allured, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Trolier-McKinstry, Susan/0000-0002-7267-9281 NR 18 TC 5 Z9 5 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 978-1-62841-769-2 J9 PROC SPIE PY 2015 VL 9603 AR 96031M DI 10.1117/12.2186411 PG 10 WC Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BE0HF UT WOS:000366020700053 ER PT S AU Allured, R Donovan, BD DeRoo, CT Marlowe, HR McEntaffer, RL Tutt, JH Cheimets, PN Hertz, E Smith, RK Burwitz, V Hartner, G Menz, B AF Allured, Ryan Donovan, Benjamin D. DeRoo, Casey T. Marlowe, Hannah R. McEntaffer, Randall L. Tutt, James H. Cheimets, Peter N. Hertz, Edward Smith, Randall K. Burwitz, Vadim Hartner, Gisela Menz, Benedikt BE ODell, ST Pareschi, G TI Optical and X-ray Alignment Approaches for Off-Plane Reflection Gratings SO OPTICS FOR EUV, X-RAY, AND GAMMA-RAY ASTRONOMY VII SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on Optics for EUV, X-Ray, and Gamma-Ray Astronomy VII as part of the SPIE Optics + Photonics International Symposium on Optical Engineering + Applications CY AUG 10-13, 2015 CL San Diego, CA SP SPIE ID SPECTROSCOPY AB Off-plane reflection gratings offer the potential for high-resolution, high-throughput X-ray spectroscopy on future missions. Typically, the gratings are placed in the path of a converging beam from an X-ray telescope. In the off-plane reflection grating case, these gratings must be co-aligned such that their diffracted spectra overlap at the focal plane. Misalignments degrade spectral resolution and effective area. In-situ X-ray alignment of a pair of off-plane reflection gratings in the path of a silicon pore optics module has been performed at the MPE PANTER beamline in Germany. However, in-situ X-ray alignment may not be feasible when assembling all of the gratings required for a satellite mission. In that event, optical methods must be developed to achieve spectral alignment. We have developed an alignment approach utilizing a Shack-Hartmann wavefront sensor and diffraction of an ultraviolet laser. We are fabricating the necessary hardware, and will be taking a prototype grating module to an X-ray beamline for performance testing following assembly and alignment. C1 [Allured, Ryan; Cheimets, Peter N.; Hertz, Edward; Smith, Randall K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Donovan, Benjamin D.; DeRoo, Casey T.; Marlowe, Hannah R.; McEntaffer, Randall L.; Tutt, James H.] Univ Iowa, Iowa City, IA USA. [Burwitz, Vadim; Hartner, Gisela; Menz, Benedikt] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. RP Allured, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 18 TC 2 Z9 2 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 978-1-62841-769-2 J9 PROC SPIE PY 2015 VL 9603 AR 960315 DI 10.1117/12.2186412 PG 11 WC Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BE0HF UT WOS:000366020700037 ER PT S AU Ames, A Bruni, R Cotroneo, V Johnson-Wilke, R Kester, T Reid, P Romaine, S Tolier-McKinstry, S Wilke, RHT AF Ames, A. Bruni, R. Cotroneo, V. Johnson-Wilke, R. Kester, T. Reid, P. Romaine, S. Tolier-McKinstry, S. Wilke, R. H. T. BE ODell, ST Pareschi, G TI Using Iridium films to compensate for piezo-electric materials processing stresses in adjustable X-ray optics SO OPTICS FOR EUV, X-RAY, AND GAMMA-RAY ASTRONOMY VII SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on Optics for EUV, X-Ray, and Gamma-Ray Astronomy VII as part of the SPIE Optics + Photonics International Symposium on Optical Engineering + Applications CY AUG 10-13, 2015 CL San Diego, CA SP SPIE DE X-ray optics; adjustable X-ray optics; piezo-electric materials; film stress AB Adjustable X-ray optics represent a potential enabling technology for simultaneously achieving large effective area and high angular resolution for future X-ray Astronomy missions. The adjustable optics employ a bimorph mirror composed of a thin (1.5 um) film of piezoelectric material deposited on the back of a 0.4 mm thick conical mirror segment. The application of localized electric fields in the piezoelectric material, normal to the mirror surface, result in localized deformations in mirror shape. Thus, mirror fabrication and mounting induced figure errors can be corrected, without the need for a massive reaction structure. With this approach, though, film stresses in the piezoelectric layer, resulting from deposition, crystallization, and differences in coefficient of thermal expansion, can distort the mirror. The large relative thickness of the piezoelectric material compared to the glass means that even 100MPa stresses can result in significant distortions. We have examined compensating for the piezoelectric processing related distortions by the deposition of controlled stress chromium/iridium films on the front surface of the mirror. We describe our experiments with tuning the product of the chromium/iridium film stress and film thickness to balance that resulting from the piezoelectric layer. We also evaluated the repeatability of this deposition process, and the robustness of the iridium coating. C1 [Ames, A.; Bruni, R.; Cotroneo, V.; Reid, P.; Romaine, S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Johnson-Wilke, R.; Tolier-McKinstry, S.; Wilke, R. H. T.] Penn State Univ, Mat Res Inst, University Pk, PA 16802 USA. [Kester, T.] NASA Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Ames, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM sromaine@cfa.harvard.edu NR 11 TC 0 Z9 0 U1 1 U2 1 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 978-1-62841-769-2 J9 PROC SPIE PY 2015 VL 9603 AR 96031I DI 10.1117/12.2191404 PG 8 WC Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BE0HF UT WOS:000366020700050 ER PT S AU Donovan, BD Hertz, E Marquez, V McMuldroch, S Reid, PB Allured, R AF Donovan, Benjamin D. Hertz, Edward Marquez, Vanessa McMuldroch, Stuart Reid, Paul B. Allured, Ryan BE ODell, ST Pareschi, G TI Coarse Alignment of Thin-Shell, Segmented Mirrors for Wolter-I Telescopes SO OPTICS FOR EUV, X-RAY, AND GAMMA-RAY ASTRONOMY VII SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on Optics for EUV, X-Ray, and Gamma-Ray Astronomy VII as part of the SPIE Optics + Photonics International Symposium on Optical Engineering + Applications CY AUG 10-13, 2015 CL San Diego, CA SP SPIE AB The alignment of thin-shell, segmented mirrors for Wolter-I telescopes frequently involves the use of a Hartmann test. In order to get optical throughput in the Hartmann test, the mirrors must first be coarsely aligned to one another and to the metrology system. In the past, the coarse alignment of these mirrors at the Smithsonian Astrophysical Observatory has largely relied upon component machine tolerances and contact measurements with a coordinate measurement machine (CMM). This process takes time and does not produce reliable nor repeatable results. Thus, methods were developed to allow for the quick and reliable coarse alignment of thin-shell, segmented mirrors at their final locations in the mirror assembly. We present the coarse alignment system developed at the Smithsonian Astrophysical Observatory and its use in the alignment of thin-shell, segmented mirrors for the adjustable X-ray optics program. C1 [Donovan, Benjamin D.] Univ Iowa, Iowa City, IA 52242 USA. [Hertz, Edward; Marquez, Vanessa; McMuldroch, Stuart; Reid, Paul B.; Allured, Ryan] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Donovan, BD (reprint author), Univ Iowa, Iowa City, IA 52242 USA. EM benjamin-donovan@uiowa.edu NR 8 TC 0 Z9 0 U1 2 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 978-1-62841-769-2 J9 PROC SPIE PY 2015 VL 9603 AR 960313 DI 10.1117/12.2186631 PG 10 WC Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BE0HF UT WOS:000366020700035 ER PT S AU Eisenhower, MJ Cohen, LM Feinberg, LD Matthews, GW Nissen, JA Park, SC Peabody, HL AF Eisenhower, Michael J. Cohen, Lester M. Feinberg, Lee D. Matthews, Gary W. Nissen, Joel A. Park, Sang C. Peabody, Hume L. BE MacEwen, HA Breckinridge, JB TI ATLAST ULE Mirror Segment Performance Analytical Predictions Based on Thermally Induced Distortions SO UV/OPTICAL/IR SPACE TELESCOPES AND INSTRUMENTS: INNOVATIVE TECHNOLOGIES AND CONCEPTS VII SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on UV/Optical/IR Space Telescopes and Instruments - Innovative Technologies and Concepts VII CY AUG 09-10, 2015 CL San Diego, CA SP SPIE DE ATLAST; thermal distortion; ULE; UV; HST; JWST AB The Advanced Technology Large-Aperture Space Telescope (ATLAST) is a concept for a 9.2 m aperture space-borne observatory operating across the UV/Optical/NIR spectra. The primary mirror for ATLAST is a segmented architecture with pico-meter class wavefront stability. Due to its extraordinarily low coefficient of thermal expansion, a leading candidate for the primary mirror substrate is Corning's ULE (R) titania-silicate glass. The ATLAST ULE (R) mirror substrates will be maintained at 'room temperature' during on orbit flight operations minimizing the need for compensation of mirror deformation between the manufacturing temperature and the operational temperatures. This approach requires active thermal management to maintain operational temperature while on orbit. Furthermore, the active thermal control must be sufficiently stable to prevent time-varying thermally induced distortions in the mirror substrates. This paper describes a conceptual thermal management system for the ATLAST 9.2 m segmented mirror architecture that maintains the wavefront stability to less than 10 pico-meters/10 minutes RMS. Thermal and finite-element models, analytical techniques, accuracies involved in solving the mirror figure errors, and early findings from the thermal and thermal-distortion analyses are presented. C1 [Eisenhower, Michael J.; Cohen, Lester M.; Park, Sang C.] Smithsonian Astrophys Observ, Cambridge, MA 02140 USA. [Feinberg, Lee D.; Peabody, Hume L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 02771 USA. [Matthews, Gary W.] Harris Corp, Rochester, NY 14606 USA. [Nissen, Joel A.] NASA, Jet Prop Lab, Pasadena, CA 91011 USA. RP Eisenhower, MJ (reprint author), Smithsonian Astrophys Observ, Cambridge, MA 02140 USA. NR 2 TC 2 Z9 2 U1 0 U2 1 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 978-1-62841-768-5 J9 PROC SPIE PY 2015 VL 9602 AR 96020A DI 10.1117/12.2188008 PG 18 WC Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BE0HC UT WOS:000366018200008 ER PT S AU Gaskin, JA Weisskopf, MC Vikhlinin, A Tananbaum, HD Bandler, SR Bautz, MW Burrows, DN Falcone, AD Harrison, FA Heilmann, RK Heinz, S Hopkins, RC Kilbourne, CA Kouveliotou, C Kraft, RP Kravtsov, AV McEntaffer, RL Natarajan, P O'Dell, SL Petre, R Prieskorn, ZR Ptak, AF Ramsey, BD Reid, PB Schnell, AR Schwartz, DA Townsley, LK AF Gaskin, Jessica A. Weisskopf, Martin C. Vikhlinin, Alexey Tananbaum, Harvey D. Bandler, Simon R. Bautz, Marshall W. Burrows, David N. Falcone, Abraham D. Harrison, Fiona A. Heilmann, Ralf K. Heinz, Sebastian Hopkins, Randall C. Kilbourne, Caroline A. Kouveliotou, Chryssa Kraft, Ralph P. Kravtsov, Andrey V. McEntaffer, Randall L. Natarajan, Priyamvada O'Dell, Stephen L. Petre, Robert Prieskorn, Zachary R. Ptak, Andrew F. Ramsey, Brian D. Reid, Paul B. Schnell, Andrew R. Schwartz, Daniel A. Townsley, Leisa K. BE Siegmund, OHW TI The X-ray Surveyor Mission: A Concept Study SO UV, X-RAY, AND GAMMA-RAY SPACE INSTRUMENTATION FOR ASTRONOMY XIX SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on UV, X-Ray, and Gamma-Ray Space Instrumentation for Astronomy XIX CY AUG 09-10, 2015 CL San Diego, CA SP SPIE DE X-ray Astronomy; X-ray optics; X-ray gratings; X-ray detectors ID SPECTROSCOPY AB NASA's Chandra X-ray Observatory continues to provide an unparalleled means for exploring the high-energy universe. With its half-arcsecond angular resolution, Chandra studies have deepened our understanding of galaxy clusters, active galactic nuclei, galaxies, supernova remnants, neutron stars, black holes, and solar system objects. As we look beyond Chandra, it is clear that comparable or even better angular resolution with greatly increased photon throughput is essential to address ever more demanding science questions-such as the formation and growth of black hole seeds at very high redshifts; the emergence of the first galaxy groups; and details of feedback over a large range of scales from galaxies to galaxy clusters. Recently, we initiated a concept study for such a mission, dubbed X-ray Surveyor. The X-ray Surveyor strawman payload is comprised of a high-resolution mirror assembly and an instrument set, which may include an X-ray microcalorimeter, a high-definition imager, and a dispersive grating spectrometer and its readout. The mirror assembly will consist of highly nested, thin, grazing-incidence mirrors, for which a number of technical approaches are currently under development-including adjustable X-ray optics, differential deposition, and new polishing techniques applied to a variety of substrates. This study benefits from previous studies of large missions carried out over the past two decades and, in most areas, points to mission requirements no more stringent than those of Chandra. C1 [Gaskin, Jessica A.; Weisskopf, Martin C.; Hopkins, Randall C.; O'Dell, Stephen L.; Schnell, Andrew R.] NASA, MSFC, Huntsville, AL 35805 USA. [Vikhlinin, Alexey; Tananbaum, Harvey D.; Kraft, Ralph P.; Reid, Paul B.; Schwartz, Daniel A.