FN Thomson Reuters Web of Science™ VR 1.0 PT J AU Curtin, AJ Zug, GR Spotila, JR AF Curtin, A. J. Zug, G. R. Spotila, J. R. TI Longevity and growth strategies of the desert tortoise (Gopherus agassizii) in two American deserts SO JOURNAL OF ARID ENVIRONMENTS LA English DT Article DE Age; Life history; Sexual maturity; Skeletochronology; Southwestern United States; Testudines ID AGE-SIZE RELATIONSHIPS; VARANUS-NILOTICUS; SOUTHERN NEVADA; EGG-PRODUCTION; SEA-TURTLES; BODY-SIZE; MATURITY; BONE; SKELETOCHRONOLOGY; TEMPERATURE AB The desert tortoise occurs in two strikingly different desert regimes in the southwestern United States In. the Mojave Desert, rainfall is more irregular and resources are more limited than in the Sonoran Desert. We examined the age structure of tortoise populations from these two deserts to determine whether the difference in resource availability has driven an evolutionary divergence in life history strategies, Age and growth rates strongly reflect the ecological adaptation of the two populations. The oldest Sonoran males reached 54 years, compared to only 43 years in females. The oldest West Mojave (WM) males reached 56 years, compared to only 27 years in females. WM tortoises grew faster than Sonoran ones, and females reached sexual maturity at earlier ages (similar to 17-19 years) than Sonoran females (similar to 22-26 years). These traits and the higher rate of clutch production in the WM population are likely the evolutionary adaptation for low juvenile survivorship and a significantly shorter life span. Frequent droughts in the WM Desert and the lowest annual rainfall area within the range of the desert tortoise cause chronic physiological stress, likely annually, and are proposed as a major selection force producing contrasting life-history strategies. (C) 2008 Elsevier Ltd. All rights reserved. C1 [Curtin, A. J.; Spotila, J. R.] Drexel Univ, Dept Biosci & Biotechnol, Philadelphia, PA 19104 USA. [Zug, G. R.] Natl Museum Nat Hist, Dept Vertebrate Zool, Smithsonian Inst, Washington, DC 20013 USA. RP Curtin, AJ (reprint author), Duke Univ, Acad Resource Ctr, Box 90694, Durham, NC 27708 USA. EM amanda.curtin@duke.edu; zugg@si.edu; spotiljr@drexel.edu FU Panaphil Foundation Fellowship FX We gratefully acknowledge funding provided by a Panaphil Foundation Fellowship to A.J. Curtin. We are also grateful to Dr William Boarman and the US Geological Society for donating the West Mojave Desert tortoise carcasses, and Roy Averill-Murray and the Arizona Game and Fish Department for donating the Sonoran Desert tortoise carcasses used in this study. We also thank Dr Mike O'Connor and especially Dr Hal Avery for comments on earlier drafts of this manuscript and for valuable discussions and insights on desert tortoise ecology. NR 58 TC 16 Z9 16 U1 6 U2 32 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0140-1963 J9 J ARID ENVIRON JI J. Arid. Environ. PD APR-MAY PY 2009 VL 73 IS 4-5 BP 463 EP 471 DI 10.1016/j.jaridenv.2008.11.011 PG 9 WC Ecology; Environmental Sciences SC Environmental Sciences & Ecology GA 425CJ UT WOS:000264614300010 ER PT J AU Bellwood, DR Meyer, CP AF Bellwood, David R. Meyer, Christopher P. TI Searching for heat in a marine biodiversity hotspot SO JOURNAL OF BIOGEOGRAPHY LA English DT Editorial Material DE Biodiversity; conservation biogeography; coral reef; coral triangle; cowries; endemism; fishes; molecular phylogenetics; species ages; species origins ID INDO-PACIFIC; CORAL-REEFS; MOLECULAR SYSTEMATICS; LINEAGE DIVERSIFICATION; HISTORICAL BIOGEOGRAPHY; CONSERVATION PRIORITIES; FISH BIODIVERSITY; PATTERNS; DIVERSITY; PHYLOGEOGRAPHY AB Coral reefs exhibit highly congruent patterns of biodiversity, with a prominent hotspot in the Indo-Australian Archipelago (IAA). Unlike many terrestrial systems, the IAA hotspot exhibits extensive latitudinal and longitudinal biodiversity gradients. Conflicting hypotheses have highlighted the importance of the area as a centre of origin, overlap or accumulation, with the location of endemics being used as the primary criterion for testing these hypotheses, by identifying the presumed geographical origins of species. We evaluate the utility of marine endemics for resolving these hypotheses, and examine recent molecular phylogenetic evidence for coral reef species that has revealed the antiquity of the endemics and the other species that make up this hotspot. These analyses emphasize the importance of the IAA in the survival rather than the origins of species. C1 [Bellwood, David R.] James Cook Univ, Sch Marine & Trop Biol, Townsville, Qld 4811, Australia. [Bellwood, David R.] James Cook Univ, Australian Res Council, Ctr Excellence Coral Reef Studies, Townsville, Qld 4811, Australia. [Meyer, Christopher P.] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. RP Bellwood, DR (reprint author), James Cook Univ, Sch Marine & Trop Biol, Townsville, Qld 4811, Australia. EM david.bellwood@jcu.edu.au NR 65 TC 58 Z9 58 U1 2 U2 45 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0305-0270 J9 J BIOGEOGR JI J. Biogeogr. PD APR PY 2009 VL 36 IS 4 BP 569 EP 576 DI 10.1111/j.1365-2699.2008.02029.x PG 8 WC Ecology; Geography, Physical SC Environmental Sciences & Ecology; Physical Geography GA 417JV UT WOS:000264073200001 ER PT J AU Grossman, RB Schneps, MH Tager-Flusberg, H AF Grossman, Ruth B. Schneps, Matthew H. Tager-Flusberg, Helen TI Slipped lips: onset asynchrony detection of auditory-visual language in autism SO JOURNAL OF CHILD PSYCHOLOGY AND PSYCHIATRY LA English DT Article DE Autism; AV-integration; language; autistic disorder; communication; language; face; voice ID HIGH-FUNCTIONING AUTISM; SPEECH-PERCEPTION; SHIFTING ATTENTION; ASPERGERS-SYNDROME; SPECTRUM DISORDER; INTEGRATION; INDIVIDUALS; RECOGNITION; SYNCHRONY; SENTENCES AB It has frequently been suggested that individuals with autism spectrum disorder (ASD) have deficits in auditory-visual (AV) sensory integration. Studies of language integration have mostly used non-word syllables presented in congruent and incongruent AV combinations and demonstrated reduced influence of visual speech in individuals with ASD. The aim of our study was to test whether adolescents with high-functioning autism are able to integrate AV information of meaningful, phrase-length language in a task of onset asynchrony detection. Participants were 25 adolescents with ASD and 25 typically developing (TD) controls. The stimuli were video clips of complete phrases using simple, commonly occurring words. The clips were digitally manipulated to have the video precede the corresponding audio by 0, 4, 6, 8, 10, 12, or 14 video frames, a range of 0-500ms. Participants were shown the video clips in random order and asked to indicate whether each clip was in-synch or not. There were no differences between adolescents with ASD and their TD peers in accuracy of onset asynchrony detection at any slip rate. These data indicate that adolescents with ASD are able to integrate auditory and visual components in a task of onset asynchrony detection using natural, phrase-length language stimuli. We propose that the meaningful nature of the language stimuli in combination with presentation in a non-distracting environment allowed adolescents with autism spectrum disorder to demonstrate preserved accuracy for bi-modal AV integration. C1 [Grossman, Ruth B.; Tager-Flusberg, Helen] Boston Univ, Sch Med, Lab Dev Cognit Neurosci, Boston, MA 02118 USA. [Schneps, Matthew H.] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Grossman, RB (reprint author), Boston Univ, Sch Med, Lab Dev Cognit Neurosci, 715 Albany St,L-814, Boston, MA 02118 USA. EM ruthberg@bu.edu RI Tager-Flusberg, Helen/D-5265-2009 FU NAAR; NIDCD [U19 DC03610]; NICHD/NIDCD Collaborative Programs of Excellence in Autism; General Clinical Research Ctr [M01-RR00533]; National Center for Research Resources; National Institutes of Health FX Funding was provided by NAAR, NIDCD (U19 DC03610; H. Tager-Flusberg, PI) which is part of the NICHD/NIDCD Collaborative Programs of Excellence in Autism, and by grant M01-RR00533 from the General Clinical Research Ctr. program of the National Center for Research Resources, National Institutes of Health. NR 40 TC 10 Z9 10 U1 0 U2 8 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0021-9630 J9 J CHILD PSYCHOL PSYC JI J. Child Psychol. Psychiatry PD APR PY 2009 VL 50 IS 4 BP 491 EP 497 DI 10.1111/j.1469-7610.2008.02002.x PG 7 WC Psychology, Developmental; Psychiatry; Psychology SC Psychology; Psychiatry GA 424KB UT WOS:000264564500014 PM 19207623 ER PT J AU Dowling, DK Maklakov, AA Friberg, U Hailer, F AF Dowling, D. K. Maklakov, A. A. Friberg, U. Hailer, F. TI Applying the genetic theories of ageing to the cytoplasm: cytoplasmic genetic covariation for fitness and lifespan SO JOURNAL OF EVOLUTIONARY BIOLOGY LA English DT Article DE ageing; antagonistic pleiotropy; cytoplasm; Drosophila melanogaster; mitochondria; mtDNA; mutation accumulation; senescence ID AGE-SPECIFIC MORTALITY; MITOCHONDRIAL-DNA MUTATIONS; DROSOPHILA-MELANOGASTER; ANTAGONISTIC PLEIOTROPY; NATURAL-SELECTION; OXIDATIVE STRESS; EVOLUTIONARY GENETICS; HISTORY; NUCLEAR; SENESCENCE AB Two genetic models exist to explain the evolution of ageing - mutation accumulation (MA) and antagonistic pleiotropy (AP). Under MA, a reduced intensity of selection with age results in accumulation of late-acting deleterious mutations. Under AP, late-acting deleterious mutations accumulate because they confer beneficial effects early in life. Recent studies suggest that the mitochondrial genome is a major player in ageing. It therefore seems plausible that the MA and AP models will be relevant to genomes within the cytoplasm. This possibility has not been considered previously. We explore whether patterns of covariation between fitness and ageing across 25 cytoplasmic lines, sampled from a population of Drosophila melanogaster, are consistent with the genetic associations predicted under MA or AP. We find negative covariation for fitness and the rate of ageing, and positive covariation for fitness and lifespan. Notably, the direction of these associations is opposite to that typically predicted under AP. C1 [Dowling, D. K.] Univ Western Australia, Sch Anim Biol, Ctr Evolutionary Biol, Crawley, WA 6009, Australia. [Maklakov, A. A.] Uppsala Univ, Dept Ecol & Evolut, Evolutionary Biol Ctr, Uppsala, Sweden. [Maklakov, A. A.] Univ New S Wales, Sch Biol Earth & Environm Sci, Sydney, NSW, Australia. [Friberg, U.] Univ Calif Santa Barbara, Dept Ecol Evolut & Marine Biol, Santa Barbara, CA 93106 USA. [Hailer, F.] Smithsonian Inst, Natl Zool Pk, Ctr Conservat & Evolutionary Genet, Washington, DC 20008 USA. [Hailer, F.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20008 USA. RP Dowling, DK (reprint author), Univ Western Australia, Sch Anim Biol, Ctr Evolutionary Biol, M092, Crawley, WA 6009, Australia. EM damiankd@cyllene.uwa.edu.au RI Dowling, Damian/C-9016-2009; Friberg, Urban/H-4569-2011; Hailer, Frank/C-9114-2012; Maklakov, Alexei/F-8167-2014; Friberg, Urban/C-9412-2015 OI Dowling, Damian/0000-0003-2209-3458; Hailer, Frank/0000-0002-2340-1726; Friberg, Urban/0000-0001-6112-9586 FU University of Western Australia; Wenner-Gren Foundations postdoctoral scholarship; Swedish Institute Guest scholarship; Marie Curie postdoctoral fellowship [MEIF-CT-2003-505891] FX We thank Goran Arnqvist for his valuable discussions on the manuscript, and two anonymous referees for their insightful comments. D.K.D. was supported by a Wenner-Gren Foundations postdoctoral scholarship, Swedish Institute Guest scholarship and the University of Western Australia; A.A.M. by a Marie Curie postdoctoral fellowship (MEIF-CT-2003-505891); U.F. by a Wenner-Gren Foundations fellowship and a stipend from Lennander's Foundation and research grants from Magn. Bergvalls Stiftelse and Stiftelsen Lars Hiertas Minne; and F.H. by the Marine Science Network and James Bond Fund of the Smithsonian Institution, TL Cross and Seabird Research. NR 71 TC 10 Z9 10 U1 0 U2 11 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1010-061X J9 J EVOLUTION BIOL JI J. Evol. Biol. PD APR PY 2009 VL 22 IS 4 BP 818 EP 827 DI 10.1111/j.1420-9101.2009.01692.x PG 10 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 418YM UT WOS:000264186000015 PM 19226414 ER PT J AU Buzas, M AF Buzas, Marty TI MEMORIAL TO DORIS L. LOW (1920-2008) SO JOURNAL OF FORAMINIFERAL RESEARCH LA English DT Biographical-Item C1 Smithsonian Inst, Washington, DC 20013 USA. RP Buzas, M (reprint author), Smithsonian Inst, Washington, DC 20013 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU CUSHMAN FOUNDATION FORAMINIFERAL RES PI CAMBRIDGE PA MUSEUM COMPARATIVE ZOOLOGY, DEPT INVERTEBRATE PALEONTOLOGY 26 OXFORD ST, HARVARD UNIV, CAMBRIDGE, MA 02138 USA SN 0096-1191 J9 J FORAMIN RES JI J. Foraminifer. Res. PD APR PY 2009 VL 39 IS 2 BP 140 EP 140 PG 1 WC Paleontology SC Paleontology GA 441YK UT WOS:000265806300007 ER PT J AU Sosa-Calvo, J Brady, SG Schultz, TR AF Sosa-Calvo, Jeffrey Brady, Sean G. Schultz, Ted R. TI The Gyne of the Enigmatic Fungus-Farming Ant Species Mycetosoritis explicata SO JOURNAL OF HYMENOPTERA RESEARCH LA English DT Article DE Attini; Mycetosoritis; Myrmicinae; Neotropics; taxonomy ID GROWING ANTS AB We describe for the first time the gyne of the Neotropical fungus-farming ant Mycetosoritis explicata, a species hitherto known from only two workers collected in Goias State, Brazil, in 1968. A redescription of the worker is presented. The likely non-monophyly of the genus Mycetosoritis and the possible position of the constituent species within the tribe Attini are discussed. C1 [Sosa-Calvo, Jeffrey; Brady, Sean G.; Schultz, Ted R.] Natl Museum Nat Hist, Dept Entomol, Smithsonian Inst, Washington, DC 20013 USA. [Sosa-Calvo, Jeffrey] Univ Maryland, Dept Entomol, Maryland Ctr Systemat Entomol, College Pk, MD 20742 USA. RP Schultz, TR (reprint author), Natl Museum Nat Hist, Dept Entomol, Smithsonian Inst, POB 37012,CE516,MRC 188, Washington, DC 20013 USA. FU National Science Foundation [IRCEB DEB 0110073, EF-0431330]; Museum of Comparative Zoology; University of Maryland FX We thank the collection of the Reserva Ecologica do Instituto Brasileiro de Geografia e Estatistica (IBGE), Jacques Delabie, and Roberto C.F. Brandao for loaning specimens; Eduardo Sanhudo and Jorge L.M. Diniz for useful information regarding the species; and Scott Whitaker (USNM) for assistance with the scanning electronic micrographs. This work was supported by National Science Foundation grants IRCEB DEB 0110073 to TRS and EF-0431330 to SGB and TRS. Additional funding was provided by the Ernst Mayr Travel Grant in Animal Systematics (Museum of Comparative Zoology) and the Jacob K. Goldhaber Travel Award (University of Maryland) to JSC. We are grateful to an anonymous reviewer for helpful comments on a previous version of the manuscript. NR 17 TC 1 Z9 1 U1 0 U2 1 PU INT SOC HYMENOPTERISTS PI MADISON PA C/O CRAIG BRABANT, TREAS, DEPT ENTOMOLOGY, 1630 LINDEN DR, RM 445, MADISON, WI 53706 USA SN 1070-9428 J9 J HYMENOPT RES JI J. Hymenopt. Res. PD APR PY 2009 VL 18 IS 1 BP 113 EP 120 PG 8 WC Entomology SC Entomology GA 700WQ UT WOS:000285775400005 ER PT J AU Helgen, KM Cole, FR Helgen, LE Wilson, DE AF Helgen, Kristofer M. Cole, F. Russell Helgen, Lauren E. Wilson, Don E. TI GENERIC REVISION IN THE HOLARCTIC GROUND SQUIRREL GENUS SPERMOPHILUS SO JOURNAL OF MAMMALOGY LA English DT Review DE biogeography; cytochrome b; genus; ground squirrels; morphology; morphometrics; phylogeny; Spermophilus; systematics; taxonomy ID SUBGENUS XEROSPERMOPHILUS; RODENTIA-SCIURIDAE; TRIDECEMLINEATUS; PHYLOGENY; DIFFERENTIATION; CHROMOSOMES; MEXICANUS; HYBRIDIZATION; SYSTEMATICS; ICTIDOMYS AB The substantial body of research on Holarctic ground squirrels amassed over the past century documents considerable variability in morphological, cytogenetic, ecological, and behavioral attributes in the genus Spermophilus F. Cuvier, 1825. Recent molecular phylogenetic studies suggest that the traditionally recognized genera Marmota Blumenbach, 1779 (marmots), Cynomys Rafinesque, 1817 (prairie dogs), and Ammospermophilus Merriam, 1892 (antelope ground squirrels) render Spermophilus paraphyletic, potentially suggesting that multiple generic-level lineages should be credited within Spermophilus. Herein, we recognize 8 genera formerly subsumed in Spermophilus, each of which is morphologically diagnosable, craniometrically distinctive, and recovered as a monophyletic clade in phylogenetic analyses utilizing the mitochondrial gene cytochrome b. Generic-level names are available for each of these ground squirrel assemblages, most of which are exclusively or predominantly North American in distribution (Notocitellus A. H. Howell, 1938; Otospermophilus Brandt, 1844; Callospermophilus Merriam, 1897; Ictidomys J. A. Allen, 1877; Poliocitellus A. H. Howell, 1938; Xerospermophilus Merriam, 1892; and Urocitellus Obolenskij, 1927). Only Spermophilus sensu stricto is restricted to Eurasia. Generic subdivision of Spermophilus more aptly illuminates the taxonomic relationships, ecomorphological disparity, and biogeographic history of Holarctic ground squirrels. C1 [Helgen, Kristofer M.; Wilson, Don E.] Smithsonian Inst, Natl Museum Nat Hist, Div Mammals, Washington, DC 20013 USA. [Cole, F. Russell] Colby Coll, Dept Biol, Waterville, ME 04901 USA. [Helgen, Lauren E.] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20013 USA. RP Helgen, KM (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Div Mammals, POB 37012, Washington, DC 20013 USA. EM helgenk@si.edu; wilsond@si.edu FU Smithsonian Institution; Colby College; Oak Foundation FX This paper is dedicated to our friend and colleague Robert S. Hoffmann. We gratefully acknowledge the logistical support, collection access, and advice provided by staff and researchers in the Division of Mammals at USNM, including R. Hoffmann, R. Thorington, S. Peurach, R. Fisher, L. Gordon, C. Ludwig, H. Kafka, J. Whatton, J. Jacobs, D. Schmidt, A. Gardner, M. Carleton, L. Emmons, J. Mead, and C. Potter. We also thank M. Herron and an anonymous reviewer for helpful reviews of our manuscript, J. Matson for helpful discussion, and B. Gunnell, E. Robinson, M. Wells, and J. van Veldhuizen for assistance in recurating the USNM ground squirrel collection. This project was supported by a Postdoctoral Fellowship from the Smithsonian Institution to KMH and funding from Colby College and the Oak Foundation provided to FRC during a sabbatical leave. NR 152 TC 95 Z9 107 U1 2 U2 30 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 APR PY 2009 VL 90 IS 2 BP 270 EP 305 DI 10.1644/07-MAMM-A-309.1 PG 36 WC Zoology SC Zoology GA 434YH UT WOS:000265309700002 ER PT J AU Calderon, I Turon, X Lessios, HA AF Calderon, Isabel Turon, Xavier Lessios, H. A. TI Characterization of the Sperm Molecule Bindin in the Sea Urchin Genus Paracentrotus SO JOURNAL OF MOLECULAR EVOLUTION LA English DT Article DE Bindin; PAML; Paracentrotus; Positive selection; Sea urchins; Speciation ID POSITIVE DARWINIAN SELECTION; AMINO-ACID SITES; GAMETE RECOGNITION PROTEINS; ADAPTIVE EVOLUTION; REPRODUCTIVE ISOLATION; RAPID EVOLUTION; MEMBRANE-FUSION; FERTILIZATION; SPECIATION; SEQUENCE AB Bindin is a sea urchin gamete-recognition protein that plays an essential role in the specificity of egg-sperm interactions and thus may be evolving under sexual selection and be related to speciation. Bindin has been found to evolve under strong selection in some sea urchin genera and neutrally in others. In this study, we characterized bindin in the two extant species of the genus Paracentrotus: P. lividus from the Atlanto-Mediterranean region and P. gaimardi from Brazil. The structure of the bindin molecule in Paracentrotus is similar to that of other genera studied thus far, consisting of a conserved core flanked by two variable regions and an intron of variable length located at the same conserved position as in other genera. Polymorphism in P. lividus is caused mainly by point substitutions and insertions/deletions, and length variations are caused mainly by the number of repeated motifs in the flanking regions. There is no evidence of recombination. Positive selection is acting on amino acid sites located in two regions flanking the conserved core. C1 [Calderon, Isabel] Univ Barcelona, Fac Biol, Dept Anim Biol, E-08028 Barcelona, Spain. [Turon, Xavier] CSIC, CEAB, Ctr Adv Studies Blanes, Blanes, Girona, Spain. [Lessios, H. A.] Smithsonian Trop Res Inst, Balboa, Panama. RP Calderon, I (reprint author), Univ Barcelona, Fac Biol, Dept Anim Biol, E-08028 Barcelona, Spain. EM calderon@ub.edu RI Turon, Xavier/J-9211-2012 OI Turon, Xavier/0000-0002-9229-5541 FU Spanish Government [CTM2007-66635]; Smithsonian Tropical Research Institute FX Special thanks to Axel and Ligia Calderon of STRI-Naos for their help in the laboratory. Thanks to Laura Geyer for providing useful comments on the manuscript. This research was funded by Project No. CTM2007-66635 of the Spanish Government and by general research funds from the Smithsonian Tropical Research Institute. NR 71 TC 15 Z9 16 U1 0 U2 6 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0022-2844 J9 J MOL EVOL JI J. Mol. Evol. PD APR PY 2009 VL 68 IS 4 BP 366 EP 376 DI 10.1007/s00239-009-9219-4 PG 11 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 432PF UT WOS:000265145500006 PM 19330367 ER PT J AU Tamura, Y Gill, JB Tollstrup, D Kawabata, H Shukuno, H Chang, Q Miyazaki, T Takahashi, T Hirahara, Y Kodaira, S Ishizuka, O Suzuki, T Kido, Y Fiske, RS Tatsumi, Y AF Tamura, Yoshihiko Gill, James B. Tollstrup, Darren Kawabata, Hiroshi Shukuno, Hiroshi Chang, Qing Miyazaki, Takashi Takahashi, Toshiro Hirahara, Yuka Kodaira, Shuichi Ishizuka, Osamu Suzuki, Toshihiro Kido, Yukari Fiske, Richard S. Tatsumi, Yoshiyuki TI Silicic Magmas in the Izu-Bonin Oceanic Arc and Implications for Crustal Evolution SO JOURNAL OF PETROLOGY LA English DT Article DE arc volcano; hot fingers; middle crust; REE; rhyolite; Sr-Nd-Pb isotope ID ANDESITE MAGMA; KERMADEC ARC; ISOTOPE GEOCHEMISTRY; PYROCLASTIC DEBRIS; CONTINENTAL-CRUST; INTRAOCEANIC ARC; MARIANA ISLANDS; VOLCANIC-ROCKS; CENTRAL JAPAN; SUMISU RIFT AB Abundant rhyolite has erupted from the Izu-Bonin-Mariana volcanic arc (IBM arc) from its earliest stage (Eocene) to the present. Geochemically, three types of Quaternary rhyolites exist in the Izu-Bonin arc front, and they are closely related to volcano type and crustal structure. The dominantly basaltic islands of the volcanic front produce small volumes of rhyolites that we call R1. The submarine calderas of the volcanic front erupt mostly rhyolite that we call R2. Seamounts, knolls, and pillow ridges in the backarc extensional zone are mostly basaltic but also contain rhyolites that we call R3. The thickest total crust, and the thickest intermediate composition middle crust, occurs below the dominantly basaltic volcanoes, whereas the intermediate composition middle crust tends to be thinner beneath the submarine calderas. R1 rhyolites may be derived from Quaternary andesitic sources whereas R2 and R3 rhyolites may be derived from Oligocene ones. The higher CaO/Al2O3 in R1 compared with R2 and R3 rhyolites can be attributed to the same difference between Quaternary and Oligocene andesite sources, respectively. Light rare earth element (LREE)-depleted REE patterns of Quaternary andesites versus flat to slightly LREE-enriched patterns of Oligocene andesites are almost parallel to those of R1 and R2, respectively. Partial melts of Quaternary andesite will have low Zr/Y values such as in R1, whereas melts of Oligocene andesites will have the higher Zr/Y values of R2. Lavas from basalt-dominant volcanoes have higher Sr, Pb, and sometimes Nd isotope ratios than those from rhyolite-dominated volcanoes, which are closer to the isotope ratios of the Oligocene arc. Why and how do crustal sources differ systematically and alternately along and behind the Izu-Bonin arc ? If locally developed regions within the mantle wedge (hot fingers) produce large basaltic volcanoes and remain stationary for millions of years, then basalt-dominant volcanoes eventually will overlie thicker crust. Remelting of middle crust to form rhyolite magmas takes place beneath both basaltic and rhyolitic volcanoes (R1 and R2 rhyolite, respectively). However, basalt volcanoes consume new middle crust to produce rhyolite magma whereas rhyolite volcanoes consume old Oligocene middle crust. Moreover, rhyolite volcanoes have no mantle roots beneath the crust. Instead, dikes from basalt volcanoes provide the heat source to partially melt the crust. C1 [Tamura, Yoshihiko; Kawabata, Hiroshi; Shukuno, Hiroshi; Chang, Qing; Miyazaki, Takashi; Takahashi, Toshiro; Hirahara, Yuka; Kodaira, Shuichi; Suzuki, Toshihiro; Tatsumi, Yoshiyuki] Japan Agcy Marine Earth Sci & Technol, IFREE, Yokosuka, Kanagawa 2370061, Japan. [Tamura, Yoshihiko; Gill, James B.; Tollstrup, Darren] Univ Calif Santa Cruz, Santa Cruz, CA 95064 USA. [Ishizuka, Osamu] Geol Survey Japan AIST, Inst Geosci, Tsukuba, Ibaraki 3058567, Japan. [Kido, Yukari] Japan Agcy Marine Earth Sci & Technol, Ctr Deep Earth Explorat, Kanazawa Ku, Yokohama, Kanagawa 2360001, Japan. [Fiske, Richard S.] Smithsonian Inst, NMNH, Washington, DC 20013 USA. RP Tamura, Y (reprint author), Japan Agcy Marine Earth Sci & Technol, IFREE, 2-15 Natsushimacho, Yokosuka, Kanagawa 2370061, Japan. EM tamuray@jamstec.go.jp FU NSF MARGINS program [OCE0325189]; JSPS [17340165, 20340122]; [19GS0211] FX This work was supported in part by the NSF MARGINS program, award OCE0325189, the JSPS Grant-in-Aid for Scientific Research (B) (17340165 and 20340122) and Grant-in-Aid for Creative Scientific Research (19GS0211). This work was made possible by the exchange visits of Y. Tamura and J. Gill between IFREE/JAMSTEC and UCSC. We are indebted to Captain F. Saito, the crews of R. V. Natsushima, K. Chiba and the operation team of ROV Hyper-Dolphin during JAMSTEC NT06-21 cruise. We thank J. Blundy, C. Macpherson and I. Smith for careful and insightful reviews, and J. Gamble for editorial help. NR 66 TC 48 Z9 48 U1 1 U2 10 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0022-3530 J9 J PETROL JI J. Petrol. PD APR PY 2009 VL 50 IS 4 BP 685 EP 723 DI 10.1093/petrology/egp017 PG 39 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 444AX UT WOS:000265953300007 ER PT J AU Place, AR Bai, XM Kim, SJ Sengco, MR Coats, DW AF Place, Allen R. Bai, Xuemei Kim, Sunju Sengco, Mario R. Coats, D. Wayne TI DINOFLAGELLATE HOST-PARASITE STEROL PROFILES DICTATE KARLOTOXIN SENSITIVITY SO JOURNAL OF PHYCOLOGY LA English DT Article DE Amoebophyra; Karlodinium; karlotoxin; parasite; sterols ID KARLODINIUM-MICRUM; AMOEBOPHRYA DINOPHYTA; KARENIA-BREVIS; FATTY-ACID; STRAINS; VENEFICUM; TOXINS; PHYTOPLANKTON; SPECIFICITY; PATTERNS AB We examined the sterol profile of Karlodinium veneficum (D. Ballant.) J. Larsen, Akashiwo sanguinea (Hiraska) Ge. Hansen et Moestrup, Alexandrium tamarense (M. Lebour) Balech, Alexandrium affine (H. Inoue et Fukuyo) Balech, Gonyaulax polygramma F. Stein, and Gymnodinium instriatum (Freud. et J. J. Lee) Coats, along with their Amoebophyra parasites. There were no consistent sterol profiles that characterized the genus Amoebophyra. Instead, in five out of six comparisons, the host and parasite sterol profiles where highly correlated. The one exception, Amoebophyra sp. ex Alex. tamarense, was least like its host in sterol profile and also possessed the widest host range for infection. There was little correlation between host and parasite in fatty acid profiles, with the parasite being deficient in fatty acids characteristic of the plastid [e.g., 18:5(n-3) associated with galactolipids of the thylakoids, as previously published by Adolf et al. (2007)]. Those hosts and parasites with sterol profiles dominated by desmethyl sterols were most sensitive to karlotoxin toxicity. In the host-parasite pairs most sensitive to karlotoxin addition, recovery of the intact karlotoxin molecule was poorest. Given the sensitivity to karlotoxin, some species of Amoebophyra may avoid infection of K. veneficum. C1 [Place, Allen R.] Univ Maryland, Ctr Marine Biotechnol, Inst Biotechnol, Baltimore, MD 21202 USA. [Bai, Xuemei; Kim, Sunju; Sengco, Mario R.; Coats, D. Wayne] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Place, AR (reprint author), Univ Maryland, Ctr Marine Biotechnol, Inst Biotechnol, 701 E Pratt St, Baltimore, MD 21202 USA. EM place@umbi.umd.edu RI Place, Allen/F-9267-2013 FU University of Maryland Biotechnology Institute [NA04NOS4780276]; Smithsonian Institution [NA05NOS4781193]; Centers for Disease Control and Prevention [U50/CCU 323376]; Maryland Department of Health and Mental Hygiene; Smithsonian Postdoctoral Fellowships; ECOHAB program [279] FX This study is partially a result of research funded by the National Oceanic and Atmospheric Administration Coastal Ocean Program under award #NA04NOS4780276 to University of Maryland Biotechnology Institute and #NA05NOS4781193 to the Smithsonian Institution, Grant # U50/CCU 323376, Centers for Disease Control and Prevention and the Maryland Department of Health and Mental Hygiene, and Smithsonian Postdoctoral Fellowships to X. Bai and S. Kim. This is contribution # 08-184 from the Center of Marine Biotechnology and contribution # 279 from the ECOHAB program. NR 50 TC 13 Z9 14 U1 0 U2 3 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0022-3646 J9 J PHYCOL JI J. Phycol. PD APR PY 2009 VL 45 IS 2 BP 375 EP 385 DI 10.1111/j.1529-8817.2009.00649.x PG 11 WC Plant Sciences; Marine & Freshwater Biology SC Plant Sciences; Marine & Freshwater Biology GA 429ZW UT WOS:000264959600007 PM 27033816 ER PT J AU Riveros, AJ Hernandez, EJ Wcislo, WT AF Riveros, Andre J. Hernandez, Edgar J. Wcislo, William T. TI Nesting Biology of Euglossa dodsoni Moure (Hymenoptera: Euglossinae) in Panama SO JOURNAL OF THE KANSAS ENTOMOLOGICAL SOCIETY LA English DT Article ID HYACINTHINA HYMENOPTERA; ORCHID BEE; APIDAE C1 [Riveros, Andre J.; Hernandez, Edgar J.] Univ Nacl Colombia, Dept Biol, Lab Invest Abejas, Bogota, Colombia. [Riveros, Andre J.] Univ Arizona, Div Neurobiol, Ctr Insect Sci, Tucson, AZ 85721 USA. [Riveros, Andre J.] Univ Arizona, Div Neurobiol, ARL, Tucson, AZ 85721 USA. [Hernandez, Edgar J.] Univ Missouri, Dept Biol, St Louis, MO 63121 USA. [Wcislo, William T.] Smithsonian Trop Res Inst, Panama City, Panama. RP Riveros, AJ (reprint author), Univ Nacl Colombia, Dept Biol, Lab Invest Abejas, Bogota, Colombia. EM anjosafat@gmail.com FU Smithsonian Tropical Research Institute; NSF [IOB-0519483] FX We thank DW Roubik for the identification of the specimens collected. This research was supported by funds of the Smithsonian Tropical Research Institute to WTW. AJR is currently supported by an NSF (IOB-0519483) grant to W. Gronenberg. We thank the Autoridad Nacional del Ambiente for permission to conduct research. NR 10 TC 2 Z9 2 U1 0 U2 2 PU KANSAS ENTOMOLOGICAL SOC PI LAWRENCE PA PO BOX 368, LAWRENCE, KS 66044 USA SN 0022-8567 J9 J KANSAS ENTOMOL SOC JI J. Kans. Entomol. Soc. PD APR PY 2009 VL 82 IS 2 BP 210 EP 214 PG 5 WC Entomology SC Entomology GA 498NN UT WOS:000270148100010 ER PT J AU Susan, GWL Laurance, WF Nascimento, HEM Andrade, A Fearnside, PM Expedito, RGR Condit, R AF Laurance Susan, G. W. Laurance, William F. Nascimento, Henrique E. M. Andrade, Ana Fearnside, Phillip M. Rebello Expedito, R. G. Condit, Richard TI Long-term variation in Amazon forest dynamics SO JOURNAL OF VEGETATION SCIENCE LA English DT Article DE Amazon; Climatic trends; El Nino; Forest dynamics; Permanent plots; Rainforest; Tree growth; Tree mortality; Tree recruitment; Tropical forests; Weather variation ID TROPICAL FORESTS; TREE COMMUNITIES; PERVASIVE ALTERATION; GLOBAL CHANGE; RAIN-FORESTS; MORTALITY; CARBON; GROWTH; TURNOVER; CLIMATE AB Have forest dynamics changed significantly in intact Amazon rainforests since the early 1980s? If so, what environmental drivers might potentially be responsible? Central Amazonia, north of Manaus, Brazil. Within 20 1-ha plots scattered over similar to 300 km(2), all trees (>= 10 cm diameter at breast height) were marked, identified, and measured five times between 1981 and 2003. We estimated stand-level dynamics (mortality, recruitment, and growth) for each census interval and evaluated weather parameters over the study period. We observed a widespread, significant increase in tree mortality across our plots. Tree recruitment also rose significantly over time but lagged behind mortality. Tree growth generally accelerated but varied considerably among census intervals, and was lowest when mortality was highest. Tree basal area rose 4% overall, but stem number exhibited no clear trend. In terms of climate variation, annual maximum and minimum temperatures increased significantly during our study. Rainfall anomalies were strongly and positively associated with ENSO events. The increasing forest dynamics, growth, and basal area observed are broadly consistent with the CO2 fertilization hypothesis. However, pronounced shorter-term variability in stand dynamics might be associated with climatic vicissitudes. Tree mortality peaked, and tree recruitment and growth declined during atypically wet periods. Tree growth was fastest during dry periods, when reduced cloudiness might have increased available solar radiation. Inferences about causality are tenuous because tree data were collected only at multi-year intervals. Mean temperatures and rainfall seasonality have both increased over time in central Amazonia, and these could potentially have long-term effects on forest dynamics and carbon storage. C1 [Laurance Susan, G. W.; Laurance, William F.; Condit, Richard] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Laurance Susan, G. W.; Laurance, William F.; Nascimento, Henrique E. M.; Andrade, Ana] Natl Inst Amazonian Res INPA, Biol Dynam Forest Fragments Project, BR-69011970 Manaus, Amazonas, Brazil. [Fearnside, Phillip M.] INPA, Dept Ecol, BR-69011970 Manaus, Amazonas, Brazil. [Rebello Expedito, R. G.] Inst Nacl Meterol INMET, Brasilia, DF, Brazil. [Condit, Richard] Univ Calif Santa Barbara, Natl Ctr Ecol Anal & Synth, Santa Barbara, CA 93106 USA. RP Susan, GWL (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Ancon, Panama. EM laurances@si.edu RI Nascimento, Henrique/F-8612-2012; Fearnside, Philip/D-6559-2011; Laurance, Susan/G-6021-2011; Laurance, William/B-2709-2012 OI Fearnside, Philip/0000-0003-3672-9082; Laurance, Susan/0000-0002-2831-2933; NR 54 TC 37 Z9 38 U1 0 U2 39 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1100-9233 EI 1654-1103 J9 J VEG SCI JI J. Veg. Sci. PD APR PY 2009 VL 20 IS 2 BP 323 EP 333 DI 10.1111/j.1654-1103.2009.01044.x PG 11 WC Plant Sciences; Ecology; Forestry SC Plant Sciences; Environmental Sciences & Ecology; Forestry GA 424LM UT WOS:000264568200014 ER PT J AU Siegal-Willott, J Citino, SB Wade, S Elder, L Hayek, LAC Lance, WR AF Siegal-Willott, Jessica Citino, Scott B. Wade, Scotty Elder, Laura Hayek, Lee-Ann C. Lance, William R. TI BUTORPHANOL, AZAPERONE, AND MEDETOMIDINE ANESTHESIA IN FREE-RANGING WHITE-TAILED DEER (ODOCOILEUS VIRGINIANUS) USING RADIOTRANSMITTER DARTS SO JOURNAL OF WILDLIFE DISEASES LA English DT Article DE Anesthesia; azaperone; butorphanol; medetomidine; Odocoileus virginianus; radiotelemetry dart; white-tailed deer ID XYLAZINE/FENTANYL CITRATE/AZAPERONE COMBINATION; FARMED DEER; MULE DEER; IMMOBILIZATION; XYLAZINE; KETAMINE; CARFENTANIL; THIAFENTANIL; ATIPAMEZOLE; TELAZOL(R) AB Fourteen free-ranging white-tailed deer (Odocoileus virginianus) were successfully anesthetized for a total of 15 anesthetic events using a combination of butorphanol (mean +/- SD, 0.58 +/- 0.1 mg/kg), azaperone (0.37 +/- 0.06 mg/kg), and medetomidine (0.19 +/- 0.03 mg/kg) (BAM) administered by radiotelemetry darts from hunting blinds between November 2006 and May 2007. Mean time to locate deer (mean +/- SD, 17.3 +/- 7 min), to recumbency (21.4 +/- 5 min), to initiation of data acquisition (27.5 +/- 8 min), total down time (37 +/- 6 min), and average distance run (161 +/- 82 m) were recorded. Physiologic monitoring was done ever), 5 min for a total of 20 min. Arterial blood gases were collected ever 10 min. Mild to moderate hypoxemia and mildly depressed ventilation occurred in some annuals. Muscle relaxation and plane of anesthesia were adequate for completion of all procedures; two deer were administered intravenous butorphanol supplementation to achieve light anesthesia (mean +/- SD, 0.19 mg/kg; 0.12 mg/kg). Recovery following intramuscular administration of naltrexone (1.34 +/- 0.42 mg/kg; 2X butorphanol dose) and atipamezole (0.93 +/- 0.14 mg/kg; 5X medetomidine dose) was rapid, smooth, and complete. Mean +/- SD recovery time was 4.5 +/- 1.5 min. Over-all efficacy of the Pneu-Dart radiotelemetry system was 65%. Negative attributes of this protocol included long induction time and dart failure. No known mortalities occurred as a result of the study. This drug combination provided safe, reliable, short-term anesthesia of free-ranging white-tailed deer. Further evaluation for use in field procedures in other cervids is warranted. C1 [Siegal-Willott, Jessica] Univ Florida, Dept Small Anim Clin Sci, Coll Vet Med, Gainesville, FL 32610 USA. [Citino, Scott B.; Wade, Scotty; Elder, Laura] White Oak Conservat Ctr, Yulee, FL 32097 USA. [Hayek, Lee-Ann C.] Smithsonian Inst, Washington, DC 20560 USA. [Lance, William R.] Wildlife Pharmaceut Inc, Ft Collins, CO 80522 USA. RP Siegal-Willott, J (reprint author), Smithsonian Inst, Natl Zool Pk, 3001 Connecticut Ave, Washington, DC 20008 USA. EM jess_sw24@hotmail.com NR 21 TC 6 Z9 6 U1 0 U2 6 PU WILDLIFE DISEASE ASSOC, INC PI LAWRENCE PA 810 EAST 10TH ST, LAWRENCE, KS 66044-8897 USA SN 0090-3558 J9 J WILDLIFE DIS JI J. Wildl. Dis. PD APR PY 2009 VL 45 IS 2 BP 468 EP 480 PG 13 WC Veterinary Sciences SC Veterinary Sciences GA 441EY UT WOS:000265753300022 PM 19395756 ER PT J AU Kuntner, M Kralj-Fiser, S Schneider, JM Li, D AF Kuntner, M. Kralj-Fiser, S. Schneider, J. M. Li, D. TI Mate plugging via genital mutilation in nephilid spiders: an evolutionary hypothesis SO JOURNAL OF ZOOLOGY LA English DT Article DE sperm competition; sexual size dimorphism; plugging; arms race; sexual conflict; sexual selection; Herennia multipuncta; Nephila pilipes ID ORB-WEB SPIDER; SEXUAL SIZE DIMORPHISM; PLUMIPES ARANEOIDEA; COPULATORY-BEHAVIOR; SPERM COMPETITION; MALE SACRIFICE; ARANEAE; CANNIBALISM; FEMALE; CONFLICT AB Nephilid spiders are known for gigantic females and tiny males. Such extreme sexual dimorphism and male-biased sex ratios result in fierce male-male competition for mates. Intense sperm competition may be responsible for behaviors such as mate guarding, mate binding, opportunistic mating, genital mutilation, mating plugs and male castration (eunuchs). We studied the mating biology of two phylogenetically, behaviorally and morphologically distinct south-east Asian nephilid spider species (Herennia multipuncta, Nephila pilipes) in nature and in the laboratory. Specifically, we established the frequencies and effectiveness of plugging (a plug is part of the male copulatory organ), and tested for male and female copulatory organ reuse. Both in nature and in the laboratory, plug frequencies were higher in H. multipuncta (75-80% females plugged) compared with N. pilipes (45-47.4%), but the differences were not significant. Plugs were single and effective (no remating) in H. multipuncta but multiple and ineffective (remating possible) in N. pilipes. In Herennia, the males plugged when the female was aggressive and in Nephila plugging was more likely when mating with previously mated and larger females. Further differences in sexual biology are complete palpal removal and higher sexual aggressiveness in Herennia (sexual cannibalism recorded for the first time), and mate binding in Nephila. Thus, we propose the following evolutionary hypothesis: nephilid plugging was ancestrally successful and enabled males to monopolize females, but plugging became ineffective in the phylogenetically derived Nephila. If the evolution of nephilid sexual mechanisms is driven by sexual conflict, then the male mechanism to monopolize females prevailed in a part of the phylogeny, but the female resistance to evade monopolization ultimately won the arms race. C1 [Kuntner, M.; Kralj-Fiser, S.] Slovenian Acad Sci & Arts, Inst Biol, Ctr Sci Res, SI-1001 Ljubljana, Slovenia. [Kuntner, M.] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20560 USA. [Schneider, J. M.] Univ Hamburg, Biozentrum Grindel, Hamburg, Germany. [Li, D.] Natl Univ Singapore, Dept Biol Sci, Singapore 117548, Singapore. RP Kuntner, M (reprint author), Slovenian Acad Sci & Arts, Inst Biol, Ctr Sci Res, Novi Trg 2,POB 306, SI-1001 Ljubljana, Slovenia. EM kuntner@gmail.com RI Schneider, Jutta /G-3727-2010; Li, Daiqin/D-6922-2013 OI Li, Daiqin/0000-0001-8269-7734 FU European Commision 6th Framework Programme (a Marie Curie International Reintegration) [MIRG-CT-2005 036536]; Slovenian Research Agency [Z1-7082-0618, 1000-06-310141]; National University of Singapore FX We thank David Court, Chris Koh, Jeremy Woon, Laura Yap, Eunice Tan, Yixiong Cai, Hui Kheng Lua, Joseph Koh, Peter Ng, Irena Kuntner, Cene Fiser and Matjaz Gregoric for their field, lab and/or logistical help and the Singapore National Parks for permits. Jonathan Coddington and Ingi Agnarsson kindly commented on the first draft of the paper. Virginia Hayssen, Lucinda Haines and two anonymous reviewers provided valuable comments and suggestions. This work was funded by the European Commision 6th Framework Programme (a Marie Curie International Reintegration Grant MIRG-CT-2005 036536), the Slovenian Research Agency (grants Z1-7082-0618 and 1000-06-310141) and the National University of Singapore (Raffles Museum Fellowship). NR 50 TC 37 Z9 38 U1 3 U2 40 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0952-8369 J9 J ZOOL JI J. Zool. PD APR PY 2009 VL 277 IS 4 BP 257 EP 266 DI 10.1111/j.1469-7998.2008.00533.x PG 10 WC Zoology SC Zoology GA 421GA UT WOS:000264346200001 ER PT J AU Riley, S AF Riley, Sheila TI You or Someone Like You SO LIBRARY JOURNAL LA English DT Book Review C1 [Riley, Sheila] Smithsonian Inst Libs, Washington, DC USA. RP Riley, S (reprint author), Smithsonian Inst Libs, Washington, DC USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU REED BUSINESS INFORMATION PI NEW YORK PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD APR 1 PY 2009 VL 134 IS 6 BP 68 EP + PG 2 WC Information Science & Library Science SC Information Science & Library Science GA 426YL UT WOS:000264744400040 ER PT J AU Rick, TC DeLong, RL Erlandson, JM Braje, TJ Jones, TL Kennett, DJ Wake, TA Walker, PL AF Rick, Torben C. DeLong, Robert L. Erlandson, Jon M. Braje, Todd J. Jones, Terry L. Kennett, Douglas J. Wake, Thomas A. Walker, Phillip L. TI A trans-Holocene archaeological record of Guadalupe fur seals (Arctocephalus townsendi) on the California coast SO MARINE MAMMAL SCIENCE LA English DT Article ID SAN-MIGUEL ISLAND; MAMMALS C1 [Rick, Torben C.] Smithsonian Inst, Dept Anthropol, Natl Museum Nat Hist, Washington, DC 20013 USA. [DeLong, Robert L.] NOAA, Natl Marine Mammal Lab, Alaska Fisheries Sci Ctr, Seattle, WA 98115 USA. [Erlandson, Jon M.; Kennett, Douglas J.] Univ Oregon, Dept Anthropol, Eugene, OR 97403 USA. [Erlandson, Jon M.] Univ Oregon, Museum Nat & Cultural Hist, Eugene, OR 97403 USA. [Braje, Todd J.] Humboldt State Univ, Dept Anthropol, Arcata, CA 95521 USA. [Jones, Terry L.] Calif Polytech State Univ San Luis Obispo, Dept Social Sci, San Luis Obispo, CA 93407 USA. [Wake, Thomas A.] Univ Calif Los Angeles, Cotsen Inst Archaeol, Los Angeles, CA 90095 USA. [Walker, Phillip L.] Univ Calif Santa Barbara, Dept Anthropol, Santa Barbara, CA 93106 USA. RP Rick, TC (reprint author), Smithsonian Inst, Dept Anthropol, Natl Museum Nat Hist, Washington, DC 20013 USA. EM rickt@si.edu RI Kennett, Douglas/I-7613-2015; OI Kennett, Douglas/0000-0001-5133-9010; Erlandson, Jon/0000-0002-4705-4319 FU Channel Islands National Park FX We thank Channel Islands National Park for supporting our research. Ann Huston, Kelly Minas, Ian Williams, Mark Senning, and Steve Schwartz have been instrumental in providing logistical and other support for our work. Finally, we thank Daryl Boness, Kathryn Ono, R. Lee Lyman, and two anonymous reviewers for comments that substantially improved this manuscript. NR 70 TC 10 Z9 11 U1 0 U2 16 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0824-0469 J9 MAR MAMMAL SCI JI Mar. Mamm. Sci. PD APR PY 2009 VL 25 IS 2 BP 487 EP 502 DI 10.1111/j.1748-7692.2008.00273.x PG 16 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA 433TM UT WOS:000265228700018 ER PT J AU Sugiura, N Petaev, MI Kimura, M Miyazaki, A Hiyagon, H AF Sugiura, N. Petaev, M. I. Kimura, M. Miyazaki, A. Hiyagon, H. TI Nebular history of amoeboid olivine aggregates SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID CV3 CHONDRITES EFREMOVKA; CARBONACEOUS CHONDRITES; SOLAR NEBULA; UNEQUILIBRATED ORDINARY; REFRACTORY INCLUSIONS; ISOTOPIC COMPOSITIONS; RICH INCLUSIONS; OXYGEN; CA; FORSTERITE AB Minor element (Ca, Cr, and Mn) concentrations in amoeboid olivine aggregates (AOAs) from primitive chondrites were measured and compared with those predicted by equilibrium condensation in the solar nebula. CaO concentrations in forsterite are low, particularly in porous aggregates. A plausible explanation appears that all equilibrium Ca activity was not maintained during the olivine condensation. CaO and MnO in forsterite are negatively correlated, with CaO being higher in compact aggregates. This suggests that the compact aggregates formed either by a prolonged reheating of the porous aggregates or by condensation and aggregation of forsterite during a very slow cooling in the nebula. C1 [Sugiura, N.; Miyazaki, A.; Hiyagon, H.] Univ Tokyo, Dept Earth & Planetary Sci, Bunkyo Ku, Tokyo, Japan. [Petaev, M. I.] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Petaev, M. I.] Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA. [Kimura, M.] Ibaraki Univ, Fac Sci, Mito, Ibaraki 3108512, Japan. RP Sugiura, N (reprint author), Univ Tokyo, Dept Earth & Planetary Sci, Bunkyo Ku, 7-3-1 Hongo, Tokyo, Japan. EM sugiura@eps.s.u-tokyo.ac.jp RI Sugiura, Naoji/A-1855-2009; HIYAGON, HAJIME/G-4879-2014 FU Japanese Society for the Promotion of Science [14340169, 16540435, 19540500]; NASA [NNGO5GI66G, NNX08AH79G] FX This work was supported by grant-in-aid of science research (14340169 for N. S., 16540435 and 19540500 for M. K.) from the Japanese Society for the Promotion of Science and NASA grants NNGO5GI66G and NNX08AH79G. The Acfer 094 polished sections were made available by Dr. A. N. Krot. We thank Dr. M. Ito for discussion on Cr diffusion rates in olivine grains. We thank Dr. M. K. Weisberg, Dr. A. Ruzicka, Dr. C. Floss, and all anonymous reviewer for valuable comments and suggestions. NR 45 TC 10 Z9 10 U1 0 U2 1 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD APR PY 2009 VL 44 IS 4 BP 559 EP 572 PG 14 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 458SZ UT WOS:000267045100007 ER PT J AU McDonald, I van Loon, JT Decin, L Boyer, ML Dupree, AK Evans, A Gehrz, RD Woodward, CE AF McDonald, Iain van Loon, Jacco Th. Decin, Leen Boyer, Martha L. Dupree, Andrea K. Evans, Aneurin Gehrz, Robert D. Woodward, Charles E. TI Giants in the globular cluster omega Centauri: dust production, mass-loss and distance SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Review DE stars: AGB and post-AGB; circumstellar matter; stars: mass-loss; stars: winds, outflows; globular clusters: individual: omega Centauri; infrared: stars ID UV-BRIGHT STARS; RICH AGB-STARS; HORIZONTAL-BRANCH MORPHOLOGY; STELLAR EVOLUTION DATABASE; MAIN-SEQUENCE STARS; RED GIANTS; ABUNDANCE ANALYSIS; CARBON STARS; GRAIN-SIZE; LOSS RATES AB We present spectral energy distribution modelling of 6875 stars in omega Centauri, obtaining stellar luminosities and temperatures by fitting literature photometry to state-of-the-art MARCS stellar models. By comparison to four different sets of isochrones, we provide a new distance estimate to the cluster of 4850 +/- 200 (random error) +/- 120 (systematic error) pc, a reddening of E(B V) = 0.08 +/- 0.02 (random) +/- 0.02 (systematic) mag and a differential reddening of Delta E(B-V) < 0.02 mag for an age of 12 Gyr. Several new post-early-AGB candidates are also found. Infrared excesses of stars were used to measure total mass-loss rates for individual stars down to similar to 7 x 10(-8) M(circle dot) yr(-1). We find a total dust mass-loss rate from the cluster of 1.3 +/- (0.8)(0.5) x 10(-9) M(circle dot) yr(-1), with the total gas mass-loss rate being > 1.2 +/- (0.6)(0.5) x 10(-6) M(circle dot) yr(-1). Half of the cluster's dust production and 30 per cent of its gas production comes from the two most extreme stars - V6 and V42 - for which we present new Gemini/T-ReCS mid-infrared spectroscopy, possibly showing that V42 has carbon-rich dust. The cluster's dust temperatures are found to be typically greater than or similar to 550 K. Mass-loss apparently does not vary significantly with metallicity within the cluster, but shows some correlation with barium enhancement, which appears to occur in cooler stars, and especially on the anomalous RGB. Limits to outflow velocities, dust-to-gas ratios for the dusty objects and the possibility of short-time-scale mass-loss variability are also discussed in the context of mass-loss from low-metallicity stars. The ubiquity of dust around stars near the RGB tip suggests significant dusty mass-loss on the RGB; we estimate that typically 0.20-0.25 M(circle dot) of mass-loss occurs on the RGB. From observational limits on intracluster material, we suggest the dust is being cleared on a time-scale of less than or similar to 10(5) yr. C1 [McDonald, Iain; van Loon, Jacco Th.; Evans, Aneurin] Univ Keele, Sch Phys & Geog Sci, Astrophys Grp, Keele ST5 5BG, Staffs, England. [Decin, Leen] Katholieke Univ Leuven, Inst Astron, Dept Phys & Astron, B-3001 Louvain, Belgium. [Boyer, Martha L.; Gehrz, Robert D.; Woodward, Charles E.] Univ Minnesota, Dept Astron, Minneapolis, MN 55455 USA. [Dupree, Andrea K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP McDonald, I (reprint author), Univ Keele, Sch Phys & Geog Sci, Astrophys Grp, Keele ST5 5BG, Staffs, England. EM iain@astro.keele.ac.uk NR 160 TC 61 Z9 61 U1 0 U2 1 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD APR 1 PY 2009 VL 394 IS 2 BP 831 EP 856 DI 10.1111/j.1365-2966.2008.14370.x PG 26 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 419TG UT WOS:000264242000020 ER PT J AU Derekas, A Kiss, LL Bedding, TR Ashley, MCB Csak, B Danos, A Fernandez, JM Furesz, G Meszaros, S Szabo, GM Szakats, R Szekely, P Szatmary, K AF Derekas, A. Kiss, L. L. Bedding, T. R. Ashley, M. C. B. Csak, B. Danos, A. Fernandez, J. M. Furesz, G. Meszaros, Sz. Szabo, Gy. M. Szakats, R. Szekely, P. Szatmary, K. TI Binarity and multiperiodicity in high-amplitude delta Scuti stars SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Review DE methods: observational; techniques: photometric; techniques: radial velocities; binaries: general; binaries: spectroscopic; delta Scuti ID LONG-TERM VARIABILITY; AD CANIS MINORIS; PERIOD VARIABLE-STARS; CY-AQUARII; DWARF CEPHEIDS; ECLIPSING BINARIES; LIGHT CURVES; SCT STARS; PHOTOELECTRIC PHOTOMETRY; FOURIER DECOMPOSITION AB We have carried out a photometric and spectroscopic survey of bright high-amplitude delta Scuti ( HADS) stars. The aim was to detect binarity and multiperiodicity ( or both) in order to explore the possibility of combining binary star astrophysics with stellar oscillations. Here, we present the first results for 10, predominantly southern, HADS variables. We detected the orbital motion of RS Gru with a semi-amplitude of similar to 6.5 kms(-1) and 11.5 d period. The companion is inferred to be a low-mass dwarf star in a close orbit around RS Gru. We found multiperiodicity in RY Lep from both photometric and radial velocity data and detected orbital motion in the radial velocities with hints of a possible period of 500-700 d. The data also revealed that the amplitude of the secondary frequency is variable on the time-scale of a few years, whereas the dominant mode is stable. Radial velocities of AD CMi revealed cycle-to-cycle variations, which might be due to non-radial pulsations. We confirmed the multiperiodic nature of BQ Ind, while we obtained the first radial velocity curves of ZZ Mic and BE Lyn. The radial velocity curve and the O-C diagram of CY Aqr are consistent with the long-period binary hypothesis. We took new time series photometry on XX Cyg, DY Her and DY Peg, with which we updated their O-C diagrams. C1 [Derekas, A.; Kiss, L. L.; Bedding, T. R.; Danos, A.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia. [Ashley, M. C. B.] Univ New S Wales, Sch Phys, Dept Astrophys & Opt, Sydney, NSW 2052, Australia. [Csak, B.; Meszaros, Sz.] Univ Szeged, Dept Opt & Quantum Elect, Szeged, Hungary. [Csak, B.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Fernandez, J. M.; Furesz, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Szabo, Gy. M.; Szakats, R.; Szekely, P.; Szatmary, K.] Univ Szeged, Dept Expt Phys, H-6720 Szeged, Hungary. [Szabo, Gy. M.; Szakats, R.; Szekely, P.; Szatmary, K.] Univ Szeged, Astron Observ, H-6720 Szeged, Hungary. RP Derekas, A (reprint author), Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia. EM derekas@physics.usyd.edu.au RI Kiss, Laszlo/A-2539-2008; Szatmary, Karoly/C-6048-2011; Szabo, Gyula/A-8310-2012; Meszaros, Szabolcs/N-2287-2014; Derekas, Aliz/G-2091-2016 OI Meszaros, Szabolcs/0000-0001-8237-5209; Derekas, Aliz/0000-0002-6526-9444 FU Hungarian Academy of Sciences; Hungarian OTKA [T042509, K76816]; Australian Research Council FX We are grateful to the referee for the comments that improved the paper. AD is supported by a University of Sydney Postgraduate ward. GyMSz is supported by the Bolyai Janos Research Fellowship of the Hungarian Academy of Sciences. The research was supported by the Hungarian OTKA Grants T042509 and K76816. This work has been supported by the Australian Research Council. The authors are grateful to Professor Chris Tinney for collecting the high-quality service observations with the AAT. We thank the CfA TAC for their support by providing telescope time for this project. The NASA ADS Abstract Service was used to access data and references. This research has made use of the SIMBAD data base, operated at CDS-Strasbourg, France. NR 127 TC 15 Z9 15 U1 0 U2 5 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD APR 1 PY 2009 VL 394 IS 2 BP 995 EP 1008 DI 10.1111/j.1365-2966.2008.14381.x PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 419TG UT WOS:000264242000032 ER PT J AU Jain, PK Xiao, YH Walsworth, R Cohen, AE AF Jain, Prashant K. Xiao, Yanhong Walsworth, Ronald Cohen, Adam E. TI Surface Plasmon Resonance Enhanced Magneto-Optics (SuPREMO): Faraday Rotation Enhancement in Gold-Coated Iron Oxide Nanocrystals SO NANO LETTERS LA English DT Article ID OPTICAL-PROPERTIES; SILVER NANOPARTICLES; RAMAN-SCATTERING; MULTILAYER FILMS; KERR ROTATION; NANOSHELLS; OXIDATION; MAGNETITE; THERAPY; SPECTRA AB We report enhanced optical Faraday rotation in gold-coated maghemite (gamma-Fe2O3) nanoparticles. The Faraday rotation spectrum measured from 480-690 nm shows a peak at about 530 nm, not present in either uncoated maghemite nanoparticles or solid gold nanoparticles. This peak corresponds to an intrinsic electronic transition in the maghemite nanoparticles and is consistent with a near-field enhancement of Faraday rotation resulting from the spectral overlap of the surface plasmon resonance in the gold with the electronic transition in maghemite. This demonstration of surface plasmon resonance-enhanced magneto-optics (SuPREMO) in a composite magnetialplasmonic nanosystem may enable design of nanostructures for remote sensing and imaging of magnetic fields and for miniaturized magneto-optical devices. C1 [Jain, Prashant K.; Cohen, Adam E.] Harvard Univ, Dept Chem & Chem Biol, Cambridge, MA 02138 USA. [Walsworth, Ronald; Cohen, Adam E.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Xiao, Yanhong; Walsworth, Ronald] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Cohen, AE (reprint author), Harvard Univ, Dept Chem & Chem Biol, Cambridge, MA 02138 USA. EM cohen@chemistry.harvard.edu RI Jain, Prashant/A-4779-2009 OI Jain, Prashant/0000-0002-7306-3972 FU Siemans Healthcare and the Materials Research Science and Engineering Center of the National Science Foundation [DMR-02-13805, 0335765] FX This work was supported partially by Siemans Healthcare and the Materials Research Science and Engineering Center of the National Science Foundation under NSF Award Number DMR-02-13805. We acknowledge the use of TEM facilities at the Center for Nanoscale Systems (CNS), a part of the Faculty of Arts and Sciences at Harvard University and a member of the National Nanotechnology Infrastructure Network (NNIN), which is supported by the National Science Foundation under award no. ECS-0335765. We thank Dr. William Croft for XRD training and Dr. Darrick Chang for helpful discussions. NR 72 TC 136 Z9 138 U1 5 U2 74 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 1530-6984 EI 1530-6992 J9 NANO LETT JI Nano Lett. PD APR PY 2009 VL 9 IS 4 BP 1644 EP 1650 DI 10.1021/nl900007k PG 7 WC Chemistry, Multidisciplinary; Chemistry, Physical; Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Physics, Applied; Physics, Condensed Matter SC Chemistry; Science & Technology - Other Topics; Materials Science; Physics GA 430ZB UT WOS:000265030000067 PM 19351194 ER PT J AU Laurance, WF AF Laurance, William F. TI Possum on the Rostrum SO NATURAL HISTORY LA English DT Editorial Material C1 Smithsonian Trop Res Inst, Balboa, Panama. RP Laurance, WF (reprint author), Smithsonian Trop Res Inst, Balboa, Panama. RI Laurance, William/B-2709-2012 NR 0 TC 0 Z9 0 U1 0 U2 0 PU NATURAL HISTORY MAGAZINE PI NEW YORK PA 36 WEST 25TH STREET, FIFTH FLOOR, NEW YORK, NY 10010 USA SN 0028-0712 J9 NAT HIST JI Nat. Hist. PD APR PY 2009 VL 118 IS 3 BP 48 EP 48 PG 1 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 426GO UT WOS:000264696200017 ER PT J AU Aalbu, RL Kanda, K Steiner, WE AF Aalbu, Rolf L. Kanda, Kojun Steiner, Warren E., Jr. TI Opatroides punctulatus Brulle now established in California (Coleoptera: Tenebrionidae) SO PAN-PACIFIC ENTOMOLOGIST LA English DT Article DE California; darkling beetles; exotic species; Opatroides; soil fauna; Tenebrionidae; turf insects AB Opatroides punctulatus Brulle, 1832 (Coleoptera; Tenebrionidae; Opatrini), is reported established for the first time in the New World in California near Sacramento. A key to distinguish Opatroides from species of similar genera is provided, with images and a brief diagnosis of O. punctulatus. The potential spread and pest status of the beetle should be monitored. C1 [Steiner, Warren E., Jr.] Smithsonian Inst, Dept Entomol, Washington, DC 20560 USA. [Aalbu, Rolf L.] Calif Acad Sci, Dept Entomol, San Francisco, CA 94118 USA. [Kanda, Kojun] Oregon State Univ, Dept Zool, Corvallis, OR 97331 USA. RP Steiner, WE (reprint author), Smithsonian Inst, Dept Entomol, NHB 187, Washington, DC 20560 USA. EM steinerw@si.edu NR 6 TC 3 Z9 3 U1 0 U2 0 PU PACIFIC COAST ENTOMOL SOC PI SAN FRANCISCO PA C/O CALIFORNIA ACADEMY SCIENCES, 875 HOWARD STREET, SAN FRANCISCO, CA 94103-3009 USA SN 0031-0603 J9 PAN-PAC ENTOMOL JI Pan-Pacific Entomol. PD APR PY 2009 VL 85 IS 2 BP 38 EP 42 PG 5 WC Entomology SC Entomology GA 540VO UT WOS:000273368600002 ER PT J AU Younge, KC Reinhard, A Pohl, T Berman, PR Raithel, G AF Younge, K. C. Reinhard, A. Pohl, T. Berman, P. R. Raithel, G. TI Mesoscopic Rydberg ensembles: Beyond the pairwise-interaction approximation SO PHYSICAL REVIEW A LA English DT Article DE atom-photon collisions; laser cooling; many-body problems; photoexcitation; potential energy functions; radiation pressure; rubidium; Rydberg states; spectral line narrowing ID ENERGY-TRANSFER; GAS AB We examine state mixing in a dense, cold Rydberg gas. Cold Rb atom clouds in an optical dipole trap are excited into nD(5/2) Rydberg levels using narrow-bandwidth laser pulses. For n=43, two atoms excited to 43D(5/2) states can be converted to 41F(7/2) and 45P(3/2) product states via a Forster resonance. We find, unexpectedly, that up to 50% of the Rydberg atoms are detected in such product states after only 100 ns of interaction time. The experiment is modeled using many-body quantum simulations. To reproduce the mixing fractions measured near Forster resonances, we use an exact, nonperturbative many-atom Hamiltonian in which product states are treated on an equal basis with the laser-excited nD(5/2) Rydberg level. Simplified many-body interaction models based on sums over pairwise atomic potentials cannot reproduce the measured mixing fractions. C1 [Younge, K. C.; Reinhard, A.; Berman, P. R.; Raithel, G.] Univ Michigan, Dept Phys, FOCUS Ctr, Ann Arbor, MI 48109 USA. [Younge, K. C.; Reinhard, A.; Berman, P. R.; Raithel, G.] Univ Michigan, Michigan Ctr Theoret Phys, Ann Arbor, MI 48109 USA. [Pohl, T.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. [Pohl, T.] Max Planck Inst Phys Komplexer Syst, D-01187 Dresden, Germany. RP Younge, KC (reprint author), Univ Michigan, Dept Phys, FOCUS Ctr, Ann Arbor, MI 48109 USA. EM kyounge@umich.edu RI Pohl, Thomas/B-5133-2013 NR 27 TC 43 Z9 43 U1 1 U2 4 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 J9 PHYS REV A JI Phys. Rev. A PD APR PY 2009 VL 79 IS 4 AR 043420 DI 10.1103/PhysRevA.79.043420 PN B PG 5 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 443YU UT WOS:000265947500020 ER PT J AU Silvera, K Santiago, LS Cushman, JC Winter, K AF Silvera, Katia Santiago, Louis S. Cushman, John C. Winter, Klaus TI Crassulacean Acid Metabolism and Epiphytism Linked to Adaptive Radiations in the Orchidaceae SO PLANT PHYSIOLOGY LA English DT Article ID CARBON-ISOTOPE RATIOS; VASCULAR EPIPHYTES; DELTA-C-13 VALUES; PHOTOSYNTHETIC PATHWAYS; SPECIES-DIVERSITY; DNA-SEQUENCES; LIFE-FORMS; PLANTS; BROMELIACEAE; EVOLUTION AB Species of the large family Orchidaceae display a spectacular array of adaptations and rapid speciations that are linked to several innovative features, including specialized pollination syndromes, colonization of epiphytic habitats, and the presence of Crassulacean acid metabolism (CAM), a water-conserving photosynthetic pathway. To better understand the role of CAM and epiphytism in the evolutionary expansion of tropical orchids, we sampled leaf carbon isotopic composition of 1,103 species native to Panama and Costa Rica, performed character state reconstruction and phylogenetic trait analysis of CAM and epiphytism, and related strong CAM, present in 10% of species surveyed, to climatic variables and the evolution of epiphytism in tropical regions. Altitude was the most important predictor of photosynthetic pathway when all environmental variables were taken into account, with CAM being most prevalent at low altitudes. By creating integrated orchid trees to reconstruct ancestral character states, we found that C(3) photosynthesis is the ancestral state and that CAM has evolved at least 10 independent times with several reversals. A large CAM radiation event within the Epidendroideae, the most species-rich epiphytic clade of any known plant group, is linked to a Tertiary species radiation that originated 65 million years ago. Our study shows that parallel evolution of CAM is present among subfamilies of orchids, and correlated divergence between photosynthetic pathways and epiphytism can be explained by the prevalence of CAM in low-elevation epiphytes and rapid speciation of high-elevation epiphytes in the Neotropics, contributing to the astounding diversity in the Orchidaceae. C1 [Silvera, Katia; Cushman, John C.] Univ Nevada, Biochem & Mol Biol MS 200, Reno, NV 89557 USA. [Silvera, Katia; Winter, Klaus] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Santiago, Louis S.] Univ Calif Riverside, Riverside, CA 92521 USA. RP Silvera, K (reprint author), Univ Nevada, Biochem & Mol Biol MS 200, Reno, NV 89557 USA. EM silverak@unr.nevada.edu RI Santiago, Louis/E-3185-2016 OI Santiago, Louis/0000-0001-5994-6122 FU Environmental Protection Agency [MA 91685201]; National Science Foundation [IOB-0543659, DEB-0706813]; National Institutes of Health [P20 RR-016464]; National Center for Research Resources; Andrew W. Mellon Foundation; Smithsonian Tropical Research Institute; Nevada Agricultural Experiment Station [NAES 03087114] FX This work was supported by the Environmental Protection Agency (Greater Research Opportunities Graduate Program Assistance Agreement no. MA 91685201 to K. S.), the National Science Foundation (grant nos. IOB-0543659 to J. C. C. and DEB-0706813 to L. S. S.), the National Institutes of Health (grant no. P20 RR-016464 from the Idea Network of Biomedical Research Excellence Program of the National Center for Research Resources supporting the Nevada Genomics, Proteomics, and Bioinformatics Center), the Andrew W. Mellon Foundation through the Smithsonian Tropical Research Institute (to K. W.), and the Nevada Agricultural Experiment Station (as publication no. NAES 03087114). NR 70 TC 56 Z9 61 U1 5 U2 53 PU AMER SOC PLANT BIOLOGISTS PI ROCKVILLE PA 15501 MONONA DRIVE, ROCKVILLE, MD 20855 USA SN 0032-0889 J9 PLANT PHYSIOL JI Plant Physiol. PD APR PY 2009 VL 149 IS 4 BP 1838 EP 1847 DI 10.1104/pp.108.132555 PG 10 WC Plant Sciences SC Plant Sciences GA 427RR UT WOS:000264796900021 PM 19182098 ER PT J AU Matthew, S Pau, VJ Luesch, H AF Matthew, Susan Pau, Valerie J. Luesch, Hendrik TI Largamides A-C, Tiglic Acid-Containing Cyclodepsipeptides with Elastase-Inhibitory Activity from the Marine Cyanobacterium Lyngbya confervoides SO PLANTA MEDICA LA English DT Article DE marine cyanobacteria; Lyngbya confervoides; cyclodepsipeptides; elastase ID BIOSYNTHESIS; PEPTIDES AB Three unusual tiglic acid-containing cyclodepsipeptides, possessing the revised regioisomeric structures for largamides A - C (1-3), have been isolated from the marine cyanobacterium Lyngbya confervoides collected from southeastern Florida. The two-dimensional structures were determined by NMR spectroscopy and the absolute configurations by chiral HPLC analysis of degradation products. Compounds 1-3 are moderate inhibitors of mammalian elastase activity in vitro with IC(50) values ranging from 0.53 to 1.41 mu M. C1 [Matthew, Susan; Luesch, Hendrik] Univ Florida, Dept Med Chem, Gainesville, FL 32610 USA. [Pau, Valerie J.] Smithsonian Marine Stn, Ft Pierce, FL USA. RP Luesch, H (reprint author), Univ Florida, Dept Med Chem, 1600 SW Archer Rd, Gainesville, FL 32610 USA. EM luesch@cop.ufl.edu RI Matthew, Susan/E-3817-2012 FU U.S Department of Commerce [NA060AR4170014]; NIGMS [P41 GM08621 0] FX This work was funded by the Florida Sea Grant College Program with support from NOAA, Office of Sea Grant, U.S Department of Commerce, Grant No. NA060AR4170014; and NIGMS grant P41 GM08621 0. We thank L. Fisher and K. Banks (Broward County Environmental Protection Department) and C. Ross, A. Capper, and R. Ritson-Williams (Smithsonian Marine Station) for assistance with collections and W. Yoshida (University of Hawaii) for providing NMR data. We also thank C. Bewley for helpful discussions and comparison with authentic largamides A - C from Oscillatoria sp. from Key Largo. Mass spectral analyses were performed at the UCR Mass Spectrometry Facility, Department of Chemistry, University of California at Riverside. This is contribution # 759 from the Smithsonian Marine Station at Fort Pierce. NR 12 TC 18 Z9 18 U1 0 U2 4 PU GEORG THIEME VERLAG KG PI STUTTGART PA RUDIGERSTR 14, D-70469 STUTTGART, GERMANY SN 0032-0943 J9 PLANTA MED JI Planta Med. PD APR PY 2009 VL 75 IS 5 BP 528 EP 533 DI 10.1055/s-0029-1185332 PG 6 WC Plant Sciences; Chemistry, Medicinal; Integrative & Complementary Medicine; Pharmacology & Pharmacy SC Plant Sciences; Pharmacology & Pharmacy; Integrative & Complementary Medicine GA 437KJ UT WOS:000265486100013 PM 19214948 ER PT J AU Adamski, D Apple, JL Bishop, JG AF Adamski, David Apple, Jennifer L. Bishop, John G. TI A NEW FILATIMA BUSCK (LEPIDOPTERA: GELECHIIDAE) ASSOCIATED WITH LUPINE AND EARLY HERBIVORE COLONIZATION ON MOUNT ST. HELENS SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE colonization; herbivory; Lupinus ID EARLY PRIMARY SUCCESSION; MECHANISMS AB Filatima loowita, n. sp. is described from the Pumice Plain on Mount St. Helens in Washington, United States. An apparent specialist on lupine, early instars feed as leaf-miners, while later instars tie leaflets together into silken tunnels and feed externally, mainly on the leaf tissue. The larvae make webbed tunnels, which extend from the root bundles to the uppermost leaves of the plant. Illustrations are provided of the adult male and female genitalia, and chaetotaxal maps of the last-instar larva, supplemented with scanning electron micrographs and images of the host on the volcano. C1 [Adamski, David] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20013 USA. [Apple, Jennifer L.] SUNY Coll Geneseo, Dept Biol, Geneseo, NY 14454 USA. [Bishop, John G.] Washington State Univ, Sch Biol Sci, Vancouver, WA 98686 USA. RP Adamski, D (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, POB 37012, Washington, DC 20013 USA. EM David.Adamski@ars.usda.gov; applej@geneseo.edu; bishopj@vancouver.wsu.edu FU NSF [DEB-008984]; M. J. Murdock Charitable Trust; Washington State University, Vancouver FX We thank Diana Marques, Lisboa, Portugal for the fine computer-generated illustrations of the male and female genitalia,, chaetotaxal maps of the larva, and production of the plates; Scott Whittaker, Lab Manager, Scanning Electron Microscopy Laboratory, Smithsonian Institution, Washington, DC, for the suggestions on larval fixation prior to SEM analysis and the scheduling to scope time; and Jon Titus, Department of Biology, SUNY-Fredonia, Fredonia, New York for Fig. 17. This research was supported by NSF grant DEB-008984 to JGB and funding frorn the M. J. Murdock Charitable Trust. The second author was supported by NSF DEB-008984 while at Washington State University, Vancouver. NR 18 TC 2 Z9 2 U1 0 U2 3 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD APR PY 2009 VL 111 IS 2 BP 293 EP 304 DI 10.4289/0013-8797-111.2.293 PG 12 WC Entomology SC Entomology GA 447YL UT WOS:000266227900001 ER PT J AU Adamski, D Boege, K AF Adamski, David Boege, Karina TI TWO NEW SPECIES OF COMPSOLECHIA MEYRICK (LEPIDOPTERA: GELECHIIDAE) ASSOCIATED WITH CASEARIA (FLACOURTIACEAE) IN COASTAL DRY-FORESTS OF WESTERN MEXICO SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE chaetotaxy; Chamela; genitalia; leafroller; leaftier; Neotropics; pupa; taxonomy AB Two new species of Compsolechia Meyrick (Lepidoptera: Gelechiidae), C camilotus Adamski and C vittatiella Adamski, are described from dry-forests In western Mexico. Larvae of both species were collected on leaves of Casearia nitida (L.) Jacq. (Flacourtiaceae), a new host record for the genus. Photographs of larvae and their shelters and adult moths are provided. In addition, illustrations of the male and female genitalia of the adults, larval chaetotaxal maps, and scanning electron micrographs for both species are included. The pupa of only C. camilotus was available for description. C1 [Adamski, David] Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, Washington, DC 20013 USA. [Boege, Karina] Univ Nacl Autonoma Mexico, Inst Ecol, Mexico City 04510, DF, Mexico. RP Adamski, D (reprint author), Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, POB 37012,NHBE523, Washington, DC 20013 USA. EM David.Adamski@ars.usda.gov; kboege@servidor.unam.mx NR 18 TC 0 Z9 0 U1 0 U2 2 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD APR PY 2009 VL 111 IS 2 BP 305 EP 321 DI 10.4289/0013-8797-111.2.305 PG 17 WC Entomology SC Entomology GA 447YL UT WOS:000266227900002 ER PT J AU Davis, SR Davis, DR AF Davis, Steven R. Davis, Donald R. TI NEOTROPICAL TINEIDAE VIII: FALSIVALVA, A NEW GENUS FROM AUSTRAL SOUTH AMERICA WITH EXTREME MODIFICATION OF THE MALE POSTABDOMINAL TERGA (LEPIDOPTERA: TINEIDAE) SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Argentina; Chile; male genitalia; morphology; pectinifer; Pelecystola; tegumen; tergum IX AB Falsivalva, new genus is described and illustrated. In addition to the previously named type species, "Tinea" prensoria Meyrick, three new species, F. clavata, F. nephophila, and F. paraprensoria, are described. The most conspicuous synapomorphy of Falsivalva is the highly specialized tergum IX (tegumen) of the male, which is greatly enlarged and almost completely divided to resemble the male gonopods (valvae). It is suggested, but not observed, that these paired structures may function either to guide or clasp the female oviscapt during copulation. The genus occurs in both coastal and Andean Nothofagus forests primarily in southern Chile from approximately 35 degrees S in Maule Province South to about 45 degrees in Chiloe Island and east to Neuquen Province, Argentina. The biology is unknown. C1 [Davis, Steven R.] Univ Kansas, Div Entomol, Nat Hist Museum, Lawrence, KS 66049 USA. [Davis, Steven R.] Univ Kansas, Dept Ecol & Evolutionary Biol, Lawrence, KS 66049 USA. [Davis, Donald R.] Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Davis, SR (reprint author), Univ Kansas, Div Entomol, Nat Hist Museum, 1501 Crestline Dr,Suite 140, Lawrence, KS 66049 USA. EM davisd@si.edu NR 9 TC 1 Z9 1 U1 0 U2 1 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD APR PY 2009 VL 111 IS 2 BP 378 EP 392 DI 10.4289/0013-8797-111.2.378 PG 15 WC Entomology SC Entomology GA 447YL UT WOS:000266227900010 ER PT J AU Gagne, RJ AF Gagne, Raymond J. TI TAXONOMY OF JANETIELLA THYMI (KIEFFER) (DIPTERA: CECIDOMYIIDAE) AND OF THE SPECIES FORMERLY IN JANETIELLA THAT FEED ON VITIS (VITACEAE) SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Holarctic; gall midges; grape; Dasineurini AB The poorly known European species Janetiella thymi (Kieffer), type species of Janetiella Kieffer (Diptera: Cecidomyiidae), is redescribed. Gall makers on grape that were formerly placed in Janetiella are shown to be distinct from that genus and transferred to Vitisiella Fedotova & Kovalev, a genus recently erected For a species on grape in Siberia. Among the distinguishing traits of Vitisiella, more fully characterized here than previously, are the closed costal vein at its juncture with R(5), the deeply divided male hypoproct, and the conspicuous dorsolateral sclerites of the ovipositor. Janetiella brevicauda Felt, also redescribed, and Cecidomyia oenephila Haimhoffen, both previously placed in Janetiella, are newly combined with Vitisiella. C1 ARS, Systemat Entomol Lab, PSI, USDA,Smithsonian Inst, Washington, DC 20013 USA. RP Gagne, RJ (reprint author), ARS, Systemat Entomol Lab, PSI, USDA,Smithsonian Inst, MRC 168,POB 37012, Washington, DC 20013 USA. EM Raymond.Gagne@ars.usda.gov NR 24 TC 0 Z9 4 U1 0 U2 0 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD APR PY 2009 VL 111 IS 2 BP 399 EP 409 DI 10.4289/0013-8797-111.2.399 PG 11 WC Entomology SC Entomology GA 447YL UT WOS:000266227900012 ER PT J AU Mathis, WN Mathis, D AF Mathis, Wayne N. Mathis, Dianne TI SPECIES OF THE SHORE-FLY GENUS GLENANTHE HALIDAY (DIPTERA: EPHYDRIDAE) FROM NEW MEXICO SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Nearctic; new species; systematics; taxonomy ID REVISION AB Species of the shore-fly genus Glenanthe Haliday from New Mexico are reviewed, including description of G. buchananorum, new species (New Mexico. Chavas: Roswell (9 km E; 33 degrees 23.8'N, 104 degrees 24'W; Pecos River)). Other species reported from New Mexico are G. caribea and G. salina. A revised key to the New World species is presented. C1 [Mathis, Wayne N.; Mathis, Dianne] Smithsonian Inst, Dept Entomol, Washington, DC 20013 USA. RP Mathis, WN (reprint author), Smithsonian Inst, Dept Entomol, NHB 169,POB 37012, Washington, DC 20013 USA. EM mathisw@si.edu NR 20 TC 1 Z9 1 U1 0 U2 0 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD APR PY 2009 VL 111 IS 2 BP 454 EP 463 DI 10.4289/0013-8797-111.2.454 PG 10 WC Entomology SC Entomology GA 447YL UT WOS:000266227900017 ER PT J AU Solis, MA AF Solis, M. Alma TI TRANSFER OF ALL WESTERN HEMISPHERE CYBALOMIINAE TO OTHER SUBFAMILIES (CRAMBIDAE: PYRALOIDEA: LEPIDOPTERA): ELUSIA SCHAUS, DICHOCHROMA FORBES, SCHACONTIA DYAR, CYBALOMIA EXTORRIS WARREN, AND C-LOJANALIS (DOGNIN) SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article ID GLAPHYRIINAE AB Munroe (1995) included four genera and nine species from the Western Hemisphere in Cybalomiinae. The species were morphologically compared with Cybalomia pentadalis Lederer, the type species of Cybalomia, and all belong to other subfamilies. Accordingly, the following new and revised combinations and/or subramilial assignments are proposed: Elusia Schaus is returned to Scopariinae; Cybalomia extorris Warren is transferred to Aethiophysa Munroe, Dichochroma Forbes and Schacontia Dyar are transferred to Glaphyriinae; and Cybalomia lojanalis (Dognin) is transferred to Diptychophora Zeller in Crambinae. A lectotype is designated for Platytes lojanalis Dognin. The adults and genitalia are figured for the first time. C1 ARS, Systemat Entomol Lab, USDA, Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20013 USA. RP Solis, MA (reprint author), ARS, Systemat Entomol Lab, USDA, Natl Museum Nat Hist,Smithsonian Inst, POB 37012,MRC 168, Washington, DC 20013 USA. EM alma.solis@ars.usda.gov NR 28 TC 3 Z9 4 U1 0 U2 1 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD APR PY 2009 VL 111 IS 2 BP 493 EP 504 DI 10.4289/0013-8797-111.2.493 PG 12 WC Entomology SC Entomology GA 447YL UT WOS:000266227900020 ER PT J AU Woodley, NE AF Woodley, Norman E. TI MICROCHRYSA FLAVIVENTRIS (WIEDEMANN), A NEW IMMIGRANT SOLDIER FLY IN THE UNITED STATES (DIPTERA: STRATIOMYIDAE) SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Sarginae; immigrant species; Virginia ID NORTH-AMERICAN RECORDS AB Microchrysa flaviventris (Wiedemann) (Diptera: Stratiomyidae: Sarginae), a species widespread in the Old World, is reported from North America for the first time. Apparently it is established in the eastern United States. Specimens were taken in Alexandria, Virginia in August 2007. C1 ARS, Systemat Entomol Lab, PSI, USDA,Smithsonian Inst, Washington, DC 20013 USA. RP Woodley, NE (reprint author), ARS, Systemat Entomol Lab, PSI, USDA,Smithsonian Inst, NHB 168,POB 37012, Washington, DC 20013 USA. EM norman.woodley@ars.usda.gov RI Woodley, Norman/M-6160-2014 NR 10 TC 0 Z9 0 U1 0 U2 0 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD APR PY 2009 VL 111 IS 2 BP 527 EP 529 DI 10.4289/0013-8797-111.2.527 PG 3 WC Entomology SC Entomology GA 447YL UT WOS:000266227900023 ER PT J AU Lin, CL Zhang, ZW Chen, WP King, SK Lin, HC Wang, JH Mondal, S Alcock, C Axelrod, T Bianco, FB Byun, YI Coehlo, NK Cook, KH Dave, R de Pater, I Descamps, P Lehner, MJ Kim, DW Lee, T Lissauer, JJ Marshall, SL Porrata, R Protopapas, P Rice, JA Schwamb, ME Wang, SY Wen, CY AF Lin, Chi-Long Zhang, Zhi-Wei Chen, W. P. King, Sun-Kun Lin, Hung-Chin Wang, J. -H. Mondal, S. Alcock, C. Axelrod, T. Bianco, F. B. Byun, Y. -I. Coehlo, N. K. Cook, K. H. Dave, R. de Pater, I. Descamps, P. Lehner, M. J. Kim, D. -W. Lee, T. Lissauer, J. J. Marshall, S. L. Porrata, R. Protopapas, P. Rice, J. A. Schwamb, M. E. Wang, S. -Y. Wen, C. -Y. TI A Close Binary Star Resolved from Occultation by 87 Sylvia SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID ASTEROIDS; DUPLICITY AB The star BD +29 1748 was resolved to be a close binary from its occultation by the asteroid 87 Sylvia on 2006 December 18 UT. Four telescopes were used to observe this event at two sites separated by some 80 km. Two flux drops were observed at one site, whereas only one flux drop was detected at the other. From the long-term variation of Sylvia, we inferred the probable shape of the shadow during the occultation, and this in turn constrains the binary parameters: the two components of BD +29 1748 have a projected separation of 0 ''.097-0 ''.140 on the sky with a position angle 104 degrees-11 degrees 0. The asteroid was clearly resolved, with a size scale ranging from 130 to 290 km as projected onto the occultation direction, consistent with the size dimensions 385 x 265 x 230 km, measured by direct adaptive optics imaging. No occultation was detected for either of the two known moonlets of 87 Sylvia. C1 [Lin, Chi-Long] Natl Museum Nat Sci, Exhibit Div, Taichung 404, Taiwan. [Zhang, Zhi-Wei; Chen, W. P.; Lin, Hung-Chin; Wang, J. -H.; Mondal, S.] Natl Cent Univ, Inst Astron, Jhongli 32054, Taiwan. [King, Sun-Kun; Wang, J. -H.; Lehner, M. J.; Lee, T.; Wang, S. -Y.; Wen, C. -Y.] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. [Mondal, S.] Aryabhatta Res Inst Observat Sci, Naini Tal 263129, India. [Alcock, C.; Bianco, F. B.; Lehner, M. J.; Protopapas, P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Axelrod, T.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Bianco, F. B.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Byun, Y. -I.; Kim, D. -W.] Yonsei Univ, Dept Astron, Seoul 120749, South Korea. [Coehlo, N. K.; Rice, J. A.] Univ Calif Berkeley, Dept Stat, Berkeley, CA 94720 USA. [Cook, K. H.; Marshall, S. L.; Porrata, R.] Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94550 USA. [Dave, R.; Protopapas, P.] Harvard Univ, Initiat Innovat Comp, Cambridge, MA 02138 USA. [de Pater, I.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Descamps, P.] Observ Paris, IMCCE, UMR 8028, F-75014 Paris, France. [Lissauer, J. J.] NASA, Space Sci & Astrobiol Div 245 3, Ames Res Ctr, Moffett Field, CA 94035 USA. [Marshall, S. L.] Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA. [Schwamb, M. E.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. RP Lin, CL (reprint author), Natl Museum Nat Sci, Exhibit Div, 1 Kuan Chien Rd, Taichung 404, Taiwan. RI Lee, Typhoon/N-8347-2013 FU U. S. Department of Energy [DE-AC52-07NA27344] FX We thank David W. Dunham, Sato Isao, Dave Herald, and Mitsuru Soma for helpful discussions. KHC's work has been performed under the auspices of the U. S. Department of Energy by Lawrence Livermore National Laboratory under Contract DE-AC52-07NA27344. We acknowledge the anonymous referee, whose suggestions improved the quality of the paper. NR 22 TC 1 Z9 1 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6280 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD APR PY 2009 VL 121 IS 878 BP 359 EP 364 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 448BO UT WOS:000266236700005 ER PT J AU Wang, T Huang, JS Gu, QS AF Wang, Tao Huang, Jia-Sheng Gu, Qiu-Sheng TI Photometric redshifts of galaxies from SDSS and 2MASS SO RESEARCH IN ASTRONOMY AND ASTROPHYSICS LA English DT Article DE galaxies: distances and redshifts; methods: statistical; techniques: photometric ID DIGITAL SKY SURVEY; HUBBLE DEEP FIELD; CREATING SPECTRAL TEMPLATES; ARTIFICIAL NEURAL-NETWORKS; BROAD-BAND PHOTOMETRY; EARLY DATA RELEASE; CATALOG; CLASSIFICATION; EVOLUTION; SYSTEM AB In order to find the physical parameters which determine the accuracy of photometric redshifts, we compare the spectroscopic and photometric redshifts (photo-z's) for a large sample of similar to 80000 SDSS-2MASS galaxies. Photo-z's in this paper are estimated by using the artificial neural network photometric redshift method (ANNz). For a subset of similar to 40000 randomly selected galaxies, we find that the photometric redshift recovers the spectroscopic redshift distribution very well with rms of 0.016. Our main results are as follows: (1) Using magnitudes directly as input parameters produces more accurate photo-z's than using colors; (2) The inclusion of 2MASS (J, H, K(s)) bands does not improve photo-z's significantly, which indicates that near infrared data might not be important for the low-redshift sample; (3) Adding the concentration index (essentially the steepness of the galaxy brightness profile) as an extra input can improve the photo-z's estimation up to similar to 10 percent; (4) Dividing the sample into early- and late-type galaxies by using the concentration index, normal and abnormal galaxies by using the emission line flux ratios, and red and blue galaxies by using color index (g - r), we can improve the accuracy of photo-z's significantly; (5) Our analysis shows that the outliers (where there is a big difference between the spectroscopic and photometric redshifts) are mainly correlated with galaxy types, e.g., most outliers are late-type (blue) galaxies. C1 [Wang, Tao; Gu, Qiu-Sheng] Nanjing Univ, Dept Astron, Nanjing 210093, Peoples R China. [Huang, Jia-Sheng] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Wang, T (reprint author), Nanjing Univ, Dept Astron, Nanjing 210093, Peoples R China. EM twang.nju@gmail.com OI Wang, Tao/0000-0002-2504-2421 FU National Natural Science Foundation of China; New Century Excellent Talents in University (NCET); National Natural Science Foundation of China [10221001, 10633040]; National Basic Research Program [2007CB815405]; Alfred P. Sloan Foundation; Participating Institutions; National Science Foundation; U.S. Department of Energy; National Aeronautics and Space Administration; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England FX This work is supported by the Program for New Century Excellent Talents in University (NCET), the National Natural Science Foundation of China under grants 10221001 and 10633040 and the National Basic Research Program (973 program No. 2007CB815405). 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 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. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. NR 35 TC 4 Z9 4 U1 0 U2 2 PU NATL ASTRONOMICAL OBSERVATORIES, CHIN ACAD SCIENCES PI BEIJING PA 20A DATUN RD, CHAOYANG, BEIJING, 100012, PEOPLES R CHINA SN 1674-4527 J9 RES ASTRON ASTROPHYS JI Res. Astron. Astrophys. PD APR PY 2009 VL 9 IS 4 BP 390 EP 400 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 437JY UT WOS:000265485000002 ER PT J AU Howard, TG Saarela, JM Paszko, B Peterson, PM Werier, D AF Howard, Timothy G. Saarela, Jeffery M. Paszko, Beata Peterson, Paul M. Werier, David TI NEW RECORDS AND A TAXONOMIC REVIEW OF CALAMAGROSTIS PERPLEXA (POACEAE: POEAE: AGROSTIDINAE), A NEW YORK STATE ENDEMIC GRASS SO RHODORA LA English DT Article DE Calamagrostis; endemic; grass; hybrid; New York; Poaceae; principal components analysis (PCA) ID PORTERI SUBSP INSPERATA; DIVERSITY AB Calamagrostis perplexa is a New York State endemic grass species, hypothesized to be of hybrid origin, that previously was known only from a single locality. We provide a summary of its taxonomic history, report new New York records and ecological information for the taxon, and include a principal components analysis and key characterizing morphological variation in C perplexa and its putative close relatives C canadensis, C porteri, C rubescens, and C scribneri. Calamagrostis perplexa is now known from two extant populations and a third Population of unknown status; it remains a New York state endemic. C1 [Howard, Timothy G.] New York Nat Heritage Program, Albany, NY 12233 USA. [Saarela, Jeffery M.] Canadian Museum Nat, Stn D, Ottawa, ON K1P 6P4, Canada. [Paszko, Beata] Polish Acad Sci, W Szafer Inst Bot, PL-31512 Krakow, Poland. [Peterson, Paul M.] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA. RP Howard, TG (reprint author), New York Nat Heritage Program, 625 Broadway,5th Floor, Albany, NY 12233 USA. EM tghoward@gw.dec.state.ny.us; jsaarela@mus-nature.ca; ibpaszko@ib-pan.krakow.pl; peterson@si.edu; nakita@lightlink.com FU Smithsonian Institution's Restricted Endowment Fund; Department of Botany; Canadian Museum of Nature; The Nature Conservancy FX Field work by J.M.S. and P.M.P. was supported by a grant from the Smithsonian Institution's Restricted Endowment Fund and the Department of Botany, and by the Canadian Museum of Nature. Field work by T.G.H. was supported by the New York State Biodiversity Research Institute and the Eastern New York Chapter of The Nature Conservancy. Troy Weldy, Tom Rawinski, Matthew Paul, and Ethan Pierce assisted in the field; Steve Young helped with the initial determinations of collections from the new site, and located the Columbia County specimen at PH. The Smithsonian Institution's Office of Research Training and Services is thanked for providing a Short-term Visitor grant to B.P. We are grateful to Ken Marr (v) for helpful discussion and Thomas Wieboldt (vpi) for specimen loans. Christopher T. Martine and an anonymous reviewer provided helpful comments on an earlier version of the manuscript. NR 25 TC 9 Z9 11 U1 2 U2 2 PU NEW ENGLAND BOTANICAL CLUB INC PI LAWRENCE PA P.O. BOX 368, LAWRENCE, KS 66044 USA SN 0035-4902 J9 RHODORA JI Rhodora PD APR-JUN PY 2009 VL 111 IS 946 BP 155 EP 170 DI 10.3119/08-5.1 PG 16 WC Plant Sciences SC Plant Sciences GA 485ZL UT WOS:000269165000002 ER PT J AU Clough, GW AF Clough, G. Wayne TI FROM THE CASTLE Long Tails SO SMITHSONIAN LA English DT Editorial Material C1 Smithsonian Inst, Washington, DC 20560 USA. RP Clough, GW (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SMITHSONIAN ASSOC PI WASHINGTON PA 900 JEFFERSON DR, WASHINGTON, DC 20560 USA SN 0037-7333 J9 SMITHSONIAN JI Smithsonian PD APR PY 2009 VL 40 IS 1 BP 28 EP 28 PG 1 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA 424CN UT WOS:000264543200011 ER PT J AU Warner, DJ AF Warner, Deborah Jean TI The Transit of Venus Enterprise in Victorian Britain SO TECHNOLOGY AND CULTURE LA English DT Book Review C1 [Warner, Deborah Jean] Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. RP Warner, DJ (reprint author), Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU JOHNS HOPKINS UNIV PRESS PI BALTIMORE PA JOURNALS PUBLISHING DIVISION, 2715 NORTH CHARLES ST, BALTIMORE, MD 21218-4363 USA SN 0040-165X J9 TECHNOL CULT JI Technol. Cult. PD APR PY 2009 VL 50 IS 2 BP 463 EP 464 PG 2 WC History & Philosophy Of Science SC History & Philosophy of Science GA 438KB UT WOS:000265553200018 ER PT J AU Goodyear, FH AF Goodyear, Frank H. TI The Origins of American Photography: From Daguerreotype to Dry-Plate, 1839-1885: The Hallmark Photographic Collection at the Nelson-Atkins Museum of Art SO TECHNOLOGY AND CULTURE LA English DT Book Review C1 [Goodyear, Frank H.] Smithsonian Inst Natl Portrait Gallery, Washington, DC USA. RP Goodyear, FH (reprint author), Smithsonian Inst Natl Portrait Gallery, Washington, DC USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU JOHNS HOPKINS UNIV PRESS PI BALTIMORE PA JOURNALS PUBLISHING DIVISION, 2715 NORTH CHARLES ST, BALTIMORE, MD 21218-4363 USA SN 0040-165X J9 TECHNOL CULT JI Technol. Cult. PD APR PY 2009 VL 50 IS 2 BP 471 EP 473 PG 3 WC History & Philosophy Of Science SC History & Philosophy of Science GA 438KB UT WOS:000265553200023 ER PT J AU Piou, C Berger, U Feller, IC AF Piou, Cyril Berger, Uta Feller, Ilka C. TI Spatial structure of a leaf-removing crab population in a mangrove of North-Brazil SO WETLANDS ECOLOGY AND MANAGEMENT LA English DT Article DE Habitat preference; Intraspecific competition; Mangrove ecology; Multiple scales; Population structure; Spatial statistics; Ucides cordatus ID UCIDES-CORDATUS OCYPODIDAE; CAETE ESTUARY; PATTERN; LITTER; DYNAMICS; FORESTS; DEGRADATION; GRAPSIDAE; ECOSYSTEM; FISHERY AB The leaf-removing decapod crab, Ucides cordatus plays a key role as ecological engineer in Brazilian mangrove ecosystems. We analyzed the spatial distribution of a specific population at two different scales to observe how individual behavior could alter spatial population structure. First, we conducted a spatial point pattern analysis of the burrow entrances and the Rhizophora mangle prop roots on the mangrove floor at a scale of few meters. Secondly, we analyzed at a large scale (10-100 m) the potential effects of surface elevation, light intensity, prop root coverage, species of neighboring tree (R. mangle, Laguncularia racemosa, Avicennia germinans) and pneumatophore density on the size and number of burrow entrances. At the same large scale, we conducted an analysis of clustering of the crabs around the R. mangle trees. At small scale, the burrow entrances, although aggregated around the prop roots, showed a regularly spaced distribution (similar to 25 cm) signaling an intraspecific competition among the crabs. At large scale, crabs preferred to install their burrows at an intermediate level of surface elevation and prop root coverage, and in R. mangle-dominated areas. At the same kind of habitats, the largest burrows, and thus potentially the largest crabs, were found in higher number than on other habitats. The R. mangle-dominated areas preference was confirmed by an aggregating around R. mangle trees in R. mangle-dominated forest, but only of large individuals in L. racemosa-dominated forest. These observations lead us to the definition of a preferred habitat for U. cordatus. Competition leading to the small-scale regular patterns was proposed as an explanation for exclusion of smaller crabs from preferred habitats seen at large scale. We hypothesize that this preferred habitat might explain at regional scale the variation of U. cordatus importance in Neotropical mangroves. C1 [Piou, Cyril; Berger, Uta] Ctr Trop Marine Ecol, D-23859 Bremen, Germany. [Feller, Ilka C.