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Bandler, Simon R.; Kilbourne, Caroline A.; Petre, Robert; Ptak, Andrew F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Bautz, Marshall W.; Heilmann, Ralf K.] MIT, Cambridge, MA 02139 USA. [Burrows, David N.; Falcone, Abraham D.; Prieskorn, Zachary R.; Townsley, Leisa K.] Penn State Univ, University Pk, PA 16802 USA. [Harrison, Fiona A.] CALTECH, Pasadena, CA 91125 USA. [Heinz, Sebastian] Univ Wisconsin, Madison, WI 53706 USA. [Kouveliotou, Chryssa] George Washington Univ, Washington, DC 20052 USA. [Kravtsov, Andrey V.] Univ Chicago, Chicago, IL 60637 USA. [McEntaffer, Randall L.] Univ Iowa, Iowa City, IA 52242 USA. [Natarajan, Priyamvada] Yale Univ, New Haven, CT 06520 USA. RP Gaskin, JA (reprint author), NASA, MSFC, ZP12,320 Sparkman Dr, Huntsville, AL 35805 USA. EM jessica.gaskin@nasa.gov RI Heilmann, Ralf/D-4680-2009 NR 43 TC 10 Z9 10 U1 0 U2 4 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 978-1-62841-767-8 J9 PROC SPIE PY 2015 VL 9601 AR 96010J DI 10.1117/12.2190837 PG 14 WC Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BE0HA UT WOS:000366016700013 ER PT S AU O'Dell, SL Swartz, DA Tice, NW Plucinsky, PP Grant, CE Marshall, HL Vikhlinin, AA Tennant, AF Dahmer, MT AF O'Dell, Stephen L. Swartz, Douglas A. Tice, Neil W. Plucinsky, Paul P. Grant, Catherine E. Marshall, Herman L. Vikhlinin, Alexey A. Tennant, Allyn F. Dahmer, Matthew T. BE Siegmund, OHW TI Modeling contamination migration on the Chandra X-ray Observatory - III SO UV, X-RAY, AND GAMMA-RAY SPACE INSTRUMENTATION FOR ASTRONOMY XIX SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on UV, X-Ray, and Gamma-Ray Space Instrumentation for Astronomy XIX CY AUG 09-10, 2015 CL San Diego, CA SP SPIE DE X-ray astronomy; CCDs; contamination; modeling and simulation; spacecraft operations ID ACIS INSTRUMENT; PERFORMANCE AB During its first 16 years of operation, the cold (about - 60 degrees C) optical blocking filter of the Advanced CCD Imaging Spectrometer (ACIS), aboard the Chandra X-ray Observatory, has accumulated a growing layer of molecular contamination that attenuates low-energy x rays. Over the past few years, the accumulation rate, spatial distribution, and composition have changed. This evolution has motivated further analysis of contamination migration within and near the ACIS cavity, in part to evaluate potential bake-out scenarios intended to reduce the level of contamination. C1 [O'Dell, Stephen L.; Tennant, Allyn F.] NASA, Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Swartz, Douglas A.] Univ Space Res Assoc, Huntsville, AL 35812 USA. [Tice, Neil W.; Grant, Catherine E.; Marshall, Herman L.] MIT, Cambridge, MA 02139 USA. [Plucinsky, Paul P.; Vikhlinin, Alexey A.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Dahmer, Matthew T.] Northrop Grumman, Cambridge, MA 02138 USA. RP O'Dell, SL (reprint author), NASA, Marshall Space Flight Ctr, MSFC ZP12, Huntsville, AL 35812 USA. EM stephen.l.odell@nasa.gov NR 15 TC 1 Z9 1 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 978-1-62841-767-8 J9 PROC SPIE PY 2015 VL 9601 AR 960107 DI 10.1117/12.2188396 PG 13 WC Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BE0HA UT WOS:000366016700005 ER PT S AU Schwadron, NA Lee, MA Gorby, M Lugaz, N Spence, HE Desai, M Torok, T Downs, C Linker, J Lionello, R Mikic, Z Riley, P Giacalone, J Jokipii, JR Kota, J Kozarev, K AF Schwadron, N. A. Lee, M. A. Gorby, M. Lugaz, N. Spence, H. E. Desai, M. Toeroek, T. Downs, C. Linker, J. Lionello, R. Mikic, Z. Riley, P. Giacalone, J. Jokipii, J. R. Kota, J. Kozarev, K. BE Zank, GP TI Broken Power-law Distributions from Low Coronal Compression Regions or Shocks SO 14TH ANNUAL INTERNATIONAL ASTROPHYSICS CONFERENCE: LINEAR AND NONLINEAR PARTICLE ENERGIZATION THROUGHOUT THE HELIOSPHERE AND BEYOND SE Journal of Physics Conference Series LA English DT Proceedings Paper CT 14th Annual International Astrophysics Conference CY APR 19-24, 2015 CL Tampa, FL ID HYDROMAGNETIC WAVE EXCITATION; FINITE-WIDTH MAGNETOTAIL; PARTICLE-ACCELERATION; SOLAR-WIND; ENERGETIC PARTICLES; TERMINATION SHOCK; ION-ACCELERATION; SPECTRAL BREAKS; MASS EJECTION; COSMIC-RAYS AB Coronal Mass Ejection (CME) expansion regions low in the corona (< 2 - 3 R-s) are highly efficient for the acceleration of energetic particles. Because the acceleration occurs over a finite spatial region, there is a regime where particles diffuse away and escape from the acceleration sites, leading to the formation of broken power-law distributions. This paper highlights recent results indicating that CME expansion and acceleration in the low corona may cause rapid particle acceleration and create large solar energetic particle events with broken power-law distributions. C1 [Schwadron, N. A.; Lee, M. A.; Gorby, M.; Lugaz, N.; Spence, H. E.] Univ New Hampshire, Durham, NC 03824 USA. [Desai, M.] Southwest Res Inst, San Antonio, TX 78228 USA. [Toeroek, T.; Downs, C.; Linker, J.; Lionello, R.; Mikic, Z.; Riley, P.] Predict Sci Inc, San Diego, CA 92121 USA. [Giacalone, J.; Jokipii, J. R.; Kota, J.] Univ Arizona, Tucson, AZ 85721 USA. [Kozarev, K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Schwadron, NA (reprint author), Univ New Hampshire, Durham, NC 03824 USA. EM n.schwadron@unh.edu RI Lugaz, Noe/C-1284-2008; OI Lugaz, Noe/0000-0002-1890-6156; Riley, Pete/0000-0002-1859-456X NR 40 TC 1 Z9 1 U1 1 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 1742-6588 J9 J PHYS CONF SER PY 2015 VL 642 AR 012025 DI 10.1088/1742-6596/642/1/012025 PG 13 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA BD9OJ UT WOS:000364992000025 ER PT J AU Rosenfeld, CE Martinez, CE AF Rosenfeld, Carla E. Martinez, Carmen E. TI Dissolution of mixed amorphous-crystalline Cd-containing Fe coprecipitates in the presence of common organic ligands SO ENVIRONMENTAL CHEMISTRY LA English DT Article ID ZINC SPECIATION; SOLID-SOLUTIONS; IRON-OXIDES; CADMIUM; SOLUBILITY; GOETHITE; FERRITES; TRANSFORMATION; RHIZOSPHERE; TEMPERATURE AB Environmental context Common soil minerals, which often contain trace metals in contaminated environments, are thought to limit metal-related risks in the environment. We studied the stability of these contaminated minerals and found that the presence of plant-derived organic compounds can alter contaminant availability in such environments. Understanding how soluble organics may change trace metal availability helps to predict risk and potentially remediate such environments more efficiently. Abstract Trace metals are common impurities in Fe oxides in soils and can be liberated by organic compounds in the soil. Impurities can also alter and potentially destabilise mineral structures by increasing amorphous or nanocrystalline components. Two Fe oxides found in smelter-contaminated soils, goethite (-FeOOH) and franklinite (ZnFe2O4), were synthesised as coprecipitates with Cd and subjected to dissolution using oxalic acid, citric acid, cysteine and histidine. Substantial quantities of amorphous- (10-60% of total) and surface-associated Cd (5-70% of total) were present in all coprecipitates. Histidine and oxalic acid consistently enhanced, while cysteine inhibited, Cd release from all coprecipitated minerals. Mixed amorphous-crystalline mineral aggregations are common in natural soils, and must be further studied to understand their role in contaminant availability. In addition, Fe oxides, often considered sinks for toxic metals, may be less effective at reducing contaminant mobility and bioavailability in biologically active soils. C1 [Rosenfeld, Carla E.; Martinez, Carmen E.] Penn State Univ, Dept Ecosyst Sci & Management, University Pk, PA 16802 USA. RP Rosenfeld, CE (reprint author), Smithsonian Inst, Dept Mineral Sci, POB 37012,MRC 119, Washington, DC 20013 USA. EM rosenfeldc@si.edu FU Department of Crop and Soil Sciences at Pennsylvania State University (PSU); National Science Foundation GK-12 graduate fellowship [0947962]; PSU Center for Environmental Chemistry and Geochemistry (CECG) summer fellowship FX This research was supported by the Department of Crop and Soil Sciences at Pennsylvania State University (PSU) and by a National Science Foundation GK-12 graduate fellowship (Award# 0947962). Portions of this research were also funded by a PSU Center for Environmental Chemistry and Geochemistry (CECG) summer fellowship. The authors are grateful to Nicole Wonderling (Materials Characterization Laboratory) for her assistance with X-ray diffraction and Sridhar Komarneni (Professor of Clay Mineralogy) for his assistance with mineral synthesis. NR 49 TC 0 Z9 0 U1 3 U2 6 PU CSIRO PUBLISHING PI CLAYTON PA UNIPARK, BLDG 1, LEVEL 1, 195 WELLINGTON RD, LOCKED BAG 10, CLAYTON, VIC 3168, AUSTRALIA SN 1448-2517 EI 1449-8979 J9 ENVIRON CHEM JI Environ. Chem. PY 2015 VL 12 IS 6 BP 739 EP 747 DI 10.1071/EN14223 PG 9 WC Chemistry, Analytical; Environmental Sciences SC Chemistry; Environmental Sciences & Ecology GA CX2IJ UT WOS:000365520100011 ER PT J AU Gregoric, M Blackledge, TA Agnarsson, I Kuntner, M AF Gregoric, Matjaz Blackledge, Todd A. Agnarsson, Ingi Kuntner, Matjaz TI A molecular phylogeny of bark spiders reveals new species from Africa and Madagascar (Araneae: Araneidae: Caerostris) SO JOURNAL OF ARACHNOLOGY LA English DT Article DE Biomaterial; spider silk; web gigantism; sexual size dimorphism; emasculation ID DNA BARCODES; ORB WEBS; ADAPTIVE RADIATION; SEXUAL SELECTION; MALE ADAPTATION; THERAPHOSIDAE; EVOLUTION; SIZE; MYGALOMORPHAE; APHONOPELMA AB Bark spiders (genus Caerostris Thorell 1868) are important models in biomaterial research due to the remarkable biomechanical properties of the silk of C. darwini Kuntner & Agnarsson 2010 and its gigantic web. They also exhibit female gigantism and are promising candidates for coevolutionary research on sexual dimorphism. However, Caerostris spiders are taxonomically understudied and the lack of a phylogeny impedes evolutionary research. Using a combination of one mitochondrial and one nuclear marker, we provide the first species-level phylogeny of Caerostris including half of its species diversity but dense terminal sampling focusing on new lineages. Our phylogenetic and morphological results provide the evidence for six previously undescribed species: C. almae n. sp., C. bojani n. sp., C. pero n. sp. and C. wallacei n. sp., all from Madagascar, C. linnaeus n. sp. from Mozambique and C. tinamaze n. sp. from the Republic of South Africa. C1 [Gregoric, Matjaz; Kuntner, Matjaz] Slovenian Acad Sci & Arts, Inst Biol, Ctr Sci Res, SI-1001 Ljubljana, Slovenia. [Gregoric, Matjaz; Blackledge, Todd A.] Univ Akron, Dept Biol, Integrated Biosci Program, Akron, OH 44325 USA. [Agnarsson, Ingi] Univ Vermont, Dept Biol, Burlington, VT USA. [Agnarsson, Ingi; Kuntner, Matjaz] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20560 USA. [Kuntner, Matjaz] Hubei Univ, Coll Life Sci, Ctr Behav Ecol & Evolut, Wuhan, Hubei, Peoples R China. RP Gregoric, M (reprint author), Slovenian Acad Sci & Arts, Inst Biol, Ctr Sci Res, Novi Trg 2,POB 306, SI-1001 Ljubljana, Slovenia. EM matjaz.gregoric@gmail.com FU Slovenian Research Agency [P1-0236, J1-2063]; United States National Science Foundation [IOS-0745379]; National Geographic Society [8655-09] FX We thank Ren-Chung Cheng, Shakira G. Qinones Lebron, Heine C. Kiesbuy, Tjasa Lokovsek, Laura May-Collado, Yadira Ortiz and Joel Duff for their laboratory and logistic help. We thank Jonathan Coddington (USNM), Jason Dunlop (ZMB), Charles Griswold (CAS), Peter Jager, Rudy Jocque, Daiqin Li, Wenjin Gan, Liu Shengjie, Honore Rabarison, Sahondra Lalao Rahanitriniaina, and MICET and ICTE crews for museum loans, fresh material and help in the field. We thank Jason Bond and an anonymous reviewer for useful comments. This contribution was funded by the Slovenian Research Agency (grants P1-0236, J1-2063), the United States National Science Foundation (IOS-0745379) and the National Geographic Society (grant 8655-09). NR 61 TC 3 Z9 3 U1 7 U2 13 PU AMER ARACHNOLOGICAL SOC PI COLLEGE PARK PA UNIV MARYLAND, DEPT ENTOMOLOGY, 4112 PLANT SCIENCES BLDG, COLLEGE PARK, MD 20742-4454 USA SN 0161-8202 EI 1937-2396 J9 J ARACHNOL JI J. Arachnol. PY 2015 VL 43 IS 3 BP 293 EP 312 PG 20 WC Entomology SC Entomology GA CX2WS UT WOS:000365558100002 ER PT J AU Eberhard, WG Barrantes, G AF Eberhard, William G. Barrantes, Gilbert TI Cues guiding uloborid construction behavior support orb web monophyly SO JOURNAL OF ARACHNOLOGY LA English DT Article DE Behavioral traits; phylogeny; orb web construction ID SPIDERS ARANEAE; WEAVING SPIDERS; LEUCAUGE-MARIANA; SINGLE