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Piou, C (reprint author), Tech Univ Dresden, Inst Forest Growth & Forest Comp Sci, Postfach 1117, D-01735 Tharandt, Germany. EM cyril.piou@forst.tu-dresden.de OI Feller, Ilka/0000-0002-6391-1608 FU Brazilian National Research Council (CNPq); German Ministry for Education and Research (BMBF) [03F0154A] FX We thank A. deMelo, S. Manuel, D. Araujo, C. D'Lima, M. L. Fontalvo-Herazo, J-P Rossi, A. R. Araujo, I. Nordhaus, K. Diele, M. Protazio and an anonymous reviewer. This study was carried out as a part of the Brazilian-German Cooperation Project MADAM and was financed by the Brazilian National Research Council (CNPq) and the German Ministry for Education and Research (BMBF) under the code 03F0154A. This is MADAM-Contribution No. 117. NR 44 TC 11 Z9 11 U1 1 U2 21 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0923-4861 J9 WETL ECOL MANAG JI Wetl. Ecol. Manag. PD APR PY 2009 VL 17 IS 2 BP 93 EP 106 DI 10.1007/s11273-008-9089-3 PG 14 WC Environmental Sciences; Water Resources SC Environmental Sciences & Ecology; Water Resources GA 442QU UT WOS:000265856500002 ER PT J AU Ranere, AJ Piperno, DR Holst, I Dickau, R Iriarte, J AF Ranere, Anthony J. Piperno, Dolores R. Holst, Irene Dickau, Ruth Iriarte, Jose TI The cultural and chronological context of early Holocene maize and squash domestication in the Central Balsas River Valley, Mexico SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE agricultural origins; Mesoamerican preceramic; maize domestication ID ZEA-MAYS; ORIGIN; MESOAMERICA; CULTIVATION; EVOLUTION; HISTORY AB Molecular evidence indicates that the wild ancestor of maize is presently native to the seasonally dry tropical forest of the Central Balsas watershed in southwestern Mexico. We report here on archaeological investigations in a region of the Central Balsas located near the Iguala Valley in Guerrero state that show for the first time a long sequence of human occupation and plant exploitation reaching back to the early Holocene. One of the sites excavated, the Xihuatoxtla Shelter, contains well-stratified deposits and a stone tool assemblage of bifacially flaked points, simple flake tools, and numerous handstones and milling stone bases radiocarbon dated to at least 8700 calendrical years B.P. As reported in a companion paper (Piperno DR, et al., in this issue of PNAS), starch grain and phytolith residues from the ground and chipped stone tools, plus phytoliths from directly associated sediments, provide evidence for maize (Zea mays L.) and domesticated squash (Cucurbita spp.) in contexts contemporaneous with and stratigraphically below the 8700 calendrical years B.P. date. The radiocarbon determinations, stratigraphic integrity of Xihuatoxtla's deposits, and characteristics of the stone tool assemblages associated with the maize and squash remains all indicate that these plants were early Holocene domesticates. Early agriculture in this region of Mexico appears to have involved small groups of cultivators who were shifting their settlements seasonally and engaging in a variety of subsistence pursuits. C1 [Ranere, Anthony J.; Dickau, Ruth] Temple Univ, Dept Anthropol, Philadelphia, PA 19122 USA. [Ranere, Anthony J.; Piperno, Dolores R.; Holst, Irene] Smithsonian Trop Res Inst, Balboa, Panama. [Piperno, Dolores R.] Natl Museum Nat Hist, Dept Anthropol, Archaeobiol Program, Washington, DC 20560 USA. [Iriarte, Jose] Univ Exeter, Dept Archaeol, Sch Geog Archaeol & Earth Resources, Exeter EX4 4QJ, Devon, England. RP Ranere, AJ (reprint author), Temple Univ, Dept Anthropol, Philadelphia, PA 19122 USA. EM ranere@temple.edu RI Iriarte, Jose /A-1141-2010; OI Iriarte, Jose/0000-0002-8155-5360 FU National Science Foundation [BSC 0514116]; National Geographic Society [7748-04]; Wenner-Gren Foundation [7299]; Smithsonian National Museum of Natural History; Smithsonian Tropical Research Institute; College of Liberal Arts, Temple University FX We thank 3 anonymous reviewers for their helpful comments on the manuscript. We also thank the Instituto Nacional de Antropologia e Historia for permission to carry out the research and Froylan Cuenca, the Xihuatoxtla Shelter landowner, for his support. This research was funded by the National Science Foundation (Grant BSC 0514116), the National Geographic Society (Grant 7748-04), the Wenner-Gren Foundation (Grant 7299), the Smithsonian National Museum of Natural History, Smithsonian Tropical Research Institute, and the College of Liberal Arts, Temple University. NR 32 TC 82 Z9 85 U1 7 U2 31 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD MAR 31 PY 2009 VL 106 IS 13 BP 5014 EP 5018 DI 10.1073/pnas.0812590106 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 427PG UT WOS:000264790600013 PM 19307573 ER PT J AU Piperno, DR Ranere, AJ Holst, I Iriarte, J Dickau, R AF Piperno, Dolores R. Ranere, Anthony J. Holst, Irene Iriarte, Jose Dickau, Ruth TI Starch grain and phytolith evidence for early ninth millennium BP maize from the Central Balsas River Valley, Mexico SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE early Holocene; maize domestication; phytoliths; starch grains ID ZEA-MAYS; DOMESTICATION; TEOSINTE; ORIGIN; EVOLUTION; ECUADOR; POACEAE; LOCUS AB Questions that still surround the origin and early dispersals of maize (Zea mays L.) result in large part from the absence of information on its early history from the Balsas River Valley of tropical southwestern Mexico, where its wild ancestor is native. We report starch grain and phytolith data from the Xihuatoxtia shelter, located in the Central Balsas Valley, that indicate that maize was present by 8,700 calendrical years ago (cal. B.P.). Phytolith data also indicate an early preceramic presence of a domesticated species of squash, possibly Cucurbita argyrosperma. The starch and phytolith data also allow an evaluation of current hypotheses about how early maize was used, and provide evidence as to the tempo and timing of human selection pressure on 2 major domestication genes in Zea and Cucurbita. Our data confirm an early Holocene chronology for maize domestication that has been previously indicated by archaeological and paleoecological phytolith, starch grain, and pollen data from south of Mexico, and reshift the focus back to an origin in the seasonal tropical forest rather than in the semiarid highlands. C1 [Piperno, Dolores R.] Smithsonian Natl Museum Nat Hist, Dept Anthropol, Archaeobiol Program, Washington, DC 20560 USA. [Piperno, Dolores R.; Ranere, Anthony J.; Holst, Irene] Smithsonian Trop Res Inst, Balboa, Panama. [Ranere, Anthony J.; Dickau, Ruth] Temple Univ, Dept Anthropol, Philadelphia, PA 19122 USA. [Iriarte, Jose] Univ Exeter, Dept Archaeol, Sch Geog Archaeol & Earth Resources, Exeter EX4 4QJ, Devon, England. RP Piperno, DR (reprint author), Smithsonian Natl Museum Nat Hist, Dept Anthropol, Archaeobiol Program, Washington, DC 20560 USA. EM pipernod@si.edu RI Iriarte, Jose /A-1141-2010; OI Iriarte, Jose/0000-0002-8155-5360 FU National Science Foundation [BSC 0514116]; National Geographic Society; Wenner-Gren Foundation; Smithsonian National Museum of Natural History; Smithsonian Tropical Research Institute; College of Liberal Arts, Temple University FX This research was funded by grants from the National Science Foundation (BSC 0514116), the National Geographic Society, the Wenner-Gren Foundation, the Smithsonian National Museum of Natural History, the Smithsonian Tropical Research Institute, and the College of Liberal Arts, Temple University. We thank the Instituto Nacional de Antropologia e Historia for permission to carry out the research and Froylan Cuenca, the Xihuatoxtla Shelter land owner, for his support. We also thank the 3 anonymous reviewers for their helpful comments on the manuscript. NR 28 TC 156 Z9 164 U1 7 U2 38 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD MAR 31 PY 2009 VL 106 IS 13 BP 5019 EP 5024 DI 10.1073/pnas.0812525106 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 427PG UT WOS:000264790600014 PM 19307570 ER PT J AU Blackledge, TA Scharff, N Coddington, JA Szuts, T Wenzel, JW Hayashi, CY Agnarsson, I AF Blackledge, Todd A. Scharff, Nikolaj Coddington, Jonathan A. Szuts, Tamas Wenzel, John W. Hayashi, Cheryl Y. Agnarsson, Ingi TI Reconstructing web evolution and spider diversification in the molecular era SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE Araneidae; behavioral evolution; cribellate silk; orb web; speciation ID ORB-WEAVING SPIDERS; RNA GENES 18S; CAPTURE THREADS; PHYLOGENETIC PLACEMENT; HAWAIIAN-ISLANDS; ARANEAE; THERIDIIDAE; ARANEOIDEA; SILK; NUCLEAR AB The evolutionary diversification of spiders is attributed to spectacular innovations in silk. Spiders are unique in synthesizing many different kinds of silk, and using silk for a variety of ecological functions throughout their lives, particularly to make prey-catching webs. Here, we construct a broad higher-level phylogeny of spiders combining molecular data with traditional morphological and behavioral characters. We use this phylogeny to test the hypothesis that the spider orb web evolved only once. We then examine spider diversification in relation to different web architectures and silk use. We find strong support for a single origin of orb webs, implying a major shift in the spinning of capture silk and repeated loss or transformation of orb webs. We show that abandonment of costly cribellate capture silk correlates with the 2 major diversification events in spiders (1). Replacement of cribellate silk by aqueous silk glue may explain the greater diversity of modern orb-weaving spiders (Araneoidea) compared with cribellate orb-weaving spiders (Deinopoidea) (2). Within the "RTA clade," which is the sister group to orb-weaving spiders and contains half of all spider diversity, >90% of species richness is associated with repeated loss of cribellate silk and abandonment of prey capture webs. Accompanying cribellum loss in both groups is a release from substrate-constrained webs, whether by aerially suspended webs, or by abandoning webs altogether. These behavioral shifts in silk and web production by spiders thus likely played a key role in the dramatic evolutionary success and ecological dominance of spiders as predators of insects. C1 [Blackledge, Todd A.; Agnarsson, Ingi] Univ Akron, Dept Biol, Akron, OH 44325 USA. [Blackledge, Todd A.; Agnarsson, Ingi] Univ Akron, Integrated Biosci Program, Akron, OH 44325 USA. [Scharff, Nikolaj; Szuts, Tamas] Univ Copenhagen, Zool Museum, Dept Entomol, DK-2100 Copenhagen, Denmark. [Coddington, Jonathan A.] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20013 USA. [Wenzel, John W.] Ohio State Univ, Dept Entomol, Columbus, OH 43212 USA. [Hayashi, Cheryl Y.] Univ Calif Riverside, Dept Biol, Riverside, CA 92521 USA. [Agnarsson, Ingi] Univ Puerto Rico, Dept Biol, Rio Piedras, PR 00931 USA. RP Blackledge, TA (reprint author), Univ Akron, Dept Biol, Akron, OH 44325 USA. EM blackledge@uakron.edu RI Szuts, Tamas/A-8241-2011; Scharff, Nikolaj/A-4787-2013 OI Scharff, Nikolaj/0000-0001-6809-2878 FU National Science Foundation [DEB-0516038, DEB-0516028, EAR-0228699]; Slovenian Research Agency Research Fellowship [ARRS Z1-9799-0618-07]; Danish Natural Science Research Council [21020502]; Marie Curie Intra European Fellowship Award [025850] FX We thank Charles Griswold (California Academy of Sciences, San Francisco), Marshal Hedin (San Diego State University, San Diego), Brent Opell (Virginia Polytechnic Institute, Blacksburg, VA), and Meghan Rector (Ohio State University, Columbus, OH) for providing specimens for this study; Mark Stowe for assisting in specimen collection; Mariam Lekveishvili and Alpana Chaudhuri for assisting with some sequencing; Ward Wheeler, Gonzalo Giribet, and Dimitar Dimitrov for advising us on POY4. This work was supported by National Science Foundation Awards DEB-0516038 (to T.A.B.), DEB-0516028 (to J.W.W.), and EAR-0228699 (to J.C.), Slovenian Research Agency Research Fellowship ARRS Z1-9799-0618-07 (to I.A.), Danish Natural Science Research Council Award 21020502 (to N.S.); and Marie Curie Intra European Fellowship Award 025850 (to T.S.). NR 76 TC 140 Z9 142 U1 15 U2 64 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD MAR 31 PY 2009 VL 106 IS 13 BP 5229 EP 5234 DI 10.1073/pnas.0901377106 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 427PG UT WOS:000264790600051 PM 19289848 ER PT J AU Ricolleau, A Fei, YW Cottrell, E Watson, H Deng, LW Zhang, L Fiquet, G Auzende, AL Roskosz, M Morard, G Prakapenka, V AF Ricolleau, Angele Fei, Yingwei Cottrell, Elizabeth Watson, Heather Deng, Liwei Zhang, Li Fiquet, Guillaume Auzende, Anne-Line Roskosz, Mathieu Morard, Guillaume Prakapenka, Vitali TI Density profile of pyrolite under the lower mantle conditions SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID EARTHS LOWER MANTLE; THERMOELASTIC PROPERTIES; HIGH-PRESSURE; SILICATE PEROVSKITE; NATURAL PERIDOTITE; MGSIO3 PEROVSKITE; CASIO3 PEROVSKITE; PHASE; TEMPERATURE; TRANSITION AB The pyrolite model is one of the possible compositions of the Earth's lower mantle. The lower mantle's composition is generally modelled by comparing seismic observations with mineral physics data of possible lower mantle end-member phases. Here, we report the compression behavior of a natural KLB-1 peridotite (a representative composition of the pyrolite model) in a quasi-hydrostatic environment at simultaneous high pressure (P) and temperature (T), covering the entire range of lower mantle P-T conditions up to 112 GPa. This is the first experimentally determined density profile of pyrolite under the lower mantle conditions. The results allow us to directly compare the measured density of peridotite mantle along the geotherm with the Preliminary Reference Earth Model (PREM) derived from seismic observations, without extrapolation. The comparison shows significant mismatch between the two, which calls for a re-evaluation of the PREM density model or a non-pyrolite lower mantle composition. Citation: Ricolleau, A., et al. (2009), Density profile of pyrolite under the lower mantle conditions, Geophys. Res. Lett., 36, L06302, doi:10.1029/2008GL036759. C1 [Ricolleau, Angele; Fei, Yingwei; Cottrell, Elizabeth; Watson, Heather; Deng, Liwei; Zhang, Li] Carnegie Inst Sci, Geophys Lab, Washington, DC 20015 USA. [Fiquet, Guillaume; Auzende, Anne-Line; Morard, Guillaume] Inst Phys Globe, IMPMC, F-75015 Paris, France. [Prakapenka, Vitali] Univ Chicago, Ctr Adv Radiat Sources, Argonne, IL 60439 USA. [Roskosz, Mathieu] Univ Sci & Tech Lille, Lab Struct & Proprietes Etat Solide, F-59655 Villeneuve Dascq, France. [Cottrell, Elizabeth] Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. [Deng, Liwei] Peking Univ, Sch Earth & Space Sci, Beijing 100871, Peoples R China. [Morard, Guillaume] European Synchrotron Radiat Facil, F-38043 Grenoble, France. RP Ricolleau, A (reprint author), Carnegie Inst Sci, Geophys Lab, 5251 Broad Branch Rd NW, Washington, DC 20015 USA. EM a.ricolleau@gl.ciw.edu RI Fei, Yingwei/F-3709-2011; Fiquet, Guillaume/H-1219-2011; 中国科学院, 地球深部研究重点实验室/E-2300-2014; Fiquet, Guillaume/M-6934-2014; Zhang, Li/I-4658-2013; OI Fei, Yingwei/0000-0001-9955-5353; Watson, Heather/0000-0003-4307-6518 FU National Science Foundation; DOE; State of Illinois FX This study was supported by the National Science Foundation (Geophysics grant to YF) and the Carnegie Institution of Washington. We thank Eiichi Takahashi for providing the KLB-1 sample. The experimental work was performed at GeoSoilEnviroCARS synchrotron beamline, supported by NSF, DOE, and the State of Illinois. NR 30 TC 36 Z9 36 U1 0 U2 27 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 MAR 24 PY 2009 VL 36 AR L06302 DI 10.1029/2008GL036759 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 426AA UT WOS:000264678500001 ER PT J AU Haeder, S Wirth, R Herz, H Spiteller, D AF Haeder, Susanne Wirth, Rainer Herz, Hubert Spiteller, Dieter TI Candicidin-producing Streptomyces support leaf-cutting ants to protect their fungus garden against the pathogenic fungus Escovopsis SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE Acromyrmex; antifungal agent; symbionts; Attini; polyketides ID GROWING ANTS; GENE-CLUSTER; GLAND SECRETION; BACTERIA; IDENTIFICATION; ANTIBIOTICS; COEVOLUTION; PARASITES; COMPLEX; DNA AB Leaf-cutting ants such as Acromyrmex octospinosus live in obligate symbiosis with fungi of the genus Leucoagaricus, which they grow with harvested leaf material. The symbiotic fungi, in turn, serve as a major food source for the ants. This mutualistic relation is disturbed by the specialized pathogenic fungus Escovopsis sp., which can overcome Leucoagaricus sp. and thus destroy the ant colony. Microbial symbionts of leaf-cutting ants have been suggested to protect the fungus garden against Escovopsis by producing antifungal compounds [Currie CR, Scott JA, Summerbell RC, Malloch D (1999) Fungus-growing ants use antibiotic-producing bacteria to control garden parasites. Nature 398: 701-704.]. To date, however, the chemical nature of these compounds has remained elusive. We characterized 19 leaf-cutting ant-associated microorganisms (5 Pseudonocardia, 1 Dermacoccus, and 13 Streptomyces) from 3 Acromyrmex species, A. octospinosus, A. echinatior, and A. volcanus, using 16S-rDNA analysis. Because the strain Streptomyces sp. Ao10 proved highly active against the pathogen Escovopsis, we identified the molecular basis of its antifungal activity. Using bioassay-guided fractionation, high-resolution electrospray mass spectrometry (HR-ESI-MS), and UV spectroscopy, and comparing the results with an authentic standard, we were able identify candicidin macrolides. Candicidin macrolides are highly active against Escovopsis but do not significantly affect the growth of the symbiotic fungus. At least one of the microbial isolates from each of the 3 leaf-cutting ant species analyzed produced candicidin macrolides. This suggests that candicidins play an important role in protecting the fungus gardens of leaf-cutting ants against pathogenic fungi. C1 [Haeder, Susanne; Spiteller, Dieter] Max Planck Inst Chem Ecol, Dept Bioorgan Chem, D-07745 Jena, Germany. [Wirth, Rainer] Tech Univ Kaiserslautern, Dept Plant Ecol & Tech, D-67663 Kaiserslautern, Germany. [Herz, Hubert] Smithsonian Trop Res Inst, Balboa, Panama. [Herz, Hubert] San Francisco State Univ, Dept Biol, San Francisco, CA 94132 USA. RP Haeder, S (reprint author), Max Planck Inst Chem Ecol, Dept Bioorgan Chem, Hans Knoll Str 8, D-07745 Jena, Germany. EM dspiteller@ice.mpg.de RI Wirth, Rainer/I-1552-2013 OI Wirth, Rainer/0000-0001-8042-3123 NR 36 TC 111 Z9 114 U1 7 U2 56 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD MAR 24 PY 2009 VL 106 IS 12 BP 4742 EP 4746 DI 10.1073/pnas.0812082106 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 423VA UT WOS:000264522600032 PM 19270078 ER PT J AU Winter, WT Takahashi, Y AF Winter, William T. Takahashi, Yae TI Nanocellulose composites with soybean oil polyesters SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract C1 [Winter, William T.] SUNY ESF, Cellulose Res Inst, Syracuse, NY 13210 USA. [Winter, William T.] SUNY ESF, Dept Chem, Syracuse, NY 13210 USA. [Takahashi, Yae] Smithsonian Inst, Washington, DC 20560 USA. EM cellulose@esf.edu; yatakaha@syr.edu NR 0 TC 0 Z9 0 U1 0 U2 5 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD MAR 22 PY 2009 VL 237 MA 90-IEC PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA V16GJ UT WOS:000207857802792 ER PT J AU Winter, WT Goodrich, JD Takahashi, Y AF Winter, William T. Goodrich, Jacob D. Takahashi, Yae TI Nanocellulose and nanochitin reinforced polycaprolactone SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract C1 [Winter, William T.] SUNY ESF, Cellulose Res Inst, Edwin C Jahn Lab 121, Syracuse, NY 13210 USA. [Winter, William T.] SUNY ESF, Dept Chem, Edwin C Jahn Lab 121, Syracuse, NY 13210 USA. [Goodrich, Jacob D.] Eastman Chem Co, Kingsport, TN 37662 USA. [Takahashi, Yae] Smithsonian Inst, Washington, DC 20560 USA. EM cellulose@esf.edu; jgoodrich@eastman.com; yatakaha@syr.edu NR 0 TC 0 Z9 0 U1 0 U2 5 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD MAR 22 PY 2009 VL 237 MA 218-CELL PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA V16GJ UT WOS:000207857801794 ER PT J AU Zhang, P Maeda, S Morokuma, K Braams, BJ AF Zhang, Peng Maeda, Satoshi Morokuma, Keiji Braams, Bastiaan J. TI Photochemical reactions of the low-lying excited states of formaldehyde: T-1/S-0 intersystem crossings, characteristics of the S-1 and T-1 potential energy surfaces, and a global T-1 potential energy surface SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article DE ab initio calculations; configuration interactions; ground states; isomerisation; least squares approximations; many-body problems; organic compounds; photodissociation; photoexcitation; potential energy surfaces; reaction kinetics theory; spin-orbit interactions ID INITIO MOLECULAR-DYNAMICS; DENSITY-FUNCTIONAL THEORY; HYPERSPHERE SEARCH METHOD; CONFIGURATION-INTERACTION CALCULATIONS; TRANSITION-STATE; UNIMOLECULAR DISSOCIATION; COUPLED-CLUSTER; BARRIER HEIGHT; TRIPLET FORMALDEHYDE; PHOTO-DISSOCIATION AB Accurate ab initio calculations using the multireference configuration interaction method have been performed to characterize the potential energy surfaces (PESs) of low-lying excited states (S-1 and T-1) of formaldehyde (H2CO) and hydroxymethylene (HCOH) with emphasis on their isomerization, dissociation, and the possible role of the T-1 state in the nonadiabatic photodissociation of H2CO. Two regions on the T-1 PES are found to contribute to the nonadiabatic transition to the ground (S-0) state. Three minima on the seam of crossing (MSXs), 80-85 kcal/mol (above the S-0 global minimum), are located in the HCOH region; they, however, are blocked by a high-energy isomerization transition state at similar to 107 kcal/mol. The other MSX discovered in the H2CO region is reachable with energy <= 91 kcal/mol and strong spin-orbit interaction; this may be a more important pathway for the T-1 to S-0 transition. A full-dimensional PES is generated for the T-1 state, fitted by a weighted least-squares method employing a many-body expansion in which each term is a function of the internuclear distances and is invariant under permutations of like atoms. The single global function covers the formaldehyde and the HCOH regions as well as dissociation pathways. The high quality of the fitted PES is demonstrated by the small root-mean-square fitting error of 119 cm(-1) and the close agreement between the critical points from ab initio calculations and from the fitted PES. C1 [Zhang, Peng; Maeda, Satoshi; Morokuma, Keiji; Braams, Bastiaan J.] Emory Univ, Dept Chem, Atlanta, GA 30322 USA. [Zhang, Peng; Maeda, Satoshi; Morokuma, Keiji; Braams, Bastiaan J.] Emory Univ, Cherry L Emerson Ctr Sci Computat, Atlanta, GA 30322 USA. [Morokuma, Keiji] Kyoto Univ, Fukui Inst Fundamental Chem, Kyoto 6068103, Japan. RP Zhang, P (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom Mol & Opt Phys ITAMP, 60 Garden St, Cambridge, MA 02138 USA. EM morokuma@emory.edu RI Braams, Bastiaan/E-7687-2011; Maeda, Satoshi/H-3613-2014 OI Braams, Bastiaan/0000-0003-4086-9969; FU AFOSR [FA9550-04-1-0080, FA9550-07-1-0395]; Office of Naval Research [N00014-05-1-0460]; Japan Society for Promotion of Sciences (JSPS) FX The research of K. M. and P. Z. was in part supported by grants from AFOSR (Grant Nos. FA9550-04-1-0080 and FA9550-07-1-0395) and of B.J.B. by the Office of Naval Research under Grant No. N00014-05-1-0460. S. M. acknowledges Postdoctoral Fellowship from the Japan Society for Promotion of Sciences (JSPS). Computational resource was provided by a grant under the DoD-High Performance Computing Program and by the Research Center for Computational Science, Okazaki, Japan. This work was carried out during 2004-2005 and has been included in the Ph.D. thesis of P. Z. NR 77 TC 17 Z9 17 U1 3 U2 22 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0021-9606 J9 J CHEM PHYS JI J. Chem. Phys. PD MAR 21 PY 2009 VL 130 IS 11 AR 114304 DI 10.1063/1.3085952 PG 10 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 421TE UT WOS:000264380400014 PM 19317536 ER PT J AU Gray, MD Wittkowski, M Scholz, M Humphreys, EML Ohnaka, K Boboltz, D AF Gray, M. D. Wittkowski, M. Scholz, M. Humphreys, E. M. L. Ohnaka, K. Boboltz, D. TI SiO maser emission in Miras SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE masers; stars: AGB and post-AGB; circumstellar matter; stars: evolution; radio lines: stars ID VARIABLE S-ORIONIS; VLBA OBSERVATIONS; RADIO PHOTOSPHERES; H+SIO COLLISIONS; MOLECULAR LAYER; CROSS-SECTIONS; DUST SHELL; AGB STARS; R-AQUARII; 4 EPOCHS AB We describe a combined dynamic atmosphere and maser propagation model of SiO maser emission in Mira variables. This model rectifies many of the defects of an earlier model of this type, particularly in relation to the infrared (IR) radiation field generated by dust and various wavelength-dependent, optically thick layers. Modelled masers form in rings with radii consistent with those found in very long baseline interferometry (VLBI) observations and with earlier models. This agreement requires the adoption of a radio photosphere of radius approximately twice that of the stellar photosphere, in agreement with observations. A radio photosphere of this size renders invisible certain maser sites with high amplification at low radii, and conceals high-velocity shocks, which are absent in radio continuum observations. The SiO masers are brightest at an optical phase of 0.1-0.25, which is consistent with observed phase lags. Dust can have both mild and profound effects on the maser emission. Maser rings, a shock and the optically thick layer in the SiO pumping band at 8.13 mu m appear to be closely associated in three out of four phase samples. C1 [Gray, M. D.] Univ Manchester, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Wittkowski, M.] ESO, D-85748 Garching, Germany. [Scholz, M.] Heidelberg Univ, Inst Theoret Astrophys, Zentrum Astron ZAH, D-69120 Heidelberg, Germany. [Scholz, M.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia. [Humphreys, E. M. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ohnaka, K.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Boboltz, D.] USN Observ, Washington, DC 20392 USA. RP Gray, MD (reprint author), Univ Manchester, Jodrell Bank Ctr Astrophys, Alan Turing Bldg, Manchester M13 9PL, Lancs, England. EM mgray@aoc.nrao.edu OI Wittkowski, Markus/0000-0002-7952-9550 FU STFC (formerly PPARC) [PP/C000250/1]; UK STFC FX MDG acknowledges STFC (formerly PPARC) for financial support under the 2005-2010 rolling grant, number PP/C000250/1. Computations were carried out at the HiPerSPACE Computing Centre, UCL, which is funded by the UK STFC. The authors would like to thank Lee Anne Willson for detailed comments on the manuscript. NR 61 TC 29 Z9 29 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 21 PY 2009 VL 394 IS 1 BP 51 EP 66 DI 10.1111/j.1365-2966.2008.14237.x PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 415WR UT WOS:000263967700005 ER PT J AU Purcell, CR Longmore, SN Burton, MG Walsh, AJ Minier, V Cunningham, MR Balasubramanyam, R AF Purcell, C. R. Longmore, S. N. Burton, M. G. Walsh, A. J. Minier, V. Cunningham, M. R. Balasubramanyam, R. TI Physical and chemical conditions in methanol maser selected hot cores and UCH II regions SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE surveys; stars: formation; stars: pre-main-sequence; ISM: abundances; ISM: molecules ID MASSIVE STAR-FORMATION; GHZ SPECTRAL SURVEY; MOLECULAR LINE SURVEY; ORION-KL; SAGITTARIUS B2; CLOUD MASSES; DARK CLOUDS; HII-REGIONS; MILLIMETER; G34.3+0.15 AB We present the results of a targeted 3-mm spectral line survey towards the eighty-three 6.67 GHz methanol maser selected star-forming clumps observed by Purcell. In addition to the previously reported measurements of HCO(+) (1-0), H(13)CO(+) (1-0) and CH(3)CN (5-4) and (6-5), we used the Mopra antenna to detect emission lines of N(2)H(+) (1-0), HCN (1-0) and HNC (1-0) towards 82/83 clumps (99 per cent), and CH(3)OH (2-1) towards 78/83 clumps (94 per cent). The molecular line data have been used to derive virial and local thermodynamic equilibrium masses, rotational temperatures and chemical abundances in the clumps, and these properties have been compared between subsamples associated with different indicators of evolution. The greatest differences are found between clumps associated with 8.6 GHz radio emission, indicating the presence of an Ultra-Compact H II (UCH II) region, and 'isolated' masers (without associated radio emission), and between clumps exhibiting CH(3)CN emission and those without. In particular, thermal CH(3)OH is found to be brighter and more abundant in UCH II regions and in sources with detected CH(3)CN, and may constitute a crude molecular clock in single dish observations. Clumps associated with 8.6 GHz radio emission tend to be more massive and more luminous than clumps without radio emission. This is likely because the most massive clumps evolve so rapidly that a Hyper-Compact H II or UCH II region is the first visible tracer of star formation. The gas mass to submm/infrared luminosity relation for the combined sample was found to be L proportional to M(0.68), considerably shallower than expected for massive main-sequence stars. This implies that the mass of the clumps is comparable to, or greater than, the mass of the stellar content. We also find that the mass of the hot core is correlated with the mass of the clump in which it is embedded. C1 [Purcell, C. R.] Univ Manchester, Jodrell Bank Observ, Macclesfield SK11 9DL, Cheshire, England. [Purcell, C. R.; Longmore, S. N.; Burton, M. G.; Walsh, A. J.; Minier, V.; Cunningham, M. R.; Balasubramanyam, R.] Univ New S Wales, Sch Phys, Sydney, NSW 2052, Australia. [Longmore, S. N.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Longmore, S. N.] CSIRO Australia Telescope Natl Facil, Epping, NSW 1710, Australia. [Walsh, A. J.] James Cook Univ, Ctr Astron, Townsville, Qld 4811, Australia. [Minier, V.] CEA Saclay, DSM, DAPNIA, Serv Astrophys, F-91191 Gif Sur Yvette, France. [Minier, V.] Univ Paris 07, CNRS, CEA, UMR 7158,CEA Saclay,AIM, F-91191 Gif Sur Yvette, France. [Balasubramanyam, R.] Raman Res Inst, Bangalore 560080, Karnataka, India. RP Purcell, CR (reprint author), Univ Manchester, Jodrell Bank Observ, Macclesfield SK11 9DL, Cheshire, England. EM Cormac.Purcell@manchester.ac.uk RI Balasubramanyam, Ramesh/A-1343-2010; Balasubramanyam, Ramesh/D-4881-2012; Astronomy & Astrophysics Group, Raman Res Institute/D-4046-2012; Walsh, Andrew/B-5627-2013; M, Manjunath/N-4000-2014; OI Cunningham, Maria/0000-0001-7020-6176; Walsh, Andrew/0000-0001-9506-0855; M, Manjunath/0000-0001-8710-0730; Purcell, Cormac/0000-0002-7491-7386; Balasubramanyam, Ramesh/0000-0003-0371-946X; Burton, Michael/0000-0001-7289-1998 FU Australian Research Council; UNSW; University of New South Wales School of Physics Scholarship; Commonwealth of Australia FX We would also like to thank the anonymous referee for being especially thorough in seeking out mistakes in the paper. His/her comments were extremely useful and have helped to improve the presentation and interpretation. NR 53 TC 26 Z9 27 U1 0 U2 0 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAR 21 PY 2009 VL 394 IS 1 BP 323 EP 339 DI 10.1111/j.1365-2966.2008.14283.x PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 415WR UT WOS:000263967700026 ER PT J AU Roelofs, GHA Groot, PJ Steeghs, D Rau, A de Groot, E Marsh, TR Nelemans, G Liebert, J Woudt, P AF Roelofs, G. H. A. Groot, P. J. Steeghs, D. Rau, A. de Groot, E. Marsh, T. R. Nelemans, G. Liebert, J. Woudt, P. TI SDSS J080449.49+161624.8: a peculiar AM CVn star from a colour-selected sample of candidates SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; binaries: close; stars: individual: SDSS J080449.49+161624.8; novae, cataclysmic variables; white dwarfs ID CANUM-VENATICORUM BINARIES; DIGITAL-SKY-SURVEY; DOUBLE-DEGENERATE BINARY; XMM-NEWTON OBSERVATIONS; ORBITAL PERIOD; CATACLYSMIC VARIABLES; ACCRETION DISCS; WHITE-DWARFS; GP COM; X-RAY AB We describe a spectroscopic survey designed to uncover an estimated similar to 40 AM Canum Venaticorum (AM CVn) stars hiding in the photometric data base of the Sloan Digital Sky Survey. We have constructed a relatively small sample of about 1500 candidates based on a colour selection, which should contain the majority of all AM CVn binaries while remaining small enough that spectroscopic identification of the full sample is feasible. We present the first new AM CVn star discovered using this strategy, SDSS J080449.49+161624.8, the ultracompact binary nature of which is demonstrated using high-time-resolution spectroscopy obtained with the Magellan telescopes at Las Campanas Observatory, Chile. A kinematic 'S-wave' feature is observed on a period P(orb) = 44.5 +/- 0.1 min, which we propose is the orbital period, although the present data cannot yet exclude its nearest daily aliases. The new AM CVn star shows a peculiar spectrum of broad, single-peaked helium emission lines with unusually strong series of ionized helium, reminiscent of the (intermediate) polars among the hydrogen-rich cataclysmic variables. We speculate that SDSS J0804+1616 may be the first magnetic AM CVn star. The accreted material appears to be enriched in nitrogen, to N/O greater than or similar to 10 and N/C > 10 by number, indicating CNO cycle hydrogen burning, but no helium burning, in the prior evolution of the donor star. C1 [Roelofs, G. H. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Steeghs, D.; Marsh, T. R.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Rau, A.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Liebert, J.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Woudt, P.] Univ Cape Town, Dept Astron, ZA-7700 Rondebosch, South Africa. [Groot, P. J.; de Groot, E.; Nelemans, G.] Radboud Univ Nijmegen, Dept Astrophys, NL-6500 GL Nijmegen, Netherlands. RP Roelofs, GHA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM groelofs@cfa.harvard.edu RI Nelemans, Gijs/D-3177-2012; Steeghs, Danny/C-5468-2009; Groot, Paul/K-4391-2016 OI Nelemans, Gijs/0000-0002-0752-2974; Steeghs, Danny/0000-0003-0771-4746; Groot, Paul/0000-0002-4488-726X FU NWO [680.50.0610]; STFC Advanced Fellowship; Netherlands Organization FX GHAR is supported by NWO Rubicon grant 680.50.0610. DS acknowledges a STFC Advanced Fellowship. GN is supported by the Netherlands Organization for Scientific Research. Based on data taken with the Magellan Telescopes at Las Campanas Observatory, Chile, and with the Isaac Newton Telescope in the Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias, Spain. This study makes use of the SDSS, see http://www.sdss.org/collaboration/credits.html for the full acknowledgment. Special thanks to P. Berlind and the 1.5-m telescope crew at F.L. Whipple Observatory (a facility of the Smithsonian Institution) for their valuable contribution and to L. Yungelson for helpful discussion. Fig. 1 makes use of white-dwarf model spectra kindly provided by D. Koester. NR 41 TC 25 Z9 25 U1 0 U2 1 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAR 21 PY 2009 VL 394 IS 1 BP 367 EP 374 DI 10.1111/j.1365-2966.2008.14288.x PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 415WR UT WOS:000263967700029 ER PT J AU Ercolano, B Clarke, CJ Robitaille, TP AF Ercolano, B. Clarke, C. J. Robitaille, T. P. TI The transition disc frequency in M stars SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; circumstellar matter; planetary systems: protoplanetary discs; stars: pre-main-sequence ID T-TAURI STARS; SPECTRAL ENERGY-DISTRIBUTIONS; YOUNG STELLAR OBJECTS; PROTOPLANETARY DISCS; SPITZER OBSERVATIONS; ENVELOPES; ACCRETION; EVOLUTION; MODELS; GROWTH AB We re-examine the recent suggestion of a high fraction of transition discs (i.e. those with a cleared inner hole) in M stars, motivated by the fact that we expect that, for M stars, even discs without inner holes should exhibit very weak excess shortwards of around 10 mu m. Our analysis of spectral energy distribution models suggests that this indeed means that M stars where a detectable excess begins at around 6 mu m may be misclassified as transition discs when in fact they have optically thick dust extending in to the dust sublimation radius. Consequently, we estimate that the transition disc fraction among M stars in the Coronet cluster is similar to 15 +/- 10 per cent (rather than the recently claimed value of 50 per cent). This revised figure would imply that the transition disc fraction is not after all markedly higher in later type stars. We suggest that, for M stars, transition discs can only be readily identified if they have emission that is close to photospheric out to > 10 mu m. C1 [Ercolano, B.; Clarke, C. J.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Robitaille, T. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Ercolano, B (reprint author), Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. EM be@ast.cam.ac.uk OI Robitaille, Thomas/0000-0002-8642-1329 FU NASA FX We thank the referee Barbara Whitney for helpful discussion and suggestions which aided to the clarity of our work. We also thank Aurora Sicilia-Aguilar for a thorough analysis of our work and for helpful suggestions. TPR acknowledges support from NASA through the Spitzer Space Telescope Fellowship Program. NR 27 TC 33 Z9 33 U1 0 U2 0 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAR 21 PY 2009 VL 394 IS 1 BP L141 EP L145 DI 10.1111/j.1745-3933.2009.00634.x PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 594ZT UT WOS:000277581200030 ER PT J AU Munoz-Darias, T Casares, J O'Brien, K Steeghs, D Martinez-Pais, IG Cornelisse, R Charles, PA AF Munoz-Darias, T. Casares, J. O'Brien, K. Steeghs, D. Martinez-Pais, I. G. Cornelisse, R. Charles, P. A. TI Dynamical constraints on the neutron star mass in EXO 0748-676 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; binaries: close; stars: individual: EXO 0748-676; X-rays: stars ID X-RAY BINARY; MULTIWAVELENGTH OBSERVATIONS; ACCRETION DISKS; URSAE-MAJORIS; BLACK-HOLE; DONOR STAR; EXO-0748-676; EMISSION; DISCOVERY; X1822-371 AB We present Very Large Telescope (VLT) intermediate resolution spectroscopy of UY Vol, the optical counterpart of the low mass X-ray binary (LMXB) X-ray burster EXO 0748-676. By using Doppler tomography we detect narrow components within the broad He II lambda 4542, lambda 4686 and lambda 5412 emission lines. The phase, velocity and narrowness of these lines are consistent with their arising from the irradiated hemisphere of the donor star, as has been observed in a number of LMXBs. Under this assumption, we provide the first dynamical constraints on the stellar masses in this system. In particular, we measure K(2) > K(em) = 300 +/- 10 km s(-1). Using this value, we derive 1 M(circle dot) <= M(1) <= 2.4 M(circle dot) and 0.11 <= q <= 0.28. We find M(1) >= 1.5 M(circle dot) for the case of a main sequence companion star. Our results are consistent with the presence of a massive neutron star as has been suggested by Ozel (2006), although we cannot discard the canonical value of similar to 1.4 M(circle dot). C1 [Munoz-Darias, T.; Casares, J.; Martinez-Pais, I. G.; Cornelisse, R.] Inst Astrofis Canarias, Tenerife 38200, Spain. [O'Brien, K.] European So Observ, Santiago 19, Chile. [Steeghs, D.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Steeghs, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Charles, P. A.] S African Astron Observ, ZA-7935 Observatory, South Africa. [Martinez-Pais, I. G.] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain. RP Munoz-Darias, T (reprint author), Inst Astrofis Canarias, Tenerife 38200, Spain. EM tmd@iac.es RI Steeghs, Danny/C-5468-2009 OI Steeghs, Danny/0000-0003-0771-4746 FU Spanish Ministry of Science and Technology [AYA2007-66887]; STFC Advanced Fellowship; Spanish MEC [CSD2006-00070] FX JC acknowledges support from the Spanish Ministry of Science and Technology through the project AYA2007-66887. DS acknowledges a STFC Advanced Fellowship. Partially funded by the Spanish MEC under the Consolider-Ingenio 2010 Program grant CSD2006-00070: first Science with the GTC. The use of the spectral analysis software package MOLLY written by Tom Marsh is acknowledged. NR 30 TC 16 Z9 16 U1 0 U2 0 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAR 21 PY 2009 VL 394 IS 1 BP L136 EP L140 DI 10.1111/j.1745-3933.2009.00630.x PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 594ZT UT WOS:000277581200029 ER PT J AU Narayan, R Kumar, P AF Narayan, Ramesh Kumar, Pawan TI A turbulent model of gamma-ray burst variability SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE radiation mechanisms: non-thermal; gamma-rays: bursts ID PHYSICAL PARAMETERS; INTERNAL SHOCKS; EMISSION; AFTERGLOWS; PROMPT AB A popular paradigm to explain the rapid temporal variability observed in gamma-ray burst (GRB) light curves is the internal shock model. We propose an alternative model in which the radiating fluid in the GRB shell is relativistically turbulent with a typical eddy Lorentz factor gamma(t). In this model, all pulses in the gamma-ray light curve are produced at roughly the same distance R from the centre of the explosion. The burst duration is similar to R/c Gamma(2), where Gamma is the bulk Lorentz factor of the expanding shell, and the duration of individual pulses in the light curve is similar to R/c Gamma(2)gamma(2)(t). The model naturally produces highly variable light curves with similar to gamma(2)(t) individual pulses. Even though the model assumes highly inhomogeneous conditions, nevertheless the efficiency for converting jet energy to radiation is high. C1 [Narayan, Ramesh] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kumar, Pawan] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. RP Narayan, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM pk@astro.as.utexas.edu OI Narayan, Ramesh/0000-0002-1919-2730 NR 30 TC 65 Z9 66 U1 2 U2 3 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAR 21 PY 2009 VL 394 IS 1 BP L117 EP L120 DI 10.1111/j.1745-3933.2009.00624.x PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 594ZT UT WOS:000277581200025 ER PT J AU Block, DL Puerari, I Elmegreen, BG Elmegreen, DM Fazio, GG Gehrz, RD AF Block, D. L. Puerari, I. Elmegreen, B. G. Elmegreen, D. M. Fazio, G. G. Gehrz, R. D. TI DETECTION OF STAR STREAMS AND TURBULENCE IN NEARBY GALAXIES: POWER SPECTRUM ANALYSIS OF SPITZER IMAGES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: ISM; galaxies: spiral ID PRELIMINARY LUMINOSITY CLASSIFICATION; FLOCCULANT SPIRAL STRUCTURE; LARGE-MAGELLANIC-CLOUD; URSA-MAJOR GROUP; INFRARED-EMISSION; SURFACE PHOTOMETRY; HYADES SUPERCLUSTER; SIRIUS SUPERCLUSTER; REFLECTION NEBULAE; INTERSTELLAR DUST AB Fourier transform power spectra of azimuthal scans in 33 galaxies imaged with the Infrared Array Camera on the Spitzer Space Telescope show an approximate power-law structure over a wide range of wavenumbers with a gradual steepening from 3.6 or 4.5 mu m to 8.0 mu m, in the order of an increasing contribution from gas and dust. At radii with active star formation, the average of the slopes of the 8 mu m power spectra at intermediate spatial frequencies is about the same for all galaxies, independent of spiral arm morphology. These power spectra are reminiscent of turbulence, although the 8 mu m slopes, averaging -2.0, are slightly steeper than expected (-1.7). Reconstructed images using only these intermediate spatial frequencies at 4.5 mu m show aging star complexes distorted by shear. These sheared features illustrate the transition from a hierarchical structure during star formation into azimuthal star streams like the Pleiades moving group in the Solar neighborhood. This is the first time that young star streams have been observed in spiral galaxies other than the Milky Way. C1 [Block, D. L.] Univ Witwatersrand, Sch Computat & Appl Math, ZA-2050 Wits, South Africa. [Puerari, I.] Inst Nacl Astrofis Opt & Electr, Puebla 72840, Mexico. [Elmegreen, B. G.] IBM Corp, Div Res, TJ Watson Res Ctr, Yorktown Hts, NY 10598 USA. [Elmegreen, D. M.] Vassar Coll, Dept Phys & Astron, Poughkeepsie, NY 12604 USA. [Fazio, G. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gehrz, R. D.] Univ Minnesota, Dept Astron, Minneapolis, MN 55455 USA. RP Block, DL (reprint author), Univ Witwatersrand, Sch Computat & Appl Math, Private Bag 3, ZA-2050 Wits, South Africa. EM david.block@wits.ac.za; puerari@inaoep.mx; bge@us.ibm.com; elmegreen@vassar.edu; gfazio@cfa.harvard.edu; gehrz@astro.umn.edu FU Mexican Foundation CONACyT [35947-E]; NASA; US Air Force FX This work is based (in part) on observations made with the SST, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. The visit of D. L. B. to the Harvard-Smithsonian Center for Astrophysics was facilitated by funding granted by the Anglo American Chairman's Fund. The Distinguished Visitor Program at the Anglo American Cosmic Dust Laboratory has partially funded the visits of I. P. over a period of several years and I. P. expresses his deep appreciation for this. I. P. also acknowledges support from the Mexican Foundation CONACyT under project 35947-E. R. D. G. was supported by NASA and the US Air Force. The authors thank C. E. Woodward and E. Polowski for their contribution to the planning, reduction, and analysis of the M33 images as members of the GGTOP collaboration. Helpful comments from the referee are appreciated. NR 71 TC 5 Z9 5 U1 1 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 20 PY 2009 VL 694 IS 1 BP 115 EP 129 DI 10.1088/0004-637X/694/1/115 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 420LQ UT WOS:000264291700011 ER PT J AU Pietsch, W Haberl, F Gaetz, TJ Hartman, JD Plucinsky, PP Tullmann, R Williams, BF Shporer, A Mazeh, T Pannuti, TG AF Pietsch, Wolfgang Haberl, Frank Gaetz, Terrance J. Hartman, Joel D. Plucinsky, Paul P. Tuellmann, Ralph Williams, Benjamin F. Shporer, Avi Mazeh, Tsevi Pannuti, Thomas G. TI DETECTION OF THE SECOND ECLIPSING HIGH-MASS X-RAY BINARY IN M 33 SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: eclipsing; galaxies: individual (M 33); X-rays: binaries; X-rays: individual ([PMH2004] 47) ID XMM-NEWTON SURVEY; LOCAL GROUP; BLACK-HOLE; INTERSTELLAR-MEDIUM; IMAGE SUBTRACTION; GALAXY M-33; H-I; M33; X-7; STARS AB Chandra data of the X-ray source [PMH2004] 47 were obtained in the ACIS Survey of M 33 (ChASeM33) in 2006. During one of the observations, the source varied from a high state to a low state and back, in two other observations it varied from a low state to respectively intermediate states. These transitions are interpreted as eclipse ingresses and egresses of a compact object in a high-mass X-ray binary (HMXB) system. The phase of mideclipse is given by HJD 245 3997.476 +/- 0.006, the eclipse half angle is 30 degrees.6 +/- 1 degrees.2. Adding XMM-Newton observations of [PMH2004] 47 in 2001 we determine the binary period to be 1.732479 +/- 0.000027 days. This period is also consistent with ROSAT HRI observations of the source in 1994. No short-term periodicity compatible with a rotation period of the compact object is detected. There are indications for a long-term variability similar to that detected for Her X-1. During the high state the spectrum of the source is hard (power-law spectrum with photon index similar to 0.85) with an unabsorbed luminosity of 2 x 10(37) erg s(-1) (0.2-4.5 keV). We identify as an optical counterpart a V similar to 21.0 mag star with T(eff) > 19000 K, log(g) > 2.5. The Canada-France-Hawaii Telescope optical light curves for this star show an ellipsoidal variation with the same period as the X-ray light curve. The optical light curve together with the X-ray eclipse can be modeled by a compact object with a mass consistent with a neutron star or a black hole in an HMXB. However, the hard power-law X-ray spectrum favors a neutron star as the compact object in this second eclipsing X-ray binary in M 33. Assuming a neutron star with a canonical mass of 1.4 M(circle dot) and the best-fit companion temperature of 33,000 K, a system inclination i = 72 degrees and a companion mass of 10.9 M(circle dot) are implied. C1 [Pietsch, Wolfgang; Haberl, Frank] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. [Gaetz, Terrance J.; Hartman, Joel D.; Plucinsky, Paul P.; Tuellmann, Ralph] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Williams, Benjamin F.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Shporer, Avi; Mazeh, Tsevi] Tel Aviv Univ, Raymond & Beverly Sackler Fac Exact Sci, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. [Pannuti, Thomas G.] Morehead State Univ, Ctr Space Sci, Morehead, KY 40351 USA. RP Pietsch, W (reprint author), Max Planck Inst Extraterr Phys, Giessenbachstr, D-85741 Garching, Germany. OI Haberl, Frank/0000-0002-0107-5237; Hartman, Joel/0000-0001-8732-6166 NR 45 TC 6 Z9 6 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 20 PY 2009 VL 694 IS 1 BP 449 EP 458 DI 10.1088/0004-637X/694/1/449 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 420LQ UT WOS:000264291700044 ER PT J AU Baldi, A Forman, W Jones, C Nulsen, P David, L Kraft, R Simionescu, A AF Baldi, A. Forman, W. Jones, C. Nulsen, P. David, L. Kraft, R. Simionescu, A. TI CHANDRA OBSERVATIONS OF THE GALAXY GROUP AWM 5: COOL CORE REHEATING AND THERMAL CONDUCTION SUPPRESSION SO ASTROPHYSICAL JOURNAL LA English DT Article DE conduction; galaxies: clusters: individual (AWM 5); galaxies: individual (NGC 6269, NGC 6265); intergalactic medium; radio continuum: galaxies; X-rays: galaxies: clusters ID DIGITAL SKY SURVEY; ACTIVE GALACTIC NUCLEI; X-RAY OBSERVATIONS; XMM-NEWTON; PERSEUS CLUSTER; POOR CLUSTERS; GASEOUS ATMOSPHERE; ELLIPTIC GALAXIES; HEAT-CONDUCTION; MAGNETIC-FIELD AB We present an analysis of a 40 ks Chandra observation of the galaxy group AWM 5. It has a small (similar to 8 kpc) dense cool core with a temperature of similar to 1.2 keV and the temperature profile decreases at larger radii, from similar to 3.5 keV just outside the core to similar to 2 keV at similar to 300 kpc from the center. The abundance distribution shows a "hole" in the central similar to 10 kpc, where the temperature declines sharply. An abundance of at least a few times solar is observed similar to 15-20 kpc from the center. The deprojected electron density profile shows a break in slope at similar to 13 kpc and can be fit by two beta models, with beta = 0.72(-0.11)(+0.16) and r(c) = 5.7(-1.5)(+1.8) kpc, for the inner part, and beta = 0.34 +/- 0.01 and r(c) = 31.3(-5.5)(+5.8) kpc, for the outer part. The mass fraction of hot gas is fairly flat in the center and increases for r > 30 kpc up to a maximum of similar to 6.5% at r similar to 380 kpc. The gas cooling time within the central 30 kpc is smaller than a Hubble time, although the temperature only declines in the central similar to 8 kpc region. This discrepancy suggests that an existing cooling core has been partially reheated. In particular, thermal conduction could have been a significant source of reheating. In order for heating due to conduction to balance cooling due to emission of X-rays, conductivity must be suppressed by a large factor (at least similar to 100). Past active galactic nuclei activity (still visible as a radio source in the center of the group) is, however, the most likely source that reheated the central regions of AWM 5. We also studied the properties of the ram pressure stripped tail in the group member NGC 6265. This galaxy is moving at M approximate to 3.4(-0.6)(+0.5)(v similar to 300 km s(-1)) through the hot group gas. The physical length of the tail is similar to 42 kpc and its mass is 2.1 +/- 0.2 x 10(9) M(circle dot). C1 [Baldi, A.; Forman, W.; Jones, C.; Nulsen, P.; David, L.; Kraft, R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Simionescu, A.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. RP Baldi, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Nulsen, Paul/0000-0003-0297-4493 NR 68 TC 7 Z9 7 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 20 PY 2009 VL 694 IS 1 BP 479 EP 491 DI 10.1088/0004-637X/694/1/479 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 420LQ UT WOS:000264291700046 ER PT J AU Blakeslee, JP Jordan, A Mei, S Cote, P Ferrarese, L Infante, L Peng, EW Tonry, JL West, MJ AF Blakeslee, John P. Jordan, Andres Mei, Simona Cote, Patrick Ferrarese, Laura Infante, Leopoldo Peng, Eric W. Tonry, John L. West, Michael J. TI THE ACS FORNAX CLUSTER SURVEY. V. MEASUREMENT AND RECALIBRATION OF SURFACE BRIGHTNESS FLUCTUATIONS AND A PRECISE VALUE OF THE FORNAX-VIRGO RELATIVE DISTANCE SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: individual (Fornax, Virgo); galaxies: distances and redshifts; galaxies: elliptical and lenticular, cD; large-scale structure of universe ID HUBBLE-SPACE-TELESCOPE; EARLY-TYPE GALAXIES; DATA REDUCTION PROCEDURES; DWARF ELLIPTIC GALAXIES; MEASURING EXTRAGALACTIC DISTANCES; MAGELLANIC STAR-CLUSTERS; STELLAR POPULATIONS; ADVANCED CAMERA; GLOBULAR-CLUSTERS; FUNDAMENTAL PLANE AB We present (g(475)-z(850)) color and z(850)-band surface brightness fluctuations (SBFs) measurements for 43 early-type galaxies in the Fornax cluster imaged with the Hubble Space Telescope Advanced Camera for Surveys. These are combined with our earlier measurements for Virgo cluster galaxies to derive a revised, nonlinear calibration of the z(850)-band SBF absolute magnitude (M) over bar (z) as a function of (g(475)-z(850)) color, valid for the AB color range 0.8 < (g(475)-z(850)) < 1.6. In all, we tabulate recalibrated SBF distances for 134 galaxies in Virgo, Fornax, the Virgo W' group, and NGC 4697 in the Virgo Southern Extension. The calibration procedure yields a highly precise relative distance modulus for Fornax with respect to Virgo of Delta(m - M)(FV) = 0.42 +/- 0.03 mag, or a distance ratio d(F) / d(V) = 1.214 +/- 0.017. The resulting Fornax distance modulus is (m - M)(For) = 31.51 +/- 0.03 +/- 0.15 mag, corresponding to d(F) = 20.0 +/- 0.3 +/- 1.4 Mpc, where the second set of error bars reflects the total systematic uncertainty from our assumed Virgo distance of 16.5 Mpc. The rms distance scatter for the early-type Fornax cluster galaxies is sigma(d) = 0.49(-0.15)(+0.11) Mpc, or a total line-of-sight depth of 2.0(-0.6)(+0.4) Mpc, consistent with its compact appearance on the sky. This translates to a depth scatter smaller than the intrinsic, or "cosmic," scatter sigma(cos) in the SBF calibration, unlike the case for the larger Virgo cluster. As a result, we are able to place the first tight constraints on the value of sigma(cos). We find sigma(cos) = 0.06 +/- 0.01 mag, with a firm upper limit of scos < 0.08 mag, for the subsample of galaxies with (g(475)-z(850)) > 1.02, but it is about twice as large for bluer galaxies. We also present an alternative SBF calibration based on the " fluctuation count" parameter (N) over bar = (m) over bar - m(tot), a proxy for galaxy mass. This gives a consistent relative distance but with larger intrinsic scatter, and we adopt the result from the calibration on (g(475)-z(850)) because of its basis in stellar population properties alone. Finally, we find no evidence for systematic trends of the galaxy distances with position or velocity (e.g., no current infall); the Fornax cluster appears both compact and well virialized. C1 [Blakeslee, John P.; Cote, Patrick; Ferrarese, Laura] Natl Res Council Canada, Herzberg Inst Astrophys, Domin Astrophys Observ, Victoria, BC V9E 2E7, Canada. [Blakeslee, John P.] Washington State Univ, Dept Phys & Astron, Pullman, WA 99163 USA. [Jordan, Andres] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Jordan, Andres; Infante, Leopoldo] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 22, Chile. [Mei, Simona] Univ Paris Denis Diderot, F-75205 Paris 13, France. [Mei, Simona] Observ Paris, Sect Meudon, GEPI, F-92195 Meudon, France. [Peng, Eric W.] Peking Univ, Dept Astron, Beijing 100871, Peoples R China. [Tonry, John L.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [West, Michael J.] European So Observ, Santiago 19, Chile. RP Blakeslee, JP (reprint author), Natl Res Council Canada, Herzberg Inst Astrophys, Domin Astrophys Observ, Victoria, BC V9E 2E7, Canada. EM John.Blakeslee@nrc.ca OI Jordan, Andres/0000-0002-5389-3944; Blakeslee, John/0000-0002-5213-3548 FU Space Telescope Science Institute [GO-10217, GO-9401] FX Support for programs GO-10217 and GO-9401 was provided through grants from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. We thank the anonymous referee for thoughtful comments that helped to improve the paper. NR 72 TC 153 Z9 153 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 20 PY 2009 VL 694 IS 1 BP 556 EP 572 DI 10.1088/0004-637X/694/1/556 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 420LQ UT WOS:000264291700051 ER PT J AU Hopkins, PF Hernquist, L AF Hopkins, Philip F. Hernquist, Lars TI A CHARACTERISTIC DIVISION BETWEEN THE FUELING OF QUASARS AND SEYFERTS: FIVE SIMPLE TESTS SO ASTROPHYSICAL JOURNAL LA English DT Review DE cosmology: theory; galaxies: active; galaxies: evolution; quasars: general ID ACTIVE GALACTIC NUCLEI; BLACK-HOLE MASS; ULTRALUMINOUS INFRARED GALAXIES; DIGITAL-SKY-SURVEY; HUBBLE-SPACE-TELESCOPE; SOFT-X-RAY; LARGE-SCALE OUTFLOWS; NARROW-LINE REGION; SPITZER MIDINFRARED SPECTROSCOPY; VELOCITY DISPERSION CORRELATION AB Given the existence of the M-BH-sigma relation, models of self-regulated black hole (BH) growth require both a fuel supply and concomitant growth of the host bulge to deepen the central potential, or else the system will either starve or immediately self-regulate without any sustained activity. This leads to a generic prediction that the brightest quasars must be triggered in major mergers: a large fraction of the galaxy mass must be added/converted to new bulge mass and a galactic supply of gas must lose angular momentum in less than a dynamical time. Low-luminosity active galactic nuclei, in contrast, require little bulge growth and small gas supplies, and could be triggered in more common nonmerger events. This leads to the expectation of a characteristic transition to merger-induced fueling around the traditional quasar-Seyfert luminosity division (growth of BH masses above/below similar to 10(7) M-circle dot). We compile and survey a number of observations in order to test several predictions of such a division, including (1) a transition to bulge-dominated hosts (which any major merger remnant, regardless of difficult-to-observe tidal features, should be). (2) A transition between "pseudobulges" and "classical" bulges hosting the remnant BHs: pseudobulges are formed in secular processes and minor mergers, whereas classical bulges are relics of major mergers. (3) An increase in the amplitude of small-scale clustering (increased halo occupation of small group environments) where mergers are more efficient. (4) Different redshift evolution, with gas-rich merger rates rising to redshifts z > 2 while secular processes are relatively constant in time. (5) An increasing prominence of post-starburst features in more luminous systems. Our compilation of observations in each of these areas provides tentative evidence for the predicted division around the Seyfert-quasar threshold, and we discuss how future observations can improve these constraints and, in combination with the tests here, break degeneracies between different fueling models. C1 [Hopkins, Philip F.; Hernquist, Lars] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Hopkins, PF (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. FU NSF [ACI 9619019, AST 00-71019, AST 02-06299, AST 03-07690]; NASA ATP [NAG5-12140, NAG5-13292, NAG513381] FX We thank Mike Brotherton, Josh Younger, and Pat Hall for helpful conversations and discussion in the development of this paper. This work was supported in part by NSF grants ACI 9619019, AST 00-71019, AST 02-06299, and AST 03-07690, and NASA ATP grants NAG5-12140, NAG5-13292, and NAG513381. NR 232 TC 75 Z9 75 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 MAR 20 PY 2009 VL 694 IS 1 BP 599 EP 609 DI 10.1088/0004-637X/694/1/599 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 420LQ UT WOS:000264291700055 ER PT J AU Martin, S Martin-Pintado, J Mauersberger, R AF Martin, Sergio Martin-Pintado, J. Mauersberger, R. TI HNCO ABUNDANCES IN GALAXIES: TRACING THE EVOLUTIONARY STATE OF STARBURSTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: abundances; galaxies: ISM; galaxies: starburst; galaxies: Seyfert; ISM: molecules; radio lines: galaxies ID PHOTON-DOMINATED REGIONS; ACTIVE GALACTIC NUCLEUS; NEARBY SEYFERT-GALAXIES; MOLECULAR GAS; DENSE GAS; PHYSICAL CONDITIONS; LUMINOUS GALAXIES; LINE EMISSION; M51; CHEMISTRY AB The chemistry in the central regions of galaxies is expected to be strongly influenced by their nuclear activity. To find the best tracers of nuclear activity is of key importance to understand the processes taking place in the most obscured regions of galactic nuclei. In this work, we present multiline observations of CS, C(34)S, HNCO, and C(18)O in a sample of 11 bright galaxies prototypical for different types of activity. The (32)S/(34)S isotopic ratio is similar to 10, supporting the idea of an isotopical (34)S enrichment due to massive star formation in the nuclear regions of galaxies. Although C(32)S and C(34)S do not seem to be significantly affected by the activity type, the HNCO abundance appears highly contrasted among starbursts (SBs). We observed HNCO abundance variations of nearly 2 orders of magnitude. The HNCO molecule is shown to be a good tracer of the amount of molecular material fueling the SB and therefore can be used as a diagnostics of the evolutionary state of a nuclear SB. C1 [Martin, Sergio] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Martin-Pintado, J.] Ctr Astrobiol CSIC INTA, E-28850 Madrid, Spain. [Mauersberger, R.] Inst Radioastron Milimetr, E-18012 Granada, Spain. [Mauersberger, R.] Joint Alma Observ, Santiago, Chile. RP Martin, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM smartin@cfa.harvard.edu RI Martin-Pintado, Jesus/H-6107-2015 OI Martin-Pintado, Jesus/0000-0003-4561-3508 FU Spanish Ministerio de Educacion y Ciencia [ESP 200400665, ESP2007-65812-C02-01]; Spanish Ministerio de Ciencia e Innovacion [AYA2005-07516-C02-02]; "Comunidad de Madrid" Government under PRICIT project [S-0505/ESP-0237] FX This work has been partially supported by the Spanish Ministerio de Educacion y Ciencia under projects ESP 200400665 and ESP2007-65812-C02-01, the Spanish Ministerio de Ciencia e Innovacion under project AYA2005-07516-C02-02, and the "Comunidad de Madrid" Government under PRICIT project S-0505/ESP-0237 (ASTROCAM). NR 63 TC 41 Z9 41 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 20 PY 2009 VL 694 IS 1 BP 610 EP 617 DI 10.1088/0004-637X/694/1/610 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 420LQ UT WOS:000264291700056 ER PT J AU Umana, G Buemi, CS Trigilio, C Hora, JL Fazio, GG Leto, P AF Umana, G. Buemi, C. S. Trigilio, C. Hora, J. L. Fazio, G. G. Leto, P. TI THE DUSTY NEBULA SURROUNDING HR CAR: A SPITZER VIEW SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; infrared: stars; stars: early-type; stars: individual (HR CAR); stars: winds, outflows ID LUMINOUS BLUE VARIABLES; STAR-FORMING REGIONS; ARRAY CAMERA IRAC; SPACE-TELESCOPE; INFRARED SPECTROGRAPH; RING NEBULA; AG CARINAE; FE-II; EMISSION; SPECTROSCOPY AB We present mid-IR observations of the Galactic Luminous Blue Variable (LBV) HR Car and its associated nebula carried out with the Spitzer Space Telescope using both Infrared Array Camera and Infrared Spectrograph, as part of a GTO program aimed to study stellar ejecta from evolved stars. Our observations reveal a rich mid-IR spectrum of the inner nebula showing both solid state and atomic gas signatures. Strong low-excitation atomic fine structure lines such as 26.0 mu m[Fe II] and 34.8 mu m[Si II], indicate, for the first time, the presence of a PDR in this object class. While the physics and chemistry of the low-excitation gas appears to be dominated by photodissociation, a possible contribution due to shocks can be inferred from the evidence of gas phase Fe abundance enhancement. The presence of amorphous silicates, inferred from the observed characteristic broad feature at 10 mu m located in the inner nebula, suggests that dust has formed during the LBV outburst. This is in contrast with the detection of crystalline dust in other probably more evolved Galactic LBVs, which is similar to the crystalline dust observed in red supergiants. This has been considered to be evidence of dust production during evolutionary phases prior to the outburst. C1 [Umana, G.; Buemi, C. S.; Trigilio, C.] Osserv Astrofis Catania, INAF, I-95123 Catania, Italy. [Hora, J. L.; Fazio, G. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Leto, P.] Inst Radioastron, INAF, Noto, Italy. RP Umana, G (reprint author), Osserv Astrofis Catania, INAF, Via S Sofia 75, I-95123 Catania, Italy. OI Buemi, Carla Simona/0000-0002-7288-4613; Leto, Paolo/0000-0003-4864-2806; Hora, Joseph/0000-0002-5599-4650 FU NASA [1256790, 960541]; National Aeronautics and Space Administration; National Science Foundation FX We thank the referee for her/his comments and suggestions. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under NASA contract 1407. Support for this work was provided by NASA through Contract Number 1256790 issued by JPL/Caltech. Support for the IRAC instrument was provided by NASA through Contract Number 960541 issued by JPL. The IRS was a collaborative venture between Cornell University and Ball Aerospace Corporation funded by NASA through the Jet Propulsion Laboratory and Ames Research Center. SMART was developed at Cornell University and is available through the Spitzer Science Center at Caltech. This publication makes use of data products from the 2MASS, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. NR 36 TC 14 Z9 14 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 20 PY 2009 VL 694 IS 1 BP 697 EP 703 DI 10.1088/0004-637X/694/1/697 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 420LQ UT WOS:000264291700062 ER PT J AU Bietenholz, MF Soderberg, AM Bartel, N AF Bietenholz, M. F. Soderberg, A. M. Bartel, N. TI VERY-LONG-BASELINE INTERFEROMETRY OBSERVATIONS OF SN 2008D SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE gamma rays: bursts; radio continuum: general; supernovae: individual (SN 2008D) ID GAMMA-RAY BURSTS; OFF-AXIS; VLBI OBSERVATIONS; IB/C SUPERNOVA; 1993J VLBI; RADIO; EMISSION; GRB-030329; CORE; CONSTRAINTS AB We report on two epochs of very-long-baseline interferometry (VLBI) observations of the Type Ib/c supernova, SN 2008D, which was associated with the X-ray outburst XRF 080109. At our first epoch, at t = 30 days after the explosion, we observed at 22 and 8.4 GHz, and at our second, at t = 133 days, at 8.4 and 5.0 GHz. The VLBI observations allow us to accurately measure the source's size and position at each epoch, and thus constrain its expansion velocity and proper motion. We find the source at best marginally resolved at both epochs, allowing us to place a 3 sigma upper limit of similar to 0.75 c on the expansion velocity of a circular source. For an elongated source, our measurements are compatible with mildly relativistic expansion. However, our 3s upper limit on the proper motion is 4 mu as day(-1), corresponding to an apparent velocity of less than 0.6 c, and is consistent with a stationary flux centroid. This limit rules out a relativistic jet such as a gamma-ray burst jet away from the line of sight, which would be expected to show apparent proper motion of greater than c. Taken together, our measurements argue against the presence of any long-lived relativistic outflow in SN 2008D. On the other hand, our measurements are consistent with the nonrelativistic expansion velocities of less than 30,000 km s(-1) and small proper motions (< 500 km s(-1)) seen in typical supernovae. C1 [Bietenholz, M. F.] Hartebeesthoek Radio Observ, ZA-1740 Krugersdorp, South Africa. [Bietenholz, M. F.; Bartel, N.] York Univ, Dept Phys & Astron, Toronto, ON M3J 1P3, Canada. [Soderberg, A. M.] Div Theory, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Bietenholz, MF (reprint author), Hartebeesthoek Radio Observ, POB 443, ZA-1740 Krugersdorp, South Africa. FU NSERC; NASA FX Research at York University was partly supported by the NSERC. A. M. S. acknowledges support by NASA through a Hubble Fellowship grant. We thank Uwe Bach for a timely intervention at Effelsberg. NR 40 TC 11 Z9 11 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD MAR 20 PY 2009 VL 694 IS 1 BP L6 EP L10 DI 10.1088/0004-637X/694/1/L6 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 419CK UT WOS:000264196500002 ER PT J AU Kawauchi, GY Rice, ME AF Kawauchi, Gisele Y. Rice, Mary E. TI Two new species of Nephasoma (Sipuncula: Golfingiidae) from the western Atlantic Ocean SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article ID REVISION AB Two new species of the genus Nephasoma, phylum Sipuncula, are described from subtropical waters of the western Atlantic. Nephasoma (Nephasoma) columbaris is described from the central east coast of Florida where it is found along the edge of the continental shelf at depths of 61 to 104 m associated with the rubble from the reefs of the deep water coral Oculina varicosa. A second species, Nephasoma (Nephasoma) ditadii, is described from Brazilian waters in sand habitats at 150 m on the continental shelf off the coast of the state of Sao Paulo. Morphology of the two species is compared with allied species in the genus and the phylum. Usage in the taxonomic literature of the diagnostic characters "shield" and "pseudoshield" is reviewed and evaluated. C1 [Rice, Mary E.] Smithsonian Marine Stn, Ft Pierce, FL 34949 USA. [Kawauchi, Gisele Y.] Harvard Univ, Dept Organism & Evolutionary Biol, Cambridge, MA 02138 USA. RP Rice, ME (reprint author), Smithsonian Marine Stn, 701 Seaway Dr, Ft Pierce, FL 34949 USA. EM g.kawa@gmail.com; rice@si.edu RI Kawauchi, Gisele/N-7464-2013 NR 21 TC 0 Z9 1 U1 0 U2 4 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD MAR 20 PY 2009 VL 122 IS 1 BP 1 EP 13 DI 10.2988/08-32.1 PG 13 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 423AS UT WOS:000264469400001 ER PT J AU Kensley, B Schotte, M Poore, GCB AF Kensley, Brian Schotte, Marilyn Poore, Gary C. B. TI Gnathiid isopods (Crustacea: Isopoda: Gnathiidae), mostly new, from the Indian Ocean SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article ID RECORDS; PERACARIDA AB Twelve new species from three genera of Gnathiidae are described: Caecognathia rhektos, Elaphognathia aldabrae, E. gladia, E ramosa, Gnathia antonbruunae, G. eumece, G. glauca, G. luxata, G. serrula, G. somalia, G. stoddarti, and G. zanzibarensis. Most are from the western Indian Ocean, with one from Thailand. Gnathia nkulu Smit & Van As, 2000, is newly recorded from Madagascar. Keys to the six species of Elaphognathia and 20 species of Gnathia from the Indian Ocean are presented. C1 [Kensley, Brian; Schotte, Marilyn] Smithsonian Inst, Dept Invertebrate Zool, Natl Museum Nat Hist, Washington, DC 20013 USA. [Poore, Gary C. B.] Museum Victoria, Melbourne, Vic 3001, Australia. RP Schotte, M (reprint author), Smithsonian Inst, Dept Invertebrate Zool, Natl Museum Nat Hist, Washington, DC 20013 USA. EM schottem@si.edu; gpoore@museum.vic.gov.au NR 29 TC 11 Z9 11 U1 2 U2 4 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD MAR 20 PY 2009 VL 122 IS 1 BP 32 EP 51 DI 10.2988/07-16.1 PG 20 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 423AS UT WOS:000264469400004 ER PT J AU Suarez, W Olson, SL AF Suarez, William Olson, Storrs L. TI A new genus for the Cuban teratorn (Aves: Teratornithidae) SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article ID QUATERNARY AB Study of the type series and Much new fossil material of the Cuban teratorn, Teratornis olsoni Arredondo & Arredondo, shows that this species possessed unique characters within the family Teratornithidae, including a shorter and more flattened humerus and femur, and a tarsometatarsus with a long trochlea II. The differences are so great as to merit a new genus, Oscaravis, for the species. Some osteological characters of Oscaravis suggest that it was less derived than Teratornis and possibly more similar to Argentavis. As the only insular member of the Teratornithidae, Oscaravis shows that teratorns were capable of overwater dispersal, so that the expansion of the family into North America from the south need not have been dependent on the presence of a land bridge. C1 [Olson, Storrs L.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20013 USA. [Suarez, William] Museo Nacl Hist Nat, Dept Paleogeog & Paleobiol, CH-10100 Havana, Cuba. RP Olson, SL (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, POB 37012, Washington, DC 20013 USA. EM wsua@mnhnc.inf.cu; olsons@si.edu NR 35 TC 3 Z9 3 U1 0 U2 0 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA SN 0006-324X EI 1943-6327 J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD MAR 20 PY 2009 VL 122 IS 1 BP 103 EP 116 DI 10.2988/08-27.1 PG 14 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 423AS UT WOS:000264469400010 ER PT J AU Woodman, N AF Woodman, Neal TI The Stephen H. Long Expedition (1819-1820), Titian R. Peale's field illustrations, and the lost holotypes of the North American shrews Sorex brevicaudus Say and Sorex parvus Say (Mammalia: Soricidae) from the Philadelphia Museum SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article ID NATURAL-HISTORY AB While encamped for the winter of 1819-1820 at Engineer Cantonment along the Missouri River in present-day eastern Nebraska, members of Major Stephen Harriman Long's Expedition to the Rocky Mountains collected a number of animals that were previously unknown. Among the mammals were two soricids that were subsequently described by Thomas Say as Sore-v brevicaudus (Northern Short-tailed Shrew, Blarina brevicauda) and Sorex parvus (Least Shrew, Cryptotis parvus). The holotypes of these species were deposited and placed on public exhibit in the Philadelphia Museum, the predominant North American systematic collection of the early nineteenth century. Like most private museums of that era, the Philadelphia Museum eventually went out of business, and its collections were dispersed and, for the most part, lost. Fortunately, Titian R. Peale made a detailed field sketch of the two specimens soon after their capture and subsequently executed a watercolor based on that sketch. In addition, an engraving of the holotypes was published in the decade following the discovery of the two species. Illustrations of holotypes are taxonomically useful when they depict diagnostic characters of species. They take on added taxonomic significance in the absence of the holotypes. In the cases of Sorex brevicaudus and Sorex parvus, Pictures provide strong confirmation of the taxonomic identities of these two species, as well as recording the early history of the specimens. C1 Smithsonian Inst, Natl Museum Nat Hist, Patuxent Wildlife Res Ctr, US Geol Survey, Washington, DC 20013 USA. RP Woodman, N (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Patuxent Wildlife Res Ctr, US Geol Survey, Washington, DC 20013 USA. EM woodmann@si.edu OI Woodman, Neal/0000-0003-2689-7373 NR 51 TC 2 Z9 2 U1 0 U2 0 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD MAR 20 PY 2009 VL 122 IS 1 BP 117 EP 129 DI 10.2988/08-36.1 PG 13 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 423AS UT WOS:000264469400011 ER PT J AU Hummer, DR Kubicki, JD Kent, PRC Post, JE Heaney, PJ AF Hummer, Daniel R. Kubicki, James D. Kent, Paul R. C. Post, Jeffrey E. Heaney, Peter J. TI Origin of Nanoscale Phase Stability Reversals in Titanium Oxide Polymorphs SO JOURNAL OF PHYSICAL CHEMISTRY C LA English DT Article ID NANOCRYSTALLINE TIO2; POWDER DIFFRACTION; ANATASE-TIO2 NANOMATERIALS; TEMPERATURE-DEPENDENCE; SYNCHROTRON-RADIATION; THERMAL-STABILITY; GRAIN-GROWTH; TRANSFORMATION; KINETICS; RUTILE AB We have monitored the hydrothermal crystallization of titania nanoparticles by in situ X-ray diffraction (XRD). Using the refined average structures from the XRD measurements, we calculated potential energy variations with particle size on periodic bulk structures using density functional theory (DFT). These variations cannot account for the enthalpy required to stabilize anatase relative to rutile. Thus, the hypothesis that the strain of the surface structure of nanoparticles accounts for the stabilization of anatase is not applicable to the growth of titania in water. DFT calculations on model nanoparticles do generate lower surface energies for anatase than for rutile that are large enough to explain the stability reversal in nanoparticles relative to the bulk phase. Rather than arising from two-dimensional surface structure alone, as previously thought, the total surface energies are critically dependent upon defects associated with edges and corners of nanocrystals at particle sizes <= 3 nm (i.e., during the nucleation process). As the particles grow, the bulk free energy becomes relatively more important, causing rutile to become stable at larger particle sizes. This study quantifies for the first time the critical role of edge and vertex energies in determining the relative phase stabilities of TiO2 nanoparticles. C1 [Hummer, Daniel R.; Kubicki, James D.; Heaney, Peter J.] Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. [Kent, Paul R. C.] Oak Ridge Natl Lab, Comp Sci & Math Div, Ctr Nanophase Mat Sci, Oak Ridge, TN 37831 USA. [Post, Jeffrey E.] Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. RP Hummer, DR (reprint author), Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. EM dhummer@geosc.psu.edu RI Kent, Paul/A-6756-2008; Kubicki, James/I-1843-2012 OI Kent, Paul/0000-0001-5539-4017; Kubicki, James/0000-0002-9277-9044 NR 52 TC 41 Z9 41 U1 1 U2 34 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 1932-7447 J9 J PHYS CHEM C JI J. Phys. Chem. C PD MAR 19 PY 2009 VL 113 IS 11 BP 4240 EP 4245 DI 10.1021/jp811332w PG 6 WC Chemistry, Physical; Nanoscience & Nanotechnology; Materials Science, Multidisciplinary SC Chemistry; Science & Technology - Other Topics; Materials Science GA 417XH UT WOS:000264111300003 ER PT J AU Smith, DR Schmidt, S AF Smith, David R. Schmidt, Stefan TI A new subfamily, genus, and species of Cephidae (Hymenoptera) from Australia SO ZOOTAXA LA English DT Letter DE Cephidae; Australcephinae; Australcephus; stem sawfly ID INDONESIA AB Australcephinae, n. subf., is described from Queensland, Australia, based on Australcephus storeyi, n. gen., n. sp. This is the only cephid known from Australia and one of the few from the Southern Hemisphere. A key is given for the three recognized subfamilies of Cephidae. C1 [Smith, David R.] ARS, Systemat Entomol Lab,PSI, USDA, Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20013 USA. [Schmidt, Stefan] Zool Staatssammlung, D-81247 Munich, Germany. RP Smith, DR (reprint author), ARS, Systemat Entomol Lab,PSI, USDA, Natl Museum Nat Hist,Smithsonian Inst, POB 37012,MRC 168, Washington, DC 20013 USA. EM dave.smith@ars.usda.gov; stefan.schmidt@zsm.mwn.de NR 9 TC 4 Z9 4 U1 0 U2 0 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD MAR 13 PY 2009 IS 2034 BP 56 EP 60 PG 5 WC Zoology SC Zoology GA 417YS UT WOS:000264115000005 ER PT J AU Liu, Y Wang, Y Liu, X Cai, ZN Chance, K AF Liu, Yi Wang, Yong Liu, Xiong Cai, Zhaonan Chance, Kelly TI Tibetan middle tropospheric ozone minimum in June discovered from GOME observations SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID SATELLITE MEASUREMENTS; PACIFIC AB Global Ozone Monitoring Experiment (GOME) observations from 1997-2000 have revealed the Tibetan Middle Tropospheric Ozone Minimum (TMTOM), a low-ozone layer that occurs in the middle troposphere over the Tibetan Plateau (TP) in June. Ozone profiles were derived from GOME observations and validated by ozonesonde measurements at two stations (Lhasa and Xining) over the TP. The mean bias is 5-10% within the troposphere. The ozone profiles reveal the TMTOM phenomenon occurs in the middle troposphere (8-13 km) over the middle and eastern TP in June. Dynamical field analyses showed that the TMTOM accompanies the onset of the Asian summer monsoon. The low-ozone air from the Bay of Bengal is transported into the middle troposphere over the TP by southwest currents while the lower troposphere over the TP is still occupied by ozone-rich air blocked by the transport barrier of the Himalayas. The TMTOM was most prominent in June 1998 likely linked to the occurrence of the intense El Nino of 1997-1998 because the Tibetan anticyclone is of large area and has strong intensity during El Nino years. The occurrence of the TMTOM can serve as an indicator of the phase of evolution of the Asian summer monsoon. Citation: Liu, Y., Y. Wang, X. Liu, Z. Cai, and K. Chance (2009), Tibetan middle tropospheric ozone minimum in June discovered from GOME observations, Geophys. Res. Lett., 36, L05814, doi:10.1029/2008GL037056. C1 [Liu, Yi; Wang, Yong; Cai, Zhaonan] Chinese Acad Sci, Inst Atmospher Phys, Key Lab Middle Atmosphere & Global Environm Obser, Beijing 100029, Peoples R China. [Chance, Kelly] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Liu, Xiong] Univ Maryland, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. RP Liu, Y (reprint author), Chinese Acad Sci, Inst Atmospher Phys, Key Lab Middle Atmosphere & Global Environm Obser, Beijing 100029, Peoples R China. EM liuyi@mail.iap.ac.cn RI Liu, Xiong/P-7186-2014; OI Liu, Xiong/0000-0003-2939-574X; Chance, Kelly/0000-0002-7339-7577 FU National Science Foundation of China [40633015, 40710059003]; NASA [NNX08AN98G]; Smithsonian Institution; European Space Agency; German Aerospace Center with GOME FX We thank Yasunobu Iwasaka from Kanazawa University, Japan, and Guangyu Shi from the Institute of Atmospheric Physics, Chinese Academy of Sciences, China, for providing the ozone-sonde data at Lhasa, China; we also thank Xiangdong Zheng from the Chinese Institute of Meteorological Science for providing ozone-sonde data at Xining, China. This work was funded by the National Science Foundation of China under grants 40633015 and 40710059003. Xiong Liu was also funded by the NASA New Investigator Program (NNX08AN98G). Kelly Chance was supported by NASA and the Smithsonian Institution. We are pleased to acknowledge the ongoing cooperation of the European Space Agency and the German Aerospace Center with GOME. NR 21 TC 12 Z9 14 U1 0 U2 6 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 MAR 12 PY 2009 VL 36 AR L05814 DI 10.1029/2008GL037056 PG 6 WC Geosciences, Multidisciplinary SC Geology GA 419LX UT WOS:000264222100007 ER PT J AU Dilkes, D Sues, HD AF Dilkes, David Sues, Hans-Dieter TI REDESCRIPTION AND PHYLOGENETIC RELATIONSHIPS OF DOSWELLIA KALTENBACHI (DIAPSIDA: ARCHOSAURIFORMES) FROM THE UPPER TRIASSIC OF VIRGINIA SO JOURNAL OF VERTEBRATE PALEONTOLOGY LA English DT Article ID REPTILE EUPARKERIA-CAPENSIS; ARCHOSAUROMORPH REPTILE; BRAINCASE; TEXAS; INTERRELATIONSHIPS; INFORMATION; VERTEBRATES; EVOLUTION; BIRDS; SKULL AB A detailed redescription of the Late Triassic archosauromorph reptile Doswellia kaltenbachi Weems, 1980 from the Poor Farm Member of the Falling Creek Formation in the Taylorsville basin (Newark Supergroup) in Virginia is presented based upon additional preparation of the holotype. The euryapsid skull has a distinctive occiput with a prominent supraoccipital process that is flanked by posterior "horn-like" projections of the squamosals. Postfrontals, tabulars, and postparietals are absent. Plesiomorphic features of the palate and braincase include a plate-like horizontal parabasisphenoid, a pair of foramina for the internal carotid arteries on the ventral surface of the basisphenoid. and two fields of teeth on the palatal surface of the pterygoid. A sharp angle along the cervical and anterior dorsal ribs clearly separates the dorsal and lateral sides of the neck and anterior thoracic region. The posterior thoracic region has shorter ribs that project laterally with only a slight curvature. The ilium has a laterally deflected blade with numerous deep grooves along its distal edge. The laterally extensive set of osteoderms includes a nuchal element that is composed of several interlocking osteoderms that lack the arrangement in distinct transverse rows that characterizes the remainder of the osteoderms. A phylogenetic analysis of basal archosauriforms incorporates new data of Doswellia and the taxa Turfanosuchus, Yonghesuchus, and Qianosuchus that have not previously been combined in a single study. Results include a sister-group relationship between Doswellia and proterochampsids, placement of Qianosuchns as a crurotarsan archosaur, and Yonghesuchus and Turfanosuchus as successive sister taxa to Archosauria. C1 [Dilkes, David] Univ Wisconsin, Dept Biol & Microbiol, Oshkosh, WI 54901 USA. [Sues, Hans-Dieter] Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20013 USA. RP Dilkes, D (reprint author), Univ Wisconsin, Dept Biol & Microbiol, Oshkosh, WI 54901 USA. EM dilkes@uwosh.edu NR 62 TC 48 Z9 48 U1 1 U2 4 PU SOC VERTEBRATE PALEONTOLOGY PI NORTHBROOK PA 60 REVERE DR, STE 500, NORTHBROOK, IL 60062 USA SN 0272-4634 J9 J VERTEBR PALEONTOL JI J. Vertebr. Paleontol. PD MAR 12 PY 2009 VL 29 IS 1 BP 58 EP + PG 22 WC Paleontology SC Paleontology GA 429DE UT WOS:000264900200006 ER PT J AU Woodley, NE AF Woodley, Norman E. TI A review of the genus Ditylometopa Kertesz (Diptera: Stratiomyidae) SO ZOOTAXA LA English DT Review DE Ditylometopa elegans; D. centralensis; new species; Stratiomyidae; Neotropical; taxonomy AB The genus Ditylometopa Kertesz (Diptera: Stratiomyidae, Clitellariinae), which occurs only in the Neotropical Region, is reviewed. Euryneura rufifrons Curran, 1934 is synonymized with Ditylometopa elegans Kertesz, 1923. A neotype is designated for D. elegans. Two species are recognized, including Ditylometopa centralensis sp. nov., which is described from Costa Rica (type locality) and Nicaragua and may occur in Brazil. C1 USDA, Syst Entomol Lab, PSI, ARS, Washington, DC 20013 USA. RP Woodley, NE (reprint author), USDA, Syst Entomol Lab, PSI, ARS, Smithsonian Inst NHB 168,POB 37012, Washington, DC 20013 USA. EM woodley@ars.usda.gov RI Woodley, Norman/M-6160-2014 NR 6 TC 0 Z9 0 U1 0 U2 0 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD MAR 11 PY 2009 IS 2032 BP 39 EP 47 PG 9 WC Zoology SC Zoology GA 417YQ UT WOS:000264114800002 ER PT J AU Staines, CL AF Staines, C. L. TI A review of the genus Chelobasis Gray, 1832 (Coleoptera: Chrysomelidae: Cassidinae) SO ZOOTAXA LA English DT Review DE Chelobasis; Chrysomelidae; Cassidinae; key to species ID HISPINE BEETLES; HELICONIA-LATISPATHA; COMMUNITIES; CHEMISTRY; EVOLUTION AB The genus Chelobasis Gray, 1832 is reviewed. Four species are recognized. A key to the species is presented. The literature is summarized and each species is illustrated. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20013 USA. RP Staines, CL (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, MRC 187,POB 37012, Washington, DC 20013 USA. EM stainesc@si.edu NR 46 TC 8 Z9 8 U1 0 U2 0 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD MAR 11 PY 2009 IS 2033 BP 58 EP 68 PG 11 WC Zoology SC Zoology GA 417YR UT WOS:000264114900006 ER PT J AU Sun, M Voit, GM Donahue, M Jones, C Forman, W Vikhlinin, A AF Sun, M. Voit, G. M. Donahue, M. Jones, C. Forman, W. Vikhlinin, A. TI CHANDRA STUDIES OF THE X-RAY GAS PROPERTIES OF GALAXY GROUPS SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; dark matter; galaxies: clusters: general; X-rays: galaxies: clusters ID MASS-TEMPERATURE RELATION; CLUSTER SCALING PROJECT; XMM-NEWTON; INTRACLUSTER MEDIUM; DARK-MATTER; ENTROPY PROFILES; COSMOLOGICAL SIMULATIONS; NEARBY CLUSTERS; COOLING FLOWS; AGN FEEDBACK AB We present a systematic analysis of 43 nearby galaxy groups (kT(500) = 0.7-2.7 keV or M-500 = 10(13)-10(14) h(-1) M-circle dot, 0.012 < z < 0.12), based on Chandra archival data. With robust background subtraction and modeling, we trace gas properties to at least r(2500) for all 43 groups. For 11 groups, gas properties can be robustly derived to r(500). For an additional 12 groups, we derive gas properties to at least r(1000) and estimate properties at r(500) from extrapolation. We show that in spite of the large variation in temperature profiles inside 0.15 r(500), the temperature profiles of these groups are similar at > 0.15 r(500) and are consistent with a "universal temperature profile." We present the K-T relations at six characteristic radii (30 kpc, 0.15 r(500), r(2500), r(1500), r(1000), and r(500)), for 43 groups from this work and 14 clusters from the Vikhlinin et al. (2008) sample. Despite large scatter in the entropy values at 30 kpc and 0.15 r(500), the intrinsic scatter at r(2500) is much smaller and remains the same (similar to 10%) to r(500). The entropy excess at r(500) is confirmed, in both groups and clusters, but the magnitude is smaller than previous ROSAT and ASCA results. We also present scaling relations for the gas fraction. It appears that the average gas fraction between r(2500) and r(500) has no temperature dependence, similar to 0.12 for 1-10 keV systems. The group gas fractions within r(2500) are generally low and have large scatter. This work shows that the difference of groups from hotter clusters stems from the difficulty of compressing group gas inside of r(2500). The large scatter of the group gas fraction within r(2500) causes large scatter in the group entropy around the center and may be responsible for the large scatter of the group luminosities. Nevertheless, the groups appear more regular and more like clusters beyond r(2500) from the results on gas fraction and entropy. Therefore, mass proxies can be extended into low- mass systems. The M-500-T-500 and M-500-Y-X,Y-500 relations derived in this work are indeed well behaved down to at least 2 x 10(13) h-1 M-circle dot. C1 [Sun, M.; Voit, G. M.; Donahue, M.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Jones, C.; Forman, W.; Vikhlinin, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Sun, M (reprint author), Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. EM msun@virginia.edu RI Donahue, Megan/B-5361-2012; OI Voit, Gerard/0000-0002-3514-0383 NR 88 TC 275 Z9 276 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 MAR 10 PY 2009 VL 693 IS 2 BP 1142 EP 1172 DI 10.1088/0004-637X/693/2/1142 PG 31 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 417RR UT WOS:000264095100010 ER PT J AU Lee, CW Bourke, TL Myers, PC Dunham, M Evans, N Lee, Y Huard, T Wu, J Gutermuth, R Kim, MR Kang, HW AF Lee, Chang Won Bourke, Tyler L. Myers, Philip C. Dunham, Mike Evans, Neal Lee, Youngung Huard, Tracy Wu, Jingwen Gutermuth, Robert Kim, Mi-Ryang Kang, Hyun Woo TI THE SPITZER c2d SURVEY OF NEARBY DENSE CORES. V. DISCOVERY OF A VeLLO IN THE "STARLESS" DENSE CORE L328 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: individual (L328, L328-IRS); stars: formation; stars: low-mass, brown dwarfs ID YOUNG STELLAR OBJECTS; INFRARED OBSERVATIONS; INTERSTELLAR CLOUDS; MOLECULAR CLOUDS; SPACE-TELESCOPE; EMBEDDED SOURCE; LEGACY CLOUDS; SCUBA SURVEY; DARK CLOUDS; MILKY-WAY AB This paper reports the discovery of a Very Low Luminosity Object (VeLLO) in the "starless" dense core L328, using the Spitzer Space Telescope and ground-based observations from near-infrared (NIR) to millimeter wavelengths. The Spitzer 8 mu m image indicates that L328 consists of three subcores of which the smallest one may harbor a source, L328-IRS, while two other subcores remain starless. L328-IRS is a Class 0 protostar according to its bolometric temperature (44 K) and the high fraction (similar to 72%) of its luminosity emitted at submillimeter wavelengths. Its inferred "internal luminosity" (0.04-0.06 L-circle dot) using a radiative transfer model under the most plausible assumption of its distance as 200 pc is much fainter than for a typical protostar, and even fainter than other VeLLOs studied previously. Note, however, that its inferred luminosity may be uncertain by a factor of 2-3 if we consider two extreme values of the distance of L328-IRS (125 or 310 pc). Low angular resolution observations of CO do not show any clear evidence of a molecular outflow activity. But broad line widths toward L328, and Spitzer and NIR images showing nebulosity possibly tracing an outflow cavity, strongly suggest the existence of outflow activity. Provided that an envelope of at most similar to 0.1 M-circle dot is the only mass accretion reservoir for L328-IRS, the star formation efficiency is close to the canonical value similar to 30%, and L328-IRS has not yet accreted more than 0.05 M-circle dot, at the assumed distance of 200 pc, L328-IRS is destined to be a brown dwarf. C1 [Lee, Chang Won; Lee, Youngung; Kim, Mi-Ryang; Kang, Hyun Woo] Korea Astron & Space Sci Inst, Taejon 305348, South Korea. [Lee, Chang Won; Bourke, Tyler L.; Myers, Philip C.; Wu, Jingwen; Gutermuth, Robert] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Dunham, Mike; Evans, Neal] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Huard, Tracy] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Kang, Hyun Woo] Seoul Natl Univ, Dept Astron, Sch Phys & Astron, Seoul 151749, South Korea. RP Lee, CW (reprint author), Korea Astron & Space Sci Inst, 61-1 Hwaam Dong, Taejon 305348, South Korea. EM cwl@kasi.re.kr FU Korea Science and Engineering Foundation [KOSEF R01-2003-000-10513-0]; NASA [1224608, 1407, 1279198, NNG04GG24G, NNX07AJ72G] FX We thank an anonymous referee for useful comments and suggestions. We also thank H. Kirk for providing unsmoothed SCUBA archive data, A. Bacmann for the 1200 mu m data, and H. J. Kim for the discussion on the DUSTY fitting. C. W. L. and Y. L. acknowledge the support by the Basic Research Program (KOSEF R01-2003-000-10513-0) of the Korea Science and Engineering Foundation. Support for this work, part of the Spitzer Legacy Science Program, was provided by NASA through contract 1224608 issued by the Jet Propulsion Laboratory, California Institute of Technology, under NASA contract 1407. Partial support for T. L. B. was also provided by NASA through contract 1279198 issued by the Jet Propulsion Laboratory, California Institute of Technology, under NASA contract 1407. Partial support was also obtained from NASA Origins grants NNG04GG24G and NNX07AJ72G to N. J. E. NR 63 TC 33 Z9 33 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 10 PY 2009 VL 693 IS 2 BP 1290 EP 1299 DI 10.1088/0004-637X/693/2/1290 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 417RR UT WOS:000264095100022 ER PT J AU Lin, J Li, J Ko, YK Raymond, JC AF Lin, J. Li, J. Ko, Y. -K. Raymond, J. C. TI INVESTIGATION OF THICKNESS AND ELECTRICAL RESISTIVITY OF THE CURRENT SHEETS IN SOLAR ERUPTIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE diffusion; Sun: coronal mass ejections (CMEs); Sun: flares; Sun: magnetic fields; turbulence ID CORONAL MASS EJECTIONS; RECONNECTING CURRENT SHEETS; MAGNETIC RECONNECTION; PARTICLE-ACCELERATION; TEARING MODE; FIELD; FLARES; WIND; TURBULENCE; MECHANISM AB A discussion of the thickness of current sheets in solar eruptions, d, led Lin et al. in 2007 to estimate very large values for the effective resistivity, eta(e). Here, we address some questions raised by that paper. We apply the limb synoptic map technique and find d between 5.0 x 10(4) and 4.6 x 10(5) km, increasing with both time and altitude. The possibility that large apparent d and eta(e) result from projection effects is examined and rejected. We derive theoretical scaling laws relating d to other observables that corroborate this conclusion and thus help confine both d and eta(e) to a reasonable range. The possible impact of our results on the existing models of particle acceleration in reconnecting current sheets is also briefly discussed. C1 [Lin, J.] Chinese Acad Sci, Yunnan Astron Observ, Natl Astron Observ China, Kunming 650011, Yunnan, Peoples R China. [Lin, J.; Ko, Y. -K.; Raymond, J. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Li, J.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. RP Lin, J (reprint author), Chinese Acad Sci, Yunnan Astron Observ, Natl Astron Observ China, POB 110, Kunming 650011, Yunnan, Peoples R China. RI LIN, JUN/B-9890-2017 FU Ministry of Science and Technology of China [2006CB806303]; National Natural Science Foundation of China [10873030, 40636031]; Chinese Academy of Sciences [KJCX2-YW-T04]; NASA [NNX07AL72G] FX We gratefully acknowledge T. G. Forbes, A. A. van Ballegooijen, G. Poletto, and A. Bemporad for valuable discussions, comments, and suggestions. We also thank the referee for carefully reading the paper, and for providing very helpful and instructive comments and suggestions for improving this paper. J. L., Y.-K. K., and J. C. R. thank ISSI (International Space Science Institute, Bern) for the hospitality provided to the members of the team on the Role of Current Sheets in Solar Eruptive Events where many of the ideas presented in this work have been discussed. J. L.'s work at YNAO was supported by the Ministry of Science and Technology of China under the 973 Program grant 2006CB806303, by the National Natural Science Foundation of China under grants 10873030 and 40636031, and by the Chinese Academy of Sciences under the grant KJCX2-YW-T04 to YNAO; and his work was supported by NASA grant NNX07AL72G when he visited to CfA. SOHO is a joint mission of the European Space Agency and the US National Aeronautics and Space Administration. NR 53 TC 41 Z9 45 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 10 PY 2009 VL 693 IS 2 BP 1666 EP 1677 DI 10.1088/0004-637X/693/2/1666 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 417RR UT WOS:000264095100057 ER PT J AU Wilson, CD Warren, BE Israel, FP Serjeant, S Bendo, G Brinks, E Clements, D Courteau, S Irwin, J Knapen, JH Leech, J Matthews, HE Muhle, S Mortier, AMJ Petitpas, G Sinukoff, E Spekkens, K Tan, BK Tilanus, RPJ Usero, A van der Werf, P Wiegert, T Zhu, M AF Wilson, C. D. Warren, B. E. Israel, F. P. Serjeant, S. Bendo, G. Brinks, E. Clements, D. Courteau, S. Irwin, J. Knapen, J. H. Leech, J. Matthews, H. E. Muehle, S. Mortier, A. M. J. Petitpas, G. Sinukoff, E. Spekkens, K. Tan, B. K. Tilanus, R. P. J. Usero, A. van der Werf, P. Wiegert, T. Zhu, M. TI THE JAMES CLERK MAXWELL TELESCOPE NEARBY GALAXIES LEGACY SURVEY. I. STAR-FORMING MOLECULAR GAS IN VIRGO CLUSTER SPIRAL GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: individual (Virgo); galaxies: individual (NGC 4254, NGC 4321, NGC 4569, NGC 4579); galaxies: ISM; galaxies: spiral; ISM: molecules; stars: formation ID FAST-ALPHA SURVEY; RESOLUTION CO SURVEY; H-ALPHA; FORMATION EFFICIENCY; J=3-2 EMISSION; CENTRAL REGION; FORMATION LAW; ATLAS; DENSITY; CLOUDS AB We present large-area maps of the CO J = 3-2 emission obtained at the James Clerk Maxwell Telescope for four spiral galaxies in the Virgo Cluster. We combine these data with published CO J = 1-0, 24 mu m, and Ha images to measure the CO line ratios, molecular gas masses, and instantaneous gas depletion times. For three galaxies in our sample (NGC 4254, NGC 4321, and NGC 4569), we obtain molecular gas masses of 7 x 10(8) - 3 x 10(9) M(circle dot) and disk-averaged instantaneous gas depletion times of 1.1-1.7 Gyr. We argue that the CO J = 3-2 line is a better tracer of the dense star-forming molecular gas than the CO J = 1-0 line, as it shows a better correlation with the star formation rate surface density both within and between galaxies. NGC 4254 appears to have a larger star formation efficiency (smaller gas depletion time), perhaps because it is on its first passage through the Virgo Cluster. NGC 4569 shows a large-scale gradient in the gas properties traced by the CO J = 3-2/J = 1-0 line ratio, which suggests that its interaction with the intracluster medium is affecting the dense star-forming portion of the interstellar medium directly. The fourth galaxy in our sample, NGC 4579, has weak CO J = 3-2 emission despite having bright 24 mu m emission; however, much of the central luminosity in this galaxy may be due to the presence of a central active galactic nucleus. C1 [Wilson, C. D.; Warren, B. E.; Sinukoff, E.] McMaster Univ, Dept Phys & Astron, Hamilton, ON L8S 4M1, Canada. [Israel, F. P.; van der Werf, P.] Leiden Univ, Sterrewacht Leiden, NL-2300 RA Leiden, Netherlands. [Serjeant, S.] Open Univ, Dept Phys & Astron, Milton Keynes MK7 6AA, Bucks, England. [Bendo, G.; Clements, D.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England. [Brinks, E.; Usero, A.] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. [Courteau, S.; Irwin, J.] Queens Univ, Dept Phys Engn Phys & Astron, Kingston, ON, Canada. [Knapen, J. H.] Inst Astrofis Canarias, E-38200 San Cristobal la Laguna, Spain. [Leech, J.; Tan, B. K.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England. [Matthews, H. E.; Zhu, M.] Natl Res Council Canada, Herzberg Inst Astrophys, Penticton, BC V2A 6J9, Canada. [Muehle, S.] Joint Inst VLBI Europe, NL-7990 AA Dwingeloo, Netherlands. [Mortier, A. M. J.] SUPA, Edinburgh EH9 3HJ, Midlothian, Scotland. Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. [Petitpas, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Spekkens, K.] Royal Mil Coll Canada, Dept Phys, Stn Forces, Kingston, ON K7K 4B4, Canada. [Tilanus, R. P. J.; Zhu, M.] Joint Astron Ctr, Hilo, HI 96720 USA. [Tilanus, R. P. J.] Netherlands Org Sci Res, The Hague, Netherlands. [Usero, A.] Observ Astron Nacl, Madrid 28014, Spain. [Wiegert, T.] Univ Manitoba, Dept Phys & Astron, Winnipeg, MB R3T 2N2, Canada. RP Wilson, CD (reprint author), McMaster Univ, Dept Phys & Astron, Hamilton, ON L8S 4M1, Canada. EM wilson@physics.mcmaster.ca; bwarren@physics.mcmaster.ca; israel@strw.leidenuniv.nl; g.bendo@imperial.ac.uk; E.Brinks@herts.ac.uk; d.clements@imperial.ac.uk; courteau@astro.queensu.ca; irwin@astro.queensu.ca; jhk@iac.es; jxl@astro.ox.ac.uk; henry.matthews@nrc-cnrc.gc.ca; muehle@jive.nl; ajm@roe.ac.uk; gpetitpa@cfa.harvard.edu; sinukoej@mcmaster.ca; Kristine.Spekkens@rmc.ca; r.tilanus@jach.hawaii.edu; a.usero@oan.es; pvdwerf@strw.leidenuniv.nl; wiegert@physics.umanitoba.ca; m.zhu@jach.hawaii.edu OI Brinks, Elias/0000-0002-7758-9699 FU NSERC (Canada); UK Science & Technology Facilities Council FX We thank the anonymous referee for a very useful referee report. The James Clerk Maxwell Telescope is operated by The Joint Astronomy Centre on behalf of the Science and Technology Facilities Council of the United Kingdom, the Netherlands Organisation for Scientific Research, and the National Research Council of Canada. The research of J. I., S. C., K. S., and C. D. W. is supported by grants from NSERC (Canada). A. U. has been supported through a Post-Doctoral Research Assistantship from the UK Science & Technology Facilities Council. This research has made use of the GOLD Mine Database. We acknowledge the usage of the HyperLeda database (http://leda.univ-lyon1.fr). NR 78 TC 61 Z9 62 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 10 PY 2009 VL 693 IS 2 BP 1736 EP 1748 DI 10.1088/0004-637X/693/2/1736 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 417RR UT WOS:000264095100063 ER PT J AU Hebb, L Collier-Cameron, A Loeillet, B Pollacco, D Hebrard, G Street, RA Bouchy, F Stempels, HC Moutou, C Simpson, E Udry, S Joshi, YC West, RG Skillen, I Wilson, DM McDonald, I Gibson, NP Aigrain, S Anderson, DR Benn, CR Christian, DJ Enoch, B Haswell, CA Hellier, C Horne, K Irwin, J Lister, TA Maxted, P Mayor, M Norton, AJ Parley, N Pont, F Queloz, D Smalley, B Wheatley, PJ AF Hebb, L. Collier-Cameron, A. Loeillet, B. Pollacco, D. Hebrard, G. Street, R. A. Bouchy, F. Stempels, H. C. Moutou, C. Simpson, E. Udry, S. Joshi, Y. C. West, R. G. Skillen, I. Wilson, D. M. McDonald, I. Gibson, N. P. Aigrain, S. Anderson, D. R. Benn, C. R. Christian, D. J. Enoch, B. Haswell, C. A. Hellier, C. Horne, K. Irwin, J. Lister, T. A. Maxted, P. Mayor, M. Norton, A. J. Parley, N. Pont, F. Queloz, D. Smalley, B. Wheatley, P. J. TI WASP-12b: THE HOTTEST TRANSITING EXTRASOLAR PLANET YET DISCOVERED SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; techniques: photometric; techniques: radial velocities ID STELLAR ATMOSPHERE MODELS; LIMB-DARKENING LAW; GAS-GIANT PLANET; LIGHT CURVES; EVOLUTIONARY TRACKS; SURFACE GRAVITIES; PHOTOMETRY; ALBEDO; STARS; TELESCOPE AB We report on the discovery of WASP-12b, a new transiting extrasolar planet with R(pl) = 1.79(-0.09)(+0.09) R(J) and M(pl) = 1.41(-0.01)(+0.01) M(J). The planet and host star properties were derived from a Monte Carlo Markov chain analysis of the transit photometry and radial velocity data. Furthermore, by comparing the stellar spectrum with theoretical spectra and stellar evolution models, we determined that the host star is a supersolar metallicity ([M/II]= 0.3(-0.15)(+0.15)), late-F (T(eff) = 6300(-100)(+200) K) star which is evolving off the zero-age main sequence. The planet has an equilibrium temperature of T(eq) = 2516 K caused by its very short period orbit (P = 1.09 days) around the hot, twelfth magnitude host star. WASP-12b has the largest radius of any transiting planet yet detected. It is also the most heavily irradiated and the shortest period planet in the literature. C1 [Hebb, L.; Collier-Cameron, A.; Stempels, H. C.; Enoch, B.; Horne, K.; Parley, N.] Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. [Loeillet, B.; Moutou, C.] Lab Astrophys Marseille, F-13376 Marseille 12, France. [Pollacco, D.; Simpson, E.; Joshi, Y. C.; Gibson, N. P.; Christian, D. J.] Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland. [Hebrard, G.; Bouchy, F.] Univ Paris 06, Inst Astrophys Paris, CNRS, UMR 7095, F-75014 Paris, France. [Street, R. A.; Lister, T. A.] Las Cumbres Observ, Santa Barbara, CA 93117 USA. [Bouchy, F.] Observ Haute Provence, F-04870 St Michel lObservatoire, France. [Udry, S.; Mayor, M.; Queloz, D.] Univ Geneva, Observ Geneve, CH-1290 Sauverny, Switzerland. [West, R. G.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Skillen, I.; Benn, C. R.] Isaac Newton Grp Telescopes, E-38700 Tenerife, Spain. [Wilson, D. M.; McDonald, I.; Anderson, D. R.; Hellier, C.; Maxted, P.; Smalley, B.] Univ Keele, Astrophys Grp, Keele ST5 5BG, Staffs, England. [Aigrain, S.; Pont, F.] Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England. [Haswell, C. A.; Norton, A. J.] Open Univ, Dept Phys & Astron, Milton Keynes MK7 6AA, Bucks, England. [Irwin, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Wheatley, P. J.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. RP Hebb, L (reprint author), Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. OI Norton, Andrew/0000-0001-7619-8269; Gibson, Neale/0000-0002-9308-2353; Christian, Damian/0000-0003-1746-3020; Wheatley, Peter/0000-0003-1452-2240 NR 41 TC 167 Z9 167 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 10 PY 2009 VL 693 IS 2 BP 1920 EP 1928 DI 10.1088/0004-637X/693/2/1920 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 417RR UT WOS:000264095100080 ER PT J AU Seth, AC Blum, RD Bastian, N Caldwell, N Debattista, VP Puzia, TH AF Seth, Anil C. Blum, Robert D. Bastian, Nate Caldwell, Nelson Debattista, Victor P. Puzia, Thomas H. TI THE ROTATING NUCLEAR STAR CLUSTER IN NGC 4244 (vol 687, pg 997, 2008) SO ASTROPHYSICAL JOURNAL LA English DT Correction C1 [Seth, Anil C.; Caldwell, Nelson] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Blum, Robert D.] Natl Opt Astron Observ, Tucson, AZ 85721 USA. [Bastian, Nate] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Debattista, Victor P.] Univ Cent Lancashire, Ctr Astrophys, Preston PR1 2HE, Lancs, England. [Puzia, Thomas H.] Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. RP Seth, AC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM aseth@cfa.harvard.edu NR 1 TC 1 Z9 1 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 10 PY 2009 VL 693 IS 2 BP 1959 EP 1959 DI 10.1088/0004-637X/693/2/1959 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 417RR UT WOS:000264095100083 ER PT J AU Acciari, VA Aliu, E Arlen, T Beilicke, M Benbow, W Bottcher, M Bradbury, SM Buckley, JH Bugaev, V Butt, Y Byrum, K Cannon, A Celik, O Cesarini, A Chow, YC Ciupik, L Cogan, P Cui, W Daniel, MK Dickherber, R Ergin, T Falcone, A Fegan, SJ Finley, JP Fortin, P Fortson, L Furniss, A Gall, D Gibbs, K Gillanders, GH Godambe, S Grube, J Guenette, R Gyuk, G Hanna, D Hays, E Holder, J Horan, D Hui, CM Humensky, TB Imran, A Kaaret, P Karlsson, N Kertzman, M Kieda, D Kildea, J Konopelko, A Krawczynski, H Krennrich, F Lang, MJ LeBohec, S Maier, G McCann, A McCutcheon, M Millis, J Moriarty, P Mukherjee, R Nagai, T Ong, RA Otte, N Pandel, D Perkins, JS Petry, D Pizlo, F Pohl, M Quinn, J Ragan, K Reyes, LC Reynolds, T Roache, E Rose, HJ Schroedter, M Sembroski, GH Smith, AW Steele, D Swordy, SP Theiling, M Toner, JA Varlotta, A Vassiliev, VV Wagner, RG Wakely, SP Ward, JE Weekes, TC Weinstein, A Williams, DA Wissel, S Wood, M Zitzer, B AF Acciari, V. A. Aliu, E. Arlen, T. Beilicke, M. Benbow, W. Boettcher, M. Bradbury, S. M. Buckley, J. H. Bugaev, V. Butt, Y. Byrum, K. Cannon, A. Celik, O. Cesarini, A. Chow, Y. C. Ciupik, L. Cogan, P. Cui, W. Daniel, M. K. Dickherber, R. Ergin, T. Falcone, A. Fegan, S. J. Finley, J. P. Fortin, P. Fortson, L. Furniss, A. Gall, D. Gibbs, K. Gillanders, G. H. Godambe, S. Grube, J. Guenette, R. Gyuk, G. Hanna, D. Hays, E. Holder, J. Horan, D. Hui, C. M. Humensky, T. B. Imran, A. Kaaret, P. Karlsson, N. Kertzman, M. Kieda, D. Kildea, J. Konopelko, A. Krawczynski, H. Krennrich, F. Lang, M. J. LeBohec, S. Maier, G. McCann, A. McCutcheon, M. Millis, J. Moriarty, P. Mukherjee, R. Nagai, T. Ong, R. A. Otte, N. Pandel, D. Perkins, J. S. Petry, D. Pizlo, F. Pohl, M. Quinn, J. Ragan, K. Reyes, L. C. Reynolds, T. Roache, E. Rose, H. J. Schroedter, M. Sembroski, G. H. Smith, A. W. Steele, D. Swordy, S. P. Theiling, M. Toner, J. A. Varlotta, A. Vassiliev, V. V. Wagner, R. G. Wakely, S. P. Ward, J. E. Weekes, T. C. Weinstein, A. Williams, D. A. Wissel, S. Wood, M. Zitzer, B. TI VERITAS OBSERVATIONS OF A VERY HIGH ENERGY gamma-RAY FLARE FROM THE BLAZAR 3C 66A SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE BL Lacertae objects: individual (3C 66A); galaxies: active; gamma rays: observations ID BL LACERTAE OBJECTS; ATMOSPHERIC CHERENKOV TELESCOPES; X-RAY; EMISSION; 3C-66A; DISCOVERY; RADIATION; ASTRONOMY; OPACITY; ARRAY AB The intermediate-frequency peaked BL Lacertae (IBL) object 3C 66A is detected during 2007-2008 in VHE ( very high energy; E > 100 GeV) gamma rays with the VERITAS stereoscopic array of imaging atmospheric Cherenkov telescopes. An excess of 1791 events is detected, corresponding to a significance of 21.2 standard deviations (sigma), in these observations (32.8 hr live time). The observed integral flux above 200 GeV is 6% of the Crab Nebula's flux and shows evidence for variability on the timescale of days. The measured energy spectrum is characterized by a soft power law with photon index Gamma = 4.1 +/- 0.4(stat) +/- 0.6(sys). The radio galaxy 3C 66B is excluded as a possible source of the VHE emission. C1 [Benbow, W.; Gibbs, K.; Kildea, J.; Perkins, J. S.; Roache, E.; Theiling, M.; Weekes, T. C.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. [Acciari, V. A.; Moriarty, P.] Galway Mayo Inst Technol, Dept Life & Phys Sci, Galway, Ireland. [Aliu, E.; Holder, J.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Aliu, E.; Holder, J.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Arlen, T.; Celik, O.; Chow, Y. C.; Fegan, S. J.; Ong, R. A.; Vassiliev, V. V.; Weinstein, A.; Wood, M.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Beilicke, M.; Buckley, J. H.; Bugaev, V.; Dickherber, R.; Krawczynski, H.] Washington Univ, Dept Phys, St Louis, MO 63130 USA. [Boettcher, M.] Ohio Univ, Dept Phys & Astron, Inst Astrophys, Athens, OH 45701 USA. [Bradbury, S. M.; Daniel, M. K.; Rose, H. J.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Butt, Y.; Ergin, T.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Byrum, K.; Smith, A. W.; Wagner, R. G.] Argonne Natl Lab, Argonne, IL 60439 USA. [Cannon, A.; Grube, J.; Quinn, J.; Ward, J. E.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland. [Cesarini, A.; Gillanders, G. H.; Lang, M. J.; Toner, J. A.] Natl Univ Ireland, Sch Phys, Galway, Ireland. [Ciupik, L.; Fortson, L.; Gyuk, G.; Karlsson, N.; Steele, D.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA. [Cogan, P.; Hanna, D.; Maier, G.; McCann, A.; McCutcheon, M.; Ragan, K.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Cui, W.; Finley, J. P.; Gall, D.; Pizlo, F.; Sembroski, G. H.; Varlotta, A.; Zitzer, B.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Falcone, A.] Penn State Univ, Davey Lab 525, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Fortin, P.; Mukherjee, R.] Columbia Univ Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA. [Furniss, A.; Otte, N.; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Furniss, A.; Otte, N.; Williams, D. A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA. [Godambe, S.; Hui, C. M.; Kieda, D.; LeBohec, S.] Univ Utah, Dept Phys, Salt Lake City, UT 84112 USA. [Hays, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Horan, D.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France. [Humensky, T. B.; Swordy, S. P.; Wakely, S. P.; Wissel, S.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Imran, A.; Krennrich, F.; Nagai, T.; Pohl, M.; Schroedter, M.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Kaaret, P.; Pandel, D.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Kertzman, M.] Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA. [Konopelko, A.] Pittsburg State Univ, Dept Phys, Pittsburg, KS 66762 USA. [Millis, J.] Anderson Univ, Dept Phys, Anderson, IN 46012 USA. [Petry, D.] European So Observ, D-85748 Garching, Germany. [Reyes, L. C.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Reynolds, T.] Cork Inst Technol, Dept Appl Phys & Instrumentat, Cork, Ireland. RP Perkins, JS (reprint author), Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. EM jperkins@cfa.harvard.edu RI Hays, Elizabeth/D-3257-2012; Daniel, Michael/A-2903-2010; OI Cui, Wei/0000-0002-6324-5772; Daniel, Michael/0000-0002-8053-7910; Cesarini, Andrea/0000-0002-8611-8610; Ward, John E/0000-0003-1973-0794 FU U. S. Department of Energy; U. S. National Science Foundation; Smithsonian Institution; NSERC in Canada; Science Foundation Ireland; STFC in the UK FX This research was supported by grants from the U. S. Department of Energy, the U. S. National Science Foundation and the Smithsonian Institution, by NSERC in Canada, by Science Foundation Ireland, and by STFC in the UK. NR 31 TC 66 Z9 66 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD MAR 10 PY 2009 VL 693 IS 2 BP L104 EP L108 DI 10.1088/0004-637X/693/2/L104 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 419CJ UT WOS:000264196400012 ER PT J AU Schmelz, JT Saar, SH DeLuca, EE Golub, L Kashyap, VL Weber, MA Klimchuk, JA AF Schmelz, J. T. Saar, S. H. DeLuca, E. E. Golub, L. Kashyap, V. L. Weber, M. A. Klimchuk, J. A. TI HINODE X-RAY TELESCOPE DETECTION OF HOT EMISSION FROM QUIESCENT ACTIVE REGIONS: A NANOFLARE SIGNATURE? SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE Sun: corona; Sun: fundamental parameters; Sun: X-rays, gamma rays ID ATOMIC DATABASE; SOLAR-A; CORONA; ABUNDANCES; MISSION; SULFUR; PLASMA; LINES; RECONSTRUCTION; SPECTRA AB The X-Ray Telescope (XRT) on the Japanese/USA/UK Hinode (Solar-B) spacecraft has detected emission from a quiescent active region core that is consistent with nanoflare heating. The fluxes from 10 broadband X-ray filters and filter combinations were used to construct differential emission measure (DEM) curves. In addition to the expected active region peak at log T = 6.3-6.5, we find a high-temperature component with significant emission measure at log T > 7.0. This emission measure is weak compared to the main peak-the DEM is down by almost three orders of magnitude-which accounts of the fact that it has not been observed with earlier instruments. It is also consistent with spectra of quiescent active regions: no Fe XIX lines are observed in a CHIANTI synthetic spectrum generated using the XRT DEM distribution. The DEM result is successfully reproduced with a simple two-component nanoflare model. C1 [Schmelz, J. T.] Univ Memphis, Dept Phys, Memphis, TN 38152 USA. [Saar, S. H.; DeLuca, E. E.; Golub, L.; Kashyap, V. L.; Weber, M. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Klimchuk, J. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Schmelz, JT (reprint author), Univ Memphis, Dept Phys, Memphis, TN 38152 USA. EM jschmelz@memphis.edu RI Klimchuk, James/D-1041-2012; DeLuca, Edward/L-7534-2013 OI Klimchuk, James/0000-0003-2255-0305; DeLuca, Edward/0000-0001-7416-2895 FU NASA/SAO; NSF [ATM-0402729] FX This work was inspired by a talk given by Fabio Reale at the 2008 September Hinode-2 Meeting in Boulder, CO. We thank Fabio as well as Paola Testa, John Raymond, and Nancy Brickhouse for helpful discussions. Hinode is a Japanese mission developed and launched by ISAS/JAXA, with NAOJ as domestic partner and NASA and STFC (UK) as international partners. It is operated by these agencies in cooperation with ESA and the NSC (Norway). Solar physics research at the University of Memphis is supported by a Hinode subcontract from NASA/SAO as well as NSF ATM-0402729. NR 32 TC 63 Z9 63 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD MAR 10 PY 2009 VL 693 IS 2 BP L131 EP L135 DI 10.1088/0004-637X/693/2/L131 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 419CJ UT WOS:000264196400018 ER PT J AU Lewis, C Bentlage, B AF Lewis, Cheryl Bentlage, Bastian TI Clarifying the identity of the Japanese Habu-kurage, Chironex yamaguchii, sp nov (Cnidaria: Cubozoa: Chirodropida) SO ZOOTAXA LA English DT Article DE Habu-kurage; Okinawa; Chironex; Chiropsalmus quadrigatus; Chiropsoides ID CHIROPSALMUS-QUADRIGATUS; CRUDE VENOM; NEMATOCYSTS; TOXIN AB Here we describe the new species Chironex yamaguchii (Cnidaria: Cubozoa) from the Ryukyu Archipelago, Japan. This highly venomous cubomedusa, commonly referred to as Habu-kurage in Japan, is the culprit for several fatalities in Japanese waters. The scientific name adopted for this species in the literature is Chiropsalmus quadrigatus, but our taxonomic investigations show that this represents a case of mistaken identity. In fact, Habu-kurage is a close relative of Chironex fleckeri, which is particularly interesting because the latter has a reputation for being the most venomous animal known. Differences in the shape of the pedalial canal bend, the number of tentacles, and bell size distinguish the two species. In addition to Japan, Chironex yamaguchii is widely distributed in the Philippines. C1 [Lewis, Cheryl; Bentlage, Bastian] Smithsonian Inst, Natl Museum Nat Hist, Natl Systemat Lab, NMFS, Washington, DC 20013 USA. [Bentlage, Bastian] Univ Kansas, Dept Ecol & Evolutionary Biol, Lawrence, KS 66045 USA. RP Lewis, C (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Natl Systemat Lab, NMFS, MRC 153,POB 37012, Washington, DC 20013 USA. EM amesc@si.edu; bentlage@ku.edu FU US National Science Foundation Assembling the Cnidarian Tree of Life; PADI Foundation; Japanese Government Monbukagakusho Scholarship FX We are grateful to M. Yamaguchi and Y. Araki for facilitating the first author's studies at the University of the Ryukyus and the Okinawa Prefectural Institute for Health and Environment in Okinawa, to K. Masato for providing type material, to A. G. Collins for photographs and helpful comments on this work, and to M. Ekins for facilitating the second author's investigations in the QM collections. Funding was provided through a US National Science Foundation Assembling the Cnidarian Tree of Life Grant, the PADI Foundation, and a Japanese Government Monbukagakusho Scholarship. Two anonymous reviewers provided helpful comments that greatly improved an earlier version of this manuscript. NR 25 TC 15 Z9 15 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 MAR 9 PY 2009 IS 2030 BP 59 EP 65 PG 7 WC Zoology SC Zoology GA 417YO UT WOS:000264114600005 ER PT J AU Phillips, OL Aragao, LEOC Lewis, SL Fisher, JB Lloyd, J Lopez-Gonzalez, G Malhi, Y Monteagudo, A Peacock, J Quesada, CA van der Heijden, G Almeida, S Amaral, I Arroyo, L Aymard, G Baker, TR Banki, O Blanc, L Bonal, D Brando, P Chave, J de Oliveira, ACA Cardozo, ND Czimczik, CI Feldpausch, TR Freitas, MA Gloor, E Higuchi, N Jimenez, E Lloyd, G Meir, P Mendoza, C Morel, A Neill, DA Nepstad, D Patino, S Penuela, MC Prieto, A Ramirez, F Schwarz, M Silva, J Silveira, M Thomas, AS ter Steege, H Stropp, J Vasquez, R Zelazowski, P Davila, EA Andelman, S Andrade, A Chao, KJ Erwin, T Di Fiore, A Honorio, E Keeling, H Killeen, TJ Laurance, WF Cruz, AP Pitman, NCA Vargas, PN Ramirez-Angulo, H Rudas, A Salamao, R Silva, N Terborgh, J Torres-Lezama, A AF Phillips, Oliver L. Aragao, Luiz E. O. C. Lewis, Simon L. Fisher, Joshua B. Lloyd, Jon Lopez-Gonzalez, Gabriela Malhi, Yadvinder Monteagudo, Abel Peacock, Julie Quesada, Carlos A. van der Heijden, Geertje Almeida, Samuel Amaral, Ieda Arroyo, Luzmila Aymard, Gerardo Baker, Tim R. Banki, Olaf Blanc, Lilian Bonal, Damien Brando, Paulo Chave, Jerome Alves de Oliveira, Atila Cristina Cardozo, Nallaret Davila Czimczik, Claudia I. Feldpausch, Ted R. Freitas, Maria Aparecida Gloor, Emanuel Higuchi, Niro Jimenez, Eliana Lloyd, Gareth Meir, Patrick Mendoza, Casimiro Morel, Alexandra Neill, David A. Nepstad, Daniel Patino, Sandra Cristina Penuela, Maria Prieto, Adriana Ramirez, Fredy Schwarz, Michael Silva, Javier Silveira, Marcos Thomas, Anne Sota ter Steege, Hans Stropp, Juliana Vasquez, Rodolfo Zelazowski, Przemyslaw Alvarez Davila, Esteban Andelman, Sandy Andrade, Ana Chao, Kuo-Jung Erwin, Terry Di Fiore, Anthony Honorio C, Euridice Keeling, Helen Killeen, Tim J. Laurance, William F. Pena Cruz, Antonio Pitman, Nigel C. A. Nunez Vargas, Percy Ramirez-Angulo, Hirma Rudas, Agustin Salamao, Rafael Silva, Natalino Terborgh, John Torres-Lezama, Armando TI Drought Sensitivity of the Amazon Rainforest SO SCIENCE LA English DT Article ID LONG-TERM PLOTS; TROPICAL FORESTS; CLIMATE-CHANGE; DRY SEASON; CARBON; MORTALITY; IMPACT; TREE; DYNAMICS; EXCHANGE AB Amazon forests are a key but poorly understood component of the global carbon cycle. If, as anticipated, they dry this century, they might accelerate climate change through carbon losses and changed surface energy balances. We used records from multiple long-term monitoring plots across Amazonia to assess forest responses to the intense 2005 drought, a possible analog of future events. Affected forest lost biomass, reversing a large long-term carbon sink, with the greatest impacts observed where the dry season was unusually intense. Relative to pre-2005 conditions, forest subjected to a 100-millimeter increase in water deficit lost 5.3 megagrams of aboveground biomass of carbon per hectare. The drought had a total biomass carbon impact of 1.2 to 1.6 petagrams (1.2 x 10(15) to 1.6 x 10(15) grams). Amazon forests therefore appear vulnerable to increasing moisture stress, with the potential for large carbon losses to exert feedback on climate change. C1 [Phillips, Oliver L.; Lewis, Simon L.; Lloyd, Jon; Lopez-Gonzalez, Gabriela; Peacock, Julie; Quesada, Carlos A.; van der Heijden, Geertje; Baker, Tim R.; Feldpausch, Ted R.; Gloor, Emanuel; Patino, Sandra; Schwarz, Michael; Chao, Kuo-Jung; Keeling, Helen] Univ Leeds, Sch Geog, Leeds LS2 9JT, W Yorkshire, England. [Aragao, Luiz E. O. C.; Lewis, Simon L.; Fisher, Joshua B.; Lloyd, Jon; Malhi, Yadvinder; Morel, Alexandra; Silva, Javier; Zelazowski, Przemyslaw] Univ Oxford, Environm Change Inst, Sch Geog & Environm, Oxford OX1 3QY, England. [Monteagudo, Abel; Vasquez, Rodolfo; Pena Cruz, Antonio] Jardin Bot Missouri, Oxapampa, Pasco, Peru. [Quesada, Carlos A.; Amaral, Ieda; Alves de Oliveira, Atila Cristina; Andrade, Ana; Laurance, William F.] Inst Nacl de Pesquisas da Amazonia, BR-69060011 Manaus, Amazonas, Brazil. [Almeida, Samuel; Freitas, Maria Aparecida; Salamao, Rafael] Museu Paraense Emilio Goeldi, BR-66077830 Belem, Para, Brazil. [Amaral, Ieda; Andelman, Sandy] Conservat Int, Trop Ecol Assessment & Monitoring Network, Arlington, VA 22202 USA. [Arroyo, Luzmila; Killeen, Tim J.] Museo Hist Nat Noel Kempff Mercado, Santa Cruz, Bolivia. [Arroyo, Luzmila; Neill, David A.] Missouri Bot Garden, St Louis, MO 63166 USA. [Aymard, Gerardo] Univ Nacl Expt Los Llanos Occidentales Ezequiel Z, Herbario Univ PORTI, Programa Ciencias Agro & Mar, Mesa De Cavacas 3350, Portuguesa, Venezuela. [Banki, Olaf] Natl Herbarium Nederland, NL-3584 CS Utrecht, Netherlands. [Blanc, Lilian; Patino, Sandra] CIRAD, UMR EcoFoG, Kourou 97387, French Guiana. [Bonal, Damien] INRA, UMR EcoFoG, Kourou 97387, French Guiana. [Brando, Paulo] Inst Pesquisa Ambiental Amazonia, BR-66035 Belem, Para, Brazil. [Brando, Paulo] Univ Florida, Dept Bot, Gainesville, FL 32611 USA. [Brando, Paulo] Univ Florida, Sch Nat Resources & Environm, Gainesville, FL 32611 USA. [Chave, Jerome] Univ Toulouse 3, Lab EDB, F-31062 Toulouse, France. [Cardozo, Nallaret Davila; Ramirez, Fredy] Univ Nacl Amazonia Peruana, Iquitos, Loreto, Peru. [Czimczik, Claudia I.] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA. [Higuchi, Niro] Inst Nacl de Pesquisas da Amazonia, Dept Silvicultura Trop, Manaus, Amazonas, Brazil. [Jimenez, Eliana; Cristina Penuela, Maria] Univ Nacl Colombia, Leticia, Amazonas, Colombia. [Lloyd, Gareth] Natl Australia Bank, UB2211, Docklands, Vic 3008, Australia. [Meir, Patrick] Univ Edinburgh, Sch Geosci, Edinburgh EH8 9XP, Midlothian, Scotland. [Mendoza, Casimiro] FOMABO Manejo Forestal Tierras Trop Bolivia, Sacta, Bolivia. [Neill, David A.] Jatun Sacha Fdn, Quito, Ecuador. [Nepstad, Daniel] Woods Hole Res Ctr, Falmouth, MA 02540 USA. [Nepstad, Daniel] Gordon & Betty Moore Fdn, San Francisco, CA 94129 USA. [Prieto, Adriana] Inst Alexander von Humboldt, Villa De Leyva, Boyaca, Colombia. [Schwarz, Michael] Univ Bayreuth, Bayreuth Ctr Ecol & Environm Res, D-95440 Bayreuth, Germany. [Silveira, Marcos] Univ Fed Acre, Dept Ciencias Nat, BR-69910900 Rio Branco, AC, Brazil. [Thomas, Anne Sota] Humboldt Univ, Fac Agr & Hort, D-10557 Berlin, Germany. [ter Steege, Hans; Stropp, Juliana] Univ Utrecht, Fac Sci, Dept Biol, Inst Environm Biol, NL-3584 CA Utrecht, Netherlands. [Alvarez Davila, Esteban] Univ Tolima, Fac Ingn Forestal, Ibague 546, Colombia. [Erwin, Terry] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20013 USA. [Di Fiore, Anthony] NYU, Dept Anthropol, Ctr Study Human Origins, New York, NY 10003 USA. [Honorio C, Euridice] Inst Invest Amazonia Peruana, Loreto, Peru. [Laurance, William F.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Pitman, Nigel C. A.] Ctr Invest & Capacitac Rio de Los Amigos, Madre De Dios, Peru. [Nunez Vargas, Percy] Univ Nacl San Antonio Abad Cusco, Cuzco, Peru. [Ramirez-Angulo, Hirma; Torres-Lezama, Armando] Univ Los Andes, Fac Ciencias Forestales, INDEFOR, Merida, Venezuela. [Rudas, Agustin] Univ Nacl Colombia, Inst Ciencias Nat, Bogota, Colombia. [Silva, Natalino] Serv Florestal Brasileiro, BR-70818900 Brasilia, DF, Brazil. [Terborgh, John] Duke Univ, Ctr Trop Conservat, Durham, NC 27708 USA. RP Phillips, OL (reprint author), Univ Leeds, Sch Geog, Leeds LS2 9JT, W Yorkshire, England. EM o.phillips@leeds.ac.uk RI BONAL, Damien/B-2384-2009; Lloyd, Jonathan/F-8893-2010; Pitman, Nigel/A-7681-2008; Phillips, Oliver/A-1523-2011; Laurance, William/B-2709-2012; Brando, Paulo/C-4302-2012; ter Steege, Amaz/B-5866-2011; Meir, Patrick/J-8344-2012; aragao, luiz/G-8387-2012; Feldpausch, Ted/D-3436-2009; Silveira, Marcos/H-7906-2013; Honorio Coronado, Euridice/K-3412-2015; OI Lloyd, Jonathan/0000-0002-5458-9960; Pitman, Nigel/0000-0002-9211-2880; Phillips, Oliver/0000-0002-8993-6168; Brando, Paulo/0000-0001-8952-7025; ter Steege, Amaz/0000-0002-8738-2659; aragao, luiz/0000-0002-4134-6708; Feldpausch, Ted/0000-0002-6631-7962; Silveira, Marcos/0000-0003-0485-7872; Honorio Coronado, Euridice/0000-0003-2314-590X; Fisher, Joshua/0000-0003-4734-9085; Lewis, Simon/0000-0002-8066-6851 FU Leverhulme Trust; NERC [NE/B503384/1, NE/D01025X/1, NER/A/S/2003/00608/2]; WOTRO [W84-581]; Royal Society; University of Leeds; Gordon and Betty Moore Foundation FX This paper is a product of the RAINFOR network. Funding for the 2006 recensuses came primarily from a Natural Environment Research Council (NERC) Urgency Grant. The results summarized here also depend on contributions from numerous field assistants and rural communities in Brazil, Bolivia, Colombia, Ecuador, French Guiana, Guyana, Peru, and Venezuela, many previously acknowledged. I. Huamantupa, N. Jaramillo, N. Saavedram (Peru), V. Pena (Ecuador), J.-C. Arias, and D. Navarrete (Colombia) assisted with recent censuses. We thank CNPQ (Brazil), MCT (Brazil), Ministerio del Medio Ambiente, Vivienda y Desarrollo Territorial (Colombia), Ministerio de Ambiente (Ecuador), the Forestry Commission (Guyana), INRENA (Peru), and Ministerio del Ambiente para el Poder Popular (Venezuela) for research permissions, and the Large Scale Biosphere-Atmosphere Experiment in Amazonia (LBA) for logistical support. This paper was supported by the Leverhulme Trust (O.L.P.), NERC grants NE/B503384/1 and NE/D01025X/1 (O.L.P.), NER/A/S/2003/00608/2 (Y.M.), WOTRO (W84-581) (H.t.S., O.B.), the Royal Society (S.L.L., Y.M.), University of Leeds (T.R.B., K.-J.C., G.L.-G.), and a Gordon and Betty Moore Foundation grant to RAINFOR. Some of the data used in these analyses were collected with support from the TEAM Network of Conservation International, funded by the Gordon and Betty Moore Foundation. We thank D. Galbraith, L. Anderson, C. Michelaki, J. Ratnam, and M. Wagner for discussions; three anonymous reviewers for comments on the manuscript; M. Garcia-Hernandez for help in managing co-author contributions; and A. Manson and D. Appleyard for help in creating the figures. NR 32 TC 615 Z9 636 U1 45 U2 406 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 MAR 6 PY 2009 VL 323 IS 5919 BP 1344 EP 1347 DI 10.1126/science.1164033 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 414PC UT WOS:000263876700042 PM 19265020 ER PT J AU Kaynak, B Hu, Y Martin, RV Sioris, CE Russell, AG AF Kaynak, B. Hu, Y. Martin, R. V. Sioris, C. E. Russell, A. G. TI Comparison of weekly cycle of NO2 satellite retrievals and NOx emission inventories for the continental United States SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID OZONE; MODEL; GOME AB Spatially resolved weekly NO2 variations are obtained from 2003 to 2005 Scanning Imaging Absorption Spectrometer for Atmospheric Cartography (SCIAMACHY) tropospheric NO2 columns for three different types of regions: urban, rural, and rural-point (rural with significant electricity generation unit (EGU) emissions). Regions are compared for magnitudes and weekly profiles. Rural regions do not show any weekly pattern, whereas urban areas show a distinct decrease on the weekends. Rural regions with EGUs show a slight decrease on Sundays. When compared with estimated mobile and stationary nitrogen oxides (NOx) emissions from the year 2004 for seven cities, the satellite data have greater variation during weekdays (Monday-Friday). Overall comparisons show that SCIAMACHY-derived NO2 correlate well with estimated NOx emissions for urban and rural but less for rural-point regions. C1 [Kaynak, B.; Hu, Y.; Russell, A. G.] Georgia Inst Technol, Sch Civil & Environm Engn, Atlanta, GA 30332 USA. [Martin, R. V.] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 1E5, Canada. [Sioris, C. E.] Environm Canada, Toronto, ON M3H 5T4, Canada. [Martin, R. V.; Sioris, C. E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kaynak, B (reprint author), Georgia Inst Technol, Sch Civil & Environm Engn, 311 Ferst Dr, Atlanta, GA 30332 USA. EM gtg354p@mail.gatech.edu RI Kaynak, Burcak/A-4728-2009; Martin, Randall/C-1205-2014; Hu, Yongtao/H-7543-2016 OI Martin, Randall/0000-0003-2632-8402; Hu, Yongtao/0000-0002-5161-0592 FU NASA [SV6-76007, NNG04GE15G]; EPA [RD83096001, RD83107601, RD83215901] FX This work was supported by NASA project SV6-76007 (NNG04GE15G), and EPA grants (RD83096001, RD83107601 and RD83215901). NR 20 TC 19 Z9 20 U1 1 U2 17 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD MAR 5 PY 2009 VL 114 AR D05302 DI 10.1029/2008JD010714 PG 10 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 415QL UT WOS:000263949300002 ER PT J AU Harbaugh, DT Wagner, WL Percy, DM James, HF Fleischer, RC AF Harbaugh, Danica T. Wagner, Warren L. Percy, Diana M. James, Helen F. Fleischer, Robert C. TI Genetic Structure of the Polymorphic Metrosideros (Myrtaceae) Complex in the Hawaiian Islands Using Nuclear Microsatellite Data SO PLOS ONE LA English DT Article AB Background: Five species of Metrosideros (Myrtaceae) are recognized in the Hawaiian Islands, including the widespread M. polymorpha, and are characterized by a multitude of distinctive, yet overlapping, habit, ecological, and morphological forms. It remains unclear, despite several previous studies, whether the morphological variation within Hawaiian Metrosideros is due to hybridization, genetic polymorphism, phenotypic plasticity, or some combination of these processes. The Hawaiian Metrosideros complex has become a model system to study ecology and evolution; however this is the first study to use microsatellite data for addressing inter-island patterns of variation from across the Hawaiian Islands. Methodology/Principal Findings: Ten nuclear microsatellite loci were genotyped from 143 individuals of Metrosideros. We took advantage of the bi-parental inheritance and rapid mutation rate of these data to examine the validity of the current taxonomy and to investigate whether Metrosideros plants from the same island are more genetically similar than plants that are morphologically similar. The Bayesian algorithm of the program STRUCTURE was used to define genetic groups within Hawaiian Metrosideros and the closely related taxon M. collina from the Marquesas and Austral Islands. Several standard and nested AMOVAs were conducted to test whether the genetic diversity is structured geographically or taxonomically. Conclusions/Significance: The results suggest that Hawaiian Metrosideros have dynamic gene flow, with genetic and morphological diversity structured not simply by geography or taxonomy, but as a result of parallel evolution on islands following rampant island-island dispersal, in addition to ancient chloroplast capture. Results also suggest that the current taxonomy requires major revisions in order to reflect the genetic structure revealed in the microsatellite data. C1 [Harbaugh, Danica T.; Wagner, Warren L.] Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, Washington, DC 20560 USA. [Percy, Diana M.] Univ British Columbia, Ctr Plant Res, Vancouver, BC V5Z 1M9, Canada. [Percy, Diana M.] Univ British Columbia, Dept Bot, Vancouver, BC V5Z 1M9, Canada. [James, Helen F.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC USA. [Fleischer, Robert C.] Smithsonian Inst, Natl Zool Pk, Washington, DC USA. RP Harbaugh, DT (reprint author), Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, Washington, DC 20560 USA. EM harbaughd@si.edu FU Center for Conservation and Evolutionary Genetics at the Smithsonian Institution; National Tropical Botanical Garden FX Laboratory expenses for this study were covered by the Center for Conservation and Evolutionary Genetics at the Smithsonian Institution, and by the National Tropical Botanical Garden. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 45 TC 16 Z9 16 U1 2 U2 20 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 185 BERRY ST, STE 1300, SAN FRANCISCO, CA 94107 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD MAR 4 PY 2009 VL 4 IS 3 AR e4698 DI 10.1371/journal.pone.0004698 PG 7 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 437MB UT WOS:000265490500013 PM 19259272 ER PT J AU Smith, BD AF Smith, B. D. TI New frameworks of understanding for the origins of agriculture SO AMERICAN JOURNAL OF HUMAN BIOLOGY LA English DT Meeting Abstract C1 [Smith, B. D.] Smithsonian Inst, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU WILEY-LISS PI HOBOKEN PA DIV JOHN WILEY & SONS INC, 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 1042-0533 J9 AM J HUM BIOL JI Am. J. Hum. Biol. PD MAR-APR PY 2009 VL 21 IS 2 BP 269 EP 269 PG 1 WC Anthropology; Biology SC Anthropology; Life Sciences & Biomedicine - Other Topics GA 409TJ UT WOS:000263528400097 ER PT J AU Kramer, M Weldon, PJ Carroll, JF AF Kramer, Matthew Weldon, Paul J. Carroll, John F. TI Composite scores for concurrent behaviours constructed using canonical discriminant analysis SO ANIMAL BEHAVIOUR LA English DT Editorial Material DE Amblyomma americanum; chemoreception; composite score; discriminant analysis; lone star tick; statistics ID LONGITUDINAL DATA; SUNFISH; MODELS; TICK; PREY C1 [Weldon, Paul J.] Smithsonian Inst, Conservat & Res Ctr, Washington, DC 20560 USA. [Carroll, John F.] Beltsville Agr Res Serv, Anim Parasit Dis Lab, USDA, Beltsville, MD USA. RP Kramer, M (reprint author), ARS, USDA, Biometr Consulting Serv, BARC W, Bldg 005, Beltsville, MD 20705 USA. EM matt.kramer@ars.usda.gov NR 22 TC 7 Z9 7 U1 0 U2 0 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0003-3472 J9 ANIM BEHAV JI Anim. Behav. PD MAR PY 2009 VL 77 IS 3 BP 763 EP 768 DI 10.1016/j.anbehav.2008.12.011 PG 6 WC Behavioral Sciences; Zoology SC Behavioral Sciences; Zoology GA 407LQ UT WOS:000263366100025 ER PT J AU Bridle, S Shawe-Taylor, J Amara, A Applegate, D Balan, ST Berge, J Bernstein, G Dahle, H Erben, T Gill, M Heavens, A Heymans, C High, FW Hoekstra, H Jarvis, M Kirk, D Kitching, T Kneib, JP Kuijken, K Lagatutta, D Mandelbaum, R Massey, R Mellier, Y Moghaddam, B Moudden, Y Nakajima, R Paulin-Henriksson, S Pires, S Rassat, A Refregier, A Rhodes, J Schrabback, T Semboloni, E Shmakova, M Van Waerbeke, L Witherick, D Voigt, L Wittman, D AF Bridle, Sarah Shawe-Taylor, John Amara, Adam Applegate, Douglas Balan, Sreekumar T. Berge, Joel Bernstein, Gary Dahle, Hakon Erben, Thomas Gill, Mandeep Heavens, Alan Heymans, Catherine High, F. William Hoekstra, Henk Jarvis, Mike Kirk, Donnacha Kitching, Thomas Kneib, Jean-Paul Kuijken, Konrad Lagatutta, David Mandelbaum, Rachel Massey, Richard Mellier, Yannick Moghaddam, Baback Moudden, Yassir Nakajima, Reiko Paulin-Henriksson, Stephane Pires, Sandrine Rassat, Anais Refregier, Alexandre Rhodes, Jason Schrabback, Tim Semboloni, Elisabetta Shmakova, Marina Van Waerbeke, Ludovic Witherick, Dugan Voigt, Lisa Wittman, David TI HANDBOOK FOR THE GREAT08 CHALLENGE: AN IMAGE ANALYSIS COMPETITION FOR COSMOLOGICAL LENSING SO ANNALS OF APPLIED STATISTICS LA English DT Article DE Inference; inverse problems; astronomy ID WEAK GRAVITATIONAL SHEAR; LARGE-SCALE STRUCTURE; NONLINEAR CLUSTER INVERSION; GALAXY SHAPE MEASUREMENT; DARK-MATTER; SYSTEMATIC-ERRORS; POLAR SHAPELETS; COSMIC SHEAR; DISTORTIONS; CALIBRATION AB The GRavitational lEnsing Accuracy Testing 2008 (GREAT08) Challenge focuses on a problem that is of crucial importance for future observations in cosmology. The shapes of distant galaxies can be used to determine the properties of dark energy and the nature of gravity, because light from those galaxies is bent by gravity from the intervening dark matter. The observed galaxy images appear distorted, although only slightly, and their shapes must be precisely disentangled from the effects of pixelisation, convolution and noise. The worldwide gravitational lensing community has made significant progress in techniques to measure these distortions via the Shear TEsting Program (STEP). Via STEP, we have run challenges within our own community, and come to recognise that this particular image analysis problem is ideally matched to experts in statistical inference, inverse problems and computational learning. Thus, in order to continue the progress seen in recent years, we are seeking an infusion of new ideas from these communities. This document details the GREAT08 Challenge for potential participants. Please visit www.great08challenge.info for the latest information. C1 [Bridle, Sarah; Shawe-Taylor, John; Balan, Sreekumar T.; Kirk, Donnacha; Witherick, Dugan; Voigt, Lisa] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Amara, Adam] Univ Hong Kong, Hong Kong, Hong Kong, Peoples R China. [Applegate, Douglas; Shmakova, Marina] Stanford Linear Accelerator Ctr, Natl Accelerator Lab, Menlo Pk, CA 94025 USA. [Berge, Joel; Moghaddam, Baback; Rhodes, Jason] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Berge, Joel; Massey, Richard; Moghaddam, Baback; Rhodes, Jason] CALTECH, Pasadena, CA 91125 USA. [Bernstein, Gary; Jarvis, Mike; Nakajima, Reiko] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Erben, Thomas; Semboloni, Elisabetta] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany. [Heavens, Alan] Univ Edinburgh, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland. [High, F. William] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kitching, Thomas] Univ Oxford, Dept Phys, Oxford OX1 3RH, England. [Berge, Joel; Moudden, Yassir; Paulin-Henriksson, Stephane; Pires, Sandrine; Rassat, Anais; Refregier, Alexandre] SAp CEA Saclay, Commissariat Energie Atom, F-91191 Gif Sur Yvette, France. [Dahle, Hakon; Kneib, Jean-Paul] Observ Astron Marseille Prov, Lab Astrophys Marseille, F-13388 Marseille 13, France. [Gill, Mandeep] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Heymans, Catherine; Van Waerbeke, Ludovic] Univ British Columbia, Vancouver, BC V6T 1Z4, Canada. [Hoekstra, Henk] Univ Victoria, Victoria, BC V8W 2Y2, Canada. [Kuijken, Konrad; Schrabback, Tim] Leiden Univ, Leiden Observ, Huygens Lab, NL-2333 CA Leiden, Netherlands. [Lagatutta, David; Wittman, David] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Mandelbaum, Rachel] Inst Adv Study, Princeton, NJ 08540 USA. [Heymans, Catherine; Mellier, Yannick] Inst Astrophys Paris, F-75014 Paris, France. RP Bridle, S (reprint author), UCL, Dept Phys & Astron, Gower St, London WC1E 6BT, England. EM sarah.bridle@ucl.ac.uk RI Witherick, Dugan/C-9403-2014; Mandelbaum, Rachel/N-8955-2014; Kneib, Jean-Paul/A-7919-2015; OI Witherick, Dugan/0000-0002-9175-0151; Mandelbaum, Rachel/0000-0003-2271-1527; Kneib, Jean-Paul/0000-0002-4616-4989; Wittman, David/0000-0002-0813-5888; Rassat, Anais/0000-0002-5476-6461; Hoekstra, Henk/0000-0002-0641-3231 FU Royal Society; European Commission; NASA FX Supported in part by the Jet Propulsion Laboratory, which is run by Caltech under a contract from NASA. NR 53 TC 61 Z9 61 U1 0 U2 2 PU INST MATHEMATICAL STATISTICS PI CLEVELAND PA 3163 SOMERSET DR, CLEVELAND, OH 44122 USA SN 1932-6157 J9 ANN APPL STAT JI Ann. Appl. Stat. PD MAR PY 2009 VL 3 IS 1 BP 6 EP 37 DI 10.1214/08-AOAS222 PG 32 WC Statistics & Probability SC Mathematics GA 522EA UT WOS:000271979400002 ER PT J AU Posada, JM Lechowicz, MJ Kitajima, K AF Posada, Juan M. Lechowicz, Martin J. Kitajima, Kaoru TI Optimal photosynthetic use of light by tropical tree crowns achieved by adjustment of individual leaf angles and nitrogen content SO ANNALS OF BOTANY LA English DT Article DE Optimal resource allocation; nitrogen; photosynthetic capacity; leaf mass per area; tropical trees; radiation use efficiency; scaling; leaf angle; canopy architecture; big leaf model ID DAILY CANOPY PHOTOSYNTHESIS; RADIATION USE EFFICIENCY; CARBON GAIN; INTERCEPTED RADIATION; ISOTOPIC COMPOSITION; SOLAR TRACKING; ACER-SACCHARUM; C-3 PLANTS; BIG-LEAF; LEAVES AB Theory for optimal allocation of foliar nitrogen (ONA) predicts that both nitrogen concentration and photosynthetic capacity will scale linearly with gradients of insolation within plant canopies. ONA is expected to allow plants to efficiently use both light and nitrogen. However, empirical data generally do not exhibit perfect ONA, and light-use optimization per se is little explored. The aim was to examine to what degree partitioning of nitrogen or light is optimized in the crowns of three tropical canopy tree species. Instantaneous photosynthetic photon flux density (PPFD) incident on the adaxial surface of individual leaves was measured along vertical PPFD gradients in tree canopies at a frequency of 0.5 Hz over 9-17 d, and summed to obtain the average daily integral of PPFD for each leaf to characterize its insolation regime. Also measured were leaf N per area (N(area)), leaf mass per area (LMA), the cosine of leaf inclination and the parameters of the photosynthetic light response curve [photosynthetic capacity (A(max)), dark respiration (R(d)), apparent quantum yield (phi) and curvature (theta)]. The instantaneous PPFD measurements and light response curves were used to estimate leaf daily photosynthesis (A(daily)) for each leaf. Leaf N(area) and A(max) changed as a hyperbolic asymptotic function of the PPFD regime, not the linear relationship predicted by ONA. Despite this suboptimal nitrogen partitioning among leaves, A(daily) did increase linearly with PPFD regime through co-ordinated adjustments in both leaf angle and physiology along canopy gradients in insolation, exhibiting a strong convergence among the three species. The results suggest that canopy tree leaves in this tropical forest optimize photosynthetic use of PPFD rather than N per se. Tropical tree canopies then can be considered simple 'big-leaves' in which all constituent 'small leaves' use PPFD with the same photosynthetic efficiency. C1 [Posada, Juan M.; Kitajima, Kaoru] Univ Florida, Dept Bot, Gainesville, FL 32611 USA. [Posada, Juan M.; Lechowicz, Martin J.] McGill Univ, Dept Biol, Montreal, PQ H3A 1B1, Canada. [Kitajima, Kaoru] Smithsonian Trop Res Inst, Panama City, Panama. RP Posada, JM (reprint author), Univ Florida, Dept Bot, 220 Bartram Hall, Gainesville, FL 32611 USA. EM juan_posada@me.com RI Kitajima, Kaoru/E-8877-2012; Posada, Juan/G-3616-2016 OI Posada, Juan/0000-0001-7794-9300 FU Colciencias Ph.D. Fellowship; Russell Dissertation Fellowship (University of Florida); World Ecology Center (University of Missouri St-Louis); Fonds Qebecois de la Recherche sur la Nature et les Technologies (FQRNT); Smithsonian Tropical Research Institute; Natural Sciences and Engineering Research Council of Canada (NSERC) FX We thank Stephen Mulkey, Joe Wright, Thomas Sinclair, Jack Putz, Tim Martin, Edward Schuur, Fernando Valladares and Grace Crummer for providing ideas and suggestions during the different stages of this research. We are grateful to Ben Bolker and Toshi Okuyama for their help with statistical theory and R programming. Eric Graham, Deborah Buehler and Anouk St-Arnaud provided valuable help in the field and during data processing. This work was supported by a Colciencias Ph.D. Fellowship; a Russell Dissertation Fellowship (University of Florida); a fellowship from the World Ecology Center (University of Missouri St-Louis); a Sigma Xi Grant-in-Aid-of-Research and a short-term post-doctoral fellowship from the Fonds Qebecois de la Recherche sur la Nature et les Technologies (FQRNT) to J.M.P. The Smithsonian Tropical Research Institute supported fieldwork in their canopy crane. A Natural Sciences and Engineering Research Council of Canada (NSERC) grant to M.J.L. supported manuscript preparation. NR 70 TC 43 Z9 60 U1 1 U2 34 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0305-7364 J9 ANN BOT-LONDON JI Ann. Bot. PD MAR PY 2009 VL 103 IS 5 BP 795 EP 805 DI 10.1093/aob/mcn265 PG 11 WC Plant Sciences SC Plant Sciences GA 410UG UT WOS:000263603200013 PM 19151040 ER PT J AU Green, WA AF Green, Walton A. TI Hatching seeds before they're counted Graphical methods for interpreting archaeobotanical data SO ARCHAEOLOGICAL AND ANTHROPOLOGICAL SCIENCES LA English DT Article DE Archaeobotany; Ancient Near East; Tell Brak; Data analysis; Quantification in archaeology; Graphical analysis AB Like other analytic aspects of archaeology, archaeobotany has been growing progressively more quantitative in the past few decades. This may be a sign of the proliferation of increasingly mature and sophisticated methodologies for analyzing botanical data, but associated with the sophistication of quantitative methods is their inherent opacity: the value and applicability of anthropological conclusions drawn from quantitative archaeobotanical data are not only limited by the amount of information that can be extracted from data by sophisticated statistical tools, but also by our ability to draw reasonable anthropologicalas opposed to merely statistical-conclusions. Even the words "classification" and "significance" have different meanings in statistics and in anthropology. In this paper, I propose the use of graphical analysis for archaeobotanical data in addition to, or instead of, typical statistical tools like significance tests, variable reduction, and clustering. Applied to data from charred seed assemblages from the ancient Near East, the visual representation of quantitative data has the advantage of handling semiquantitative data better and being interpretable without reliance on the paradigm of a formal statistical test. C1 [Green, Walton A.] Univ Cambridge, McDonald Inst Archaeol Res, Pitt Rivers Lab, Cambridge, England. RP Green, WA (reprint author), Smithsonian Inst, Natl Museum Nat Hist, POB 37012,MRC 121, Washington, DC 20013 USA. EM wagreen@bricol.net NR 21 TC 0 Z9 0 U1 0 U2 6 PU SPRINGER HEIDELBERG PI HEIDELBERG PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY SN 1866-9557 EI 1866-9565 J9 ARCHAEOL ANTHROP SCI JI Archaeol. Anthropol. Sci. PD MAR PY 2009 VL 1 IS 1 BP 1 EP 13 DI 10.1007/s12520-009-0001-8 PG 13 WC Anthropology; Archaeology; Geosciences, Multidisciplinary SC Anthropology; Archaeology; Geology GA V29TV UT WOS:000208771600001 ER PT J AU Hodapp, KW Bressert, E AF Hodapp, Klaus W. Bressert, Eli TI THE VARIABLE REFLECTION NEBULA CEPHEUS A EAST SO ASTRONOMICAL JOURNAL LA English DT Article DE ISM: individual (Cepheus A); ISM: jets and outflows; reflection nebulae; stars: formation; stars: pre-main sequence; stars: variables: other ID YOUNG STELLAR OBJECTS; STAR-FORMING REGION; INFRARED OBSERVATIONS; MOLECULAR OUTFLOW; BIPOLAR OUTFLOWS; PROPER MOTIONS; A EAST; HW2; VARIABILITY; EVOLUTION AB We report K '-band imaging observations of the reflection nebula associated with Cepheus A East covering the time interval from 1990 to 2004. Over this time the reflection nebula shows variations of flux distribution, which we interpret as the effect of inhomogeneous and varying extinction in the light path from the illuminating source HW2 to the reflection nebula. The obscuring material is located within typical distances of approximate to 10 AU from the illuminating source. C1 [Hodapp, Klaus W.] Univ Hawaii, Inst Astron, Hilo, HI 96720 USA. [Bressert, Eli] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Hodapp, KW (reprint author), Univ Hawaii, Inst Astron, 640 N Aohoku Pl, Hilo, HI 96720 USA. EM hodapp@ifa.hawaii.edu; ebressert@cfa.harvard.edu OI Bressert, Eli/0000-0002-6564-6182 FU Jet Propulsion Laboratory; California Institute of Technology under a contract with NASA; National Aeronautics and Space Administration; National Science Foundation FX This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center / California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. NR 36 TC 3 Z9 3 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD MAR PY 2009 VL 137 IS 3 BP 3501 EP 3508 DI 10.1088/0004-6256/137/3/3501 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 412IZ UT WOS:000263719800005 ER PT J AU Bowler, BP Waller, WH Megeath, ST Patten, BM Tamura, M AF Bowler, Brendan P. Waller, William H. Megeath, S. Thomas Patten, Brian M. Tamura, Motohide TI AN INFRARED CENSUS OF STAR FORMATION IN THE HORSEHEAD NEBULA SO ASTRONOMICAL JOURNAL LA English DT Article DE ISM: clouds; ISM: globules; ISM: individual (Horsehead Nebula); stars: formation; stars: pre-main sequence ID YOUNG STELLAR OBJECTS; RADIATION-DRIVEN IMPLOSION; SPITZER-SPACE-TELESCOPE; BRIGHT-RIMMED CLOUDS; NEARBY OB ASSOCIATIONS; IRAS POINT SOURCES; X-RAY OBSERVATIONS; ARRAY CAMERA IRAC; LOW-MASS STARS; MOLECULAR CLOUD AB At similar to 400 pc, the Horsehead Nebula (B33) is the closest radiatively sculpted pillar to the Sun, but the state and extent of star formation in this structure is not well understood. We present deep near-infrared (IRSF/SIRIUS JHK(S)) and mid-infrared (Spitzer/IRAC) observations of the Horsehead Nebula to characterize the star-forming properties of this region and to assess the likelihood of triggered star formation. Infrared color-color and color magnitude diagrams are used to identify young stars based on infrared excess emission and positions to the right of the zero-age main sequence, respectively. Of the 45 sources detected at both near- and mid-infrared wavelengths, three bona fide and five candidate young stars are identified in this 7 ' x 7 ' region. Two bona fide young stars have flat infrared spectral energy distributions and are located at the western irradiated tip of the pillar. The spatial coincidence of the protostars at the leading edge of this elephant trunk is consistent with the radiation-driven implosion model of triggered star formation. There is no evidence, however, for sequential star formation within the immediate similar to 1.5 (0.17 pc) region from the cloud/H II region interface. C1 [Bowler, Brendan P.