ORIGIN; PHYLOGENY; TETRAGNATHIDAE; EVOLUTION; ARANEIDAE; PREY; THERIDIIDAE AB Behavior can provide useful traits for testing phylogenetic hypotheses, and some details of orb web construction behavior have been especially useful in characterizing higher-level groups in spiders. The cues used to guide construction behavior and behavioral responses to these cues hold similar promise, but have never been used in phylogenetic studies. Here we use several techniques to test the hypothesis that orb webs in the two major branches of orb-weaving araneomorph spiders (Araneoidea and Deinopoidea) are monophyletic, using both the cues that guide orb construction and the spiders' responses to these cues. If orb webs evolved only once, the expectation is that these traits should be similar in members of both evolutionary lines. This prediction was supported: species in the two groups use several of the same cues, and respond to them in similar ways. These cues include two identical reference stimuli for positioning sticky spiral lines; supplies of silk available in their glands that affect the positioning of sticky spiral loops; and at least one stimulus related to the size of the available space for the orb, which is used to trigger similar modifications of seven independent orb design traits. Neither group used tension-related cues to guide sticky spiral placement. These comparisons reinforce previous conclusions supporting orb web monophyly that were derived from morphological, molecular, and behavioral traits. C1 [Eberhard, William G.] Univ Costa Rica, Smithsonian Trop Res Inst, Rodrigo Facio Brenes, Costa Rica. [Eberhard, William G.; Barrantes, Gilbert] Univ Costa Rica, Escuela Biol, Rodrigo Facio Brenes, Costa Rica. RP Eberhard, WG (reprint author), Univ Costa Rica, Smithsonian Trop Res Inst, Ciudad Univ, Rodrigo Facio Brenes, Costa Rica. EM william.eberhard@gmail.com FU Smithsonian Tropical Research Institute; Vicerectoria de Investigacion of the Universidad de Costa Rica FX We thank Ingi Agnarsson, an anonymous reviewer, and Matjaz Kuntner for useful comments, Robert Suter for considerate handling of the manuscript, and the Smithsonian Tropical Research Institute and the Vicerectoria de Investigacion of the Universidad de Costa Rica for financial support. NR 61 TC 0 Z9 0 U1 5 U2 7 PU AMER ARACHNOLOGICAL SOC PI COLLEGE PARK PA UNIV MARYLAND, DEPT ENTOMOLOGY, 4112 PLANT SCIENCES BLDG, COLLEGE PARK, MD 20742-4454 USA SN 0161-8202 EI 1937-2396 J9 J ARACHNOL JI J. Arachnol. PY 2015 VL 43 IS 3 BP 371 EP 387 PG 17 WC Entomology SC Entomology GA CX2WS UT WOS:000365558100008 ER PT J AU Eberhard, WG AF Eberhard, William G. TI How Micrathena duodecimspinosa (Araneae: Araneidae) uses the elasticity of her dragline to hide her egg sac SO JOURNAL OF ARACHNOLOGY LA English DT Article DE Camouflage; oviposition; orb weaver ID PREDATORS AB A female Micrathena duodecimspinosa (O. P. Cambridge, 1890) used the elasticity of her long dragline to repeatedly jerk her newly constructed egg sac up and down as she lowered it into the leaf litter below. Jerking may reduce the chances that the sac will be entangled in vegetation before it reaches the leaf litter or help insert it deeper into the litter, where it is visually camouflaged. C1 [Eberhard, William G.] Univ Costa Rica, Escuela Biol, Smithsonian Trop Res Inst, Rodrigo Facio Brenes, Costa Rica. RP Eberhard, WG (reprint author), Univ Costa Rica, Escuela Biol, Smithsonian Trop Res Inst, Ciudad Univ, Rodrigo Facio Brenes, Costa Rica. EM william.eberhard@gmail.com NR 6 TC 0 Z9 0 U1 2 U2 3 PU AMER ARACHNOLOGICAL SOC PI COLLEGE PARK PA UNIV MARYLAND, DEPT ENTOMOLOGY, 4112 PLANT SCIENCES BLDG, COLLEGE PARK, MD 20742-4454 USA SN 0161-8202 EI 1937-2396 J9 J ARACHNOL JI J. Arachnol. PY 2015 VL 43 IS 3 BP 417 EP 418 PG 2 WC Entomology SC Entomology GA CX2WS UT WOS:000365558100014 ER PT J AU Greenwalt, DE Wingerath, JG Evenhuis, NL AF Greenwalt, Dale E. Wingerath, Jonathan G. Evenhuis, Neal L. TI Two new and disparate fossil bee flies (Bombyliidae: Anthracinae) from the Americas and reassessment of Anthrax dentoni Lewis, 1969 SO PALAEONTOLOGIA ELECTRONICA LA English DT Article DE Bombyliidae; Anthrax; Dominican amber; Kishenehn Formation; new species; new genus ID DIPTERA; CLASSIFICATION AB In this study, two new species of anthracine bee flies are described and one previously described species is reassessed. Anthrax succini Greenwalt and Evenhuis sp. nov. is the first of the very speciose genus Anthrax and only the second bombyliid to be described from Dominican amber. The previously described Anthrax dentoni Lewis, 1969 was re-examined and reassigned to Anthracinae incertae sedis due to lack of morphological detail required for generic assignment. Eoanomala melas Greenwalt and Evenhuis gen. and sp. nov. is described from the Middle Eocene oil shales of the Kishenehn Formation. Eoanomala melas contains a number of character states that are not found together in any extant genera and, although it may fit within the tribe Villini, it does not appear to be closely related to the extant constituents of that clade. C1 [Greenwalt, Dale E.; Wingerath, Jonathan G.] Smithsonian Inst, Natl Museum Nat Hist MRC 121, Dept Paleobiol, Washington, DC 20013 USA. [Evenhuis, Neal L.] Bernice P Bishop Museum, Dept Nat Sci, Honolulu, HI 96817 USA. RP Greenwalt, DE (reprint author), Smithsonian Inst, Natl Museum Nat Hist MRC 121, Dept Paleobiol, 10th & Constitut Ave NW, Washington, DC 20013 USA. EM GreenwaltD@si.edu; WINGERAT@si.edu; neale@bishopmuseum.org NR 25 TC 0 Z9 0 U1 0 U2 2 PU COQUINA PRESS PI AMHERST PA C/O WHITEY HAGADORN, EXECUTIVE EDITOR, AMHERST COLLEGE, DEPT GEOLOGY, AMHERST, MA 01002 USA SN 1935-3952 EI 1094-8074 J9 PALAEONTOL ELECTRON JI Palaeontol. electron. PY 2015 VL 18 IS 3 AR 51A PG 10 WC Paleontology SC Paleontology GA CX0QE UT WOS:000365400900007 ER PT B AU Olson, KA van der Ree, R AF Olson, Kirk A. van der Ree, Rodney BE VanderRee, R Smith, DJ Grilo, C TI RAILWAYS, ROADS AND FENCES ACROSS KAZAKHSTAN AND MONGOLIA THREATEN THE SURVIVAL OF WIDE-RANGING WILDLIFE SO HANDBOOK OF ROAD ECOLOGY LA English DT Article; Book Chapter ID MIGRATION AB The temperate grasslands of Central Asia are habitat for a number of wide-ranging and endangered species such as Mongolian gazelle. saiga antelope, black-tailed gazelle and Asiatic wild ass. These species' habitat covers hundreds of thousands of square kilometres of largely ecologically intact grassland. Unless carefully planned and managed, the development of railways, highways and fences will be the catalyst for population decline and loss of important wild natural resources. 58.1 The temperate grasslands of Kazakhstan and Mongolia are the largest in the world and are critically important to the survival of Mongolian gazelle. Asiatic wild ass and saiga antelope. 58.2 Kazakhstan and Mongolia are rapidly expanding their overland transportation network to support increased transcontinental trade and resource extraction. 58.3 Railways, highways and fences prevent access to important seasonal resources for various species and cause the decline of wildlife populations. 58.4 Future roads and railways must avoid further fragmentation. existing roads and railways should be modified to restore wildlife movements, and fences should be modified or removed to increase connectivity. 58.5 GPS tracking of long-distance migratory species that identifies preferred movement paths and existing barriers to movement is essential to properly plan infrastructure projects. Achieving a balance between healthy ecosystems and economic development is a significant and critical challenge for developing nations such as Kazakhstan and Mongolia. Experience from other regions has led to an established hierarchy of measures to meet this challenge - avoid, minimise, mitigate and offset. Kazakhstan and Mongolia should adopt these approaches now to ensure that the imminent massive expansion of their road and railway networks has a minimal effect on biodiversity and may even result in a positive effect. C1 [Olson, Kirk A.] Natl Zool Pk, Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA. [van der Ree, Rodney] Royal Bot Gardens Melbourne, Australian Res Ctr Urban Ecol, Melbourne, Vic, Australia. [van der Ree, Rodney] Univ Melbourne, Sch Biosci, Melbourne, Vic, Australia. RP Olson, KA (reprint author), Natl Zool Pk, Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA. NR 14 TC 0 Z9 0 U1 2 U2 5 PU JOHN WILEY & SONS LTD PI CHICHESTER PA THE ATRIUM, SOUTHERN GATE, CHICHESTER PO19 8SQ, WEST SUSSEX, ENGLAND BN 978-1-118-56817-0; 978-1-118-56818-7 PY 2015 BP 472 EP 478 D2 10.1002/9781118568170 PG 7 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA BD7CR UT WOS:000362893600060 ER PT S AU Temkin, I Eldredge, N AF Temkin, Ilya Eldredge, Niles BE Serrelli, E Gontier, N TI Networks and Hierarchies: Approaching Complexity in Evolutionary Theory SO MACROEVOLUTION: EXPLANATION, INTERPRETATION AND EVIDENCE SE Interdisciplinary Evolution Research LA English DT Article; Book Chapter DE Causality; Complexity; Disparity; Diversity; Emergence; Patterns; Trends ID SMALL-WORLD NETWORKS; PROTEIN-INTERACTION NETWORKS; FOOD-WEB STRUCTURE; DROSOPHILA-MELANOGASTER; BIOLOGICAL NETWORKS; SPECIES SELECTION; GENETICAL EVOLUTION; METABOLIC NETWORKS; GENE NETWORKS; RANDOM CLADES AB This expansion of the hierarchy theory of evolution provides a new perspective in which biological phenomena are conceptualized. In this work, we (1) attempt to revise the ontology of levels of biological organization and clarify the relationship between the economic and genealogical hierarchies; (2) explore the implications of network theory for evolutionary dynamics in a hierarchical context; and (3) elucidate evolutionary causality by disentangling abiotic drivers from proximal evolutionary processes (the origin and sorting of variation) and their integration across hierarchies. We suggest that a pervasive pattern of stability in living systems across scale results from the architecture of nature's economy itself-biological systems consisting of hierarchically nested, complex networks are extremely robust to extrinsic perturbations. We further argue that instances of evolution are episodic and rapid; they are transient between equilibrial states that ensue when network stability is compromised by sufficiently strong disturbances affecting biological entities at multiple levels of organization. We also claim that environmental abiotic factors are ultimately responsible for these perturbations that, when filtered through the economic hierarchy, shape the patterns of diversity and disparity of life as we know it. C1 [Temkin, Ilya] No Virginia Community Coll, Dept Biol, Annandale, VA 22003 USA. [Temkin, Ilya] Smithsonian Inst, Smithsonian Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. [Eldredge, Niles] Amer Museum Nat Hist, Div Paleontol, New York, NY 10024 USA. RP Temkin, I (reprint author), No Virginia Community Coll, Dept Biol, Annandale, VA 22003 USA. EM TemkinI@si.edu NR 257 TC 2 Z9 2 U1 1 U2 1 PU SPRINGER INT PUBLISHING AG PI CHAM PA GEWERBESTRASSE 11, CHAM, CH-6330, SWITZERLAND SN 2199-3068 BN 978-3-319-15045-1; 978-3-319-15044-4 J9 INTERDISC EVOL RES PY 2015 VL 2 BP 183 EP 226 DI 10.1007/978-3-319-15045-1_6 D2 10.1007/978-3-319-15045-1 PG 44 WC Evolutionary Biology SC Evolutionary Biology GA BD9RW UT WOS:000365174200007 ER PT J AU Breedy, O Guzman, HM AF Breedy, Odalisca Guzman, Hector M. TI A revision of the genus Muricea Lamouroux, 1821 (Anthozoa, Octocorallia) in the eastern Pacific. Part I: Eumuricea Verrill, 1869 revisited SO ZOOKEYS LA English DT Article DE Alcyonacea; Astrogorgia; Cnidaria; eastern Pacific; Eumuricea; Muricea; Leptogorgia; plexaurid gorgonian; soft corals; Swiftia; taxonomy ID COELENTERATA; GORGONIIDAE; PLEXAURIDAE; CNIDARIA AB Muricea is an amphi-American genus. Verrill proposed dividing the species from the Pacific Ocean into three genera and established the genus Eumuricea for five eastern Pacific species with tubular calyces. Eumuricea is basically characterized by colonies with elongate, cylindrical calyces with truncate margins and star-like opercula, and the occurrence of unilateral spinous spindles. According to these characteristics, Eumuricea does not show enough difference from Muricea to be treated as a separate genus. Original type material of Eumuricea was morphologically analysed and illustrated using optical and scanning electron microscopy. We conclude that the eastern Pacific species should be placed in the genus Muricea and form a group characterised by tubular calyces that comprises four species at present, M. acervata, M. hispida, M. squarrosa, and M. tubigera and a dubious species M. horrida. Lectotypes were designated for M. squarrosa and M. hispida to establish their taxonomic status. The genus Eumuricea has also been misunderstood by former authors who erroneously assigned species to it. For these species we propose new combinations: Swiftia pusilla, Astrogorgia splendens and A. ramosa. C1 [Breedy, Odalisca] Univ Costa Rica, Ctr Invest Ciencias Mar & Limnol, Ctr Invest Estruct Microscop, San Jose, Costa Rica. [Breedy, Odalisca; Guzman, Hector M.] Smithsonian Trop Res Inst, Panama City, Panama. RP Breedy, O (reprint author), Univ Costa Rica, Ctr Invest Ciencias Mar & Limnol, Ctr Invest Estruct Microscop, POB 11501-2060, San Jose, Costa Rica. EM odaliscab@gmail.com FU Smithsonian Tropical Research Institute; Vicerrectoria de Investigacion, Universidad de Costa Rica [808-A9-072] FX Our appreciation to Leen van Ofwegen (Naturalis Biodiversity Center, Leiden, The Netherlands), Stephen Cairns (USNM) and the anonymous reviewers for critical comments and suggestions that improved our manuscript. We acknowledge the following people and institutions for their generosity in making available the specimens and information used in this study: YPM: Eric Lazo-Wasem and Lourdes Rojas; MCZ: Adam Baldinger; MNHUK: Andrew Cabrinovic and Tracy Heath; USNM: Stephen Cairns; IMARPE: Miguel Romero; UPCH: Yuri Hooker; INN: Fernando Rivera and Priscilla Martinez; CRBMco: Katherine Mejia; and UNIANDES-BIOMMAR: Juan Armando Sanchez for allowing the examination of the octocoral collections. We thank Peter Stiewe and Helma Roggenbuck (ZMH) for information about collections; Alexander Rodriguez (UCR) for the composition of the plates; Ingo Wehrtmann (UCR) for helping with the German translation; Eleazar Ruiz (CIMAR), Carlos Guevara (STRI) and Minor Lara and Maria Marta Chavarria (Area de Conservacion Guanacaste, Costa Rica), for helping in the fieldwork. Thanks to the governments of Costa Rica and Panama for allowing visits and collections in their national parks and reserves. This project was partially sponsored by the Smithsonian Tropical Research Institute and the Vicerrectoria de Investigacion, Universidad de Costa Rica, projet 808-A9-072. NR 56 TC 4 Z9 4 U1 0 U2 5 PU PENSOFT PUBL PI SOFIA PA 12 PROF GEORGI ZLATARSKI ST, SOFIA, 1700, BULGARIA SN 1313-2989 EI 1313-2970 J9 ZOOKEYS JI ZooKeys PY 2015 IS 537 BP 1 EP 32 DI 10.3897/zookeys.537.6025 PG 32 WC Zoology SC Zoology GA CW4CW UT WOS:000364939900001 PM 26798234 ER PT J AU Hewson, W Barkley, MP Abad, GG Bosch, H Kurosu, T Spurr, R Tilstra, LG AF Hewson, W. Barkley, M. P. Abad, G. Gonzalez Boesch, H. Kurosu, T. Spurr, R. Tilstra, L. G. TI Development and characterisation of a state-of-the-art GOME-2 formaldehyde air-mass factor algorithm SO ATMOSPHERIC MEASUREMENT TECHNIQUES LA English DT Article ID OZONE MONITORING INSTRUMENT; SURFACE REFLECTANCE ANISOTROPY; TROPOSPHERIC NITROGEN-DIOXIDE; ABSORPTION CROSS-SECTIONS; BAND CLOUD RETRIEVAL; NO2 COLUMN RETRIEVAL; ISOPRENE EMISSIONS; TEMPERATURE-DEPENDENCE; SATELLITE-OBSERVATIONS; ORGANIC NITRATES AB Space-borne observations of formaldehyde (HCHO) are frequently used to derive surface emissions of isoprene, an important biogenic volatile organic compound. The conversion of retrieved HCHO slant column concentrations from satellite line-of-sight measurements to vertical columns is determined through application of an air mass factor (AMF), accounting for instrument viewing geometry, radiative transfer, and vertical profile of the absorber in the atmosphere. This step in the trace gas retrieval is subject to large errors. This work presents the AMF algorithm in use at the University of Leicester (UoL), which introduces scene-specific variables into a per-observation full radiative transfer AMF calculation, including increasing spatial resolution of key environmental parameter databases, input variable area weighting, instrument-specific scattering weight calculation, and inclusion of an ozone vertical profile climatology. Application of these updates to HCHO slant columns from the GOME-2 instrument is shown to typically adjust the AMF by +/- 20 %, compared to a reference algorithm without these advanced parameterisations. On average the GOME-2 AMFs increase by 4 %, with over 70% of locations having an AMF of 0-20% larger than originally, largely resulting from the use of the latest GOME-2 reflectance product. Furthermore, the new UoL algorithm also incorporates a full radiative transfer error calculation for each scene to help characterise AMF uncertainties. Global median AMF errors are typically 50-60 %, and are driven by uncertainties in the HCHO profile shape and its vertical distribution relative to clouds and aerosols. If uncertainty on the a priori HCHO profile is relatively small (< 10 %) then the median AMF total error decreases to about 30-40 %. C1 [Hewson, W.; Barkley, M. P.; Boesch, H.] Univ Leicester, Dept Phys & Astron, EOS Grp, Leicester LE1 7RH, Leics, England. [Abad, G. Gonzalez] Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA. [Kurosu, T.] NASA, Jet Prop Lab, Pasadena, CA USA. [Spurr, R.] RT Solut Inc, Cambridge, MA USA. [Tilstra, L. G.] Royal Netherlands Meteorol Inst KNMI, De Bilt, Netherlands. RP Barkley, MP (reprint author), Univ Leicester, Dept Phys & Astron, EOS Grp, Leicester LE1 7RH, Leics, England. EM mpb14@le.ac.uk RI Boesch, Hartmut/G-6021-2012; OI Gonzalez Abad, Gonzalo/0000-0002-8090-6480 FU UK National Centre for Earth Observation (NCEO); UK Natural Environment Research Council (NERC) [NE/G523763/1, NE/GE013810/2, NE/D001471] FX This work was supported by the UK National Centre for Earth Observation (NCEO) and the UK Natural Environment Research Council (NERC) (grants NE/G523763/1, NE/GE013810/2 and NE/D001471). NR 70 TC 4 Z9 4 U1 0 U2 3 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1867-1381 EI 1867-8548 J9 ATMOS MEAS TECH JI Atmos. Meas. Tech. PY 2015 VL 8 IS 10 BP 4055 EP 4074 DI 10.5194/amt-8-4055-2015 PG 20 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CV5NM UT WOS:000364317600006 ER PT J AU Vollmer, NL Hayek, LAC Heithaus, MR Connor, RC AF Vollmer, Nicole L. Hayek, Lee-Ann C. Heithaus, Michael R. Connor, Richard C. TI Further evidence of a context-specific agonistic signal in bottlenose dolphins: the influence of consortships and group size on the pop vocalization SO BEHAVIOUR LA English DT Article DE agonistic vocalizations; alliances; consortship; pops; Shark Bay; Tursiops aduncus ID TURSIOPS-TRUNCATUS; SOCIAL-STRUCTURE; COMPLEX; ALLIANCE; WHISTLES; SOUNDS; BAND; COMMUNICATION; CETACEANS; EVOLUTION AB Pops are a low-frequency, pulsed vocalization produced by Indo-Pacific bottlenose dolphins (Tursiops cf. aduncus) in Shark Bay, Western Australia and are often heard when male alliances are consorting or 'herding' a female. Previous research indicated that pops produced in this context are an agonistic 'come-hither' demand produced by males and directed at female consorts. Here we examine pop occurrence during focal follows on bottlenose dolphin alliances with and without female consorts present. Regression analysis was conducted to determine if pop numbers were higher in the presence of female consorts, and if variables including group size alone and the interaction between presence/absence of a consortship and group size, influenced pop production. While the presence or absence of a consortship significantly affected the number of pops, average group size had no significant effect on pop production. Our research provides further evidence that the pop vocalization plays an important role in consortships. C1 [Vollmer, Nicole L.] NOAA, Natl Systemat Lab, Natl Marine Fisheries Serv, Smithsonian Inst, Washington, DC 20013 USA. [Hayek, Lee-Ann C.] Smithsonian Inst Math & Stat, MRC 121, Washington, DC 20013 USA. [Heithaus, Michael R.] Florida Int Univ, Dept Biol Sci, North Miami, FL 33181 USA. [Connor, Richard C.] UMASS Dartmouth, Dept Biol, N Dartmouth, MA 02747 USA. RP Vollmer, NL (reprint author), NOAA, Natl Systemat Lab, Natl Marine Fisheries Serv, Smithsonian Inst, POB 37012, Washington, DC 20013 USA. EM vollmern@si.edu FU U.S. NIH fellowship; National Geographic Society FX This study was funded by a U.S. NIH fellowship to RCC and a grant from the National Geographic Society to RCC and MRH. We gratefully acknowledge assistance from the Monkey Mia Dolphin Resort, the Department of Human Biology at the University of Western Australia (notably Richard Holst and Ron Swan), C.A.L.M. (now DEC) and project volunteers. We would also like to sincerely thank Laura Eierman and Paul Leberg for assistance with statistical analyses and two anonymous reviewers for providing helpful comments on this manuscript. NR 52 TC 1 Z9 1 U1 4 U2 7 PU BRILL ACADEMIC PUBLISHERS PI LEIDEN PA PLANTIJNSTRAAT 2, P O BOX 9000, 2300 PA LEIDEN, NETHERLANDS SN 0005-7959 EI 1568-539X J9 BEHAVIOUR JI Behaviour PY 2015 VL 152 IS 14 BP 1979 EP 2000 DI 10.1163/1568539X-00003311 PG 22 WC Behavioral Sciences; Zoology SC Behavioral Sciences; Zoology GA CW2HF UT WOS:000364811500006 ER PT J AU Nottingham, AT Turner, BL Whitaker, J Ostle, NJ McNamara, NP Bardgett, RD Salinas, N Meir, P AF Nottingham, A. T. Turner, B. L. Whitaker, J. Ostle, N. J. McNamara, N. P. Bardgett, R. D. Salinas, N. Meir, P. TI Soil microbial nutrient constraints along a tropical forest elevation gradient: a belowground test of a biogeochemical paradigm SO BIOGEOSCIENCES LA English DT Article ID NET PRIMARY PRODUCTIVITY; N-P STOICHIOMETRY; RAIN-FOREST; PHOSPHORUS LIMITATION; PERUVIAN ANDES; CARBON-CYCLE; COMMUNITY COMPOSITION; POTASSIUM ADDITION; EXTRACTION METHOD; GROWTH-RATE AB Aboveground primary productivity is widely considered to be limited by phosphorus (P) availability in lowland tropical forests and by nitrogen (N) availability in montane tropical forests. However, the extent to which this paradigm applies to belowground processes remains unresolved. We measured indices of soil microbial nutrient status in lowland, sub-montane and montane tropical forests along a natural gradient spanning 3400m in elevation in the Peruvian Andes. With increasing elevation there were marked increases in soil concentrations of total N, total P, and readily exchangeable P, but a decrease in N mineralization determined by in situ resin bags. Microbial carbon (C) and N increased with increasing elevation, but microbial C : N: P ratios were relatively constant, suggesting homeostasis. The activity of hydrolytic enzymes, which are rich in N, decreased with increasing elevation, while the ratio of enzymes involved in the acquisition of N and P increased with increasing elevation, further indicating an increase in the relative demand for N compared to P with increasing elevation. We conclude that soil microorganisms shift investment in nutrient acquisition from P to N between lowland and montane tropical forests, suggesting that different nutrients regulate soil microbial metabolism and the soil carbon balance in these ecosystems. C1 [Nottingham, A. T.; Meir, P.] Univ Edinburgh, Sch Geosci, Edinburgh EH8 9XP, Midlothian, Scotland. [Turner, B. L.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Whitaker, J.; McNamara, N. P.] Lancaster Environm Ctr, Ctr Ecol & Hydrol, Lancaster LA1 4AP, England. [Ostle, N. J.] Univ Lancaster, Lancaster Environm Ctr, Lancaster LA1 4YQ, England. [Bardgett, R. D.] Univ Manchester, Fac Life Sci, Manchester M13 9PT, Lancs, England. [Salinas, N.] Pontificia Univ Catolica Peru, Secc Quim, Lima, Peru. [Salinas, N.] Univ Nacl San Antonio Abad del Cusco, Fac Biol, Cuzco, Peru. [Salinas, N.] Sch Geog & Environm, Environm Change Inst, Oxford OX1 3QY, England. [Meir, P.] Australian Natl Univ, Res Sch Biol, Canberra, ACT 0200, Australia. RP Nottingham, AT (reprint author), Univ Edinburgh, Sch Geosci, Drummond St, Edinburgh EH8 9XP, Midlothian, Scotland. EM anotting@staffmail.ed.ac.uk RI Turner, Benjamin/E-5940-2011; McNamara, Niall/B-4907-2008; Whitaker, Jeanette/A-9266-2013; Ostle, Nicholas/E-4847-2014; Meir, Patrick/J-8344-2012; OI Turner, Benjamin/0000-0002-6585-0722; Whitaker, Jeanette/0000-0001-8824-471X; Ostle, Nicholas/0000-0003-3263-3702; Salinas, Norma/0000-0001-9941-2109 FU UK Natural Environment Research Council (NERC) [NE/G018278/1, NE/F002149/1]; Australian Research Council grant [FT110100457]; European Union Marie Curie Fellowship [FP7-2012-329360] FX This study is a product of the Andes Biodiversity and Ecosystem Research Group consortium (www.andesconservation.org) and was financed by the UK Natural Environment Research Council (NERC), grant nos. NE/G018278/1 and NE/F002149/1 and also supported by Australian Research Council grant FT110100457 to P. Meir and a European Union Marie Curie Fellowship FP7-2012-329360 to A. T. Nottingham. We thank the Asociacion para la Conservacion de la Cuenca Amazonica (ACCA) in Cusco and the Instituto Nacional de Recursos Naturales (INRENA) in Lima for access to the study sites. For their logistical support we thank Eric Cosio and Eliana Esparza Ballon at Pontificia Universidad Catolica del Peru (PUCP). For their support in the laboratory we thank Tania Romero and Dayana Agudo. For their support in the field we thank Adan J. Q. Ccahuana, Walter H. Huasco and Javier E. S. Espejo. NR 82 TC 5 Z9 5 U1 12 U2 38 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1726-4170 EI 1726-4189 J9 BIOGEOSCIENCES JI Biogeosciences PY 2015 VL 12 IS 20 BP 6071 EP 6083 DI 10.5194/bg-12-6071-2015 PG 13 WC Ecology; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Geology GA CV5PO UT WOS:000364323500001 ER PT B AU Marvin, UB AF Marvin, Ursula B. BE Righter, K Corrigan, CM McCoy, TJ Harvey, RP TI The Origin and Early History of the US Antarctic Search for Meteorites Program (ANSMET) SO 35 SEASONS OF U.S. ANTARCTIC METEORITES (1976-2010): A PICTORIAL GUIDE TO THE COLLECTION SE American Geophysical Union Special Publications LA English DT Article; Book Chapter C1 Harvard Smithsonian Ctr Astrophys, HCO SAO, Cambridge, MA 02138 USA. RP Marvin, UB (reprint author), Harvard Smithsonian Ctr Astrophys, HCO SAO, 60 Garden St, Cambridge, MA 02138 USA. NR 9 TC 0 Z9 0 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA BN 978-1-118-79847-8; 978-1-118-79832-4 J9 AM GEOPHYS UNION SP PY 2015 VL 68 BP 1 EP 22 PG 22 WC Astronomy & Astrophysics; Geochemistry & Geophysics SC Astronomy & Astrophysics; Geochemistry & Geophysics GA BD6LC UT WOS:000362338600002 ER PT B AU Righter, K Corrigan, C McCoy, T Harvey, R AF Righter, Kevin Corrigan, Cari McCoy, Tim Harvey, Ralph BE Righter, K Corrigan, CM McCoy, TJ Harvey, RP TI 35 Seasons of US Antarctic Meteorites (1976-2010) A Pictorial Guide to the Collection PREFACE SO 35 SEASONS OF U.S. ANTARCTIC METEORITES (1976-2010): A PICTORIAL GUIDE TO THE COLLECTION SE American Geophysical Union Special Publications LA English DT Editorial Material; Book Chapter C1 [Righter, Kevin] NASA, Lyndon B Johnson Space Ctr, Mailcode KT, Houston, TX 77058 USA. [Corrigan, Cari; McCoy, Tim] Smithsonian Museum Nat Hist, Washington, DC USA. [Harvey, Ralph] Case Western Reserve Univ, Dept Earth Environm & Planetary Sci, Cleveland, OH 44106 USA. RP Righter, K (reprint author), NASA, Lyndon B Johnson Space Ctr, Mailcode KT, Houston, TX 77058 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA BN 978-1-118-79847-8; 978-1-118-79832-4 J9 AM GEOPHYS UNION SP PY 2015 VL 68 BP V EP VI PG 2 WC Astronomy & Astrophysics; Geochemistry & Geophysics SC Astronomy & Astrophysics; Geochemistry & Geophysics GA BD6LC UT WOS:000362338600001 ER PT B AU Righter, K Satterwhite, CE McBride, KM Corrigan, CM Welzenbach, LC AF Righter, Kevin Satterwhite, Cecilia E. McBride, Kathleen M. Corrigan, Catherine M. Welzenbach, Linda C. BE Righter, K Corrigan, CM McCoy, TJ Harvey, RP TI Curation and Allocation of Samples in the US Antarctic Meteorite Collection SO 35 SEASONS OF U.S. ANTARCTIC METEORITES (1976-2010): A PICTORIAL GUIDE TO THE COLLECTION SE American Geophysical Union Special Publications LA English DT Article; Book Chapter ID AMINO-ACIDS; SMITHSONIAN-INSTITUTION; CHEMICAL-ANALYSES; PARENT BODIES; MARS; CHONDRITES; CHEMISTRY; ALH84001; SEARCH C1 [Righter, Kevin] NASA, Lyndon B Johnson Space Ctr, Mailcode KT, Houston, TX 77058 USA. [Satterwhite, Cecilia E.; McBride, Kathleen M.] NASA, Lyndon B Johnson Space Ctr, Jacobs Technol, Houston, TX 77058 USA. [Corrigan, Catherine M.; Welzenbach, Linda C.] Smithsonian Inst, Dept Mineral Sci, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Righter, K (reprint author), NASA, Lyndon B Johnson Space Ctr, Mailcode KT, Houston, TX 77058 USA. NR 58 TC 0 Z9 0 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA BN 978-1-118-79847-8; 978-1-118-79832-4 J9 AM GEOPHYS UNION SP PY 2015 VL 68 BP 43 EP 63 PG 21 WC Astronomy & Astrophysics; Geochemistry & Geophysics SC Astronomy & Astrophysics; Geochemistry & Geophysics GA BD6LC UT WOS:000362338600004 ER PT B AU Mittlefehldt, DW McCoy, TJ AF Mittlefehldt, David W. McCoy, Timothy J. BE Righter, K Corrigan, CM McCoy, TJ Harvey, RP TI Achondrites and Irons: Products of Magmatism on Strongly Heated Asteroids SO 35 SEASONS OF U.S. ANTARCTIC METEORITES (1976-2010): A PICTORIAL GUIDE TO THE COLLECTION SE American Geophysical Union Special Publications LA English DT Article; Book Chapter ID UREILITE PARENT BODY; ANGRA-DOS-REIS; CORE FORMATION; NOBLE-GASES; BASALTIC ACHONDRITES; SIDEROPHILE ELEMENTS; EUCRITIC METEORITES; OLIVINE DIOGENITES; POLYMICT EUCRITES; NEBULAR PROCESSES C1 [Mittlefehldt, David W.] NASA, Lyndon B Johnson Space Ctr, Astromat Res Off, Mailcode KR, Houston, TX 77058 USA. [McCoy, Timothy J.] Smithsonian Inst, Dept Mineral Sci, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Mittlefehldt, DW (reprint author), NASA, Lyndon B Johnson Space Ctr, Astromat Res Off, Mailcode KR, Houston, TX 77058 USA. NR 113 TC 0 Z9 0 U1 2 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA BN 978-1-118-79847-8; 978-1-118-79832-4 J9 AM GEOPHYS UNION SP PY 2015 VL 68 BP 79 EP 99 PG 21 WC Astronomy & Astrophysics; Geochemistry & Geophysics SC Astronomy & Astrophysics; Geochemistry & Geophysics GA BD6LC UT WOS:000362338600006 ER PT B AU McSween, HY Harvey, RP Corrigan, CM AF McSween, Harry Y., Jr. Harvey, Ralph P. Corrigan, Catherine M. BE Righter, K Corrigan, CM McCoy, TJ Harvey, RP TI Meteorites from Mars, via Antarctica SO 35 SEASONS OF U.S. ANTARCTIC METEORITES (1976-2010): A PICTORIAL GUIDE TO THE COLLECTION SE American Geophysical Union Special Publications LA English DT Article; Book Chapter ID ELEPHANT MORAINE A79001; ALLAN HILLS 84001; ALH84001 MARTIAN METEORITE; ALEXANDRA RANGE 94201; SNC METEORITES; NAKHLITE METEORITES; OXYGEN FUGACITY; LOW-TEMPERATURE; ELEMENT MICRODISTRIBUTIONS; CRYSTALLIZATION HISTORY C1 [McSween, Harry Y., Jr.] Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA. [Harvey, Ralph P.] Case Western Reserve Univ, Dept Earth Environm & Planetary Sci, Cleveland, OH 44106 USA. [Corrigan, Catherine M.] Smithsonian Inst, Dept Mineral Sci, Natl Museum Nat Hist, Washington, DC 20560 USA. RP McSween, HY (reprint author), Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA. NR 107 TC 0 Z9 0 U1 1 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA BN 978-1-118-79847-8; 978-1-118-79832-4 J9 AM GEOPHYS UNION SP PY 2015 VL 68 BP 131 EP 143 PG 13 WC Astronomy & Astrophysics; Geochemistry & Geophysics SC Astronomy & Astrophysics; Geochemistry & Geophysics GA BD6LC UT WOS:000362338600008 ER PT B AU McCoy, TJ AF McCoy, Timothy J. BE Righter, K Corrigan, CM McCoy, TJ Harvey, RP TI Meteorite Misfits: Fuzzy Clues to Solar System Processes SO 35 SEASONS OF U.S. ANTARCTIC METEORITES (1976-2010): A PICTORIAL GUIDE TO THE COLLECTION SE American Geophysical Union Special Publications LA English DT Article; Book Chapter ID AL-RICH CHONDRULES; ORDINARY CHONDRITES; 4 VESTA; PETROLOGY; ORIGIN; HISTORY; AGES C1 Smithsonian Inst, Dept Mineral Sci, Natl Museum Nat Hist, Washington, DC 20560 USA. RP McCoy, TJ (reprint author), Smithsonian Inst, Dept Mineral Sci, Natl Museum Nat Hist, Washington, DC 20560 USA. NR 31 TC 0 Z9 0 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA BN 978-1-118-79847-8; 978-1-118-79832-4 J9 AM GEOPHYS UNION SP PY 2015 VL 68 BP 145 EP 152 PG 8 WC Astronomy & Astrophysics; Geochemistry & Geophysics SC Astronomy & Astrophysics; Geochemistry & Geophysics GA BD6LC UT WOS:000362338600009 ER PT B AU Corrigan, CM Welzenbach, LC Righter, K McBride, KM McCoy, TJ Harvey, RP Satterwhite, CE AF Corrigan, Catherine M. Welzenbach, Linda C. Righter, Kevin McBride, Kathleen M. McCoy, Timothy J. Harvey, Ralph P. Satterwhite, Cecilia E. BE Righter, K Corrigan, CM McCoy, TJ Harvey, RP TI A Statistical Look at the US Antarctic Meteorite Collection SO 35 SEASONS OF U.S. ANTARCTIC METEORITES (1976-2010): A PICTORIAL GUIDE TO THE COLLECTION SE American Geophysical Union Special Publications LA English DT Article; Book Chapter ID H CHONDRITES; MODERN FALLS; FINDS; MASS; DISTRIBUTIONS; RECOVERY C1 [Corrigan, Catherine M.; Welzenbach, Linda C.; McCoy, Timothy J.] Smithsonian Inst, Dept Mineral Sci, Natl Museum Nat Hist, Washington, DC 20560 USA. [Righter, Kevin; McBride, Kathleen M.; Satterwhite, Cecilia E.] NASA, Lyndon B Johnson Space Ctr, Jacobs Technol, Houston, TX 77058 USA. [Harvey, Ralph P.] Case Western Reserve Univ, Dept Earth Environm & Planetary Sci, Cleveland, OH 44106 USA. RP Corrigan, CM (reprint author), Smithsonian Inst, Dept Mineral Sci, Natl Museum Nat Hist, Washington, DC 20560 USA. NR 34 TC 0 Z9 0 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA BN 978-1-118-79847-8; 978-1-118-79832-4 J9 AM GEOPHYS UNION SP PY 2015 VL 68 BP 173 EP 187 PG 15 WC Astronomy & Astrophysics; Geochemistry & Geophysics SC Astronomy & Astrophysics; Geochemistry & Geophysics GA BD6LC UT WOS:000362338600011 ER PT J AU McCoy, TJ Beck, AW Prettyman, TH Mittlefehldt, DW AF McCoy, Timothy J. Beck, Andrew W. Prettyman, Thomas H. Mittlefehldt, David W. TI Asteroid (4) Vesta II: Exploring a geologically and geochemically complex world with the Dawn Mission SO CHEMIE DER ERDE-GEOCHEMISTRY LA English DT Review DE Asteroid; Craters; Impacts; Meteorites; Dawn mission ID HUBBLE-SPACE-TELESCOPE; DIOGENITE PARENT BODY; OLIVINE DIOGENITES; POLYMICT BRECCIAS; NEUTRON DETECTOR; DARK MATERIAL; MAGMA OCEAN; GAMMA-RAY; CONSTRAINTS; METEORITES AB More than 200 years after its discovery, asteroid (4) Vesta is thought to be the parent body for the howardite, eucrite and diogenite (HED) meteorites. The Dawn spacecraft spent 14 months in orbit around this largest, intact differentiated asteroid to study its internal structure, geology, mineralogy and chemistry. Carrying a suite of instruments that included two framing cameras, a visible-near infrared spectrometer, and a gamma-ray and neutron detector, coupled with radio tracking for gravity, Dawn revealed a geologically and geochemically complex world. A constrained core size of similar to 110-130 km radius is consistent with predictions based on differentiation models for the HED meteorite parent body. Hubble Space Telescope observations had already shown that Vesta is scarred by a south polar basin comparable in diameter to that of the asteroid itself. Dawn showed that the south polar Rheasilvia basin dominates the asteroid, with a central uplift that rivals the large shield volcanoes of the Solar System in height. An older basin, Veneneia, partially underlies Rheasilvia. A series of graben-like equatorial and northern troughs were created during these massive impact events 1-2 Ga ago. These events also resurfaced much of the southern hemisphere and exposed deeper-seated diogenitic lithologies. Although the mineralogy and geochemistry vary across the surface for rock-forming elements and minerals, the range is small, suggesting that impact processes have efficiently homogenized the surface of Vesta at scales observed by the instruments on the Dawn spacecraft. The distribution of hydrogen is correlated with surface age, which likely results from the admixture of exogenic carbonaceous chondrites with Vesta's basaltic surface. Clasts of such material are observed within the surficial howardite meteorites in our collections. Dawn significantly strengthened the link between (4) Vesta and the HED meteorites, but the pervasive mixing, lack of a convincing and widespread detection of olivine, and poorly-constrained lateral and vertical extents of units leaves unanswered the central question of whether Vesta once had a magma ocean. Dawn is continuing its mission to the presumed ice-rich asteroid (1) Ceres. Published by Elsevier GmbH. C1 [McCoy, Timothy J.; Beck, Andrew W.] Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. [Beck, Andrew W.