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Waller, William H.] Tufts Univ, Dept Phys & Astron, Medford, MA 02155 USA. [Megeath, S. Thomas] Univ Toledo, Dept Phys & Astron, Toledo, OH 43606 USA. [Patten, Brian M.] Natl Sci Fdn, Arlington, VA 22230 USA. [Patten, Brian M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Tamura, Motohide] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. RP Bowler, BP (reprint author), Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA. EM bpbowler@ifa.hawaii.edu; william.waller@tufts.edu; megeath@physics.utoledo.edu; bpatten@nsf.gov; motohide.tamura@nao.ac.jp FU Massachusetts Space Grant Consortium; Tufts Summer Scholars FX We thank the referee for the useful feedback, and Bo Reipurth for his helpful comments on a draft of this manuscript. This work makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. This research made use of the SIMBAD database, operated at CDS, Strasbourg, France. B. P. Bowler extends special thanks to the Massachusetts Space Grant Consortium and the Tufts Summer Scholars Program for their support. He also thanks Bill Oliver and Robert Willson of Tufts University for their advice. NR 87 TC 13 Z9 14 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD MAR PY 2009 VL 137 IS 3 BP 3685 EP 3699 DI 10.1088/0004-6256/137/3/3685 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 412IZ UT WOS:000263719800023 ER PT J AU Evans, NR Massa, D Proffitt, C AF Evans, Nancy Remage Massa, Derck Proffitt, Charles TI MASSIVE STAR MULTIPLICITY: THE CEPHEID W Sgr SO ASTRONOMICAL JOURNAL LA English DT Article DE binaries: general; Cepheids ID COMPANIONS; PARALLAXES; PRAESEPE AB We have obtained spectra of the W Sgr system with the Space Telescope Imaging Spectrograph on the Hubble Space Telescope (HST). The spectra resolve the system into a distant companion B which is the hottest star in the system and the spectroscopic binary (A = Aa + Ab). A and B are separated by 0 ''.16. We have extracted the spectra of both of these. We see no flux in the Aa + Ab spectrum which cannot be accounted for by the Cepheid, and put an upper limit on the spectral type and mass of the companion Ab of F5 V and <= 1.4 M(circle dot). Using the orbit from HST fine guidance sensor measurements from Benedict et al., this results in an upper limit to the mass of the Cepheid of <= 5.4 M(circle dot). We also discuss two possible distant companions. Based on the photometry from the Two Micron All Sky Survey Point Source Catalog, they are not physical companions of the W Sgr system. C1 [Evans, Nancy Remage] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Massa, Derck] Comp Sci Corp, Space Telescope Sci Inst, Sci Programs, Baltimore, MD 21218 USA. [Proffitt, Charles] Space Telescope Sci Inst CSC, Baltimore, MD 21218 USA. RP Evans, NR (reprint author), Smithsonian Astrophys Observ, MS 4,60 Garden St, Cambridge, MA 02138 USA. EM nevans@cfa.harvard.edu FU Chandra X-ray Center NASA [NAS8-03060]; STScI [STI-111271]; HST [9105]; NASA [NAS5-26555] FX We acknowledge valuable conversations with Brian Mason about double stars. We thank Karla Peterson of STScI for valuable guidance in the preparation of the observations. Financial support was provided by Chandra X-ray Center NASA Contract NAS8-03060 (for NRE). Support from the research program for CSC astronomers at STScI under contract STI-111271 is gratefully acknowledged. Support for HST Program number 9105 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. (AURA), for the National Aeronautics and Space Administration (NASA) under Contract NAS5-26555. This research made use of the SIMBAD database, operated at CDS, Strasbourg, France, and of the IUE reduction software package. NR 24 TC 16 Z9 16 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD MAR PY 2009 VL 137 IS 3 BP 3700 EP 3705 DI 10.1088/0004-6256/137/3/3700 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 412IZ UT WOS:000263719800024 ER PT J AU Siemiginowska, A AF Siemiginowska, A. TI X-ray emission from GPS and CSS sources SO ASTRONOMISCHE NACHRICHTEN LA English DT Article; Proceedings Paper CT 4th Workshop on Compact Steep Spectrum and Gigahertz-Peaked Spectrum Radio Sources CY MAY 26-29, 2008 CL Riccione, ITALY SP Natl Inst Astrophys, Univ Bologna DE galaxies: active; galaxies: jets; radio continuum: galaxies; X-rays: galaxies ID COMPACT STEEP-SPECTRUM; RADIO GALAXIES; CHANDRA OBSERVATIONS; JET; QUASAR; DISCOVERY; MODELS; GHZ; PKS-1127-145; CLUSTER AB Many X-ray observations of GigaHertz Peaked Spectrum and Compact Steep Spectrum sources have been made with Chandra X-ray Observatory and XMM-Newton Observatory over the last few years. The X-ray spectra contribute the important information to the total energy distribution of the compact radio sources. In addition the spatial resolution of Chandra allows for studies of the X-ray morphology of these sources on arcsec scales and provide a direct view of their environments. This paper gives a review of the current status of the X-ray observations and their contribution to our understanding of the nature of these compact radio sources. It also describes primary physical processes that lead to the observed X-ray emission and summarize X-ray emission properties expected from interactions between an expanding radio source and the intergalactic environment. (C) 2009 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Siemiginowska, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM asiemiginowska@cfa.harvard.edu NR 46 TC 13 Z9 13 U1 0 U2 1 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA POSTFACH 101161, 69451 WEINHEIM, GERMANY SN 0004-6337 EI 1521-3994 J9 ASTRON NACHR JI Astro. Nachr. PD MAR PY 2009 VL 330 IS 2-3 BP 264 EP 269 DI 10.1002/asna.200811172 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 420RJ UT WOS:000264306600037 ER PT J AU Ercolano, B Drake, JJ Clarke, CJ AF Ercolano, B. Drake, J. J. Clarke, C. J. TI Gas phase diagnostics of protoplanetary disc extension (Research Note) SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE accretion, accretion disks; stars: planetary systems: protoplanetary disks; line: formation ID T-TAURI STARS; NE-II EMISSION; CIRCUMSTELLAR DISKS; TRANSITIONAL DISK; ACCRETION DISKS; LINE EMISSION; GRAIN-GROWTH; ORION NEBULA; DUST; PHOTOEVAPORATION AB Aims. We investigate the potential of using ratios of fine structure and near-infrared forbidden-line transitions of atomic carbon to diagnose protoplanetary disc extension. Methods. Using results from 2D photoionisation and radiative transfer modelling of a realistic protoplanetary disc structure irradiated by X-rays from a T Tauri star, we obtain theoretical emission maps from which we construct radial distributions of the strongest emission lines produced in the disc. Results. We show that ratios of fine structure to near-infrared forbidden-line emission of atomic carbon are especially promising for constraining the minimum size of gaseous protoplanetary discs. While theoretically viable, the method presents a number of observational difficulties that are also discussed here. C1 [Ercolano, B.; Clarke, C. J.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Drake, J. J.] Smithsonian Astrophys Observ, MS 3, Cambridge, MA 02138 USA. RP Ercolano, B (reprint author), Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. EM be@ast.cam.ac.uk; jdrake@cfa.harvard.edu; cclarke@ast.cam.ac.uk FU NASA [NAS839073]; HEFCE; STFC FX We thank the anonymous referee for a thorough and constructive assessment of our work. J.J.D. was funded by NASA contract NAS839073 to the Chandra X-ray Center during the course of this research. The simulations were partially run on the Cosmos (SGI altix 4700) supercomputer at DAMTP in Cambridge. Cosmos is a UK-CCC facility which is supported by HEFCE and STFC. NR 48 TC 10 Z9 10 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAR PY 2009 VL 496 IS 3 BP 725 EP 729 DI 10.1051/0004-6361/200810776 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 425VL UT WOS:000264665600015 ER PT J AU Rodriguez-Gil, P Torres, MAP Gansicke, BT Munoz-Darias, T Steeghs, D Schwarz, R Rau, A Hagen, HJ AF Rodriguez-Gil, P. Torres, M. A. P. Gaensicke, B. T. Munoz-Darias, T. Steeghs, D. Schwarz, R. Rau, A. Hagen, H. -J. TI An evolved donor star in the long-period cataclysmic variable HS 0218+3229 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE accretion, accretion discs; stars: binaries: close; stars: novae, cataclysmic variables ID OPTIMAL EXTRACTION ALGORITHM; LIMB-DARKENING COEFFICIENTS; INTERMEDIATE POLAR; ORBITAL PERIOD; DWARF NOVA; MASS; SPECTROSCOPY; PHOTOMETRY; BINARIES; A0620-00 AB Context. We present time-resolved spectroscopy and photometry of HS 0218+3229, a new long-period cataclysmic variable discovered within the Hamburg Quasar Survey. It is one of the few systems that allow a dynamical measurement of the masses of the stellar components. Aims. We combine the analysis of time-resolved optical spectroscopy and R-band photometry with the aim of measuring the mass of the white dwarf and the donor star and the orbital inclination. Methods. Cross-correlation of the spectra with K-type dwarf templates is used to derive the radial velocity curve of the donor star. An optimal subtraction of the broadened templates is performed to measure the rotational broadening and constrain the spectral type of the donor. Finally, an ellipsoidal model is fitted to the R-band light curve to obtain constraints upon the orbital inclination of the binary system. Results. The orbital period of HS 0218+3229 is found to be 0.297229661 +/- 0.000000001 d (7.13351186 +/- 0.00000002 h), and the amplitude of the donor's radial velocity curve is K(2) = 162.4 +/- 1.4 km s(-1). Modelling the ellipsoidal light curves gives an orbital inclination in the range i = 59 degrees +/- 3 degrees. A rotational broadening between 82.4 +/- 1.2 km s(-1) and 89.4 +/- 1.3 km s(-1) is found when assuming zero and continuum limb darkening, respectively. The secondary star has most likely a spectral type K5 and contributes similar to 80-85% to the R-band light. Our analysis yields a mass ratio of 0.52 < q < 0.65, a white dwarf mass of 0.44 < M(1)(M(circle dot)) < 0.65, and a donor star mass of 0.23 < M(2)(M(circle dot)) < 0.44. Conclusions. We find that the donor star in HS 0218+3229 is significantly undermassive for its spectral type. It is therefore very likely that it has undergone nuclear evolution prior to the onset of mass transfer. C1 [Rodriguez-Gil, P.] Isaac Newton Grp Telescopes, Santa Cruz De La Palma 38700, Spain. [Rodriguez-Gil, P.; Munoz-Darias, T.] Inst Astrofis Canarias, Santa Cruz de Tenerife 38205, Spain. [Rodriguez-Gil, P.; Gaensicke, B. T.; Steeghs, D.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Torres, M. A. P.; Steeghs, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Schwarz, R.] Astrophys Inst Potsdam, D-14482 Potsdam, Germany. [Rau, A.] CALTECH, Caltech Opt Observ, Pasadena, CA 91125 USA. [Hagen, H. -J.] Univ Hamburg, D-21029 Hamburg, Germany. RP Rodriguez-Gil, P (reprint author), Isaac Newton Grp Telescopes, Apartado Correos 321, Santa Cruz De La Palma 38700, Spain. EM prguez@ing.iac.es RI Gaensicke, Boris/A-9421-2012; Steeghs, Danny/C-5468-2009; Rodriguez-Gil, Pablo/H-7709-2015 OI Gaensicke, Boris/0000-0002-2761-3005; Steeghs, Danny/0000-0003-0771-4746; Rodriguez-Gil, Pablo/0000-0002-4717-5102 FU XMM-Newton [NNG05GJ22G]; Deutsche Forschungsgemeinschaft [353/11, 353/22] FX This work was supported by XMM-Newton Grant NNG05GJ22G. The HQS was supported by the Deutsche Forschungsgemeinschaft through grants Re 353/11 and Re 353/22. The use of the MOLLY package developed and maintained by Tom Marsh is acknowledged. Thanks to the anonymous referee for valuable input. NR 40 TC 3 Z9 3 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAR PY 2009 VL 496 IS 3 BP 805 EP 812 DI 10.1051/0004-6361/200811312 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 425VL UT WOS:000264665600024 ER PT J AU Simionescu, A Roediger, E Nulsen, PEJ Bruggen, M Forman, WR Bohringer, H Werner, N Finoguenov, A AF Simionescu, A. Roediger, E. Nulsen, P. E. J. Brueggen, M. Forman, W. R. Boehringer, H. Werner, N. Finoguenov, A. TI The large-scale shock in the cluster of galaxies Hydra A SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE X-rays: galaxies: clusters; galaxies: clusters: individual: Hydra A; galaxies: cooling flows; shock waves ID RAY-EMITTING GAS; X-RAY; XMM-NEWTON; INTRACLUSTER MEDIUM; CENTAURUS CLUSTER; HIGH-RESOLUTION; ABELL CLUSTERS; COOLING-FLOW; EVENT FILES; A CLUSTER AB We analyzed a deep XMM-Newton observation of the cluster of galaxies Hydra A, focusing on the large-scale shock discovered in Chandra images as a discontinuity in the surface brightness. The shock front can be seen both in the pressure map and in temperature profiles in several sectors. We compared the results of a spherically symmetric hydrodynamic model to surface brightness profiles and temperature jumps across the shock to determine the shock properties. The Mach numbers determined from the temperature jumps are in good agreement with the Mach numbers derived from EPIC/pn surface brightness profiles and previously from Chandra data and are consistent with M similar to 1.3. In this simple model, the estimated shock age in the different sectors ranges between 130 and 230 Myr and the outburst energy between 1.5 and 3 x 10(61) erg. The shape of the shock seen in the pressure map can be approximated with an ellipse centered similar to 70 kpc towards the NE from the cluster center. This is a good simple approximation to the shock shape seen in the Chandra image, although this shape shows additional small deviations from ellipticity. We aimed to develop a better model that can explain the offset between the shock center and the AGN, as well as give a consistent result on the shock age and energy. To this end, we performed 3D hydrodynamical simulations in which the shock is produced by a symmetrical pair of AGN jets launched in a spherical galaxy cluster. As an explanation of the observed offset between the shock center and the AGN, we consider large-scale bulk flows in the intracluster medium, which were included in the simulation. The simulation successfully reproduces the size, ellipticity, and average Mach number of the observed shock front. The predicted age of the shock is 160 Myr and the total input energy 3 x 10(61) erg. Both values are within the range determined by the spherically symmetric model. To match the observed 70 kpc offset of the shock ellipse from the cluster center by large-scale coherent motions, these would need to have a high velocity of 670 km s(-1). We discuss the feasibility of this scenario and offer alternative ways to produce the observed offset and to further improve the simulation. C1 [Simionescu, A.; Boehringer, H.; Finoguenov, A.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Roediger, E.; Brueggen, M.] Jacobs Univ Bremen, D-28759 Bremen, Germany. [Nulsen, P. E. J.; Forman, W. R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Werner, N.] SRON Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands. [Finoguenov, A.] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA. RP Simionescu, A (reprint author), Max Planck Inst Extraterr Phys, Giessenbachstr, D-85748 Garching, Germany. EM aurora@mpe.mpg.de OI Nulsen, Paul/0000-0003-0297-4493 FU DFG [BR 2026/3]; NIC [2195, 2256, 2877]; NASA [NNX07AQ18G 16610022]; BMBF/DLR [50 OR 0207]; ESA science mission; The Netherlands Institute for Space Research (SRON); Netherlands Organization for Scientific Research FX We acknowledge the support by the DFG grant BR 2026/3 within the Priority Programme "Witnesses of Cosmic History", the supercomputing grants NIC 2195, 2256 and 2877 at the John-Neumann Institut at the Forschungszentrum Julich, and NASA grant NNX07AQ18G 16610022. A. S. would like to thank the Harvard-Smithsonian CfA and Jacobs University Bremen for their hospitality. A. F. acknowledges support from BMBF/DLR under grant 50 OR 0207 and MPG. This work is based on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA member states and the USA (NASA). The Netherlands Institute for Space Research (SRON) is supported financially by NWO, the Netherlands Organization for Scientific Research. Part of the results presented were produced using the FLASH code, a product of the DOE ASC/Alliances-funded Center for Astrophysical Thermonuclear Flashes at the University of Chicago. NR 42 TC 34 Z9 34 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAR PY 2009 VL 495 IS 3 BP 721 EP 732 DI 10.1051/0004-6361:200811071 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 415XJ UT WOS:000263969500003 ER PT J AU Lommen, D Maddison, ST Wright, CM van Dishoeck, EF Wilner, DJ Bourke, TL AF Lommen, D. Maddison, S. T. Wright, C. M. van Dishoeck, E. F. Wilner, D. J. Bourke, T. L. TI Large grains in discs around young stars: ATCA observations of WW Chamaeleontis, RU Lupi, and CS Chamaeleontis SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: circumstellar matter; stars: planetary systems: protoplanetary disks; stars: individual: WW Cha; stars: individual: RU Lup; stars: individual: CS Cha; stars: formation ID T-TAURI-STARS; CHAMELEON-I; CIRCUMSTELLAR DISKS; STELLAR OBJECTS; RADIO-EMISSION; LOW-MASS; PLANETESIMAL FORMATION; PROTOPLANETARY DISKS; BINARY-SYSTEM; DUST AB Context. Grains in discs around young stars grow from interstellar submicron sizes to planetesimals, up to thousands of kilometres in size, over the course of several Myr. Thermal emission of large grains or pebbles can be best observed at centimetre wavelengths. However, other emission mechanisms can contribute, most notably free-free emission from stellar winds and chromospheric activity. Aims. We aim to determine the mechanisms of centimetre emission for three T Tauri stars. WW Cha and RU Lup have recently been found to have grain growth at least up to millimetre sizes in their circumstellar discs, based on millimetre data up to 3.3 mm. CS Cha has similar indications of grain growth in its circumbinary disc. Methods. The T Tauri stars WW Cha and RU Lup were monitored over the course of several years at millimetre and centimetre wavelengths, using the Australia Telescope Compact Array (ATCA). The new ATCA 7 mm system was also used to observe CS Cha at 7 mm. Results. WW Cha was detected on several occasions at 7 and 16 mm. We obtained one detection of WW Cha at 3.5 cm and upper limits only for 6.3 cm. The emission at 16 mm was stable over periods of days, months, and years, whereas the emission at 3.5 cm is found to be variable. A second young stellar object, Ced 112 IRS 4, was found in the field of WW Cha at 16 mm. RU Lup was detected at 7 mm. It was observed at 16 mm three times and at 3 and 6 cm four times and found to be variable in all three wavebands. CS Cha was detected at 7 mm, but the signal-to-noise ratio was not high enough to resolve the gap in the circumbinary disc. The typical resolution of the 7 and 16 mm observations was 5-10 arcsec with rms similar to 0.2 mJy. Conclusions. The emission at 3, 7, and 16 mm for WW Cha is explained well by thermal emission from millimetre and centimetre-sized "pebbles". The cm spectral index between 3.5 and 6.3 cm is consistent with the emission from an optically-thick ionised wind, although the high variability of the cm emission points to a non-thermal contribution. The spectral energy distributions of both RU Lup and CS Cha from 1 to 7 mm are consistent with thermal emission from mm-sized grains. The variability of the longer-wavelength emission for RU Lup and the negative spectral index suggests non-thermal emission, arising from an optically-thin plasma. C1 [Lommen, D.; van Dishoeck, E. F.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Maddison, S. T.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Maddison, S. T.] Ecole Normale Super Lyon, Ctr Rech Astrophys Lyon, F-69364 Lyon, France. [Wright, C. M.] UNSW ADFA, Sch Phys Environm & Math Sci, Canberra, ACT 2600, Australia. [van Dishoeck, E. F.] Max Planck Inst Extraterr Phys MPE, D-85748 Garching, Germany. [Wilner, D. J.; Bourke, T. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Lommen, D (reprint author), Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. EM dave@strw.leidenuniv.nl FU Netherlands Research School; Netherlands Organisation; Swinburne Researcher Development Scheme; Swinburne Special Studies Program; Programme National de Physique Stellaire (PNPS); INSU/CNRS (STM); ARC Australian Research Fellowship FX D. L. acknowledges Swinburne University and UNSW@ADFA for their hospitality. This work was partially supported by a Netherlands Research School For Astronomy network 2 grant and a Netherlands Organisation for Scientific Research Spinoza grant (D. L. and E. F. vD), a Swinburne Researcher Development Scheme, a Swinburne Special Studies Program, and the Programme National de Physique Stellaire (PNPS), INSU/CNRS (STM), and by an ARC Australian Research Fellowship (CMW). We would like to thank the ATNF sta. at Narrabri for their hospitality and assistance, and Annie Hughes and Steve Longmore for assisting with some of the observations. We also thank Fran ois Menard for useful discussions, and we are indepted to the anonymous referee, whose comments helped to considerably improve this paper. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. NR 56 TC 37 Z9 37 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAR PY 2009 VL 495 IS 3 BP 869 EP 879 DI 10.1051/0004-6361:200810999 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 415XJ UT WOS:000263969500014 ER PT J AU Schroedter, M Krennrich, F LeBohec, S Falcone, A Fegan, SJ Horan, D Kildea, J Smith, AW Toner, J Weekes, TC AF Schroedter, M. Krennrich, F. LeBohec, S. Falcone, A. Fegan, S. J. Horan, D. Kildea, J. Smith, A. W. Toner, J. Weekes, T. C. TI Search for primordial black holes with SGARFACE SO ASTROPARTICLE PHYSICS LA English DT Article DE Primordial black holes: general; Gamma-rays: bursts; Techniques: air-Cherenkov ID GAMMA-RAY BURSTS; GLUON-JET EMISSION; HIGH-ENERGY; EARLY UNIVERSE; IMAGING TECHNIQUE; GALACTIC HALO; COSMIC-RAYS; UPPER LIMIT; QUARK-JET; EXPLOSIONS AB The short gamma-ray front air-cherenkov experiment (SGARFACE) uses the Whipple 10 m telescope to search for bursts of gamma-rays. SGARFACE is sensitive to bursts with duration from a few ns to similar to 20 mu s and with gamma-ray energy above 100 MeV. SGARFACE began operating in March 2003 and has collected 2.2 million events during an exposure time of 2267 h. A search for bursts of gamma-rays from explosions of primordial black holes (PBH) was carried out. A Hagedorn-type PBH explosion is predicted to be visible within 60 pc of Earth. Background events were caused by cosmic rays and by atmospheric phenomena and their rejection was accomplished to a large extent using the time-resolved images. No unambiguous detection of bursts of gamma-rays could be made as the remaining background events mimic the expected shape and time-development of bursts. Upper limits on the PBH explosion rate were. derived from the SGARFACE data and are compared to previous and future experiments. We note that a future array of large wide-field air-Cherenkov telescopes equipped with a SGARFACE-like trigger would be able to operate background-free with a 20-30 times higher sensitivity for PBH explosions. (C) 2008 Elsevier B.V. All rights reserved. C1 [Schroedter, M.; Krennrich, F.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [LeBohec, S.] Univ Utah, Dept Phys, Salt Lake City, UT 84112 USA. [Falcone, A.] Penn State Univ, Davey Lab 525, University Pk, PA 16802 USA. [Fegan, S. J.; Horan, D.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France. [Smith, A. W.] Argonne Natl Lab, Argonne, IL 60439 USA. [Toner, J.] Natl Univ Ireland, Sch Phys, Galway, Ireland. [Kildea, J.; Weekes, T. C.] Harvard Smithsonian Ctr Astrophys, Whipple Observ, Amado, AZ 85645 USA. RP Schroedter, M (reprint author), Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. EM schroedt@iastate.edu FU Iowa State University FX We thank the VERITAS Collaboration and the staff at the Whipple Observatory for operating and maintaining the 10 m project. We thank Roy McKay, Harold Skank, and Gary Sleedge at ISU for their help in the electronics design and testing. We would also like to thank Jianwei Qiu at ISU for discussing with us the physics of PBH evaporation and the unknown referee for valuable comments and criticism. FK acknowledges support for the SGARFACE project by the Department of Energy, High-Energy Physics Division, through the Outstanding junior Investigator program and generous financial support by Iowa State University. NR 76 TC 4 Z9 4 U1 0 U2 0 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 MAR PY 2009 VL 31 IS 2 BP 102 EP 115 DI 10.1016/j.astropartphys.2008.12.002 PG 14 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 414HO UT WOS:000263854700005 ER PT J AU Brusa, M Comastri, A Gilli, R Hasinger, G Iwasawa, K Mainieri, V Mignoli, M Salvato, M Zamorani, G Bongiorno, A Cappelluti, N Civano, F Fiore, F Merloni, A Silverman, J Trump, J Vignali, C Capak, P Elvis, M Ilbert, O Impey, C Lilly, S AF Brusa, M. Comastri, A. Gilli, R. Hasinger, G. Iwasawa, K. Mainieri, V. Mignoli, M. Salvato, M. Zamorani, G. Bongiorno, A. Cappelluti, N. Civano, F. Fiore, F. Merloni, A. Silverman, J. Trump, J. Vignali, C. Capak, P. Elvis, M. Ilbert, O. Impey, C. Lilly, S. TI HIGH-REDSHIFT QUASARS IN THE COSMOS SURVEY: THE SPACE DENSITY OF z > 3 X-RAY SELECTED QSOs SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; surveys; X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; DIGITAL-SKY-SURVEY; WIDE-FIELD SURVEY; SUPERMASSIVE BLACK-HOLES; EVOLUTION SURVEY COSMOS; STELLAR RADIO SOURCES; LUMINOSITY FUNCTION; HELLAS2XMM SURVEY; HOST GALAXIES; OPTICAL IDENTIFICATIONS AB We present a new measurement of the space density of high-redshift (z similar or equal to 3.0-4.5), X-ray-selected quasi-stellar objects (QSOs) obtained by exploiting the deep and uniform multiwavelength coverage of the COSMOS survey. We have assembled a large (40 objects), homogeneous sample of z > 3 QSOs with X-ray flux F(0.5-2 keV) > 10(-15) erg cm(-2) s(-1), and available spectroscopic (22) or photometric (18) redshifts. We discuss their optical (color-color diagrams) and X-ray properties, their number counts and space densities and compare our findings with previous works and model predictions. We find that the optical properties of X-ray-selected quasars are not significantly different from those of optically selected samples. There is evidence for substantial X-ray absorption (logN(H) > 23 cm(-2)) in about 20% of the sources in the sample. We find that the comoving space density of luminous (L(X) greater than or similar to 10(44) erg s(-1)) QSOs declines exponentially (by an e-folding per unit redshift) in the z similar to 3.0-4.5 range, with a behavior similar to that observed for optically bright unobscured QSOs selected in large area optical surveys. Prospects for future, large and deep X-ray surveys are also discussed. C1 [Brusa, M.; Hasinger, G.; Iwasawa, K.; Bongiorno, A.; Cappelluti, N.; Merloni, A.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Comastri, A.; Gilli, R.; Iwasawa, K.; Mignoli, M.; Zamorani, G.] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy. [Mainieri, V.] European So Observ, D-85748 Garching, Germany. [Salvato, M.; Capak, P.] CALTECH, Pasadena, CA 91125 USA. [Civano, F.; Elvis, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Fiore, F.] INAF Osservatorio Astron Roma, I-00040 Rome, Italy. [Merloni, A.] Excellence Cluster Univ, D-85748 Garching, Germany. [Silverman, J.; Lilly, S.] ETH Honggerberg, Inst Astron, Swiss Fed Inst Technol, CH-8093 Zurich, Switzerland. [Trump, J.; Impey, C.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Vignali, C.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. [Ilbert, O.] Univ Hawaii, Honolulu, HI 96822 USA. RP Brusa, M (reprint author), Max Planck Inst Extraterr Phys, Giessenbachstr 1, D-85748 Garching, Germany. RI Vignali, Cristian/J-4974-2012; Mignoli, Marco/O-9426-2015; OI Vignali, Cristian/0000-0002-8853-9611; Mignoli, Marco/0000-0002-9087-2835; Bongiorno, Angela/0000-0002-0101-6624; Cappelluti, Nico/0000-0002-1697-186X; Fiore, Fabrizio/0000-0002-4031-4157 FU ESA Member States; USA (NASA); Bundesministerium fur Wirtschaft und Technologie/Deutsches Zentrum fur Luft- und Raumfahrt (BMWI/DLR) [FKZ 50 OX 0001]; Max-Planck Society; XMM-Newton DLR [50-G-0502]; Leibniz Prize of the Deutsche Forschungsgemeinschaft [HA 1850/28-1]; ASI-INAF; PRIN/MIUR [I/023/05/00, 2006-02-5203]; zCOSMOS ESO Large [175.A-0839] FX This work is based on observations obtained with XMM-Newton, an ESA Science Mission with instruments and contributions directly funded by ESA Member States and the USA (NASA). In Germany, the XMM-Newton project is supported by the Bundesministerium fur Wirtschaft und Technologie/Deutsches Zentrum fur Luft- und Raumfahrt (BMWI/DLR, FKZ 50 OX 0001), and the Max-Planck Society. M. B. acknowledges support from the XMM-Newton DLR grant 50-G-0502, G. H. acknowledges the contribution from the Leibniz Prize of the Deutsche Forschungsgemeinschaft under the grant HA 1850/28-1. In Italy, the XMM-COSMOS project is supported by ASI-INAF and PRIN/MIUR under grants I/023/05/00 and 2006-02-5203. The zCOSMOS ESO Large Program Number 175.A-0839 is acknowledged. These results are also based in part on observations obtained with the Walter Baade telescope of the Magellan Consortium at Las Campanas Observatory, and with the MMT which is operated by the MMT Observatory (MMTO), a joint venture of the Smithsonian Institution and the University of Arizona. We gratefully acknowledge the contributions of the entire COSMOS collaboration; more information on the COSMOS survey is available at http://www.astro.caltech.edu/ cosmos. This research has made use of the NASA/IPAC Extragalactic Database (NED) and the SDSS spectral archive. We thank the anonymous referee for his/her useful comments and suggestions. NR 75 TC 75 Z9 75 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 2009 VL 693 IS 1 BP 8 EP 22 DI 10.1088/0004-637X/693/1/8 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 414ZE UT WOS:000263903300002 ER PT J AU Murray-Clay, RA Chiang, EI Murray, N AF Murray-Clay, Ruth A. Chiang, Eugene I. Murray, Norman TI ATMOSPHERIC ESCAPE FROM HOT JUPITERS SO ASTROPHYSICAL JOURNAL LA English DT Article DE hydrodynamics; planetary systems; stars: individual (HD 209458) ID EXTRASOLAR PLANET HD209458B; CLASSICAL T-TAURI; GIANT PLANETS; HD 209458B; EXOPLANET HD-209458B; SOLAR-WIND; HYDRODYNAMIC ESCAPE; MAGNETIC-FIELD; HYDROGEN; MASS AB Photoionization heating from ultraviolet (UV) radiation incidents on the atmospheres of hot Jupiters may drive planetary mass loss. Observations of stellar Lyman-alpha (Ly alpha) absorption have suggested that the hot Jupiter HD 209458b is losing atomic hydrogen. We construct a model of escape that includes realistic heating and cooling, ionization balance, tidal gravity, and pressure confinement by the host star wind. We show that mass loss takes the form of a hydrodynamic (Parker) wind, emitted from the planet's dayside during lulls in the stellar wind. When dayside winds are suppressed by the confining action of the stellar wind, nightside winds might pick up if there is sufficient horizontal transport of heat. A hot Jupiter loses mass at maximum rates of similar to 2 x 10(12) g s(-1) during its host star's pre-main-sequence phase and similar to 2 x 10(10) g s(-1) during the star's main-sequence lifetime, for total maximum losses of similar to 0.06% and similar to 0.6% of the planet's mass, respectively. For UV fluxes F(UV) less than or similar to 10(4) erg cm(-2) s(-1), the mass-loss rate is approximately energy limited and scales as (M) over dot alpha F(UV)(0.9). For larger UV fluxes, such as those typical of T Tauri stars, radiative losses and plasma recombination force (M) over dot to increase more slowly as F(UV)(0.6). Dayside winds are quenched during the T Tauri phase because of confinement by overwhelming stellar wind pressure. During this early stage, nightside winds can still blow if the planet resides outside the stellar Alfven radius; otherwise, even nightside winds are stifled by stellar magnetic pressure, and mass loss is restricted to polar regions. We conclude that while UV radiation can indeed drive winds from hot Jupiters, such winds cannot significantly alter planetary masses during any evolutionary stage. They can, however, produce observable signatures. Candidates for explaining why the Lyman-alpha photons of HD 209458 are absorbed at Doppler-shifted velocities of +/- 100 km s(-1) include charge-exchange in the shock between the planetary and stellar winds. C1 [Murray-Clay, Ruth A.; Chiang, Eugene I.] Univ Calif Berkeley, Dept Astron, Ctr Integrat Planetary Sci, Berkeley, CA 94720 USA. [Murray-Clay, Ruth A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Murray, Norman] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. RP Murray-Clay, RA (reprint author), Univ Calif Berkeley, Dept Astron, Ctr Integrat Planetary Sci, Berkeley, CA 94720 USA. EM rmurray-clay@cfa.harvard.edu FU Berkeley Atmospheric Sciences Center Fellowship; American Association of University Women Fellowship; Hubble Space Telescope Theory Grant [HST-AR-11240.01-A] FX This work was supported by a Berkeley Atmospheric Sciences Center Fellowship and an American Association of University Women Fellowship, both held by R.M.-C., and by Hubble Space Telescope Theory Grant HST-AR-11240.01-A. We thank Jon Arons for a careful reading of the manuscript and for helping us appreciate some aspects of magnetospheric physics. We also thank Lofti Ben-Jaffel, Steven Cranmer, Doug Lin, Geoff Marcy, Eliot Quataert, John Raymond, Jim Stone, and Josh Winn for helpful and encouraging conversations. Finally we are grateful to the referee for an authoritative and thorough report that led to substantive improvements in our work, especially regarding the interpretation of the observations. NR 62 TC 189 Z9 191 U1 3 U2 17 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 2009 VL 693 IS 1 BP 23 EP 42 DI 10.1088/0004-637X/693/1/23 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 414ZE UT WOS:000263903300003 ER PT J AU Matsushita, S Iono, D Petitpas, GR Chou, RCY Gurwell, MA Hunter, TR Muller, JLS Peck, AB Sakamoto, K Satoh, SS Wiedner, MC Wilner, DJ Wilson, CD AF Matsushita, Satoki Iono, Daisuke Petitpas, Glen R. Chou, Richard C. -Y. Gurwell, Mark A. Hunter, Todd R. Muller, Jeremy Lim Sebastien Peck, Alison B. Sakamoto, Kazushi Satoh, Satoko Sawada Wiedner, Martina C. Wilner, David J. Wilson, Christine D. TI SMA (CO)-C-12(J=6-5) AND 435 mu m INTERFEROMETRIC IMAGING OF THE NUCLEAR REGION OF Arp 220 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: individual (Arp 220); galaxies: ISM; galaxies: nuclei; galaxies: starburst ID LUMINOUS INFRARED GALAXIES; DEEP SUBMILLIMETER SURVEY; DENSE MOLECULAR GAS; STAR-FORMATION; ULTRALUMINOUS GALAXIES; PHYSICAL CONDITIONS; STARBURST GALAXIES; MERGER REMNANTS; NUMBER COUNTS; IRAS GALAXIES AB We have used the Submillimeter Array (SMA) to make the first interferometric observations (beam size similar to 1 '' or similar to 400 pc) of the (CO)-C-12 J = 6 - 5 line and 435 mu m (690 GHz) continuum emission toward the central region (half power field of view 17 '') of the nearby ultra-luminous infrared galaxy (ULIRG) Arp 220. These observations resolve the eastern and western nuclei from each other, in both the molecular line and dust continuum emission. At 435 mu m, the peak intensity of the western nucleus is stronger than the eastern nucleus, and the difference in peak intensities is less than at longer wavelengths. Fitting a simple model to the dust emission observed between 1.3 mm and 435 mu m suggests that dust emissivity power law index in the western nucleus is near unity and steeper in the eastern nucleus, about 2, and that the dust emission is optically thick at the shorter wavelength. Comparison with single dish measurements indicate that the interferometer observations are missing similar to 60% of the dust emission, most likely from a spatially extended component to which these observations are not sensitive. The (CO)-C-12 J = 6 - 5 line observations clearly resolve kinematically the two nuclei. The distribution and kinematics of the (CO)-C-12 J = 6 - 5 line appear to be very similar to lower J CO lies observed at similar resolution. Analysis of multiple (CO)-C-12 line intensities indicates that the molecular gas in both nuclei have similar excitation conditions, although the western nucleus is warmer and denser. The excitation conditions are similar to those found in other extreme environments, including the nearby starburst galaxy M82, the active galactic nucleus (AGN) hosting ULIRG Mrk 231, and the high-z QSO BR 1202-0725. Simultaneous lower resolution observations of the (CO)-C-12, (CO)-C-13, and (CO)-O-18 J = 2 - 1 lines show that the (CO)-C-13 and (CO)-O-18 lines have similar intensities, which suggests that both of these lines are optically thick, or possibly that extreme high mass star formation has produced in an overabundance of (CO)-O-18. C1 [Matsushita, Satoki; Chou, Richard C. -Y.; Muller, Jeremy Lim Sebastien; Sakamoto, Kazushi] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Iono, Daisuke] Natl Astron Observ Japan, Tokyo 1810015, Japan. [Petitpas, Glen R.; Gurwell, Mark A.; Hunter, Todd R.; Wilner, David J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Chou, Richard C. -Y.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Hunter, Todd R.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Peck, Alison B.] Joint ALMA Off, Santiago, Chile. [Satoh, Satoko Sawada] Yamaguchi Univ, Dept Phys, Fac Sci, Yamaguchi 7528512, Japan. [Wiedner, Martina C.] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. [Wilson, Christine D.] McMaster Univ, Dept Phys & Astron, Hamilton, ON L8S 4M1, Canada. RP Matsushita, S (reprint author), Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 10617, Taiwan. EM satoki@asiaa.sinica.edu.tw FU Smithsonian Institution; Academia Sinica; National Science Council (NSC) of Taiwan [NSC 96-2112-M-001-009, NSC 97-2112-M-001-021-MY3] FX We thank all the past and present SMA staff for designing, constructing, and supporting the SMA, especially those who worked for and realized the 690 GHz observations. 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. This work is supported by the National Science Council (NSC) of Taiwan, NSC 96-2112-M-001-009 and NSC 97-2112-M-001-021-MY3. NR 68 TC 31 Z9 31 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 2009 VL 693 IS 1 BP 56 EP 68 DI 10.1088/0004-637X/693/1/56 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 414ZE UT WOS:000263903300005 ER PT J AU Blondin, S Prieto, JL Patat, F Challis, P Hicken, M Kirshner, RP Matheson, T Modjaz, M AF Blondin, S. Prieto, J. L. Patat, F. Challis, P. Hicken, M. Kirshner, R. P. Matheson, T. Modjaz, M. TI A SECOND CASE OF VARIABLE Na I D LINES IN A HIGHLY REDDENED TYPE Ia SUPERNOVA SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; dust; extinction; supernovae: general ID ACCRETION-INDUCED COLLAPSE; WHITE-DWARFS; CIRCUMSTELLAR MATERIAL; INTERSTELLAR-MEDIUM; ABSORPTION-LINES; LIGHT CURVES; SN 2005GJ; PROGENITORS; MASS; STARS AB Recent high-resolution spectra of the Type Ia supernova SN 2006X have revealed the presence of time-variable and blueshifted Na I D features, interpreted by Patat et al. as originating in circumstellar material within the progenitor system. The variation seen in SN 2006X induces relatively large changes in the total Na I D equivalent width (Delta EW similar to 0.5 angstrom in just over two weeks) that would be detectable at lower resolutions. We have used a large data set comprising 2400 low-resolution spectra of 450 Type Ia supernovae (SNe Ia) obtained by the CfA Supernova Program to search for variable Na I D features. Out of the 31 SNe Ia (including SN 2006X) in which we could have detected similar EW variations, only one other (SN 1999cl) shows variable Na I D features, with an even larger change over a similar similar to 10 day timescale (Delta EW = 1.66 +/- 0.21 angstrom). Interestingly, both SN 1999cl and SN 2006X are the two most highly reddened objects in our sample, raising the possibility that the variability is connected to dusty environments. C1 [Blondin, S.; Challis, P.; Hicken, M.; Kirshner, R. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Blondin, S.; Patat, F.] European So Observ, D-85748 Garching, Germany. [Prieto, J. L.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Matheson, T.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Modjaz, M.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. RP Blondin, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM sblondin@eso.org; prieto@astronomy.ohio-state.edu; fpatat@eso.org; pchallis@cfa.harvard.edu; mhicken@cfa.harvard.edu; rkirshner@cfa.harvard.edu; matheson@noao.edu; mmodjaz@astro.berkeley.edu OI Patat, Ferdinando/0000-0002-0537-3573 FU Miller Institute Research Fellowship; NSF [AST 06-06772] FX It is a pleasure to thank all observers on the FLWO 1.5 m telescope, and in particular Perry Berlind and Mike Calkins, for their continued support and dedication in obtaining data for the CfA Supernova Program. We further thank Gaston Folatelli and Mario Hamuy of the Carnegie Supernova Project for communicating their Delta m15(B) value for SN 2005am ahead of publication. Similar thanks go to Weidong Li for sharing the results of his MLCS2k2 fit to SN 2005am. We also acknowledge useful discussions with Joe Liske, Josh Simon, Xiaofeng Wang, and David Weinberg. M. M. acknowledges support from a Miller Institute Research Fellowship during the time in which part of this work was completed. We are grateful to the anonymous referee for prompting us to investigate possible differences in the nature of the Na I D variability seen in SN 1999cl and SN 2006X. Support for supernova research at Harvard University, including the CfA Supernova Archive, is provided in part by NSF grant AST 06-06772. NR 87 TC 91 Z9 91 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 2009 VL 693 IS 1 BP 207 EP 215 DI 10.1088/0004-637X/693/1/207 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 414ZE UT WOS:000263903300016 ER PT J AU Ruiter, AJ Belczynski, K Benacquista, M Holley-Bockelmann, K AF Ruiter, Ashley J. Belczynski, Krzysztof Benacquista, Matthew Holley-Bockelmann, Kelly TI THE CONTRIBUTION OF HALO WHITE DWARF BINARIES TO THE LASER INTERFEROMETER SPACE ANTENNA SIGNAL SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: close; Galaxy: halo; gravitational waves; white dwarfs ID GALACTIC HALO; MILKY-WAY; GRAVITATIONAL-RADIATION; MAGELLANIC CLOUDS; LISA SOURCES; STARS; DISK; EVOLUTION; GALAXY; POPULATION AB Galactic double white dwarfs were postulated as a source of confusion limited noise for the Laser Interferometer Space Antenna (LISA), the future space-based gravitational wave observatory. Until very recently, the Galactic population consisted of a relatively well-studied disk population, a somewhat studied smaller bulge population and a mostly unknown, but potentially large halo population. It has been argued that the halo population may produce a signal that is much stronger (factor of similar to 5 in spectral amplitude) than the disk population. However, this surprising result was not based on an actual calculation of a halo white dwarf population, but was derived on (1) the assumption that one can extrapolate the halo population properties from those of the disk population and (2) the postulated (unrealistically) high number of white dwarfs in the halo. We perform the first calculation of a halo white dwarf population using population synthesis models. Our comparison with the signal arising from double white dwarfs in the Galactic disk+bulge clearly shows that it is impossible for the double white dwarf halo signal to exceed that of the rest of the Galaxy. Using microlensing results to give an upper limit on the content of white dwarfs in the halo (similar to 30% baryonic mass in white dwarfs), our predicted halo signal is a factor of 10 lower than the disk+bulge signal. Even in the implausible case, where all of the baryonic halo mass is found in white dwarfs, the halo signal does not become comparable to that of the disk+bulge, and thus would still have a negligible effect on the detection of other LISA sources. C1 [Ruiter, Ashley J.] New Mexico State Univ, Dept Astron, Las Cruces, NM 88003 USA. [Ruiter, Ashley J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Belczynski, Krzysztof] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Belczynski, Krzysztof] Univ Zielona Gora, J Kepler Inst Astron, Zielona Gora, Poland. [Benacquista, Matthew] Univ Texas Brownsville, Ctr Gravitat Wave Astron, Brownsville, TX 78520 USA. [Holley-Bockelmann, Kelly] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA. RP Ruiter, AJ (reprint author), New Mexico State Univ, Dept Astron, 1320 Frenger Mall, Las Cruces, NM 88003 USA. EM aruiter@nmsu.edu; kbelczyn@nms.edu; benacquista@phys.utb.edu; k.holley@vanderbilt.edu FU NASA [NNG94GD52G]; Center for Gravitational Wave Astronomy [NAG5-13396] FX A.J.R. is thankful to S. Torres for informative discussion. M. J. B. acknowledges the support of NASA through grant NNG94GD52G and the Center for Gravitational Wave Astronomy (NAG5-13396). We also thank S. Larson for LISA sensitivity curve dNASAata, and G. Nelemans for the use of Nelemans et al. ( 2004) LISA amplitude data and helpful discussion. The StarTrack simulations were run at the Nicolaus Copernicus Astronomical Center and the Advanced Center for Computation, Research and Education. NR 46 TC 10 Z9 10 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 2009 VL 693 IS 1 BP 383 EP 387 DI 10.1088/0004-637X/693/1/383 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 414ZE UT WOS:000263903300032 ER PT J AU Reid, MJ Menten, KM Brunthaler, A Zheng, XW Moscadelli, L Xu, Y AF Reid, M. J. Menten, K. M. Brunthaler, A. Zheng, X. W. Moscadelli, L. Xu, Y. TI TRIGONOMETRIC PARALLAXES OF MASSIVE STAR-FORMING REGIONS. I. S 252 & G232.6+1.0 SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrometry; Galaxy: fundamental parameters; Galaxy: kinematics and dynamics; masers; stars: formation; techniques: high angular resolution ID SAGITTARIUS-A-ASTERISK; MILKY-WAY; PROPER MOTION; GALAXY; DISTANCE; KINEMATICS; W3(OH) AB We are conducting a large program with the NRAO Very Long Baseline Array (VLBA) to measure trigonometric parallaxes of massive star-forming regions across the Milky Way. Here we report measurement of the parallax and proper motion of methanol masers in S 252 and G232.6+1.0. The parallax of S 252 is 0.476 +/- 0.006 mas (2.10+(0.027)(-0.026) kpc), placing it in the Perseus spiral arm. The parallax of G232.6+1.0 is 0.596 +/- 0.035 mas (1.68+-(0.11)(0.09) kpc), placing it between the Carina-Sagittarius and Perseus arms, possibly in a Local ( Orion) spur of the Carina-Sagittarius arm. For both sources, kinematic distances are significantly greater than their parallax distances. Our parallaxes and proper motions yield full space motions accurate to approximate to 1 km s(-1). Both sources orbit the Galaxy similar to 13 km s(-1) slower than circular rotation. C1 [Reid, M. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Menten, K. M.; Brunthaler, A.; Xu, Y.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Zheng, X. W.] Nanjing Univ, Dept Astron, Nanjing 210093, Peoples R China. [Moscadelli, L.] Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy. [Xu, Y.] Chinese Acad Sci, Purple Mt Observ, Nanjing 210008, Peoples R China. RP Reid, MJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Moscadelli, Luca/0000-0002-8517-8881 FU National Science Foundation of China [10133020, 10103003, 10373025]; DFG FX Research on the structure of the Galaxy in Nanjing University is supported by the National Science Foundation of China under grants 10133020, 10103003 and 10373025, and A. Brunthaler is supported by DFG Priority Programme 1177. NR 26 TC 83 Z9 84 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 2009 VL 693 IS 1 BP 397 EP 405 DI 10.1088/0004-637X/693/1/397 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 414ZE UT WOS:000263903300034 ER PT J AU Moscadelli, L Reid, MJ Menten, KM Brunthaler, A Zheng, XW Xu, Y AF Moscadelli, L. Reid, M. J. Menten, K. M. Brunthaler, A. Zheng, X. W. Xu, Y. TI TRIGONOMETRIC PARALLAXES OF MASSIVE STAR-FORMING REGIONS. II. CEP A AND NGC 7538 SO ASTROPHYSICAL JOURNAL LA English DT Article DE Galaxy: structure; ISM: individual (NGC 7538, Cep A); masers; stars: distances; techniques: interferometric ID GHZ METHANOL MASERS; CIRCUMSTELLAR DISK; NGC-7538 IRS-1; CEPHEUS-A; KINEMATICS; RESOLUTION; DISTANCE; HW2 AB We report trigonometric parallaxes for the sources NGC 7538 and Cep A, corresponding to distances of 2.65+(0.12)(-0.11) and 0.70+(0.04)(-0.04) kpc, respectively. The distance to NGC 7538 is considerably smaller than its kinematic distance and places it in the Perseus spiral arm. The distance to Cep A is also smaller than its kinematic distance and places it in the "Local" arm or spur. Combining the distance and proper motions with observed radial velocities gives the location and full space motion of the star-forming regions. We find significant deviations from circular galactic orbits for these sources: both sources show large peculiar motions (greater than 10 km s(-1)) counter to galactic rotation and NGC 7538 has a comparable peculiar motion toward the Galactic center. C1 [Moscadelli, L.] Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy. [Reid, M. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Menten, K. M.; Brunthaler, A.; Xu, Y.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Zheng, X. W.] Nanjing Univ, Dept Astron, Nanjing 210093, Peoples R China. [Xu, Y.] Chinese Acad Sci, Purple Mt Observ, Nanjing 210008, Peoples R China. RP Moscadelli, L (reprint author), Osserv Astrofis Arcetri, INAF, Largo E Fermi 5, I-50125 Florence, Italy. OI Moscadelli, Luca/0000-0002-8517-8881 FU DFG; Chinese NSF [NSF 10673024, NSF 10733030, NSF 10703010, NSF 10621303] FX Andreas Brunthaler was supported by the DFG Priority Programme 1177. Ye Xu was supported by Chinese NSF through grants NSF 10673024, NSF 10733030, NSF 10703010 and NSF 10621303. Facilities: VLBA NR 17 TC 91 Z9 91 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 2009 VL 693 IS 1 BP 406 EP 412 DI 10.1088/0004-637X/693/1/406 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 414ZE UT WOS:000263903300035 ER PT J AU Xu, Y Reid, MJ Menten, KM Brunthaler, A Zheng, XW Moscadelli, L AF Xu, Y. Reid, M. J. Menten, K. M. Brunthaler, A. Zheng, X. W. Moscadelli, L. TI TRIGONOMETRIC PARALLAXES OF MASSIVE STAR-FORMING REGIONS. III. G59.7+0.1 AND W 51 IRS2 SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrometry; Galaxy: structure; stars: individual (G59.7+0.1, W 51 IRS2); techniques: interferometric ID MILKY-WAY; SPIRAL GALAXIES; CLUSTERS; 2MASS; KINEMATICS; DISTANCE; MOTIONS; M51 AB We report trigonometric parallaxes for G59.7+0.1 and W 51 IRS2, corresponding to distances of 2.16+(0.10)(-0.09) kpc and 5.1+(2.9)(-1.4) kpc, respectively. The distance to G59.7+0.1 is smaller than its near kinematic distance and places it between the Carina-Sagittarius and Perseus spiral arms, probably in the Local (Orion) spur. The distance to W 51 IRS2, while subject to significant uncertainty, is close to its kinematic distance and places it near the tangent point of the Carina-Sagittarius arm. It also agrees well with a recent estimate based on O-type star spectro/photometry. Combining the distances and proper motions with observed radial velocities gives the full space motions of the star-forming regions. We find modest deviations of 5-10 km s(-1) from circular Galactic orbits for these sources, both counter to Galactic rotation and toward the Galactic center. C1 [Xu, Y.; Menten, K. M.; Brunthaler, A.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Xu, Y.] Chinese Acad Sci, Purple Mt Observ, Nanjing 210008, Peoples R China. [Reid, M. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Zheng, X. W.] Nanjing Univ, Nanjing 20093, Peoples R China. [Moscadelli, L.] Arcetri Obs, Florence, Italy. RP Xu, Y (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. OI Moscadelli, Luca/0000-0002-8517-8881 FU Chinese NSF [NSF 10673024, NSF 10733030, NSF 10703010, NSF 10621303]; NBRPC [2007CB815403]; DFG Priority Programme [1177] FX This work was supported by Chinese NSF through grants NSF 10673024, NSF 10733030, NSF 10703010 and NSF 10621303, and NBRPC ( 973 Program) under grant 2007CB815403. Andreas Brunthaler was supported by the DFG Priority Programme 1177. NR 24 TC 67 Z9 68 U1 1 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 2009 VL 693 IS 1 BP 413 EP 418 DI 10.1088/0004-637X/693/1/413 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 414ZE UT WOS:000263903300036 ER PT J AU Zhang, B Zheng, XW Reid, MJ Menten, KM Xu, Y Moscadelli, L Brunthaler, A AF Zhang, B. Zheng, X. W. Reid, M. J. Menten, K. M. Xu, Y. Moscadelli, L. Brunthaler, A. TI TRIGONOMETRIC PARALLAXES OF MASSIVE STAR-FORMING REGIONS. IV. G35.20-0.74 AND G35.20-1.74 SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrometry; Galaxy: structure; stars: individual (G35.20-0.74, G35.20-1.74); techniques: interferometric ID VLBA CALIBRATOR SURVEY; H2O MASERS; DISTANCE; OH AB We report trigonometric parallaxes for the high-mass star-forming regions G35.20-0.74 and G35.20-1.74, corresponding to distances of 2.19+(0.24)(-0.20) kpc and 3.27+(0.56)(-0.42) kpc, respectively. The distances to both sources are close to their near kinematic distances and place them in the Carina-Sagittarius spiral arm. Combining the distances and proper motions with observed radial velocities gives the locations and full space motions of the star-forming regions. Assuming a standard model of the Galaxy, G35.20-0.74 and G35.20-1.74 have peculiar motions of approximate to 13 km s(-1) and approximate to 16 km s(-1) counter to Galactic rotation and approximate to 9 km s(-1) toward the North Galactic Pole. C1 [Zhang, B.; Zheng, X. W.] Nanjing Univ, Dept Astron, Nanjing 210093, Peoples R China. [Zhang, B.] Chinese Acad Sci, Shanghai Astron Observ, Shanghai 200030, Peoples R China. [Reid, M. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Menten, K. M.; Xu, Y.; Brunthaler, A.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Xu, Y.] Chinese Acad Sci, Purple Mt Observ, Nanjing 210008, Peoples R China. [Moscadelli, L.] Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy. RP Zhang, B (reprint author), Nanjing Univ, Dept Astron, Nanjing 210093, Peoples R China. OI Moscadelli, Luca/0000-0002-8517-8881 FU Galaxy in Nanjing University is supported by the National Science Foundation of China ( NSFC) [1062130, 10673024, 10703010, 10733030]; NBRPC [2007CB815403]; DFG Priority Programme FX Research on the structure of the Galaxy in Nanjing University is supported by the National Science Foundation of China ( NSFC) under grants 1062130, 10673024, 10703010 and 10733030, and NBRPC ( 973 Program) under grant 2007CB815403. Andreas Brunthaler was supported by the DFG Priority Programme 1177. NR 25 TC 51 Z9 52 U1 1 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 2009 VL 693 IS 1 BP 419 EP 423 DI 10.1088/0004-637X/693/1/419 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 414ZE UT WOS:000263903300037 ER PT J AU Brunthaler, A Reid, MJ Menten, KM Zheng, XW Moscadelli, L Xu, Y AF Brunthaler, A. Reid, M. J. Menten, K. M. Zheng, X. W. Moscadelli, L. Xu, Y. TI TRIGONOMETRIC PARALLAXES OF MASSIVE STAR-FORMING REGIONS. V. G23.01-0.41 AND G23.44-0.18 SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrometry; Galaxy: fundamental parameters; Galaxy: kinematics and dynamics; masers; stars: formation; techniques: high angular resolution ID VLBA CALIBRATOR SURVEY; GALACTIC BAR; KINEMATICS; SEARCH; MASERS AB We report trigonometric parallaxes for the massive star-forming regions G23.01-0.41 and G23.44-0.18, corresponding to distances of 4.59+(0.38)(-0.33) kpc and 5.88+(1.37)(-0.93) kpc, respectively. The distance to G23.01-0.41 is smaller than its near kinematic distance assuming a standard model of the Milky Way and less than half of its far kinematic distance, which has usually been assumed. This places it in the Crux-Scutum spiral arm. The distance to G23.44-0.18 is close to its near kinematic distance and most likely places it in the Norma spiral arm near the end of the Galactic bar. Combining the distance and proper motions with observed radial velocities gives the location and full space motion of the star-forming regions. We find large deviations from circular Galactic orbits for these sources: both sources show peculiar motions of 20-30 km s(-1) counter to Galactic rotation and toward the Galactic center. These large peculiar motions might be the result of gravitational perturbations from the Galactic bar. C1 [Brunthaler, A.; Menten, K. M.; Xu, Y.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Reid, M. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Zheng, X. W.] Nanjing Univ, Dept Astron, Nanjing 210093, Peoples R China. [Moscadelli, L.] Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy. [Xu, Y.] Chinese Acad Sci, Purple Mt Observ, Nanjing 210008, Peoples R China. RP Brunthaler, A (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. OI Moscadelli, Luca/0000-0002-8517-8881 FU DFG; Chinese NSF [NSF 10673024, NSF 10733030, NSF 10703010, NSF 10621303] FX A.B. was supported by the DFG Priority Programme 1177. Y. X. was supported by Chinese NSF through grants NSF 10673024, NSF 10733030, NSF 10703010, and NSF 10621303. NR 17 TC 56 Z9 57 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 2009 VL 693 IS 1 BP 424 EP 429 DI 10.1088/0004-637X/693/1/424 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 414ZE UT WOS:000263903300038 ER PT J AU Fiore, F Puccetti, S Brusa, M Salvato, M Zamorani, G Aldcroft, T Aussel, H Brunner, H Capak, P Cappelluti, N Civano, F Comastri, A Elvis, M Feruglio, C Finoguenov, A Fruscione, A Gilli, R Hasinger, G Koekemoer, A Kartaltepe, J Ilbert, O Impey, C Le Floc'h, E Lilly, S Mainieri, V Martinez-Sansigre, A McCracken, HJ Menci, N Merloni, A Miyaji, T Sanders, DB Sargent, M Schinnerer, E Scoville, N Silverman, J Smolcic, V Steffen, A Santini, P Taniguchi, Y Thompson, D Trump, JR Vignali, C Urry, M Yan, L AF Fiore, F. Puccetti, S. Brusa, M. Salvato, M. Zamorani, G. Aldcroft, T. Aussel, H. Brunner, H. Capak, P. Cappelluti, N. Civano, F. Comastri, A. Elvis, M. Feruglio, C. Finoguenov, A. Fruscione, A. Gilli, R. Hasinger, G. Koekemoer, A. Kartaltepe, J. Ilbert, O. Impey, C. Le Floc'h, E. Lilly, S. Mainieri, V. Martinez-Sansigre, A. McCracken, H. J. Menci, N. Merloni, A. Miyaji, T. Sanders, D. B. Sargent, M. Schinnerer, E. Scoville, N. Silverman, J. Smolcic, V. Steffen, A. Santini, P. Taniguchi, Y. Thompson, D. Trump, J. R. Vignali, C. Urry, M. Yan, L. TI CHASING HIGHLY OBSCURED QSOs IN THE COSMOS FIELD SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: high-redshift; X-rays: diffuse background ID ACTIVE GALACTIC NUCLEI; SUPERMASSIVE BLACK-HOLES; SPITZER MIDINFRARED SPECTROSCOPY; RAY SPECTRAL PROPERTIES; INFRARED LUMINOUS GALAXIES; COMPTON-THICK QUASARS; X-RAY; HELLAS2XMM SURVEY; STAR-FORMATION; HIGH-REDSHIFT AB A large population of heavily obscured, Compton-thick active galactic nuclei (AGNs) is predicted by AGN synthesis models for the cosmic X-ray background and by the "relic" supermassive black hole mass function measured from local bulges. However, even the deepest X-ray surveys are inefficient to search for these elusive AGNs. Alternative selection criteria, combining mid-infrared with near-infrared, and optical photometry, have instead been successful in pinpointing a large population of Compton-thick AGNs. We take advantage of the deep Chandra and Spitzer coverage of a large area (more than 10 times the area covered by the Chandra deep fields, CDFs) in the Cosmic Evolution Survey (COSMOS) field to extend the search of highly obscured, Compton-thick active nuclei to higher luminosity. These sources have low surface density, and therefore large samples can be provided only through large area surveys, like the COSMOS survey. We analyze the X-ray properties of COSMOS MIPS sources with 24 mu m fluxes higher than 550 mu Jy. For the MIPS sources not directly detected in the Chandra images, we produce stacked images in soft and hard X-rays bands. To estimate the fraction of Compton-thick AGN in the MIPS source population, we compare the observed stacked count rates and hardness ratios to those predicted by detailed Monte Carlo simulations, including both obscured AGN and star-forming galaxies. The volume density of Compton-thick QSOs (log L(2-10 keV) = 44-45 erg s(-1), or log lambda L(lambda)(5.8 mu m) = 44.79-46.18 erg s(-1) for a typical infrared to X-ray luminosity ratio) evaluated in this way is (4.8 +/- 1.1) x 10(-6) Mpc(-3) in the redshift bin 1.2-2.2. This density is similar to 44% of all X-ray-selected QSOs in the same redshift and luminosity bin, and it is consistent with the expectation of the most up-to-date AGN synthesis models for the cosmic X-ray background (Gilli et al. 2007). The density of lower luminosity Compton-thick AGNs (log L(2-10 keV) = 43.5-44) at z = 0.7-1.2 is (3.7 +/- 1.1) x 10(-5) Mpc(-3), corresponding to similar to 67% of X-ray-selected AGNs. The comparison between the fraction of infrared-selected, Compton- thick AGNs to the X-ray selected, unobscured, and moderately obscured AGNs at high and low luminosity suggests that Compton-thick AGNs follow a luminosity dependence similar to that discovered for Compton- thin AGNs, becoming relatively rarer at high luminosities. We estimate that the fraction of AGNs (unobscured, moderately obscured, and Compton thick) to the total MIPS source population is 49 +/- 10%, a value significantly higher than that previously estimated at similar 24 mu m fluxes. We discuss how our findings can constrain AGN feedback models. C1 [Fiore, F.; Menci, N.; Santini, P.] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Rm, Italy. [Puccetti, S.] ASI Sci Data Ctr, I-00044 Frascati, Italy. [Brusa, M.; Brunner, H.; Cappelluti, N.; Finoguenov, A.; Hasinger, G.; Merloni, A.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Salvato, M.; Capak, P.; Scoville, N.; Steffen, A.; Thompson, D.; Yan, L.] CALTECH, Pasadena, CA 91125 USA. [Zamorani, G.; Comastri, A.; Gilli, R.] Osservatorio Astron Bologna, INAF, I-40127 Bologna, Italy. [Aldcroft, T.; Civano, F.; Elvis, M.; Fruscione, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Aussel, H.; Feruglio, C.] Univ Paris Diderot, CEA DSM CNRS, DAPNIA SAp, F-91191 Gif Sur Yvette, France. [Koekemoer, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Kartaltepe, J.; Ilbert, O.; Le Floc'h, E.; Sanders, D. B.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Impey, C.; Trump, J. R.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Lilly, S.; Silverman, J.] ETH, Dept Phys, CH-8093 Zurich, Switzerland. [Mainieri, V.] European So Observ, D-85748 Garching, Germany. [Martinez-Sansigre, A.; Sargent, M.; Schinnerer, E.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [McCracken, H. J.; Smolcic, V.] Univ Paris 06, CNRS, UMR7095, Inst Astrophys, F-75014 Paris, France. [Miyaji, T.] Univ Nacl Autonoma Mexico, 1IA, Ensenada, Baja California, Mexico. [Taniguchi, Y.] Ehime Univ, Dept Phys, Matsuyama, Ehime 7908577, Japan. [Thompson, D.] Univ Arizona, Large Binocular Telescope Observ, Tucson, AZ 85721 USA. [Vignali, C.] Univ Bologna, Bologna, Italy. [Urry, M.] Yale Univ, Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA. RP Fiore, F (reprint author), Osserv Astron Roma, INAF, Via Frascati 33, I-00040 Monte Porzio Catone, Rm, Italy. EM fiore@oa-roma.inaf.it RI Vignali, Cristian/J-4974-2012; Comastri, Andrea/O-9543-2015; Gilli, Roberto/P-1110-2015; OI Vignali, Cristian/0000-0002-8853-9611; Koekemoer, Anton/0000-0002-6610-2048; Comastri, Andrea/0000-0003-3451-9970; Gilli, Roberto/0000-0001-8121-6177; Cappelluti, Nico/0000-0002-1697-186X; Santini, Paola/0000-0002-9334-8705; Puccetti, Simonetta/0000-0002-2734-7835; Menci, Nicola/0000-0002-4096-2680; Zamorani, Giovanni/0000-0002-2318-301X; Urry, Meg/0000-0002-0745-9792; Schinnerer, Eva/0000-0002-3933-7677; Brusa, Marcella/0000-0002-5059-6848; Fiore, Fabrizio/0000-0002-4031-4157 FU ASI/INAF [I/023/05/0, I/024/05/0]; PRIN/MUR [2006-025203] FX We acknowledge support from ASI/INAF contracts I/023/05/0 and I/024/05/0 and by PRIN/MUR grant 2006-025203. F. F. thanks Mari Polletta for useful comments. The zCOSMOSESO Large Program Number 175. A-0839 is also acknowledged. NR 97 TC 133 Z9 133 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 2009 VL 693 IS 1 BP 447 EP 462 DI 10.1088/0004-637X/693/1/447 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 414ZE UT WOS:000263903300040 ER PT J AU Mueller, M Schwartz, DA AF Mueller, M. Schwartz, D. A. TI CONSTRAINTS ON THE LOW-ENERGY CUTOFF IN THE ELECTRON DISTRIBUTION OF THE PKS 0637-752 JET SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: jets; quasars: individual (pks); X-rays: galaxies ID X-RAY JET; ACTIVE GALACTIC NUCLEI; HUBBLE-SPACE-TELESCOPE; EXTENDED RADIO JETS; SYNCHROTRON RADIATION; COMPTON-SCATTERING; CHANDRA DISCOVERY; INVERSE COMPTON; PKS-0637-752; SPECTRUM AB We reanalyze the Chandra ACIS spectrum of the kpc-scale jet in PKS 0637-752 to investigate the possible low-energy cutoff in the relativistic electron spectrum producing the nonthermal radiation in the scenario of inverse Compton (IC) emission off the cosmic microwave background. This was among the first objects targeted by the Chandra Observatory and gives a unique opportunity to study the low-energy X-ray emission free of detector contamination. As previously reported in the literature, the spectrum can be fit by a power law, with the slope predicted by the radio spectrum, modified by low energy absorption through the Galaxy as determined from the spectrum of the quasar core and by HI 21 cm observations. We obtain a marginally better fit with a model of IC emission produced by an electron population that exhibits a cutoff at gamma(min) delta(10) between about 50 and 80 ( assuming Gamma = delta). This range for gamma(min) is higher than has previously been assumed in broadband spectral fits to the jet emission. The observed optical flux can be used to place a lower limit on gamma(min); the constraint is not very strong, but does suggest that gamma(min) must be higher than 1 to avoid overproducing the optical emission. We investigate the effect of uncertainties in the column density for galactic absorption as well as the calibration of Chandra for these early observations. Finally, we discuss the implication of these limits on the jet luminosity in this source. C1 [Mueller, M.] Stanford Linear Accelerator Ctr, Menlo Pk, CA 94025 USA. [Mueller, M.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Schwartz, D. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Mueller, M (reprint author), Stanford Linear Accelerator Ctr, 2575 Sand Hill Rd, Menlo Pk, CA 94025 USA. EM mmueller@slac.stanford.edu; das@head.cfa.harvard.edu FU NASA [NAS8-39073]; CXC [GO3-4120X]; Department of Energy [DE-AC02-76SF00515] FX This research was supported in part by NASA Contract NAS8-39073 to the Chandra X-ray Center and CXC grant GO3-4120X to SAO, as well as by the Department of Energy Contract DE-AC02-76SF00515 to the Stanford Linear Accelerator Center. The data reduction made use of the Chandra Interactive Analysis of Observations tools (http://cxc.harvard.edu/ciao), version 3.3, CALDB version 3.2.4. Spectral fits were obtained in xspec (Arnaud 1996). We wish to thank the anonymous referee for many helpful comments, and Mark Bautz and Catherine Grant for assistance in understanding the low-energy response of Chandra. Further thanks to Greg Madejski and Lukasz Stawarz for fruitful discussions at all stages of this work. NR 32 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 MAR 1 PY 2009 VL 693 IS 1 BP 648 EP 655 DI 10.1088/0004-637X/693/1/648 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 414ZE UT WOS:000263903300053 ER PT J AU Winn, JN Holman, MJ Henry, GW Torres, G Fischer, D Johnson, JA Marcy, GW Shporer, A Mazeh, T AF Winn, Joshua N. Holman, Matthew J. Henry, Gregory W. Torres, Guillermo Fischer, Debra Johnson, John Asher Marcy, Geoffrey W. Shporer, Avi Mazeh, Tsevi TI THE TRANSIT LIGHT CURVE PROJECT. X. A CHRISTMAS TRANSIT OF HD 17156b SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; stars: individual (HD 17156) ID STELLAR ATMOSPHERE MODELS; EXTRASOLAR GIANT PLANETS; SPIN-ORBIT ALIGNMENT; LIMB-DARKENING LAW; IMPROVED PARAMETERS; SURFACE GRAVITIES; ECCENTRIC ORBIT; Y-2 ISOCHRONES; SCINTILLATION; RADIUS AB Photometry is presented of the 2007 December 25 transit of HD 17156b, which has the longest orbital period and highest orbital eccentricity of all the known transiting exoplanets. New measurements of the stellar radial velocity are also presented. All the data are combined and integrated with stellar-evolutionary modeling to derive refined system parameters. The planet's mass and radius are found to be 3.212(-0.082)(+0.069) M-Jup and 1.023(-0.055)(+0.070) R-Jup. The corresponding stellar properties are 1.263(-0.047)(+0.035) M-circle dot and 1.446(-0.069)(+0.099) R-circle dot. The planet is smaller by 1 sigma than a theoretical solar-composition gas giant with the same mass and equilibrium temperature, a possible indication of heavy-element enrichment. The midtransit time is measured to within 1 minute and shows no deviation from a linear ephemeris (and therefore no evidence for orbital perturbations from other planets). We provide ephemerides for future transits and superior conjunctions. There is an 18% chance that the orbital plane is oriented close enough to edge-on for secondary eclipses to occur at superior conjunction. Observations of secondary eclipses would reveal the thermal emission spectrum of a planet that experiences unusually large tidal heating and insolation variations. C1 [Winn, Joshua N.] MIT, Dept Phys, Cambridge, MA 02139 USA. [Winn, Joshua N.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Holman, Matthew J.; Torres, Guillermo] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Henry, Gregory W.] Tennessee State Univ, Ctr Excellence Informat Syst, Nashville, TN 37209 USA. [Fischer, Debra] San Francisco State Univ, Dept Phys & Astron, San Francisco, CA 94132 USA. [Johnson, John Asher] Univ Hawaii, Astron Inst, Honolulu, HI 96822 USA. [Marcy, Geoffrey W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Shporer, Avi; Mazeh, Tsevi] Tel Aviv Univ, Wise Observ, IL-69978 Tel Aviv, Israel. RP Winn, JN (reprint author), MIT, Dept Phys, 77 Massachusetts Ave, Cambridge, MA 02139 USA. OI Fischer, Debra/0000-0003-2221-0861 FU United States-Israel Binational Science Foundation (BSF) [2006234]; NASA [NNG06GH69G, NNG04LG89G]; NASA; NSF; State of Tennessee through its Centers of Excellence program; NSF [AST-0702821]; Kepler Mission under NASA Cooperative Agreement [NCC2-1390]; Kepler Mission FX We are grateful to the referee, Kaspar von Braun, for a timely and detailed critique. This research was partly supported by Grant No. 2006234 from the United States-Israel Binational Science Foundation (BSF). Partial support also came from NASA Origins grants NNG06GH69G (to M. J. H.) and NNG04LG89G (to G. T.). G. W. H. acknowledges support from NASA, NSF, and the State of Tennessee through its Centers of Excellence program. J. A. J. is a National Science Foundation Astronomy and Astrophysics Postdoctoral Fellow with support from the NSF grant AST-0702821. KeplerCam was developed with partial support from the Kepler Mission under NASA Cooperative Agreement NCC2-1390 and the Keplercam observations described in this paper were partly supported by grants from the Kepler Mission to SAO and PSI. NR 55 TC 38 Z9 38 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 2009 VL 693 IS 1 BP 794 EP 803 DI 10.1088/0004-637X/693/1/794 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 414ZE UT WOS:000263903300065 ER PT J AU Owers, MS Couch, WJ Nulsen, PEJ AF Owers, Matt S. Couch, Warrick J. Nulsen, Paul E. J. TI SUBSTRUCTURE IN THE COLD FRONT CLUSTER ABELL 3667 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: individual (Abell 3667) ID GALAXY REDSHIFT SURVEY; EXTENDED RADIO-EMISSION; INTERGALACTIC MEDIUM; MAGNETIC-FIELD; A3667; SPECTROSCOPY; VELOCITIES; AAOMEGA; MERGERS; ORIGIN AB We present evidence for the existence of significant substructure in the cold front cluster Abell 3667 based on multiobject spectroscopy taken with the 3.9 m Anglo-Australian Telescope. This paper is the second in a series analyzing the relationship between cold fronts observed in Chandra X-ray images and merger activity observed at optical wavelengths. We have obtained 910 galaxy redshifts in the field of Abell 3667 out to 3.5 Mpc, of which 550 are confirmed cluster members, more than doubling the number of spectroscopically confirmed members previously available and probing some 3 mag down the luminosity function. From this sample, we derive a cluster redshift of z = 0.0553 +/- 0.0002 and velocity dispersion of 1056 +/- 38 km s(-1) and use a number of statistical tests to search for substructure. We find significant evidence for substructure in the spatial distribution of member galaxies and also in the localized velocity distributions and, in spite of this evidence, find the global velocity distribution does not deviate significantly from a Gaussian. Using combined spatial and velocity information, we found the cluster can be separated into two major structures, with roughly equal velocity dispersions, but offset in peculiar velocity from each other by similar to 500 km s(-1), and a number of minor substructures. We propose two scenarios which explain the radio and X-ray observations. Our data show the cold front is directly related to cluster merger activity, and also highlights the extent of optical data required to unambiguously detect the presence of substructure. C1 [Owers, Matt S.] Univ New S Wales, Sch Phys, Sydney, NSW 2052, Australia. [Couch, Warrick J.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Nulsen, Paul E. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Owers, MS (reprint author), Univ New S Wales, Sch Phys, Sydney, NSW 2052, Australia. EM mowers@phys.unsw.edu.au OI Owers, Matt/0000-0002-2879-1663; Nulsen, Paul/0000-0003-0297-4493 FU NASA [NAS8-01130]; Australian Postgraduate Award; National Aeronautics and Space Administration FX This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 43 TC 32 Z9 32 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 2009 VL 693 IS 1 BP 901 EP 913 DI 10.1088/0004-637X/693/1/901 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 414ZE UT WOS:000263903300075 ER PT J AU Hopkins, PF Cox, TJ Dutta, SN Hernquist, L Kormendy, J Lauer, TR AF Hopkins, Philip F. Cox, Thomas J. Dutta, Suvendra N. Hernquist, Lars Kormendy, John Lauer, Tod R. TI DISSIPATION AND EXTRA LIGHT IN GALACTIC NUCLEI. II. "CUSP" ELLIPTICALS SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Review DE cosmology: theory; galaxies: active; galaxies: evolution; galaxies: nuclei; quasars: general ID EARLY-TYPE GALAXIES; SUPERMASSIVE BLACK-HOLES; HUBBLE-SPACE-TELESCOPE; CCD SURFACE PHOTOMETRY; DIGITAL SKY SURVEY; SMOOTHED PARTICLE HYDRODYNAMICS; QUASAR LUMINOSITY FUNCTION; SPATIALLY-RESOLVED SPECTROSCOPY; ULTRALUMINOUS INFRARED GALAXIES; BRIGHTEST CLUSTER GALAXIES AB We study the origin and properties of "extra" or "excess" central light in the surface brightness profiles of cusp or power-law elliptical galaxies. Dissipational mergers give rise to two-component profiles: an outer profile established by violent relaxation acting on stars already present in the progenitor galaxies prior to the final stages of the merger, and an inner stellar population comprising the extra light, formed in a compact central starburst. By combining a large set of hydrodynamical simulations with data that span a broad range of profiles at various masses, we show that observed cusp ellipticals appear consistent with the predicted "extra light" structure, and we use our simulations to motivate a two-component description of the observations that allows us to examine how the properties and mass of this component scale with, e. g., the mass, gas content, and other properties of the galaxies. We show how to robustly separate the physically meaningful extra light and outer, violently relaxed profile, and demonstrate that the observed cusps and "extra light" are reliable tracers of the degree of dissipation in the spheroid-forming merger. We show that the typical degree of dissipation is a strong function of stellar mass, roughly tracing the observed gas fractions of disks of the same mass over the redshift range z similar to 0-2. We demonstrate a correlation between the strength of this component and effective radius at fixed mass, in the sense that systems with more dissipation are more compact, sufficient to explain the discrepancy in the maximum phase-space and mass densities of ellipticals and their progenitor spirals. We show that the outer shape of the light profile in simulated and observed systems (when fit to properly account for the central light) does not depend on mass, with a mean outer Sersic index similar to 2.5. We also explore how this relates to, e. g., the shapes, kinematic properties, and stellar population gradients of ellipticals. Extra light contributes to making remnants rounder and diskier, and imprints stellar population gradients. Simulations with the gas content needed to match observed surface brightness profiles reproduce the observed age, metallicity, and color gradients of cusp ellipticals, and we make predictions for how these can be used as tracers of the degree of dissipation in spheroid formation. C1 [Hopkins, Philip F.; Cox, Thomas J.; Dutta, Suvendra N.; Hernquist, Lars] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kormendy, John] Univ Texas Austin, Dept Astron, Univ Stn 1, Austin, TX 78712 USA. [Lauer, Tod R.] Natl Opt Astron Observ, Tucson, AZ 85726 USA. RP Hopkins, PF (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 233 TC 157 Z9 157 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD MAR PY 2009 VL 181 IS 1 BP 135 EP 182 DI 10.1088/0067-0049/181/1/135 PG 48 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 415CR UT WOS:000263912400006 ER PT J AU Casares, J Orosz, JA Zurita, C Shahbaz, T Corral-Santana, JM McClintock, JE Garcia, MR Martinez-Pais, IG Charles, PA Fender, RP Remillard, RA AF Casares, J. Orosz, J. A. Zurita, C. Shahbaz, T. Corral-Santana, J. M. McClintock, J. E. Garcia, M. R. Martinez-Pais, I. G. Charles, P. A. Fender, R. P. Remillard, R. A. TI REFINED ORBITAL SOLUTION AND QUIESCENT VARIABILITY IN THE BLACK HOLE TRANSIENT GS 1354-64 (= BW CIR) SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE accretion, accretion disks; binaries: close; stars: individual (BW Cir, GS 1354-64); X-rays: binaries ID X-RAY; V404 CYG; MASS; OUTBURST; BINARIES; FLARES; CURVE AB In Casares et al. we presented the first radial velocity curve of the companion star to BW Cir which demonstrates the presence of a black hole in this historical X-ray transient. But these data were affected by aliasing and two possible periods at 2.5445 days and 2.5635 days were equally possible. Here we present new spectroscopic data that enable us to break the 1-year aliasing and confirm 2.5445 days as the correct orbital period. We also present R-band photometry over 14 years, which reveals the presence of important flaring activity dominating the light curves. C1 [Casares, J.; Zurita, C.; Shahbaz, T.; Corral-Santana, J. M.; Martinez-Pais, I. G.] Inst Astrofis Canarias, Tenerife 38200, Spain. [Orosz, J. A.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA. [Charles, P. A.] South African Astron Observ, ZA-7935 Cape Town, South Africa. [McClintock, J. E.; Garcia, M. R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Charles, P. A.] Univ Southampton, Dept Phys & Astron, Southampton SO17 1BJ, Hants, England. [Fender, R. P.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. [Remillard, R. A.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA USA. RP Casares, J (reprint author), Inst Astrofis Canarias, Tenerife 38200, Spain. EM jcv@iac.es; orosz@sciences.sdsu.edu; czurita@iac.es; tsh@iac.es; jcorral@iac.es; jem@head.cfa.harvard.edu; mgarcia@head.cfa.harvard.edu; igm@iac.es; pac@saao.ac.za; rpf@science.uva.nl; rr@space.mit.edu RI Corral-Santana, Jesus/A-6956-2016 OI Corral-Santana, Jesus/0000-0003-1038-9104 NR 25 TC 25 Z9 25 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 EI 1538-4365 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD MAR PY 2009 VL 181 IS 1 BP 238 EP 243 DI 10.1088/0067-0049/181/1/238 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 415CR UT WOS:000263912400011 ER PT J AU Anderson, LD Bania, TM Jackson, JM Clemens, DP Heyer, M Simon, R Shah, RY Rathborne, JM AF Anderson, L. D. Bania, T. M. Jackson, J. M. Clemens, D. P. Heyer, M. Simon, R. Shah, R. Y. Rathborne, J. M. TI THE MOLECULAR PROPERTIES OF GALACTIC H II REGIONS SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE H II regions; ISM: clouds; ISM: evolution; ISM: lines and bands; ISM: structure; radio lines: ISM ID ULTRACOMPACT HII-REGIONS; RADIO RECOMBINATION LINES; PLANE-CO SURVEY; DISTANCE AMBIGUITY; INNER GALAXY; RING SURVEY; MILKY-WAY; CLOUDS; RESOLUTION; CATALOG AB We derive the molecular properties for a sample of 301 Galactic H II regions including 123 ultra compact (UC), 105 compact, and 73 diffuse nebulae. We analyze all sources within the BU-FCRAO Galactic Ring Survey (GRS) of (13)CO emission known to be H II regions based upon the presence of radio continuum and cm-wavelength radio recombination line emission. Unlike all previous large area coverage 13CO surveys, the GRS is fully sampled in angle and yet covers similar to 75 deg(2) of the Inner Galaxy. The angular resolution of the GRS (46 '') allows us to associate molecular gas with H II regions without ambiguity and to investigate the physical properties of this molecular gas. We find clear CO/H II morphological associations in position and velocity for similar to 80% of the nebular sample. Compact H II region molecular gas clouds are on average larger than UC clouds: 2'.2 compared to 1'.7. Compact and UC H II regions have very similar molecular properties, with similar to 5 K line intensities and similar to 4 km s(-1) line widths. The diffuse H II region molecular gas has lower line intensities, similar to 3 K, and smaller line widths, similar to 3.5 km s(-1). These latter characteristics are similar to those found for quiescent molecular clouds in the GRS. Our sample nebulae thus show evidence for an evolutionary sequence wherein small, dense molecular gas clumps associated with UC H II regions grow into older compact nebulae and finally fragment and dissipate into large, diffuse nebulae. C1 [Anderson, L. D.; Bania, T. M.; Jackson, J. M.; Clemens, D. P.] Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA. [Heyer, M.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Simon, R.] Univ Cologne, Inst Phys, D-50937 Cologne, Germany. [Shah, R. Y.] MIT, Lincoln Lab, Lexington, MA 02420 USA. [Rathborne, J. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Anderson, LD (reprint author), Boston Univ, Inst Astrophys Res, 725 Commonwealth Ave, Boston, MA 02215 USA. RI Bania, Thomas/H-2318-2014; OI Shah, Ronak/0000-0002-2801-6317 FU National Science Foundation [AST-9800334, AST-0098562, AST-0100793] FX 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 National Science Foundation under grants AST-9800334, AST-0098562, and AST-0100793. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. NR 53 TC 28 Z9 28 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD MAR PY 2009 VL 181 IS 1 BP 255 EP 271 DI 10.1088/0067-0049/181/1/255 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 415CR UT WOS:000263912400013 ER PT J AU Reynolds, SM Christman, MC Uy, JAC Patricelli, GL Braun, MJ Borgia, G AF Reynolds, Sheila M. Christman, Mary C. Uy, J. Albert C. Patricelli, Gail L. Braun, Michael J. Borgia, Gerald TI Lekking satin bowerbird males aggregate with relatives to mitigate aggression SO BEHAVIORAL ECOLOGY LA English DT Article DE aggression; bowerbirds; genetic population structure; kin selection; leks; microsatellites; relatedness; sexual selection ID PTILONORHYNCHUS-VIOLACEUS; KIN SELECTION; MICROSATELLITE MARKERS; COOPERATIVE COURTSHIP; SEXUAL COMPETITION; GENETIC-STRUCTURE; GROUSE LEKS; RELATEDNESS; POPULATION; EVOLUTION AB Males in several lekking species aggregate with their relatives to display for females, suggesting that kin selection can affect sexual selection. Several hypotheses have been proposed to explain this behavior, but no general explanation has emerged. In most species with lek mating systems, neighboring males have intense aggressive interactions that can affect the quality of their sexual displays. Here we test the hypothesis that the presence of related neighbors mitigates the negative consequences of this aggression. Male bowerbirds build stick display structures (bowers) that are used by females in mate assessment and are commonly destroyed by males' 2 nearest neighbors. We show that kin aggregate as first or second nearest neighbors, and males direct fewer bower destructions toward kin than equidistant nonkin. Males with more relatives nearby receive fewer bower destructions. These results suggest that the restraining effect of relatedness on aggression favors the close spatial association of related males' display sites. An alternative hypothesis, that related males aggregate to gain copulations from females attracted to successful relatives, was not supported. C1 [Reynolds, Sheila M.; Braun, Michael J.; Borgia, Gerald] Univ Maryland, Behav Ecol Evolut & Systemat Program, College Pk, MD 20742 USA. [Reynolds, Sheila M.; Braun, Michael J.] Smithsonian Inst, Dept Vertebrate Zool, Natl Museum Nat Hist, Suitland, MD 20746 USA. [Christman, Mary C.] Univ Florida, Dept Stat, Gainesville, FL 32611 USA. [Uy, J. Albert C.] Syracuse Univ, Dept Biol, Syracuse, NY 13244 USA. [Patricelli, Gail L.] Univ Calif Davis, Sect Evolut & Ecol, Davis, CA 95616 USA. [Braun, Michael J.; Borgia, Gerald] Univ Maryland, Dept Biol, College Pk, MD 20742 USA. RP Reynolds, SM (reprint author), Univ Maryland, Behav Ecol Evolut & Systemat Program, Biol Psychol Bldg, College Pk, MD 20742 USA. EM sheilar@umd.edu OI Uy, J. Albert C./0000-0002-8437-5525 NR 47 TC 15 Z9 15 U1 3 U2 20 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1045-2249 J9 BEHAV ECOL JI Behav. Ecol. PD MAR-APR PY 2009 VL 20 IS 2 BP 410 EP 415 DI 10.1093/beheco/arn146 PG 6 WC Behavioral Sciences; Biology; Ecology; Zoology SC Behavioral Sciences; Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Zoology GA 421VZ UT WOS:000264387700026 ER PT J AU Laurance, WF AF Laurance, William F. TI How Should the ATBC Approach Conservation ? SO BIOTROPICA LA English DT Editorial Material ID FOREST C1 Smithsonian Trop Res Inst, Balboa, Panama. RP Laurance, WF (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Panama. EM laurancew@si.edu RI Laurance, William/B-2709-2012 NR 10 TC 3 Z9 3 U1 0 U2 0 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0006-3606 J9 BIOTROPICA JI Biotropica PD MAR PY 2009 VL 41 IS 2 BP 139 EP 141 DI 10.1111/j.1744-7429.2009.00497.x PG 3 WC Ecology SC Environmental Sciences & Ecology GA 412TL UT WOS:000263747000001 ER PT J AU Chazdon, RL Harvey, CA Komar, O Griffith, DM Ferguson, BG Martinez-Ramos, M Morales, H Nigh, R Soto-Pinto, L van Breugel, M Philpott, SM AF Chazdon, Robin L. Harvey, Celia A. Komar, Oliver Griffith, Daniel M. Ferguson, Bruce G. Martinez-Ramos, Miguel Morales, Helda Nigh, Ronald Soto-Pinto, Lorena van Breugel, Michiel Philpott, Stacy M. TI Beyond Reserves: A Research Agenda for Conserving Biodiversity in Human-modified Tropical Landscapes SO BIOTROPICA LA English DT Review DE agricultural matrix; agroecology; conservation value; ecosystem services; remnant vegetation; restoration; traditional knowledge ID AMAZONIAN FOREST FRAGMENTS; AGRICULTURAL LANDSCAPES; RAIN-FOREST; AGROFORESTRY SYSTEMS; PLANTATION FORESTS; COSTA-RICA; ECOSYSTEM SERVICES; PROTECTED AREAS; SEED DISPERSAL; CLIMATE-CHANGE AB To truly understand the current status of tropical diversity and to forecast future trends, we need to increase emphasis on the study of biodiversity in rural landscapes that are actively managed or modified by people. We present an integrated landscape approach to promote research in human-modified landscapes that includes the effects of landscape structure and dynamics on conservation of biodiversity, provision of ecosystem services, and sustainability of rural livelihoods. We propose research priorities encompassing three major areas: biodiversity, human-environment interactions, and restoration ecology. We highlight key areas where we lack knowledge and where additional understanding is most urgent for promoting conservation and sustaining rural livelihoods. Finally, we recommend participatory and multidisciplinary approaches in research and management. Lasting conservation efforts demand new alliances among conservation biologists, agroecologists, agronomists, farmers, indigenous peoples, rural social movements, foresters, social scientists, and land managers to collaborate in research, co-design conservation programs and policies, and manage human-modified landscapes in ways that enhance biodiversity conservation and promote sustainable livelihoods. C1 [Chazdon, Robin L.] Univ Connecticut, Dept Ecol & Evolutionary Biol, Storrs, CT 06269 USA. [Harvey, Celia A.] Conservat Int, Arlington, VA 22202 USA. [Komar, Oliver] SalvaNATURA, Programa Ciencias Conservac, San Salvador, El Salvador. [Griffith, Daniel M.] Biodivers BOSAWAS Biosphere Reserve, Managua, Nicaragua. [Ferguson, Bruce G.; Morales, Helda; Soto-Pinto, Lorena] Colegio Frontera Sur, Dept Agroecol, San Cristobal de las Casa, Chiapas, Mexico. [Martinez-Ramos, Miguel] Univ Nacl Autonoma Mexico, Ctr Invest Ecosistemas, Morelia 58089, Michoacan, Mexico. [Nigh, Ronald] Ctr Invest & Estudios Super Antropol Social, San Cristobal de las Casa, Chiapas, Mexico. [van Breugel, Michiel] Smithsonian Trop Forest Res Inst, Ctr Trop Forest Sci, Unit 0948, APO, AA 34002 USA. [Philpott, Stacy M.] Univ Toledo, Dept Environm Sci, Toledo, OH 43606 USA. RP Chazdon, RL (reprint author), Univ Connecticut, Dept Ecol & Evolutionary Biol, Storrs, CT 06269 USA. EM Chazdon@uconn.edu RI Morales, Helda /F-6200-2010; Ferguson, Bruce/F-6201-2010; Trejo, Yesenia/D-9257-2012; Philpott, Stacy/F-2330-2011; OI Ferguson, Bruce/0000-0003-3963-2024; van Breugel, Michiel/0000-0003-2778-7803; Chazdon, Robin/0000-0002-7349-5687 FU National Center for Ecological Analysis and Synthesis (NCEAS); National Science Foundation [DEB-0072909] FX This paper was written by a subgroup of the Working Group on Biodiversity and Conservation Value of Agricultural Landscapes of Mesoamerica supported by the National Center for Ecological Analysis and Synthesis (NCEAS). Funding for the working group was provided by National Science Foundation (grant DEB-0072909), the University of California, and the University of California's Santa Barbara campus. The working group was organized by R.C. and D.G. We thank E. Bruna, T. Gardner, S. Paladino, and three anonymous reviewers for constructive comments on earlier versions of this manuscript. NR 177 TC 185 Z9 193 U1 26 U2 213 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 2009 VL 41 IS 2 BP 142 EP 153 DI 10.1111/j.1744-7429.2008.00471.x PG 12 WC Ecology SC Environmental Sciences & Ecology GA 412TL UT WOS:000263747000002 ER PT J AU Van Bael, SA Valencia, MC Rojas, EI Gomez, N Windsor, DM Herre, EA AF Van Bael, Sunshine A. Valencia, Mariana C. Rojas, Enith I. Gomez, Nelida Windsor, Donald M. Herre, Edward A. TI Effects of Foliar Endophytic Fungi on the Preference and Performance of the Leaf Beetle Chelymorpha alternans in Panama SO BIOTROPICA LA English DT Article DE Colletotrichum gloeosporoides; endophyte; fecundity; Glomerella cingulata; herbivory; horizontal transmission; Merremia umbellata; mutualism ID HOST; DIVERSITY; EVOLUTION; PATHOGEN; INSECTS; TREES; MUTUALISTS; PARASITISM; INFECTION; QUALITY AB Foliar endophytic fungi live inside healthy plant leaves, and in some cases they confer herbivore resistance to the host. All previous studies of endophyte-herbivore interactions have occurred in temperate areas, and many use correlations rather than experiments. In Panama, Glomerella cingulata is a common endophyte species found in healthy leaves, and Chelymorpha alternans is a common herbivore on Merremia umbellata, a tropical vine. We manipulated the abundance of G. cingulata in the leaves of M. umbellata. We then assessed the effects of high and low endophyte densities on the food choice, development, and reproductive success of the leaf beetle, C. alternans. In 'choice' experiments, adult females with a history of feeding on wild plants showed no preference when offered food plants with high and low endophyte densities. Further, in 'no-choice' experiments, C. alternans larvae that were fed high- or low-density endophyte leaves did not differ in development or survivorship. However, when larvae fed on leaves with low endophyte densities became adults, they produced 80 percent more offspring. This suggests high endophyte levels in hosts can have a negative effect on herbivore fecundity. Further experiments are necessary to understand whether the reproductive effects are due to feeding on low-density endophytes in the larval or adult stages, and whether changes in reproductive success are motivated by the adult's perception of food quality or by physiological constraint due to food quality. C1 [Van Bael, Sunshine A.; Valencia, Mariana C.; Rojas, Enith I.; Gomez, Nelida; Windsor, Donald M.; Herre, Edward A.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Van Bael, SA (reprint author), Smithsonian Trop Res Inst, Apartado Postal 0843-03092, Balboa, Ancon, Panama. EM vanbaels@si.edu FU NSF IRFP [OISE-0401957]; The American Association of University FX We thank G. Gilbert, L. Ramirez, and L. Mejia for technical advice and comments; A. Aiello, M. Kaspari, S. Vidal and several anonymous reviewers for commenting on the manuscript. For help in the greenhouse and field we thank D. Alvarez, A. Portugal, B. Perez, M. Sosa, and Y. Jaramillo. This research was funded by a NSF IRFP (Award # OISE-0401957) and The American Association of University Women post-doctoral fellowship to SAV. Permission to do this research was given by the ANAM of the Republic of Panama. NR 30 TC 15 Z9 15 U1 4 U2 21 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0006-3606 J9 BIOTROPICA JI Biotropica PD MAR PY 2009 VL 41 IS 2 BP 221 EP 225 DI 10.1111/j.1744-7429.2008.00476.x PG 5 WC Ecology SC Environmental Sciences & Ecology GA 412TL UT WOS:000263747000012 ER PT J AU Mello, MAR Kalko, EKV Silva, WR AF Mello, M. A. R. Kalko, E. K. V. Silva, W. R. TI Ambient temperature is more important than food availability in explaining reproductive timing of the bat Sturnira lilium (Mammalia: Chiroptera) in a montane Atlantic Forest SO CANADIAN JOURNAL OF ZOOLOGY-REVUE CANADIENNE DE ZOOLOGIE LA English DT Article ID RAIN-FOREST; FRENCH-GUIANA; PATTERNS; PHYLLOSTOMIDAE; COMMUNITIES; STRATEGY; TORPOR; DIET AB Reproduction of bats is determined by a suite of endogenous and exogenous factors. Among exogenous influences, special attention has been given to the influence of food availability. However, in highland forests, severe decreases in temperature during the cold and dry season may also play an important role. In the present study we tested the influence of ambient temperature and food availability on the timing of reproduction in the frugivorous bat Sturnira lilium (E. Geoffroy, 1810). We conducted a 15-month mist-netting sampling in a mountain area of the Brazilian Atlantic Forest during which time we assessed the bats' diet through fecal samples, monitored fruit production of the main food plants, and recorded variations in ambient temperature. Sturnira lilium fed almost exclusively on Solanaceae. Similarly to the lowlands, reproduction was bimodal, but reproductive season tended to be shorter in the highlands and peaked in the warmer months of the year. Overall, 44% to 53% of the reproductive pattern was explained by variations in ambient temperature, while the relationship with food availability was nonsignificant. We conclude that variations in ambient temperature in tropical mountains may be a stronger selection pressure than food availability in determining reproductive timing of bats. C1 [Mello, M. A. R.] Univ Fed Sao Carlos, Dept Bot, BR-13565905 Sao Carlos, SP, Brazil. [Kalko, E. K. V.] Univ Ulm, Inst Expt Ecol, D-89069 Ulm, Germany. [Kalko, E. K. V.] Smithsonian Trop Res Inst, Balboa, Panama. [Silva, W. R.] Univ Estadual Campinas, Dept Zool, BR-13083970 Campinas, SP, Brazil. RP Mello, MAR (reprint author), Univ Fed Sao Carlos, Dept Bot, Rodovia Washington Luis Km 235, BR-13565905 Sao Carlos, SP, Brazil. EM marmello@gmail.com RI Mello, Marco/B-1095-2008; Silva, Wesley/E-2651-2013 OI Mello, Marco/0000-0002-9098-9427; FU CAPES; FAPESP [02/09286-0]; CNPq/DAAD [290088/2004-6]; Bat Conservation International; Idea Wild FX We thank our colleagues at Programa de Pos-Graduacao em Ecologia of Universidade Estadual de Campinas, Institut Experimentelle Okologie of Universitat Ulm, and Parque Estadual Intervales, who helped us a lot during field and laboratory work: Aparecido, Ariovaldo Neto, Benedito Oliveira, Bruno Buzatto, Eliseu, Glauco Machado, Gustavo Requena, Jakob Fahr, Joao Vasconcellos-Neto, Marcelo Gonzaga, Marcelo Oliveira, Mauro Galetti, Natalia Leiner, Pedro Jordano, Regina Alonso, Renato Paiva, and Sandra Silva. M. A. R. M. was sponsored, at different periods, by CAPES, FAPESP (02/09286-0), CNPq/DAAD (290088/2004-6), Bat Conservation International, and Idea Wild. NR 40 TC 13 Z9 14 U1 2 U2 13 PU NATL RESEARCH COUNCIL CANADA-N R C RESEARCH PRESS PI OTTAWA PA BUILDING M 55, OTTAWA, ON K1A 0R6, CANADA SN 0008-4301 J9 CAN J ZOOL JI Can. J. Zool.