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Prettyman, Thomas H.] Planetary Sci Inst, Tucson, AZ 85719 USA. [Mittlefehldt, David W.] NASA, Johnson Space Ctr, Astromat Res Off, Houston, TX 77058 USA. RP McCoy, TJ (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. EM mccoyt@si.edu RI Beck, Andrew/J-7215-2015; OI Beck, Andrew/0000-0003-4455-2299; Prettyman, Thomas/0000-0003-0072-2831 FU NASA Dawn at Vesta Participating Scientist Program; Planetary Science Institute under NASA Jet Propulsion Laboratory FX We thank the entire Dawn engineering and science teams, without whom this mission would not have succeeded. We thank the NASA Dawn at Vesta Participating Scientist Program for funding for this work and Associate Editor Dr. Klaus Keil for inviting submission of this paper. Reviews by Vishnu Reddy, Jessica Sunshine and an anonymous reviewer significantly improved the manuscript. A portion of this work was carried out by the Planetary Science Institute under contract with the NASA Jet Propulsion Laboratory. NR 85 TC 1 Z9 2 U1 5 U2 7 PU ELSEVIER GMBH, URBAN & FISCHER VERLAG PI JENA PA OFFICE JENA, P O BOX 100537, 07705 JENA, GERMANY SN 0009-2819 EI 1611-5864 J9 CHEM ERDE-GEOCHEM JI Chem Erde-Geochem. PY 2015 VL 75 IS 3 BP 273 EP 285 DI 10.1016/j.chemer.2014.12.001 PG 13 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CU8UA UT WOS:000363818400001 ER PT J AU Bohnemeyer, J Donelson, KT Moore, RE Benedicto, E Eggleston, A O'Meara, CK Baez, GP Garza, AC Green, NH Gomez, MDSH Castro, SH Palancar, E Polian, G Mendez, RR AF Bohnemeyer, Juergen Donelson, Katharine T. Moore, Randi E. Benedicto, Elena Eggleston, Alyson O'Meara, Carolyn K. Perez Baez, Gabriela Capistran Garza, Alejandra Hernandez Green, Nestor Selene Hernandez Gomez, Maria de Jess Herrera Castro, Samuel Palancar, Enrique Polian, Gilles Romero Mendez, Rodrigo TI The Contact Diffusion of Linguistic Practices Reference Frames in Mesoamerica SO LANGUAGE DYNAMICS AND CHANGE LA English DT Article DE language contact; Linguistic Transmission Hypothesis; spatial cognition; areality; Mesoamerica ID SPATIAL COGNITION; LANGUAGE; ORIENTATION; TYPOLOGY; GESTURE; TABLES; SPACE AB We examine the extent to which practices of language use may be diffused through language contact and areally shared, using data on spatial reference frame use by speakers of eight indigenous languages from in and around the Mesoamerican linguistic area and three varieties of Spanish. Regression models show that the frequency of L2-Spanish use by speakers of the indigenous languages predicts the use of relative reference frames in the L1 even when literacy and education levels are accounted for. A significant difference in frame use between the Mesoamerican and non-Mesoamerican indigenous languages further supports the contact diffusion analysis. C1 [Bohnemeyer, Juergen; Donelson, Katharine T.; Moore, Randi E.] SUNY Buffalo, Buffalo, NY 14260 USA. [Benedicto, Elena] Purdue Univ, W Lafayette, IN 47907 USA. [Eggleston, Alyson] Coll Charleston, Charleston, SC USA. [O'Meara, Carolyn K.; Herrera Castro, Samuel; Romero Mendez, Rodrigo] Univ Nacl Autonoma Mexico, Mexico City 04510, DF, Mexico. [Perez Baez, Gabriela] Smithsonian Inst, Washington, DC 20560 USA. [Capistran Garza, Alejandra] Univ Autonoma Metropolitana Iztapalapa, Ciudad Mexico, DF, Mexico. [Hernandez Green, Nestor; Polian, Gilles] Ctr Invest & Estudios Super Antropol Social Dist, Lisbon, Portugal. [Selene Hernandez Gomez, Maria de Jess] Univ Autonoma Queretaro, Santiago, Chile. [Palancar, Enrique] Univ Surrey, Guildford GU2 5XH, Surrey, England. RP Bohnemeyer, J (reprint author), SUNY Buffalo, Buffalo, NY 14260 USA. EM jb77@buffalo.edu NR 63 TC 1 Z9 1 U1 0 U2 1 PU BRILL ACADEMIC PUBLISHERS PI LEIDEN PA PLANTIJNSTRAAT 2, P O BOX 9000, 2300 PA LEIDEN, NETHERLANDS SN 2210-5824 EI 2210-5832 J9 LANG DYN CHANG JI Lang. Dyn. Chang. PY 2015 VL 5 IS 2 BP 169 EP 201 DI 10.1163/22105832-00502002 PG 33 WC Language & Linguistics SC Linguistics GA CV3JY UT WOS:000364156700002 ER PT B AU Horton, JL Berlo, JC AF Horton, Jessica L. Berlo, Janet Catherine BE Davis, J Greenhill, JA LaFountain, JD TI Pueblo Painting in 1932 Folding Narratives of Native Art into American Art History SO COMPANION TO AMERICAN ART SE Wiley Blackwell Companions to Art History LA English DT Article; Book Chapter C1 [Horton, Jessica L.] Smithsonian Amer Art Museum, Washington, DC USA. [Horton, Jessica L.] Amer Indian, Natl Museum, Jaipur, Rajasthan, India. [Berlo, Janet Catherine] Univ Rochester, Art Hist & Visual & Cultural Studies, Rochester, NY 14627 USA. NR 60 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN STREET, MALDEN 02148, MA USA BN 978-1-118-54264-4; 978-0-470-67102-3 J9 WILEY BLACK COMP ART PY 2015 BP 264 EP 280 D2 10.1002/9781118542644 PG 17 WC Art SC Art GA BD5QY UT WOS:000361742000017 ER PT J AU Tang, M Arevalo, R Goreva, Y McDonough, WF AF Tang, Ming Arevalo, Ricardo, Jr. Goreva, Yulia McDonough, William F. TI Elemental fractionation during condensation of plasma plumes generated by laser ablation: a ToF-SIMS study of condensate blankets SO JOURNAL OF ANALYTICAL ATOMIC SPECTROMETRY LA English DT Article ID PARTICLE-SIZE DISTRIBUTION; LA-ICP-MS; MASS SPECTROMETRY; SILICATE GLASS; NANOSECOND; BRASS; AEROSOLS AB Ion imaging of the condensate blanket around a laser ablation site provides a window to study elemental fractionation during condensation of a plasma plume. Here we used a Time-of-Flight Secondary Ion Mass Spectrometer (ToF-SIMS) to conduct depth profiling of the condensate blanket produced by excimer 193 nm laser ablation of NIST 610 glass. Compositional zonings (Ca normalized) revealed by ToF-SIMS are associated with texture gradients in the condensate blanket, as characterized by Secondary Electron Microprobe (SEM) images. Elements that are more volatile than Ca are relatively enriched in the inner zones (proximal to the ablation site) while more refractory elements are variable in their distributions. Volatility and ionization potential exert influence on elemental fractionation in plasma plume condensation processes as documented by the contrasting fractionation behaviors of alkaline and alkaline earth metals. Compositional zonings in the condensate blanket are due to physical and chemical zonings (e.g., temperature, pressure, electron density, speciation, etc.) within the condensing plume as it expands and cools. Zoned condensation may be a primary mechanism driving the elemental fractionation associated with laser ablation. C1 [Tang, Ming; McDonough, William F.] Univ Maryland, Dept Geog, College Pk, MD 20742 USA. [Arevalo, Ricardo, Jr.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Goreva, Yulia] Smithsonian Inst, Washington, DC 20013 USA. RP Tang, M (reprint author), Univ Maryland, Dept Geog, College Pk, MD 20742 USA. EM tangmyes@gmail.com RI McDonough, William/I-7720-2012 OI McDonough, William/0000-0001-9154-3673 FU NSF [EAR-0739006, EAR-0948549]; NASA [NNX14AF27G]; Deep Carbon Observatory; graduate school of University of Maryland (Ann G. Wylie Fellowship) FX This project is funded by NSF grants EAR-0739006 and EAR-0948549. The first author also appreciates the support from the graduate school of the University of Maryland (Ann G. Wylie Fellowship). ToF-SIMS work (Yulia Goreva) was supported by NASA grant NNX14AF27G and funding from Deep Carbon Observatory. We thank editor Harriet Brewerton for handling our paper, and two anonymous reviewers for their comments and suggestions. NR 31 TC 0 Z9 0 U1 2 U2 10 PU ROYAL SOC CHEMISTRY PI CAMBRIDGE PA THOMAS GRAHAM HOUSE, SCIENCE PARK, MILTON RD, CAMBRIDGE CB4 0WF, CAMBS, ENGLAND SN 0267-9477 EI 1364-5544 J9 J ANAL ATOM SPECTROM JI J. Anal. At. Spectrom. PY 2015 VL 30 IS 11 BP 2316 EP 2322 DI 10.1039/c5ja00320b PG 7 WC Chemistry, Analytical; Spectroscopy SC Chemistry; Spectroscopy GA CU5PF UT WOS:000363583700005 ER PT J AU Frias-Torres, S Goehlich, H Reveret, C Montoya-Maya, PH AF Frias-Torres, S. Goehlich, H. Reveret, C. Montoya-Maya, P. H. TI Reef fishes recruited at midwater coral nurseries consume biofouling and reduce cleaning time in Seychelles, Indian Ocean SO AFRICAN JOURNAL OF MARINE SCIENCE LA English DT Article DE animal-assisted cleaning; coral gardening; coral reef restoration; endangered species; floating ecosystem ID DAMSELFISHES POMACENTRIDAE; RESTORATION; RESILIENCE; ECOSYSTEMS; MANAGEMENT AB In coral reef restoration, coral gardening involves rearing coral fragments in underwater nurseries prior to transplantation. These nurseries become fish-aggregating devices and attract biofouling. We hypothesised that: (1) the presence of corals at a nursery is critical to recruit fish assemblages and (2) the recruited fish assemblages control biofouling, reducing person-hours invested in nursery cleaning. Three midwater coral nurseries were deployed at 8 m depth for 27 months within the marine protected area of Cousin Island Special Reserve, Seychelles, Indian Ocean. Each nursery consisted of a 6 m x 6 m PVC pipe frame, layered with a recycled 5.5-cm-mesh tuna net. Human cleaning effort was calculated based on daily dive logs. Nursery-associated fish assemblages and behaviour were video-recorded prior to harvesting corals after a 20-month growth period and seven months post-coral harvesting. The density (ind. m(-2)) of blue-yellow damselfish Pomacentrus caeruleus was 12-16 times higher when corals were present than when corals were absent at the nurseries. Fish assemblages recruited into the nurseries included three trophic levels, from herbivores to omnivores, in six families: Ephippidae, Pomacentridae, Labridae (Scarinae), Gobiidae, Siganidae and Monacanthidae. Higher abundance of large fish (total number of individuals) resulted in 2.75 times less person-hours spent in nursery cleaning. These results have important implications for cost-effective coral reef restoration. C1 [Frias-Torres, S.; Goehlich, H.; Reveret, C.; Montoya-Maya, P. H.] Nat Seychelles, Isl Conservat Ctr, Amitie, Praslin, Seychelles. [Frias-Torres, S.] Smithsonian Marine Stn, Ft Pierce, FL USA. [Goehlich, H.] Univ Rostock, Inst Biol Sci, D-18055 Rostock, Germany. [Reveret, C.] CREOCEAN, La Rochelle, France. RP Frias-Torres, S (reprint author), Nat Seychelles, Isl Conservat Ctr, Amitie, Praslin, Seychelles. EM sfriastorres@gmail.com FU United States Agency for International Development (USAID) Reef Rescuers Project [674-A-00-10-00123-00] FX We thank K Rowe, M Mullins, D Quinlan and D Soto for help during fieldwork and N Shah for commenting on an earlier draft of the manuscript. Funding to Nature Seychelles was received through the United States Agency for International Development (USAID) Reef Rescuers Project 674-A-00-10-00123-00. NR 23 TC 2 Z9 2 U1 3 U2 8 PU NATL INQUIRY SERVICES CENTRE PTY LTD PI GRAHAMSTOWN PA 19 WORCESTER STREET, PO BOX 377, GRAHAMSTOWN 6140, SOUTH AFRICA SN 1814-232X EI 1814-2338 J9 AFR J MAR SCI JI Afr. J. Mar. Sci. PY 2015 VL 37 IS 3 BP 421 EP 426 DI 10.2989/1814232X.2015.1078259 PG 6 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA CU2GP UT WOS:000363342200014 ER PT J AU Lin, JT Liu, MY Xin, JY Boersma, KF Spurr, R Martin, R Zhang, Q AF Lin, J. -T. Liu, M. -Y. Xin, J. -Y. Boersma, K. F. Spurr, R. Martin, R. Zhang, Q. TI Influence of aerosols and surface reflectance on satellite NO2 retrieval: seasonal and spatial characteristics and implications for NOx emission constraints SO ATMOSPHERIC CHEMISTRY AND PHYSICS LA English DT Article ID TROPOSPHERIC NITROGEN-DIOXIDE; OZONE MONITORING INSTRUMENT; OPTICAL DEPTH RETRIEVAL; AIR-POLLUTION; EAST-ASIA; CHINA; SPACE; OXIDES; OMI; ALGORITHM AB Satellite retrievals of vertical column densities (VCDs) of tropospheric nitrogen dioxide (NO2) normally do not explicitly account for aerosol optical effects and surface reflectance anisotropy that vary with space and time. Here, we conduct an improved retrieval of NO2 VCDs over China, called the POMINO algorithm, based on measurements from the Ozone Monitoring Instrument (OMI), and we test the importance of a number of aerosol and surface reflectance treatments in this algorithm. POMINO uses a parallelized LIDORT-driven AMFv6 package to derive tropospheric air mass factors via pixel-specific radiative transfer calculations with no look-up tables, taking slant column densities from DOMINO v2. Prerequisite cloud optical properties are derived from a dedicated cloud retrieval process that is fully consistent with the main NO2 retrieval. Aerosol optical properties are taken from GEOS-Chem simulations constrained by MODIS aerosol optical depth (AOD) data. MODIS bidirectional reflectance distribution function (BRDF) data are used for surface reflectance over land. For the present analysis, POMINO level-2 data for 2012 are aggregated into monthly means on a 0.25 degrees long. x 0.25 degrees lat. grid. POMINO-retrieved annual mean NO2 VCDs vary from 15-25 x 10(15) cm(-2) over the polluted North China Plain (NCP) to below 10(15) cm(-2) over much of western China. Using POMINO to infer Chinese emissions of nitrogen oxides leads to annual anthropogenic emissions of 9.05 TgN yr(-1), an increase from 2006 (Lin, 2012) by about 19 %. Replacing the MODIS BRDF data with the OMLER v1 monthly climatological albedo data affects NO2 VCDs by up to 40% for certain locations and seasons. The effect on constrained NOx emissions is small. Excluding aerosol information from the retrieval process (this is the traditional "implicit" treatment) enhances annual mean NO2 VCDs by 15-40% over much of eastern China. Seasonally, NO2 VCDs are reduced by 10-20% over parts of the NCP in spring and over northern China in winter, despite the general enhancements in summer and fall. The effect on subsequently constrained annual emissions is between -5 and +30% with large seasonal and spatial dependence. The implicit aerosol treatment also tends to exclude days with high pollution, since aerosols are interpreted as effective clouds and the respective OMI pixels are often excluded by cloud screening; this is a potentially important sampling bias. Therefore an explicit treatment of aerosols is important for space-based NO2 retrievals and emission constraints. A comprehensive independent measurement network with sufficient spatial and temporal representativeness is needed to further evaluate the different satellite retrieval approaches. C1 [Lin, J. -T.; Liu, M. -Y.] Peking Univ, Sch Phys, Dept Atmospher & Ocean Sci, Lab Climate & Ocean Atmosphere Studies, Beijing 100871, Peoples R China. [Xin, J. -Y.] Chinese Acad Sci, Inst Atmospher Phys, State Key Lab Atmospher Boundary Layer Phys & Atm, Beijing 100029, Peoples R China. [Boersma, K. F.] Royal Netherlands Meteorol Inst, NL-3730 AE De Bilt, Netherlands. [Boersma, K. F.] Wageningen Univ, Meteorol & Air Qual Dept, NL-6700 AP Wageningen, Netherlands. [Spurr, R.] RT Solut Inc, Cambridge, MA 02138 USA. [Martin, R.] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS, Canada. [Martin, R.] Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA. [Zhang, Q.] Tsinghua Univ, Ctr Earth Syst Sci, Minist Educ, Key Lab Earth Syst Modeling, Beijing 100084, Peoples R China. RP Lin, JT (reprint author), Peking Univ, Sch Phys, Dept Atmospher & Ocean Sci, Lab Climate & Ocean Atmosphere Studies, Beijing 100871, Peoples R China. EM linjt@pku.edu.cn RI Boersma, Klaas/H-4559-2012; Zhang, Qiang/D-9034-2012; Lin, Jintai/A-8872-2012; Chem, GEOS/C-5595-2014; 辛, 金元/F-7310-2012 OI Boersma, Klaas/0000-0002-4591-7635; Lin, Jintai/0000-0002-2362-2940; 辛, 金元/0000-0003-4243-5072 FU National Natural Science Foundation of China [41175127, 41422502]; 973 program [2014CB441302]; NWO Vidi grant [864.09.001]; European Community [607405 (QA4ECV)] FX This research is supported by the National Natural Science Foundation of China, grants 41175127 and 41422502, and by the 973 program, grant 2014CB441302. We acknowledge the free use of NO2 and cloud products from http://www.temis.nl, GMTED2010 surface elevation data from USGS, GLCNMO land use type data from ISCGM, MODIS aerosol and surface reflectance data from NASA, and several AOD measurements from AERONET. Folkert Boersma acknowledges receiving funding for this research from NWO Vidi grant 864.09.001 and from the European Community's Seventh Frame-work Programme under grant agreement no. 607405 (QA4ECV). The calculation was supported in part by the National Institute of Supercomputing and Network/Korea Institute of Science and Technology Information with supercomputing resources including technical support (KSC-2014-C2-034). NR 66 TC 8 Z9 8 U1 5 U2 21 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 2015 VL 15 IS 19 BP 11217 EP 11241 DI 10.5194/acp-15-11217-2015 PG 25 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CT7CN UT WOS:000362971000019 ER PT J AU Heineman, KD Russo, SE Baillie, IC Mamit, JD Chai, PPK Chai, L Hindley, EW Lau, BT Tan, S Ashton, PS AF Heineman, K. D. Russo, S. E. Baillie, I. C. Mamit, J. D. Chai, P. P. -K. Chai, L. Hindley, E. W. Lau, B. -T. Tan, S. Ashton, P. S. TI Evaluation of stem rot in 339 Bornean tree species: implications of size, taxonomy, and soil-related variation for aboveground biomass estimates SO BIOGEOSCIENCES LA English DT Article ID MIXED DIPTEROCARP FOREST; WOOD DECOMPOSITION RATES; TROPICAL RAIN-FOREST; ANTIMICROBIAL DEFENSES; LANDSCAPE-SCALE; HOLLOW TRUNKS; CARBON STOCKS; DECAY; DENSITY; GROWTH AB Fungal decay of heart wood creates hollows and areas of reduced wood density within the stems of living trees known as stem rot. Although stem rot is acknowledged as a source of error in forest aboveground biomass (AGB) estimates, there are few data sets available to evaluate the controls over stem rot infection and severity in tropical forests. Using legacy and recent data from 3180 drilled, felled, and cored stems in mixed dipterocarp forests in Sarawak, Malaysian Borneo, we quantified the frequency and severity of stem rot in a total of 339 tree species, and related variation in stem rot with tree size, wood density, taxonomy, and species' soil association, as well as edaphic conditions. Predicted stem rot frequency for a 50 cm tree was 53% of felled, 39% of drilled, and 28% of cored stems, demonstrating differences among methods in rot detection ability. The percent stem volume infected by rot, or stem rot severity, ranged widely among trees with stem rot infection (0.1-82.8 %) and averaged 9% across all trees felled. Tree taxonomy explained the greatest proportion of variance in both stem rot frequency and severity among the predictors evaluated in our models. Stem rot frequency, but not severity, increased sharply with tree diameter, ranging from 13% in trees 10-30 cm DBH to 54% in stems >= 50 cm DBH across all data sets. The frequency of stem rot increased significantly in soils with low pH and cation concentrations in topsoil, and stem rot was more common in tree species associated with dystrophic sandy soils than with nutrient-rich clays. When scaled to forest stands, the maximum percent of stem biomass lost to stem rot varied significantly with soil properties, and we estimate that stem rot reduces total forest AGB estimates by up to 7% relative to what would be predicted assuming all stems are composed strictly of intact wood. This study demonstrates not only that stem rot is likely to be a significant source of error in forest AGB estimation, but also that it strongly covaries with tree size, taxonomy, habitat association, and soil resources, underscoring the need to account for tree community composition and edaphic variation in estimating carbon storage in tropical forests. C1 [Heineman, K. D.; Lau, B. -T.] Univ Illinois, Program Ecol Evolut & Conservat Biol, Urbana, IL 61801 USA. [Russo, S. E.] Univ Nebraska, Sch Biol Sci, Lincoln, NE USA. [Baillie, I. C.] Cranfield Univ, Natl Soil Resources Inst, Cranfield MK43 0AL, Beds, England. [Baillie, I. C.; Mamit, J. D.; Chai, P. P. -K.; Chai, L.; Lau, B. -T.] Forest Dept, Kuching, Sarawak, Malaysia. [Mamit, J. D.] Fed Parliament Malaysia, Kuala Lumpur, Malaysia. [Tan, S.] Smithsonian Inst, Ctr Trop Forest Sci, Washington, DC 20560 USA. [Ashton, P. S.] Harvard Univ, Organism & Evolutionary Biol, Cambridge, MA 02138 USA. [Ashton, P. S.] Royal Bot Gardens, Richmond, Surrey, England. RP Heineman, KD (reprint author), Univ Illinois, Program Ecol Evolut & Conservat Biol, Urbana, IL 61801 USA. EM kheineman@life.illinois.edu FU Center for Tropical Forest Science; NSF [DUE-0531920]; University of Nebraska-Lincoln (UNL) UCARE undergraduate research program; UNL School of Biological Sciences FX We thank Sarawak Conservator of Forests for permission to use Central Sarawak inventory and soils data and photographs for research, and Sarawak Forest Department and the Protected Areas and Biodiversity Conservation unit of Sarawak Forestry Corporation for permission to conduct research in Lambir Hills National Park. We are grateful to many colleagues in the FIDP inventory, which was a substantial team effort involving scores of people working for several field seasons in difficult conditions. We thank two anonymous reviewers, James Dalling, and Amy Zanne for providing comments that improved this manuscript. Data collection at Lambir was funded by the Center for Tropical Forest Science, NSF DUE-0531920, the University of Nebraska-Lincoln (UNL) UCARE undergraduate research program, and the UNL School of Biological Sciences. NR 111 TC 3 Z9 3 U1 3 U2 10 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1726-4170 EI 1726-4189 J9 BIOGEOSCIENCES JI Biogeosciences PY 2015 VL 12 IS 19 BP 5735 EP 5751 DI 10.5194/bg-12-5735-2015 PG 17 WC Ecology; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Geology GA CT7CY UT WOS:000362972200012 ER PT J AU Smith, DR Naito, T AF Smith, David R. Naito, Tikahiko TI Studies on Adelestini (Hymenoptera,Tenthredinidae), particularly the long-tongued Nipponorhynchus Takeuchi of Japan SO JOURNAL OF HYMENOPTERA RESEARCH LA English DT Article DE Sawflies; Selandriinae; Adelesta; Chrysosplenium AB Nipponorhynchus brevis Smith & Naito, sp. n., is described from Hokkaido, Japan. It is characterized by shorter mouthparts than those of the other two species of the genus, N. bimaculatus Naito and N. mirabilis Takeuchi. The previously unknown female of N. bimaculatus is described. Larvae of N. bimaculatus and N. mirabilis feed on Chrysosplenium macrostemon var. shiobarense (Saxifragaceae), and notes on the life history are given. Nipponorhynchus is compared with the Nearctic Adelesta Ross, the only other genus of Adelestini. A key to the genera and species of Adelestini is provided. C1 [Smith, David R.] ARS, Systemat Entomol Lab, USDA, Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20013 USA. RP Smith, DR (reprint author), ARS, Systemat Entomol Lab, USDA, Natl Museum Nat Hist,Smithsonian Inst, POB 37012,MRC 168, Washington, DC 20013 USA. EM sawfly2@aol.com NR 15 TC 0 Z9 0 U1 0 U2 1 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. PY 2015 VL 45 BP 1 EP 14 DI 10.3897/JHR.45.5442 PG 14 WC Entomology SC Entomology GA CT6MR UT WOS:000362927600001 ER PT J AU Liu, C Liu, X Kowalewski, MG Janz, SJ Abad, GG Pickering, KE Chance, K Lamsal, LN AF Liu, C. Liu, X. Kowalewski, M. G. Janz, S. J. Abad, G. Gonzalez Pickering, K. E. Chance, K. Lamsal, L. N. TI Analysis of ACAM Data for Trace Gas Retrievals during the 2011 DISCOVER-AQ Campaign SO JOURNAL OF SPECTROSCOPY LA English DT Article ID SLANT COLUMN MEASUREMENTS; MAX-DOAS; NO2; SPECTROPHOTOMETER; IRRADIANCE; UV AB To improve the trace gas retrieval from Airborne Compact Atmospheric Mapper (ACAM) during the DSICOVER-AQ campaigns, we characterize the signal to noise ratio (SNR) of the ACAM measurement. From the standard deviations of the fitting residuals, the SNRs of ACAM nadir measurements are estimated to vary from similar to 300 at 310 nm to similar to 1000 in the blue spectral region; the zenith data are noisier due to reduced levels of illumination and lower system throughput and also show many more pixels with abrupt anomalous values; therefore, a new method is developed to derive a solar irradiance reference at the top of the atmosphere (TOA) from average nadir measurements, at instrument spectral resolution and including instrument calibration characteristics. Using this reference can significantly reduce fitting residuals and improve the retrievals. This approach derives an absolute reference for direct fitting algorithms involving radiative transfer calculations and thus can be applied to both aircraft and ground-based measurements. The comparison of ACAM radiance with simulations using coincident ozonesonde and OMI data shows large wavelength-dependent biases in ACAM data, varying from similar to-19% at 310nm to 5% at 360 nm. Correcting ACAM radiance in direct-fitting based ozone profile algorithm significantly improves the consistency with OMI total ozone. C1 [Liu, C.; Liu, X.; Abad, G. Gonzalez; Chance, K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kowalewski, M. G.; Lamsal, L. N.] Univ Space Res Assoc, Goddard Earth Sci Technol & Res, Columbia, MD 21044 USA. [Kowalewski, M. G.; Janz, S. J.; Pickering, K. E.; Lamsal, L. N.] NASA Goddard Space & Flight Ctr, Greenbelt, MD 20771 USA. RP Liu, C (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM chliu81@ustc.edu.cn RI Liu, Xiong/P-7186-2014; Pickering, Kenneth/E-6274-2012; OI Liu, Xiong/0000-0003-2939-574X; Gonzalez Abad, Gonzalo/0000-0002-8090-6480 FU NASA, NASA Earth Venture-1 DISCOVER-AQ project [NNX11AH77G, NNX12AJ66G]; Smithsonian Institution FX Funding for this work at SAO is provided by NASA Grants NNX11AH77G and NNX12AJ66G as part of the NASA Earth Venture-1 DISCOVER-AQ project and by the Smithsonian Institution. The authors thank Anne Thompson (NASA/GSFC) and Everette Joseph (Howard University) who provided the ozonesonde data from the Edgewood and Beltsville sites, respectively. They acknowledge James Crawford for his strong support on this work. NR 23 TC 4 Z9 4 U1 1 U2 5 PU HINDAWI PUBLISHING CORP PI NEW YORK PA 315 MADISON AVE 3RD FLR, STE 3070, NEW YORK, NY 10017 USA SN 2314-4920 EI 2314-4939 J9 J SPECTROSC JI J. Spectrosc. PY 2015 BP 1 EP 7 AR 827160 DI 10.1155/2015/827160 PG 7 WC Biochemical Research Methods; Spectroscopy SC Biochemistry & Molecular Biology; Spectroscopy GA CT4QB UT WOS:000362790600001 ER PT J AU McKamey, SH Wallner, AM Porter, MJ AF McKamey, Stuart H. Wallner, Adam M. Porter, Mitchell J. TI Immatures of the New World treehopper tribe Amastrini (Hemiptera, Membracidae, Smiliinae) with a key to genera SO ZOOKEYS LA English DT Article DE Nymph; Amastris; Bajulata; Erosne; Harmonides; Idioderma; Neotynelia; Vanduzea ID TAXONOMIC NOTES; HOST PLANTS; HOMOPTERA; BIOLOGY; GENUS AB The immatures stages of 8 of the 11 genera (Amastris Stal, Bajulata Ball, Erosne Stal, Harmonides Kirkaldy, Idioderma Van Duzee, Neotynelia Creao-Duarte & Sakakibara, Tynelia Stal, and Vanduzea Goding) of the tribe Amastrini are described for the first time along with brief diagnoses of Membracidae and the subfamily Smiliinae. A key to genera and notes on biology are provided. Multiple species of most genera are illustrated. Based on its distinct nymphal morphology, Vanduzea laeta nolina Ball is elevated to specific rank as Vanduzea nolina stat. n., and Bajulata, despite the superficial similarity of its adults to those of Vanduzea, is confirmed as warranting generic rank based on its unique nymphal morphology. Colombia is a new country record for Tynelia. C1 [McKamey, Stuart H.] ARS, USDA, Systemat Entomol Lab, Smithsonian Inst, Washington, DC 20560 USA. [Wallner, Adam M.] USDA, APHIS, PPQ, Plant Inspect Stn, Miami, FL 33266 USA. [Porter, Mitchell J.] Univ Maryland, Dept Biol, College Pk, MD 20742 USA. RP McKamey, SH (reprint author), ARS, USDA, Systemat Entomol Lab, Smithsonian Inst, NMNH MRC 168, Washington, DC 20560 USA. EM stuart.mckamey@ars.usda.gov NR 49 TC 2 Z9 2 U1 0 U2 3 PU PENSOFT PUBL PI SOFIA PA 12 PROF GEORGI ZLATARSKI ST, SOFIA, 1700, BULGARIA SN 1313-2989 EI 1313-2970 J9 ZOOKEYS JI ZooKeys PY 2015 IS 524 BP 65 EP 87 DI 10.3897/zookeys.524.5951 PG 23 WC Zoology SC Zoology GA CT0VI UT WOS:000362515200004 PM 26478706 ER PT J AU Robbins, RK Heredia, MD Busby, RC AF Robbins, Robert K. Dolores Heredia, Maria Busby, Robert C. TI Male secondary sexual structures and the systematics of the Thereus oppia species group (Lepidoptera, Lycaenidae, Eumaeini) SO ZOOKEYS LA English DT Article DE Dollo's Law; Loranthaceae; Scent pads; Thereus brocki; Thereus lomalarga; Thereus orasus AB The Thereus oppia species group includes species with and without a scent pad, which is a histologically and morphologically characterized male secondary sexual structure on the dorsal surface of the forewing. To assess the hypothesis that these structures are lost evolutionarily, but not regained (Dollo's Law), the taxonomy of this species group is revised. Thereus lomalarga sp. n., and Thereus brocki sp. n., are described. Diagnostic traits, especially male secondary structures, within the T. oppia species group are illustrated. Distributional and biological information is summarized for each species. Three species have been reared, and the caterpillars eat Loranthaceae. An inferred phylogeny is consistent with the hypothesis that scent pads in the T. oppia species group have been lost evolutionarily twice (in allopatry), and not re-gained. C1 [Robbins, Robert K.] Smithsonian Inst, Dept Entomol, Washington, DC 20013 USA. RP Robbins, RK (reprint author), Smithsonian Inst, Dept Entomol, POB 37012,NHB Stop 105, Washington, DC 20013 USA. EM RobbinsR@si.edu NR 26 TC 1 Z9 1 U1 3 U2 4 PU PENSOFT PUBL PI SOFIA PA 12 PROF GEORGI ZLATARSKI ST, SOFIA, 1700, BULGARIA SN 1313-2989 EI 1313-2970 J9 ZOOKEYS JI ZooKeys PY 2015 IS 520 BP 109 EP 130 DI 10.3897/zookeys.520.10134 PG 22 WC Zoology SC Zoology GA CT0UI UT WOS:000362512300006 PM 26448715 ER PT J AU Zattara, EE AF Zattara, E. E. TI Transplants in annelids, nemerteans and planarians: a tool for embryology, immunology, endocrinology and regeneration research SO ISJ-INVERTEBRATE SURVIVAL JOURNAL LA English DT Review DE transplantation; Annelida; Nemertea; Platyhelmintha; immunity; regeneration ID SPIRALIAN DEVELOPMENTAL PROGRAM; EISENIA FOETIDA TYPICA; D QUADRANT MICROMERES; NON-SELF RECOGNITION; GRAFT-REJECTION; NEREIS-DIVERSICOLOR; GROWTH-CONTROL; GENUS LINEUS; SEGMENT REGENERATION; CEREBRATULUS LACTEUS AB While transplantation procedures are often associated with biomedical applications, they are also an invaluable tool for basic research. This review focuses on how transplantation techniques have been used to understand the biology of three large lophotrochozoan phyla: Annelida, Nemertea and Platyhelmintha. I describe how transplantation paradigms have uncovered fundamental principles regarding the embryology, immunology, endocrinology and regeneration biology of representative species within these three groups. In particular, embryologists have used blastomere transplantations to show that both mosaic and regulative development occurs in animals within the phyla. Immunologists have used transplantation techniques to demonstrate that these invertebrates mount a variety of innate immune responses, some of which include surprising features that classically characterize adaptive immunity. Endocrinologists have used transplantation experiments to uncover hormonal requirements for sexual development and maturation. Meanwhile, regeneration biologists continue to address fundamental questions regarding tissue polarity, post-embryonic patterning, stem cell physiology, and the role of the nervous system in regeneration. Along with recent technical and conceptual advances, transplantation remains a powerful tool for invertebrate research. C1 Indiana Univ, Dept Biol, Smithsonian Inst, Natl Museum Nat Hist, Bloomington, IN 47405 USA. RP Zattara, EE (reprint author), Indiana Univ, Dept Biol, Smithsonian Inst, Natl Museum Nat Hist, 915 E Third St,Myers Hall 150, Bloomington, IN 47405 USA. EM ezattara@gmail.com RI Zattara, Eduardo/A-3760-2012 OI Zattara, Eduardo/0000-0002-9947-9036 NR 161 TC 1 Z9 1 U1 2 U2 7 PU INVERTEBRATE SURVIVAL JOURNAL PI MODENA PA C/O ENZO OTTAVIANI UNIV MODENA & REGGIO EMILIA, DEPT BIOLOGIA ANIMALE, VIA CAMPI, 213-D, MODENA, 41100, ITALY SN 1824-307X J9 ISJ-INVERT SURVIV J JI ISJ-Invertebr. Surviv. J. PY 2015 VL 12 BP 247 EP 263 PG 17 WC Immunology; Zoology SC Immunology; Zoology GA CT0KO UT WOS:000362484300004 ER PT J AU Hayashida, S Liu, X Ono, A Yang, K Chance, K AF Hayashida, S. Liu, X. Ono, A. Yang, K. Chance, K. TI Observation of ozone enhancement in the lower troposphere over East Asia from a space-borne ultraviolet spectrometer SO ATMOSPHERIC CHEMISTRY AND PHYSICS LA English DT Article ID SATELLITE MEASUREMENTS; MONITORING INSTRUMENT; STRATOSPHERIC OZONE; AIR-POLLUTION; COLUMN OZONE; CHINA; PROFILES; MTX2006; OMI; ALGORITHM AB We report observations from space using ultraviolet (UV) radiance for significant enhancement of ozone in the lower troposphere over central and eastern China (CEC). The recent retrieval products of the Ozone Monitoring Instrument (OMI) onboard the Earth Observing System (EOS) Aura satellite revealed the spatial and temporal variation of ozone distributions in multiple layers in the troposphere. We compared the OMI-derived ozone over Beijing with airborne measurements by the Measurement of Ozone and Water Vapor by Airbus In-Service Aircraft (MOZAIC) program. The correlation between OMI and MOZAIC ozone in the lower troposphere was reasonable, which assured the reliability of OMI ozone retrievals in the lower troposphere under enhanced ozone conditions. The ozone enhancement was clearly observed over CEC, with Shandong Province as its center, and was most notable in June in any given year. Similar seasonal variations were observed throughout the 9-year OMI measurement period of 2005 to 2013. A considerable part of this ozone enhancement could be attributed to the emissions of ozone precursors from industrial activities and automobiles, and possibly from open crop residue burning (OCRB) after the winter wheat harvest. The ozone distribution presented in this study is also consistent with some model studies. The lower tropospheric ozone distribution is first shown from OMI retrieval in this study, and the results will be useful in clarifying any unknown factors that influence ozone distribution by comparison with model simulations. C1 [Hayashida, S.; Ono, A.] Nara Womens Univ, Fac Sci, Nara 6308263, Japan. [Liu, X.; Chance, K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Yang, K.] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA. [Yang, K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Hayashida, S (reprint author), Nara Womens Univ, Fac Sci, Nara 6308263, Japan. EM sachiko@ics.nara-wu.ac.jp RI Liu, Xiong/P-7186-2014 OI Liu, Xiong/0000-0003-2939-574X FU European Commission; Green Network of Excellence, Environmental Information (GRENE-ei) program, MEXT, Japan; NASA; Smithsonian Institution FX We express our thanks to the European Commission for the support to the MOZAIC project (1994-2003), to partner institutions of the IAGOS Research Infrastructure (FZJ, DLR, MPI, and KIT in Germany; CNRS, CNES, and Meteo-France in France; and the University of Manchester in the United Kingdom), ETHER (CNES-CNRS/INSU) for hosting the database, and to participating airlines (Lufthansa, Air France, Austrian, China Airlines, Iberia, and Cathay Pacific) for transporting the instrumentation free of charge. We also express our gratitude to H. Araki and M. Nakazawa for their help with the data analysis and creation of figures, and to Yugo Kanaya for his helpful comments on MTX2006. S. Hayashida and A. Ono were supported by a Grant-in-Aid from the Green Network of Excellence, Environmental Information (GRENE-ei) program, MEXT, Japan. X. Liu and K. Chance were supported by NASA and the Smithsonian Institution. NR 42 TC 2 Z9 2 U1 2 U2 18 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 2015 VL 15 IS 17 BP 9865 EP 9881 DI 10.5194/acp-15-9865-2015 PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CR7YH UT WOS:000361567600008 ER PT B AU Munroe, TA AF Munroe, Thomas A. BE Gibson, RN Nash, RDM Geffen, AJ VanDerVeer, HW TI Systematic diversity of the Pleuronectiformes SO FLATFISHES: BIOLOGY AND EXPLOITATION, 2ND EDITION LA English DT Article; Book Chapter DE Flatfish diversity; species accumulation; species discovery; pleuronectiform diversity; Pleuronectiformes; flatfish systematics; flatfish taxonomy; flatfish fossils; flatfish diversification; latitudinal diversity gradients ID SCOPHTHALMID FISHES PLEURONECTIFORMES; SYMPHURINE TONGUEFISHES SYMPHURUS; SPECIES ALIAS PROBLEM; WEST PACIFIC-OCEAN; SP-NOV SAMARIDAE; NEW-CALEDONIA; TELEOSTEI PLEURONECTIFORMES; GENUS ASERAGGODES; RIGHTEYE FLOUNDER; FLATFISHES TELEOSTEI AB The evolutionary history of flatfishes dates back to the early Tertiary. Currently, 14 families and 123 genera are recognised in this third most diverse order of marine euteleosts. Of 1363 nominal species described or currently recognized by taxonomists, 822 are valid. A species accumulation curve for flatfishes reveals that we are not yet close to knowing the total diversity of this group. Since 2000, approximately 10% of flatfish diversity was described and another 4% recognized as new to science. Species-rich families include Soleidae, Cynoglossidae and Bothidae. Geographic occurrence, size and distributions of species, and activities of systematists influence rates of species discovery. Species accumulation curves for flatfishes inhabiting temperate and Arctic regions indicate species discoveries still occur there but at much slower rates than for flatfishes of tropical waters. Considerable diversity remains to be discovered in tropical marine waters and flatfish taxonomy continues to be an active area of research. C1 NOAA, Natl Systemat Lab, NMFS, Smithsonian Inst,NHB, Washington, DC 20113 USA. RP Munroe, TA (reprint author), NOAA, Natl Systemat Lab, NMFS, Smithsonian Inst,NHB, POB 37012 WC 60 MRC 153, Washington, DC 20113 USA. EM munroet@si.edu NR 139 TC 2 Z9 2 U1 0 U2 0 PU JOHN WILEY & SONS LTD PI CHICHESTER PA THE ATRIUM, SOUTHERN GATE, CHICHESTER PO19 8SQ, WEST SUSSEX, ENGLAND BN 978-1-118-50115-3; 978-1-118-50119-1 PY 2015 BP 13 EP 51 PG 39 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA BD5UQ UT WOS:000361829300003 ER PT B AU Munroe, TA AF Munroe, Thomas A. BE Gibson, RN Nash, RDM Geffen, AJ VanDerVeer, HW TI Distributions and biogeography SO FLATFISHES: BIOLOGY AND EXPLOITATION, 2ND EDITION LA English DT Article; Book Chapter DE Flatfish distribution; ecological distribution; latitudinal gradients; geographical distribution of flatfishes; species diversity estimates; point diversity estimates; flatfish biogeography; flatfish depth distribution ID CORAL-REEF FISHES; EASTERN PACIFIC-OCEAN; GOMEZ SUBMARINE RIDGE; INDO-WEST PACIFIC; SP-NOV SAMARIDAE; POPULATION-GENETICS; NEW-CALEDONIA; HISTORICAL BIOGEOGRAPHY; TONGUEFISH PLEURONECTIFORMES; PISCES PLEURONECTIFORMES AB Flatfishes inhabit marine, estuarine and freshwater environments from the southern Arctic Ocean to continental seas off Antarctica. Geographical and ecological distributions reveal distinctly asymmetrical global patterns of flatfish species diversity. The greatest diversity is found in marine waters of the Indo-West Pacific; other tropical seas support fewer species (diversity decreases progressively from western Atlantic, tropical Eastern Pacific, to Eastern Atlantic, respectively). Fewer species inhabit temperate waters, while the least diverse flatfish assemblages are in northern and southern polar waters and at isolated islands. Ecologically, flatfishes range from estuaries to the outer continental shelf and upper continental slope to about 2000 m. Notable differences in diversity occur between continental and insular locations. Few species inhabit freshwaters. Maximal species richness within regions occurs on extensive continental shelves featuring complex shallow-water (< 200 m) habitats. Phylogenetic studies of interrelationships and intrarelationships of flatfishes are currently insufficient for analyses of their historical biogeography. C1 NOAA, NMFS, Natl Systemat Lab, Smithsonian Inst,NHB, Washington, DC 20113 USA. RP Munroe, TA (reprint author), NOAA, NMFS, Natl Systemat Lab, Smithsonian Inst,NHB, POB 37012 WC 60 MRC 153, Washington, DC 20113 USA. EM munroet@si.edu NR 115 TC 1 Z9 1 U1 1 U2 1 PU JOHN WILEY & SONS LTD PI CHICHESTER PA THE ATRIUM, SOUTHERN GATE, CHICHESTER PO19 8SQ, WEST SUSSEX, ENGLAND BN 978-1-118-50115-3; 978-1-118-50119-1 PY 2015 BP 52 EP 82 PG 31 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA BD5UQ UT WOS:000361829300004 ER EF