-Rev. Can. Zool. PD MAR PY 2009 VL 87 IS 3 BP 239 EP 245 DI 10.1139/Z09-010 PG 7 WC Zoology SC Zoology GA 439CV UT WOS:000265606100006 ER PT J AU O'Connor, KA Ferrell, RJ Brindle, E Shofer, J Holman, DJ Miller, RC Schechter, DE Singer, B Weinstein, M AF O'Connor, Kathleen A. Ferrell, Rebecca J. Brindle, Eleanor Shofer, Jane Holman, Darryl J. Miller, Rebecca C. Schechter, Deborah E. Singer, Burton Weinstein, Maxine TI Total and Unopposed Estrogen Exposure across Stages of the Transition to Menopause SO CANCER EPIDEMIOLOGY BIOMARKERS & PREVENTION LA English DT Article ID FOLLICLE-STIMULATING-HORMONE; BREAST-CANCER RISK; MENSTRUAL-CYCLE; PROGESTERONE CONCENTRATIONS; POSTMENOPAUSAL WOMEN; LUTEINIZING-HORMONE; ENDOMETRIAL CANCER; OVARIAN-CANCER; SEX-HORMONES; OLDER WOMEN AB Detailed characterization of estrogen dynamics during the transition to menopause is an important step toward understanding its potential implications for reproductive cancers developing in the transition years. We conducted a 5-year prospective study of endogenous levels of total and unopposed estrogen. Participants (n = 108; ages 25-58 years) collected daily urine specimens for 6 months in each of 5 consecutive years. Specimens were assayed for estrone-3-glucuronide (E1G) and pregnanediol-3-glucuronide. Linear mixed-effects models were used to estimate exposure to total and unopposed estrogen by age and reproductive stage. Reproductive stage was estimated using menstrual cycle length variance. E1G mean area under the curve and mean E1G 5th and 95th percentiles represented total estrogen exposure. An algorithm identifying days of above-baseline E1G that coincided with the days of baseline pregnanediol-3-glucuronide was used to identify days of unopposed estrogen. Mean E1G area under the curve increased with age in the pretransition and early transition and decreased in the late transition. Ninety-fifth percentile E1G levels did not decline until after menopause, whereas 5th percentile levels declined from the early transition to the postmenopause. The number of days of unopposed estrogen was significantly higher during the transition compared with the pretransition. Given the length of time women spend in the transition, they are exposed to more total and unopposed estrogen than has been previously appreciated. Coupled with epidemiologic evidence on lifetime exposure to estrogen, these results suggest that variation in the amount of time spent in the transition may be an important risk factor for reproductive cancers. (Cancer Epidemiol Biomarkers Prev 2009;18(3):828-36) C1 [O'Connor, Kathleen A.; Holman, Darryl J.; Schechter, Deborah E.] Univ Washington, Dept Anthropol, Seattle, WA 98195 USA. [O'Connor, Kathleen A.; Brindle, Eleanor; Shofer, Jane; Holman, Darryl J.] Univ Washington, Ctr Studies Demog & Ecol, Seattle, WA 98195 USA. [Weinstein, Maxine] Georgetown Univ, Ctr Populat & Hlth, Washington, DC USA. [Singer, Burton] Princeton Univ, Off Populat Res, Princeton, NJ 08544 USA. [Miller, Rebecca C.] Temple Univ Hosp & Med Sch, Dept Emergency Med, Philadelphia, PA 19140 USA. [Ferrell, Rebecca J.] Smithsonian Inst, Dept Anthropol, Washington, DC 20560 USA. RP O'Connor, KA (reprint author), Univ Washington, Dept Anthropol, Box 353100, Seattle, WA 98195 USA. EM oconnork@u.washington.edu FU NIH [NIA RO1 AG15141, NICHD HD34159, NIA 5 T32 AG00208, NICHD 2 P30 HD28263, NICHD F32 HD 07994-02]; Population Research Institute, Pennsylvania State University; Center for Studies in Demography and Ecology, University of Washington; Center for Population and Health, Georgetown University FX NIH grants NIA RO1 AG15141, NICHD HD34159, NIA 5 T32 AG00208, NICHD 2 P30 HD28263, and NICHD F32 HD 07994-02; Population Research Institute, Pennsylvania State University; Center for Studies in Demography and Ecology, University of Washington; and Center for Population and Health, Georgetown University. NR 57 TC 18 Z9 19 U1 0 U2 1 PU AMER ASSOC CANCER RESEARCH PI PHILADELPHIA PA 615 CHESTNUT ST, 17TH FLOOR, PHILADELPHIA, PA 19106-4404 USA SN 1055-9965 EI 1538-7755 J9 CANCER EPIDEM BIOMAR JI Cancer Epidemiol. Biomarkers Prev. PD MAR PY 2009 VL 18 IS 3 BP 828 EP 836 DI 10.1158/1055-9965.EPI-08-0996 PG 9 WC Oncology; Public, Environmental & Occupational Health SC Oncology; Public, Environmental & Occupational Health GA 419NK UT WOS:000264226100021 PM 19240232 ER PT J AU Konstantinov, AS Chamorro-Lacayo, ML Savini, VP AF Konstantinov, Alexander S. Lourdes Chamorro-Lacayo, Maria Savini, Vilma P. TI A NEW GENUS OF MOSS-INHABITING FLEA BEETLES (COLEOPTERA: CHRYSOMELIDAE) FROM NICARAGUA SO COLEOPTERISTS BULLETIN LA English DT Article AB Nicaltica new genus and new species (N. selvanegra Konstantinov, Chamorro-Lacayo and Savini) from moss habitat in Nicaragua are described and illustrated. Nicaltica is compared to Kiskeya Konstantinov and Chamorro-Lacayo, Monotalla Bechyne, and Normaltica Konstantinov. C1 [Konstantinov, Alexander S.] USDA ARS, Systemat Entomol Lab, PSI, Smithsonian Inst,Natl Museum Nat Hist, Washington, DC 20013 USA. [Lourdes Chamorro-Lacayo, Maria] Univ Minnesota, Dept Entomol, St Paul, MN 55108 USA. [Savini, Vilma P.] Cent Univ Venezuela, Fac Agron, Museo Inst Zool Agr, Maracay 2101A, Aragua, Venezuela. RP Konstantinov, AS (reprint author), USDA ARS, Systemat Entomol Lab, PSI, Smithsonian Inst,Natl Museum Nat Hist, POB 37012,MRC 168, Washington, DC 20013 USA. EM alex.konstantinov@ars.usda.gov; cham0138@umn.edu; vsgioia@gmail.com NR 7 TC 3 Z9 4 U1 0 U2 0 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 2009 VL 63 IS 1 BP 1 EP 12 DI 10.1649/1127b.1 PG 12 WC Entomology SC Entomology GA 436WV UT WOS:000265447700001 ER PT J AU Lee, CF Staines, CL AF Lee, Chi-Feng Staines, Charles L. TI HEMIPYXIS YUI, A NEW SPECIES FROM TAIWAN, WITH REDESCRIPTION OF ITS ALLIED SPECIES H. QUADRIMACULATA (JACOBY, 1892) (COLEOPTERA: CHRYSOMELIDAE: GALERUCINAE) SO COLEOPTERISTS BULLETIN LA English DT Article ID ALTICINAE AB Hemipyxis yui Lee and Staines, new species, is described and its allied species, H. quadrimaculata (Jacoby, 1892), is redescribed. Male and female reproductive systems are illustrated in detail. C1 [Lee, Chi-Feng] Taiwan Agr Res Inst, Appl Zool Div, Taichung 413, Wufeng, Taiwan. [Staines, Charles L.] Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Lee, CF (reprint author), Taiwan Agr Res Inst, Appl Zool Div, 189 Chung Cheng Rd, Taichung 413, Wufeng, Taiwan. EM cflee@gate.sinica.edu.tw; stainesc@si.edu FU National Science Council of Taiwan [NSC 96-2313-B-055-005-MY2] FX We thank the Taiwan Chrysomelid Research Team for assisting in collecting materials, including Su-Fang Yu, Mei-Hua Tsao, Hou-Jay Chen, Hsueh Lee. We also thank Hsing-Tzung Cheng for taking color photographs. This study is supported financially by the National Science Council of Taiwan (NSC 96-2313-B-055-005-MY2). NR 16 TC 1 Z9 1 U1 0 U2 0 PU COLEOPTERISTS SOC PI ATHENS PA UNIV GEORGIA, 413 BIOLOGICAL SCIENCES BUILDING, ATHENS, GA 30602-2603 USA SN 0010-065X J9 COLEOPTS BULL JI Coleopt. Bull. PD MAR PY 2009 VL 63 IS 1 BP 62 EP 70 DI 10.1649/0010-065X-63.1.62 PG 9 WC Entomology SC Entomology GA 436WV UT WOS:000265447700009 ER PT J AU Rodriguez, S Croquer, A Guzman, HM Bastidas, C AF Rodriguez, S. Croquer, A. Guzman, H. M. Bastidas, C. TI A mechanism of transmission and factors affecting coral susceptibility to Halofolliculina sp infection SO CORAL REEFS LA English DT Article DE Caribbean ciliate infection; Coral reefs; Diseases; Syndromes ID BLACK-BAND-DISEASE; SEA-SURFACE TEMPERATURE; GREAT-BARRIER-REEF; CARIBBEAN CORALS; NUTRIENT ENRICHMENT; ECOLOGICAL DATA; ERODING BAND; SPREAD; REGENERATION; COMMUNITIES AB Anecdotal evidence collected since 2004 suggests that infections caused by ciliates in the genus Halofolliculina may be related to coral mortality in more than 25 scleractinian species in the Caribbean. However, the relationship between the presence of ciliates and coral mortality has not yet been firmly established. Field and laboratory manipulations were used to test if ciliate infections harm corals, if ciliates are able to infect healthy colonies, and if coral susceptibility to ciliate infection depends on temperature, depth, distance to an infected colony, and the presence of injuries. Ciliate infections were always characterized by a visually detectable front of ciliates located on recently exposed coral skeletons. These infections altered the normal structure of the colony by causing tissue mortality (0.8 +/- A 0.95 cm month(-1), mean +/- A SD) and by delaying or preventing recovery from injuries. Under laboratory conditions, ciliates transmitted directly and horizontally from infected to healthy hosts, and coral susceptibility to ciliate infections increased with the presence of injuries. After invasion, the ciliate population grew, rapidly and after 8 d, produced tissue mortality on 32% of newly infected hosts. Thus, our results support the existence of a new Caribbean coral syndrome that is associated with tissue mortality, is infectious, and transmits directly and horizontally. Even though the role of ciliates in the development of lesions on coral tissues remains unclear, their presence is by far the most conspicuous sign of this syndrome; thus, we propose to name this condition Caribbean ciliate infection (CCI). C1 [Rodriguez, S.; Croquer, A.; Bastidas, C.] Univ Simon Bolivar, Dept Biol Organismos, Caracas 1080A, Venezuela. [Guzman, H. M.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Rodriguez, S (reprint author), Univ Simon Bolivar, Dept Biol Organismos, Caracas 1080A, Venezuela. EM sebastianr@usb.ve OI Croquer, Aldo/0000-0001-8880-9338 NR 50 TC 13 Z9 13 U1 1 U2 6 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0722-4028 J9 CORAL REEFS JI Coral Reefs PD MAR PY 2009 VL 28 IS 1 BP 67 EP 77 DI 10.1007/s00338-008-0419-y PG 11 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 403GT UT WOS:000263071800009 ER PT J AU Long, WC Seitz, RD AF Long, William Christopher Seitz, Rochelle Diane TI Hypoxia in Chesapeake Bay Tributaries: Worsening effects on Macrobenthic Community Structure in the York River SO ESTUARIES AND COASTS LA English DT Article DE Hypoxia; Benthic community; Macrobenthos; Low dissolved oxygen; Environmental stressor ID CLAM MACOMA-BALTHICA; BLUE CRABS; BEHAVIORAL-RESPONSES; SEASONAL DYNAMICS; BENTHIC COMMUNITY; EPISODIC HYPOXIA; PERIODIC HYPOXIA; FISH; ENVIRONMENT; PREDATION AB We assessed the effects of hypoxia on macrobenthic communities in the York and Rappahannock Rivers, Chesapeake Bay, in box-core samples before and after hypoxic episodes in 2003 and 2004. Hypoxia occurred in both years and was associated with a decrease in biomass and a shift in community structure toward opportunistic species in both rivers. Long-term data indicate that the frequency of hypoxia in the York has increased over the last 22 years. In previous work from similar to 20 years ago, the macrobenthic community structure did not change in response to hypoxia in the York; however, in the present study hypoxia was associated with a reduction in community biomass and a change in community structure. We conclude that currently hypoxia is a more important environmental problem in the York than in previous years. Hypoxia likely negatively affects the estuarine food web, as lower macrobenthic biomass could decrease food availability to epibenthic predators. C1 [Long, William Christopher] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Long, William Christopher; Seitz, Rochelle Diane] Coll William & Mary, Sch Marine Sci, Virginia Inst Marine Sci, Gloucester Point, VA 23062 USA. RP Long, WC (reprint author), Smithsonian Environm Res Ctr, 647 Contees Wharf Rd, Edgewater, MD 21037 USA. EM longw@si.edu RI Long, William/C-7074-2009; OI Long, William/0000-0002-7095-1245; Seitz, Rochelle/0000-0001-8044-7424 FU National Oceanographic and Atmospheric Administration; Essential Fish Habitat Program; Commonwealth of Virginia; Virginia Institute of Marine Science [2982] FX We thank K. Delano, B. Brylawski, K. Knick, K. Erickson, R. Burke, J. Falls, D. Lambert, and M. Seebo for help with the field sampling; K. Knick and B. Brylawski for help with the laboratory work; and R. Diaz, D. Wolcott, J. Long, and six anonymous reviewers for help with the revision of this manuscript. W. C. Long was funded by an Environmental Protection Agency GRO fellowship. Funding was provided by National Oceanographic and Atmospheric Administration National Sea Grant, Essential Fish Habitat Program, by the Commonwealth of Virginia, and by a grant to the Blue Crab Advanced Research Consortium from the National Oceanographic and Atmospheric Administration Chesapeake Bay Program. This is contribution 2982 from the Virginia Institute of Marine Science. NR 53 TC 13 Z9 13 U1 1 U2 11 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1559-2723 EI 1559-2731 J9 ESTUAR COAST JI Estuaries Coasts PD MAR PY 2009 VL 32 IS 2 BP 287 EP 297 DI 10.1007/s12237-009-9132-5 PG 11 WC Environmental Sciences; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 407KJ UT WOS:000263361700006 ER PT J AU Diaz-Marrero, AR Brito, I de la Rosa, JM D'Croz, L Fabelo, O Ruiz-Perez, C Darias, J Cueto, M AF Diaz-Marrero, Ana R. Brito, Inmaculada de la Rosa, Jose M. D'Croz, Luis Fabelo, Oscar Ruiz-Perez, Catalina Darias, Jose Cueto, Mercedes TI Novel Lactone Chamigrene-Derived Metabolites from Laurencia majuscula SO EUROPEAN JOURNAL OF ORGANIC CHEMISTRY LA English DT Article DE Natural products; Terpenoids; Structure elucidation; Configuration determination; Lactones; Laurencia sp. ID SESQUITERPENE; OBTUSA; CONFIGURATION AB Gomerolactones A-D along with the known majusculone, obtusol, and elatol were isolated from Laurencia majuscula, and their structures were determined spectroscopically. With the aid of Pirkle's reagent at low temperature, NMR spectroscopy was used to determine the absolute configuration at the ring closure carbon atom of a alpha-alkyhdene-gamma-lactone and an alpha-alkylidene-delta-lactone unit embedded in the chamigrene network of compounds 1 and 2, respectively. The absolute stereochemistry of compounds 3 and 4 was determined by Xray analysis. ((C) Wiley-VCH Verlag GmbH & Co. KGaA, 69451 Weinheim, Germany, 2009) C1 [Diaz-Marrero, Ana R.; Brito, Inmaculada; de la Rosa, Jose M.; Darias, Jose; Cueto, Mercedes] CSIC, Inst Prod Nat & Agrobiol, Tenerife 38206, Spain. [D'Croz, Luis] Smithsonian Trop Res Inst, Balboa, Panama. [D'Croz, Luis] Univ Panama, Estafeta Univ, Dept Biol Marina & Limnol, Panama City, Panama. [Fabelo, Oscar; Ruiz-Perez, Catalina] Univ La Laguna, Fac Fis, Dpto Fis Fundamental 2, Lab Rayos X & Mat Mol, Tenerife 38204, Spain. RP Cueto, M (reprint author), CSIC, Inst Prod Nat & Agrobiol, Avda Astrofis F Sanchez 3,Apdo 195, Tenerife 38206, Spain. EM mcueto@ipna.csic.es RI Fabelo, Oscar/F-2437-2012; Diaz-Marrero, Ana/L-2899-2014; Cueto, MERCEDES/L-3185-2014; Ruiz-Perez, Catalina/A-6299-2008 OI Diaz-Marrero, Ana/0000-0002-8886-7519; Cueto, MERCEDES/0000-0002-9112-6877; Ruiz-Perez, Catalina/0000-0002-5966-6101 FU Ministerio de Educacion y Ciencia [BIO2007-61745, SAF2006-03004]; DGUI Gobierno de Canar ias [PIO42005, PUB2005/030] FX This work was supported by the Ministerio de Educacion y Ciencia (BIO2007-61745, SAF2006-03004) and DGUI Gobierno de Canar ias (PIO42005. PUB2005/030). A. R. D.-M. acknowledges financial support from Programa Juan de la Cierva (Ministerio de Educacion v Ciencia of Spain). We are grateful to J. Afonso-Carrillo and M. Sanson (University of La Laguna) for the taxonomic classification of the alga. We gratefully acknowledge A. Corrales for her technical support. NR 20 TC 7 Z9 7 U1 1 U2 10 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA PO BOX 10 11 61, D-69451 WEINHEIM, GERMANY SN 1434-193X J9 EUR J ORG CHEM JI Eur. J. Org. Chem. PD MAR PY 2009 IS 9 BP 1407 EP 1411 DI 10.1002/ejoc.200801006 PG 5 WC Chemistry, Organic SC Chemistry GA 426BZ UT WOS:000264683800018 ER PT J AU Colwell, RK Gotelli, NJ Rahbek, C Entsminger, GL Farrell, C Graves, GR AF Colwell, Robert K. Gotelli, Nicholas J. Rahbek, Carsten Entsminger, Gary L. Farrell, Catherine Graves, Gary R. TI Peaks, plateaus, canyons, and craters: the complex geometry of simple mid-domain effect models SO EVOLUTIONARY ECOLOGY RESEARCH LA English DT Article DE biogeography; boundary effects; doughnut; geographical range; geometric constraints; null models; spatial scale; species richness gradients; stochastic models ID SPECIES RICHNESS PATTERNS; GEOGRAPHIC RANGE SIZE; LATITUDINAL GRADIENTS; NULL MODEL; ELEVATIONAL GRADIENTS; SPATIAL-PATTERNS; NEW-WORLD; DIVERSITY; CONSTRAINTS; AREA AB Background: Geographic ranges, randomly located within a bounded geographical domain, produce a central hump of species richness (the mid-domain effect, MDE). The hump arises from geometric constraints on the location of ranges, especially larger ones. Questions: (1) How do patterns of species richness in one- and two-dimensional MDE models change as a function of range size? (2) How does dispersal affect these patterns? Methods: We used a spreading dye algorithm to place assemblages of species of uniform range size in one-dimensional or two-dimensional bounded domains. In some models, we allowed dispersal to introduce range discontinuity. Results: As uniform range size increases from small to medium, a flat pattern of species richness is replaced by a pair of peripheral peaks, separated by a valley (one-dimensional models), or by a cratered ring (two-dimensional models) of species richness. With large range sizes, the peaks or rings fuse to form a central plateau (one-dimensional) or a flat-topped mound (two-dimensional) of highest species richness. Adding dispersal to the two-dimensional model weakens the peripheral ring and introduces complex patterns for long-distance dispersal. Conclusions: Heterogeneous range size distributions (whether theoretical or empirical) used in most MDE models produce species richness patterns dominated by wide-ranged species, hiding complex patterns formed by small- to medium-ranged species. These patterns, which are analogous for one and two dimensions, are complicated further by long-distance dispersal and discontinuous ranges. Although geometric constraints lead to classic mid-domain effects for large-ranged species and for mixed range-size frequency distributions, small- and medium-sized ranges of a uniform size generate more complex patterns, including peaks, plateaus, canyons, and craters of species richness. C1 [Colwell, Robert K.] Univ Connecticut, Dept Ecol & Evolutionary Biol, Storrs, CT 06269 USA. [Gotelli, Nicholas J.] Univ Vermont, Dept Biol, Burlington, VT USA. [Rahbek, Carsten] Univ Copenhagen, Ctr Macroecol & Evolut, Dept Biol, Copenhagen, Denmark. [Entsminger, Gary L.] Acquired Intelligence Inc, Montrose, CO USA. [Entsminger, Gary L.] Rocky Mt Biol Labs, Montrose, CO USA. [Farrell, Catherine] Essex High Sch, Essex Jct, VT USA. [Graves, Gary R.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA. RP Colwell, RK (reprint author), Univ Connecticut, Dept Ecol & Evolutionary Biol, Storrs, CT 06269 USA. EM colwell@uconn.edu RI Rahbek, Carsten/D-9372-2013; Rahbek, Carsten/L-1129-2013; Colwell, Robert/C-7276-2015 FU US National Science Foundation [DEB-0072702]; NSF [DEB-0107403, DEB 05-41936]; Alexander Wetmore fund of the Smithsonian Institution; Danish National Science Foundation [J. 21-03-0221] FX We dedicate this paper to Larry Slobodkin, who taught his students to think beyond the constraint of orthodoxy, while learning from the wisdom of the past. 'Classical', he liked to say, 'means old, and mostly wrong, but worth studying'. We are grateful to Hector Arita, Sean Connolly, Walter Jetz, and Thiago Rangel for their critical comments and useful suggestions. R.K.C. was supported by the US National Science Foundation, DEB-0072702. N.J.G. and G.L.E. acknowledge NSF grants DEB-0107403 and DEB 05-41936 for support of modelling and null model research. G.R.G. was supported by the Alexander Wetmore fund of the Smithsonian Institution and the Danish National Science Foundation (Grant J. 21-03-0221). C.R. acknowledges the Danish National Science Foundation (Grant J. 21-03-0221) for support of macroecological research. NR 60 TC 17 Z9 18 U1 2 U2 12 PU EVOLUTIONARY ECOLOGY LTD PI TUCSON PA UNIV ARIZONA, 321 BIOSCIENCES WEST, TUCSON, AZ 85721 USA SN 1522-0613 J9 EVOL ECOL RES JI Evol. Ecol. Res. PD MAR PY 2009 VL 11 IS 3 BP 355 EP 370 PG 16 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 457QI UT WOS:000266946800003 ER PT J AU Koechlin, L Serre, D Deba, P Pello, R Peillon, C Duchon, P de Castro, AIG Karovska, M Desert, JM Ehrenreich, D Hebrard, G Des Etangs, AL Ferlet, R Sing, D Vidal-Madjar, A AF Koechlin, Laurent Serre, Denis Deba, Paul Pello, Roser Peillon, Christelle Duchon, Paul Ines Gomez de Castro, Ana Karovska, Margarita Desert, Jean-Michel Ehrenreich, David Hebrard, Guillaume des Etangs, Alain Lecavelier Ferlet, Roger Sing, David Vidal-Madjar, Alfred TI The fresnel interferometric imager SO EXPERIMENTAL ASTRONOMY LA English DT Article DE Diffractive focussing; Formation-flying; Exoplanet detection ID PLANET HD 209458B; EXTRASOLAR PLANET; PROTOPLANETARY DISKS; 2-DIMENSIONAL DISTRIBUTIONS; INTERSTELLAR-MEDIUM; GASEOUS MOLECULES; COLUMN DENSITIES; ATMOSPHERE; UV; SPECTRUM AB The Fresnel Interferometric Imager has been proposed to the European Space Agency (ESA) Cosmic Vision plan as a class L mission. This mission addresses several themes of the CV Plan: Exoplanet study, Matter in extreme conditions, and The Universe taking shape. This paper is an abridged version of the original ESA proposal. We have removed most of the technical and financial issues, to concentrate on the instrumental design and astrophysical missions. The instrument proposed is an ultra-lightweight telescope, featuring a novel optical concept based on diffraction focussing. It yields high dynamic range images, while releasing constraints on positioning and manufacturing of the main optical elements. This concept should open the way to very large apertures in space. In this two spacecraft formation-flying instrument, one spacecraft holds the focussing element: the Fresnel interferometric array; the other spacecraft holds the field optics, focal instrumentation, and detectors. The Fresnel array proposed here is a 3.6 x3.6 m square opaque foil punched with 10(5) to 10(6) void "subapertures". Focusing is achieved with no other optical element: the shape and positioning of the subapertures (holes in the foil) is responsible for beam combining by diffraction, and 5% to 10% of the total incident light ends up into a sharp focus. The consequence of this high number of subapertures is high dynamic range images. In addition, as it uses only a combination of vacuum and opaque material, this focussing method is potentially efficient over a very broad wavelength domain. The focal length of such diffractive focussing devices is wavelength dependent. However, this can be corrected. We have tested optically the efficiency of the chromatism correction on artificial sources (500 < lambda < 750 nm): the images are diffraction limited, and the dynamic range measured on an artificial double source reaches 6.2 10 (-aEuro parts per thousand 6). We have also validated numerical simulation algorithms for larger Fresnel interferometric arrays. These simulations yield a dynamic range (rejection factor) close to 10 (-aEuro parts per thousand 8) for arrays such as the 3.6 m one we propose. A dynamic range of 10 (-aEuro parts per thousand 8) allows detection of objects at contrasts as high as than 10 (-aEuro parts per thousand 9) in most of the field. The astrophysical applications cover many objects in the IR, visible an UV domains. Examples are presented, taking advantage of the high angular resolution and dynamic range capabilities of this concept. C1 [Koechlin, Laurent; Serre, Denis; Deba, Paul; Pello, Roser; Peillon, Christelle] Univ Toulouse, Lab Astrophys Toulouse Tarbes, CNRS, F-31400 Toulouse, France. [Duchon, Paul] Ctr Natl Etud Spatiales, F-31400 Toulouse, France. [Ines Gomez de Castro, Ana] Univ Complutense Madrid, Fac CC Matemat, E-28040 Madrid, Spain. [Karovska, Margarita] Harvard Smithsonian Ctr Astrophys CfA, Cambridge, MA 02138 USA. [Desert, Jean-Michel; Ehrenreich, David; Hebrard, Guillaume; des Etangs, Alain Lecavelier; Ferlet, Roger; Sing, David; Vidal-Madjar, Alfred] Univ Paris 06, CNRS, F-75014 Paris, France. RP Koechlin, L (reprint author), Univ Toulouse, Lab Astrophys Toulouse Tarbes, CNRS, F-31400 Toulouse, France. EM laurent.koechlin@ast.obs-mip.fr RI Pello, Roser/G-4754-2010; OI Ehrenreich, David/0000-0001-9704-5405; Sing, David /0000-0001-6050-7645 NR 39 TC 11 Z9 11 U1 0 U2 4 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0922-6435 J9 EXP ASTRON JI Exp. Astron. PD MAR PY 2009 VL 23 IS 1 BP 379 EP 402 DI 10.1007/s10686-008-9112-y PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 409KZ UT WOS:000263505900017 ER PT J AU Cockell, CS Herbst, T Leger, A Absil, O Beichman, C Benz, W Brack, A Chazelas, B Chelli, A Cottin, H du Foresto, V Danchi, W Defrere, D Den Herder, JW Eiroa, C Fridlund, M Henning, T Johnston, K Kaltenegger, L Labadie, L Lammer, H Launhardt, R Lawson, P Lay, OP Liseau, R Martin, SR Mawet, D Mourard, D Moutou, C Mugnier, L Paresce, F Quirrenbach, A Rabbia, Y Rottgering, HJA Rouan, D Santos, N Selsis, F Serabyn, E Westall, F White, G Ollivier, M Borde, P AF Cockell, Charles S. Herbst, Tom Leger, Alain Absil, O. Beichman, Charles Benz, Willy Brack, Andre Chazelas, Bruno Chelli, Alain Cottin, Herve du Foresto, Vincent Coude Danchi, William Defrere, Denis den Herder, Jan-Willem Eiroa, Carlos Fridlund, Malcolm Henning, Thomas Johnston, Kenneth Kaltenegger, Lisa Labadie, Lucas Lammer, Helmut Launhardt, Ralf Lawson, Peter Lay, Oliver P. Liseau, Rene' Martin, Stefan R. Mawet, Dimitri Mourard, Denis Moutou, Claire Mugnier, Laurent Paresce, Francesco Quirrenbach, Andreas Rabbia, Yves Rottgering, Huub J. A. Rouan, Daniel Santos, Nuno Selsis, Franck Serabyn, Eugene Westall, Frances White, Glenn Ollivier, Marc Borde, Pascale TI Darwin-an experimental astronomy mission to search for extrasolar planets SO EXPERIMENTAL ASTRONOMY LA English DT Article DE Interferometer; Nulling interferometry; Direct imaging of exoplanets; Exoplanets; Habitable zone ID NULLING INTERFEROMETERS; SYSTEMATIC-ERRORS AB As a response to ESA call for mission concepts for its Cosmic Vision 2015-2025 plan, we propose a mission called Darwin. Its primary goal is the study of terrestrial extrasolar planets and the search for life on them. In this paper, we describe different characteristics of the instrument. C1 [Cockell, Charles S.] Open Univ, Planetary & Space Sci Res Inst, Milton Keynes MK7 6AA, Bucks, England. [Herbst, Tom; Henning, Thomas; Labadie, Lucas; Launhardt, Ralf] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Leger, Alain; Chazelas, Bruno; Ollivier, Marc; Borde, Pascale] Univ Paris 11, IAS, F-91405 Orsay, France. [Absil, O.] Lab Astrophys Observ Grenoble, F-38400 St Martin Dheres, France. [Beichman, Charles] CALTECH, Michelson Sci Ctr, Pasadena, CA 91125 USA. [Benz, Willy] Univ Bern, Inst Phys, Bern, Switzerland. [Brack, Andre; Westall, Frances] CNRS, Ctr Biophys Mol, F-45071 Orleans 2, France. [Chelli, Alain] Lab Astrophys Grenoble LAOG, F-38041 Grenoble 9, France. [Cottin, Herve] Univ Paris 12, CNRS, UMR 7583 91, Lab Interuniv Syst Atmospher, F-94010 Creteil, France. [du Foresto, Vincent Coude; Rouan, Daniel] Observ Paris, PHASE, LESIA, F-92190 Meudon, France. [Danchi, William] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Defrere, Denis] Inst Astrophys & Geophys Liege, F-4000 Liege, Belgium. [den Herder, Jan-Willem] SRON Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands. [Eiroa, Carlos] Univ Autonoma Madrid, Fac Ciencias, Dpto Fis Toer CXI, E-28049 Madrid, Spain. [Fridlund, Malcolm] Estec, European Space Agcy, Astrophys Mission Div, NL-2200 AG Noordwijk, Netherlands. [Johnston, Kenneth] USN Observ, Washington, DC 20392 USA. [Kaltenegger, Lisa] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lammer, Helmut] Austrian Acad Sci, Space Res Inst, A-8042 Graz, Austria. [Lawson, Peter; Lay, Oliver P.; Martin, Stefan R.; Mawet, Dimitri; Serabyn, Eugene] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Liseau, Rene'] Chalmers, Onsala Space Observ, SE-43992 Onsala, Sweden. [Rabbia, Yves] CNRS, Dpt GEMINI, UMR 6203, Observ Cote Azur, F-06130 Grasse, France. [Moutou, Claire] CNRS, LAM, F-13376 Marseille 12, France. [Mugnier, Laurent] DOTA, ONERA, F-92322 Chatillon, France. [Paresce, Francesco] INAF, IASF Bologna, Bologna, Italy. [Quirrenbach, Andreas] Univ Heidelberg, ZAH, D-69117 Heidelberg, Germany. [Rottgering, Huub J. A.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Santos, Nuno] Univ Porto, Ctr Astrofis, P-4150762 Oporto, Portugal. [Selsis, Franck] Univ Lyon, Ecole Super Lyon, CNRS, CRAL,UMR 5574, F-69007 Lyon, France. [White, Glenn] Open Univ, Dept Phys & Astron, Milton Keynes MK7 6AA, Bucks, England. [White, Glenn] Rutherford Appleton Lab, CCLRC, Space Sci & Technol Dept, Didcot OX11 0QX, Oxon, England. RP Cockell, CS (reprint author), Open Univ, Planetary & Space Sci Res Inst, Milton Keynes MK7 6AA, Bucks, England. EM c.s.cockell@open.ac.uk RI Santos, Nuno/E-9957-2011; Mugnier, Laurent/A-7630-2012; Cottin, Herve/H-5654-2013; OI Santos, Nuno/0000-0003-4422-2919; Cottin, Herve/0000-0001-9170-5265; Mugnier, Laurent/0000-0002-8364-4957; Absil, Olivier/0000-0002-4006-6237 NR 16 TC 29 Z9 29 U1 0 U2 8 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0922-6435 J9 EXP ASTRON JI Exp. Astron. PD MAR PY 2009 VL 23 IS 1 BP 435 EP 461 DI 10.1007/s10686-008-9121-x PG 27 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 409KZ UT WOS:000263505900019 ER PT J AU Holguin, CM Pena, JE Henry, TJ Acevedo, F AF Holguin, C. M. Pena, J. E. Henry, T. J. Acevedo, F. TI BIOLOGY OF STETHOCONUS PRAEFECTUS (DISTANT) (HETEROPTERA: MIRIDAE), A NEWLY ESTABLISHED PREDATOR OF THE AVOCADO LACE BUG, PSEUDACYSTA PERSEAE (HETEROPTERA: TINGIDAE), IN FLORIDA SO FLORIDA ENTOMOLOGIST LA English DT Article ID JAPONICUS HETEROPTERA; HEMIPTERA AB The Asian plant bug Stethoconus praefectus (Distant) (Heteroptera: Miridae) was recently discovered in Florida preying on the avocado lace bug, Pseudacysta perseae (Heidemann) (Heteroptera: Tingidae). Its life cycle and effectiveness as a predator of R perseae were investigated at 26 +/- 1 degrees C, 60 +/- 5 RH, and 12: 12 (L: D) under laboratory conditions. Stethoconus praefectus developed from egg to adult in 16.5 +/- 0.2 d. On average, the first 4 instars consumed 2 to 4 prey per day, whereas the last 2 instars consumed 2 to 7 lace bugs per day. Stethoconus praefectus was observed in the field from Aug through Dec 2007. C1 [Holguin, C. M.; Pena, J. E.; Acevedo, F.] Univ Florida, Dept Entomol & Nematol, Trop Res & Educ Ctr, Homestead, FL 33031 USA. [Henry, T. J.] ARS, Systemat Entomol Lab, USDA, Natl Museum Nat Hist,Smithsonian Inst,MRC 168, Washington, DC 20013 USA. RP Holguin, CM (reprint author), Univ Florida, Dept Entomol & Nematol, Trop Res & Educ Ctr, 18905 SW 280th St, Homestead, FL 33031 USA. EM jepena@ufl.edu; thenry@ars.usda.gov FU California Department of Agriculture FX We thank Nancy Epsky (USDA, ARS, Miami), Josep Jacas (Univerisa Jaume I, Castell, Spain), Michael G. Pogue (Systematic Entomology Laboratory [SEL], USDA, ARS, Washington, DC), F. Christian Thompson (SEL), and Alfred G. Wheeler, Jr. (Clemson University, Clemson, SC) for critically reviewing this manuscript, and David Long (University of Florida, Homestead) for help with fieldwork and laboratory rearing. This research was partially supported by a grant from the California Department of Agriculture to JER. NR 15 TC 3 Z9 3 U1 0 U2 4 PU FLORIDA ENTOMOLOGICAL SOC PI LUTZ PA 16125 E LAKE BURRELL DR, LUTZ, FL 33548 USA SN 0015-4040 J9 FLA ENTOMOL JI Fla. Entomol. PD MAR PY 2009 VL 92 IS 1 BP 54 EP 57 DI 10.1653/024.092.0109 PG 4 WC Entomology SC Entomology GA 418PZ UT WOS:000264161900009 ER PT J AU Kula, RR AF Kula, Robert R. TI A NEW SPECIES OF CHAENUSA (HYMENOPTERA: BRACONIDAE) REARED FROM HYDRELLIA PAKISTANAE AND HYDRELLIA SARAHAE LATICAPSULA (DIPTERA: EPHYDRIDAE) INFESTING HYDRILLA VERTICILLATA (ALISMATALES: HYDROCHARITACEAE) IN INDIA AND PAKISTAN SO FLORIDA ENTOMOLOGIST LA English DT Article DE Alysiinae; biological control; Dacnusini; Oriental Region; parasitoid ID BIOLOGICAL-CONTROL AGENT; HOST-RANGE; DISTRIBUTION RECORDS; ALYSIINAE; IMPACT AB Chaenusa glabra Kula, new species from India and Pakistan is described, and sexual dimorphism is reported and discussed. A diagnosis is provided to differentiate it from all other species of Chaenusa Haliday sensu lato. It was reared from Hydrellia pakistanae Deonier and Hydrellia sarahae laticapsula Deonier infesting Hydrilla verticillata (L. f.) Royale during foreign exploration for natural enemies of H. verticillata, and is in quarantine at the Florida Biological Control Laboratory in Gainesville. It is the first species of Chaenusa described from the Oriental Region and the only species of Chaenusa known to attack species of Hydrellia Robineau-Desvoidy infesting plants from a genus other than Potamogeton L. C1 ARS, Systemat Entomol Lab, Inst Plant Sci, USDA,Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20013 USA. RP Kula, RR (reprint author), ARS, Systemat Entomol Lab, Inst Plant Sci, USDA,Natl Museum Nat Hist,Smithsonian Inst, POB 37012,MRC 168, Washington, DC 20013 USA. NR 31 TC 7 Z9 7 U1 0 U2 1 PU FLORIDA ENTOMOLOGICAL SOC PI LUTZ PA 16125 E LAKE BURRELL DR, LUTZ, FL 33548 USA SN 0015-4040 J9 FLA ENTOMOL JI Fla. Entomol. PD MAR PY 2009 VL 92 IS 1 BP 139 EP 146 DI 10.1653/024.092.0121 PG 8 WC Entomology SC Entomology GA 418PZ UT WOS:000264161900021 ER PT J AU Dimichele, WA Montanez, IP Poulsen, CJ Tabor, NJ AF Dimichele, W. A. Montanez, I. P. Poulsen, C. J. Tabor, N. J. TI Climate and vegetational regime shifts in the late Paleozoic ice age earth SO GEOBIOLOGY LA English DT Review ID MULTIPLE STABLE STATES; CENTRAL APPALACHIAN BASIN; ROCKY INTERTIDAL SHORES; COAL-SWAMP VEGETATION; SOUTH WALES COALFIELD; ILLINOIS BASIN; ATMOSPHERIC CIRCULATION; ARBORESCENT LYCOPSIDS; PALEOCLIMATE CONTROLS; ECOLOGICAL SURPRISES AB The late Paleozoic earth experienced alternation between glacial and non-glacial climates at multiple temporal scales, accompanied by atmospheric CO2 fluctuations and global warming intervals, often attended by significant vegetational changes in equatorial latitudes of Pangaea. We assess the nature of climate-vegetation interaction during two time intervals: middle-late Pennsylvanian transition and Pennsylvanian-Permian transition, each marked by tropical warming and drying. In case study 1, there is a catastrophic intra-biomic reorganization of dominance and diversity in wetland, evergreen vegetation growing under humid climates. This represents a threshold-type change, possibly a regime shift to an alternative stable state. Case study 2 is an inter-biome dominance change in western and central Pangaea from humid wetland and seasonally dry to semi-arid vegetation. Shifts between these vegetation types had been occurring in Euramerican portions of the equatorial region throughout the late middle and late Pennsylvanian, the drier vegetation reaching persistent dominance by Early Permian. The oscillatory transition between humid and seasonally dry vegetation appears to demonstrate a threshold-like behavior but probably not repeated transitions between alternative stable states. Rather, changes in dominance in lowland equatorial regions were driven by long-term, repetitive climatic oscillations, occurring with increasing intensity, within overall shift to seasonal dryness through time. In neither case study are there clear biotic or abiotic warning signs of looming changes in vegetational composition or geographic distribution, nor is it clear that there are specific, absolute values or rates of environmental change in temperature, rainfall distribution and amount, or atmospheric composition, approach to which might indicate proximity to a terrestrial biotic-change threshold. C1 [Dimichele, W. A.] Smithsonian Inst, Washington, DC 20560 USA. [Montanez, I. P.] Univ Calif Davis, Dept Geol, Davis, CA 95616 USA. [Poulsen, C. J.] Univ Michigan, Dept Geol Sci, Ann Arbor, MI 48109 USA. [Tabor, N. J.] So Methodist Univ, Huffington Dept Earth Sci, Dallas, TX 75275 USA. RP Dimichele, WA (reprint author), Smithsonian Inst, Natl Museum Nat Hist MRC-121, Washington, DC 20560 USA. EM dimichel@si.edu RI DiMichele, William/K-4301-2012; Poulsen, Christopher/C-6213-2009 OI Poulsen, Christopher/0000-0001-5104-4271 NR 202 TC 79 Z9 79 U1 8 U2 32 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1472-4677 EI 1472-4669 J9 GEOBIOLOGY JI Geobiology PD MAR PY 2009 VL 7 IS 2 BP 200 EP 226 DI 10.1111/j.1472-4669.2009.00192.x PG 27 WC Biology; Environmental Sciences; Geosciences, Multidisciplinary SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Geology GA 425KQ UT WOS:000264635800008 PM 19320746 ER PT J AU Logan, MAV Wise, MA AF Logan, M. Amelia V. Wise, Michael A. TI Characterisation of Two New Reference Materials: STL-1, the Stewart Lepidolite and ZA-1, the Zapot Amazonite SO GEOSTANDARDS AND GEOANALYTICAL RESEARCH LA English DT Article DE XRF; reference materials; pegmatite; rubidium; cesium; gallium; thalium AB The analysis of granitic pegmatites still remains a challenge because suitable natural reference materials are scarce or not available. Two new reference materials were prepared at the Smithsonian Institution, to provide an avenue to pursue the geochemical analysis of micas and feldspars in granitic pegmatites: STL-1, the Stewart lepidolite (NMNH 174041) and ZA-1, the Zapot amazonite (NMNH 174042). STL-1 was prepared from lepidolite collected from the lithium-rich Stewart pegmatite, San Diego County, California (33 degrees 22'52''N, 117 degrees 03'41''W). ZA-1 was prepared from an amazonite from the topaz-bearing Zapot pegmatite, Mineral County, Nevada, (38 degrees 41'N, 118 degrees 33'W). The results of this study indicated that STL-1 and ZA-1 are homogeneous and could be used as reference materials that would allow the expansion of calibration curves in XRF analysis up to 16000 mu g g(-1) for Rb, 2000 mu g g(-1) for Cs and 100 mu g g(-1) for Tl. STL-1 and ZA-1 also contain unusually high concentrations of Ga and Tl, and STL-1 of Nb. C1 [Logan, M. Amelia V.; Wise, Michael A.] Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. RP Logan, MAV (reprint author), Smithsonian Inst, Dept Mineral Sci, NHB 119, Washington, DC 20560 USA. EM logana@si.edu NR 14 TC 3 Z9 3 U1 3 U2 10 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1639-4488 J9 GEOSTAND GEOANAL RES JI Geostand. Geoanal. Res. PD MAR PY 2009 VL 33 IS 1 BP 85 EP 93 DI 10.1111/j.1751-908X.2009.00855.x PG 9 WC Geosciences, Multidisciplinary SC Geology GA 409QH UT WOS:000263520400007 ER PT J AU Sengco, MR AF Sengco, Mario R. TI Prevention and control of Karenia brevis blooms SO HARMFUL ALGAE LA English DT Article; Proceedings Paper CT Scientific Workshop on State of the Research on Red Tide in the Gulf of Mexico CY JUL 17-20, 2006 CL Sarasota, FL SP Mote Marine Lab, Natl Oceanic & Atmospher Adm, Florida Fish & Wildlife Conservat Commiss Fish, Wildlife Res Inst DE Karenia brevis; Prevention; Control; Clav; Flocculation; Copper sulfate ID HARMFUL ALGAL BLOOMS; PRYMNESIUM-PARVUM HAPTOPHYCEAE; GYMNODINIUM-BREVE; CLAY FLOCCULATION; RED-TIDE; OZONE INACTIVATION; REMOVAL; SEAWATER; TOXINS; CELLS AB With the recurrent and potentially severe impacts of Karenia brevis blooms in the Gulf of Mexico, new management approaches have been examined to potentially prevent and control these blooms. This paper summarizes past and present research and strategies for the prevention and control of K. brevis blooms. Prevention presumes a certain level of understanding about the cause or causes of these blooms. This may not yet be available, however, for K. brevis in the Gulf of Mexico. Some efforts to synthesize the current understanding of bloom dynamics for the region were recommended. The earliest attempts to control K. brevis blooms in the field used copper sulfate minerals seeded from ships and crop-dusting planes. Although effective for short term applications, the method was abandoned as it provided only temporary relief at a high cost with unknown collateral damage to the ecosystem. Results from chemical screenings and ozone treatments were also presented. Algicidal bacteria have shown some promise in controlling K. brevis in laboratory experiments, either through direct contact or release of algicidal compounds. Finally, the state of the research into the use of natural clays was presented, beginning with laboratory and mesocosm tests, to larger-scale experiments and flume studies. Several impacts studies were reviewed. While much progress has been made in examining control methods in recent years, more research in the field is needed to fully evaluate the efficacy and impacts of these strategies. Furthermore, the social and human dimensions of this potentially controversial area of research may have to be explored more fully to gauge the receptiveness of the public to these management approaches. Published by Elsevier B.V. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21012 USA. RP Sengco, MR (reprint author), Smithsonian Environm Res Ctr, POB 28,647 Contees Wharf Rd, Edgewater, MD 21012 USA. EM sengcom@si.edu NR 40 TC 24 Z9 25 U1 4 U2 26 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 1568-9883 J9 HARMFUL ALGAE JI Harmful Algae PD MAR PY 2009 VL 8 IS 4 SI SI BP 623 EP 628 DI 10.1016/j.hal.2008.11.005 PG 6 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 425QG UT WOS:000264651600010 ER PT J AU Collins, M AF Collins, Martin TI A note from the new editor SO HISTORY AND TECHNOLOGY LA English DT Editorial Material C1 Smithsonian Inst, Washington, DC 20560 USA. RP Collins, M (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 1 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 J9 HIST TECHNOL JI Hist. Technol. PD MAR PY 2009 VL 25 IS 1 BP 1 EP 2 DI 10.1080/07341510902738559 PG 2 WC History SC History GA 453EG UT WOS:000266592400001 ER PT J AU Burr, DM Enga, MT Williams, RME Zimbelman, JR Howard, AD Brennand, TA AF Burr, Devon M. Enga, Marie-Therese Williams, Rebecca M. E. Zimbelman, James R. Howard, Alan D. Brennand, Tracy A. TI Pervasive aqueous paleoflow features in the Aeolis/Zephyria Plana region, Mars SO ICARUS LA English DT Article DE Mars, surface; Mars, climate; Geological processes ID MEDUSAE FOSSAE FORMATION; ORBITER LASER ALTIMETER; GLOBAL SURVEYOR; CHRONOLOGY; MELTWATER; PLANITIA; ESKERS; CANADA; CRATER; FLOW AB A survey of THEMIS visible wavelength images in the Aeolis/Zephyria Plana region over the two western lobes of the equatorial Medusae Fossae Formation (MFF) shows similar to 150 sinuous ridges having a variety of morphologies and contexts. To systematize investigation, we use a classification scheme including both individual ridge and ridge network types, as well as associations with impact craters and fan-shaped features. The morphology of the ridges, their location downslope from higher topography (e.g., crater rims and scarps), and their association with fan-shaped forms indicate that most sinuous ridges formed through overland aqueous flow. Analysis of observations by individual ridge type leads to interpretation of most of these sinuous ridges as inverted fluvial channels or floodplains and a few as possible eskers, with the origin of the remaining ridges under continuing investigation. About 15% of the sinuous ridges are associated with impact craters, but data analysis does not support a genetic relationship between the craters and the sinuous ridges. Instead, analysis of one sinuous ridge network associated with a crater indicates that the water source for the network was atmospheric in origin, namely, precipitation runoff. The broad areal distribution of these similar to 150 ridges and the network morphologies, in particular the branched and subparallel types, suggest that an atmospheric water source is generally applicable to the population of sinuous ridges as a whole. This concentration of sinuous ridges is the largest single population of such landforms on Mars and among the youngest. These ridges are situated at a paleoscarp between Cerberus Palus and the Aeolis highlands, suggesting that the precipitation that formed them was orographic in origin. The ages of the equatorial MFF units in which this population of sinuous ridges is found imply that this orographic rain and/or snow fell during some period from the late Hesperian through the middle Amazonian. (C) 2008 Elsevier Inc. All rights reserved. C1 [Burr, Devon M.] Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA. [Burr, Devon M.] SETI Inst, Carl Sagan Ctr Study Life Universe, Mountain View, CA 94043 USA. [Enga, Marie-Therese] No Arizona Univ, Dept Phys & Astron, Flagstaff, AZ 86011 USA. [Williams, Rebecca M. E.] Inst Plant Sci, Tucson, AZ 85719 USA. [Zimbelman, James R.] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Sci, Washington, DC 20013 USA. [Howard, Alan D.] Univ Virginia, Dept Environm Sci, Charlottesville, VA 22904 USA. [Brennand, Tracy A.] Simon Fraser Univ, Dept Geog, Burnaby, BC V5A 1S6, Canada. RP Burr, DM (reprint author), Univ Tennessee, Dept Earth & Planetary Sci, 306 EPS Bldg,1412 Circle Dr, Knoxville, TN 37996 USA. EM dburr1@utk.edu OI Howard, Alan/0000-0002-5423-1600 FU NASA Mars Data Analysis Program [NNX07AV32G]; Natural Science and Engineering Research Council (NSERC ); National Science Foundation [AST-0552751] FX We acknowledge support by the NASA Mars Data Analysis Program (grant NNX07AV32G) and the Natural Science and Engineering Research Council (NSERC discovery grant to T.A.B.). M.T.E. was supported by a Research Experience to Undergraduates grant from the National Science Foundation to the SETI Institute (grant AST-0552751). Reviews by Jeff Moore and Phil Christensen helped us to improve this manuscript. NR 94 TC 39 Z9 39 U1 1 U2 4 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD MAR PY 2009 VL 200 IS 1 BP 52 EP 76 DI 10.1016/j.icarus.2008.10.014 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 419IN UT WOS:000264213000006 ER PT J AU Song, JK Popper, AN AF Song, Jiakun Popper, Arthur N. TI New perspectives in fish evolution and neurobiology SO INTEGRATIVE ZOOLOGY LA English DT Editorial Material C1 [Song, Jiakun] Shanghai Ocean Univ, Inst Marine Biosyst & Neurosci, Shanghai, Peoples R China. [Song, Jiakun; Popper, Arthur N.] Univ Maryland, Dept Biol, College Pk, MD 20742 USA. [Song, Jiakun] Smithsonian Inst, Natl Museum Nat Hist, Div Fishes, Washington, DC 20560 USA. [Popper, Arthur N.] Univ Maryland, Ctr Comparat & Evolutionary Biol Hearing, College Pk, MD 20742 USA. RP Song, JK (reprint author), Shanghai Ocean Univ, Inst Marine Biosyst & Neurosci, Shanghai, Peoples R China. NR 13 TC 0 Z9 0 U1 1 U2 5 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1749-4877 J9 INTEGR ZOOL JI Integr. Zool. PD MAR PY 2009 VL 4 IS 1 BP 1 EP 2 DI 10.1111/j.1749-4877.2009.00128.x PG 2 WC Zoology SC Zoology GA 581TM UT WOS:000276547500001 PM 21392271 ER PT J AU Forman, P AF Forman, Paul TI Uncertainty: Einstein, Heisenberg, Bohr, and the Struggle for the Soul of Science SO ISIS LA English DT Book Review C1 [Forman, Paul] Smithsonian Inst Natl Museum Amer Hist, Washington, DC USA. RP Forman, P (reprint author), Smithsonian Inst Natl Museum Amer Hist, Washington, DC USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0021-1753 J9 ISIS JI Isis PD MAR PY 2009 VL 100 IS 1 BP 180 EP 181 PG 3 WC History & Philosophy Of Science SC History & Philosophy of Science GA 448LP UT WOS:000266264400063 ER PT J AU Neufeld, MJ AF Neufeld, Michael J. TI Red Prometheus: Engineering and Dictatorship in East Germany, 1945-1990 SO ISIS LA English DT Book Review C1 [Neufeld, Michael J.] Smithsonian Inst, Natl Air & Space Museum, Space Hist Div, Washington, DC 20560 USA. RP Neufeld, MJ (reprint author), Smithsonian Inst, Natl Air & Space Museum, Space Hist Div, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0021-1753 J9 ISIS JI Isis PD MAR PY 2009 VL 100 IS 1 BP 194 EP 195 PG 3 WC History & Philosophy Of Science SC History & Philosophy of Science GA 448LP UT WOS:000266264400074 ER PT J AU Ceruzzi, PE AF Ceruzzi, Paul E. TI The Internet Imaginaire SO ISIS LA English DT Book Review C1 [Ceruzzi, Paul E.] Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA. RP Ceruzzi, PE (reprint author), Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0021-1753 J9 ISIS JI Isis PD MAR PY 2009 VL 100 IS 1 BP 197 EP 197 PG 1 WC History & Philosophy Of Science SC History & Philosophy of Science GA 448LP UT WOS:000266264400076 ER PT J AU Launius, RD AF Launius, Roger D. TI Keep Watching the Skies! The Story of Operation Moonwatch and the Dawn of the Space Age SO JOURNAL OF AMERICAN HISTORY LA English DT Book Review C1 [Launius, Roger D.] Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA. RP Launius, RD (reprint author), Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU ORGANIZATION AMER HISTORIANS PI BLOOMINGTON PA 112 N BRYAN ST, BLOOMINGTON, IN 47408 USA SN 0021-8723 J9 J AM HIST JI J. Am. Hist. PD MAR PY 2009 VL 95 IS 4 BP 1233 EP 1234 PG 2 WC History SC History GA 419JQ UT WOS:000264216000140 ER PT J AU Kiso, W Schmitt, D Brown, J Pukazhenthi, B AF Kiso, Wendy Schmitt, Dennis Brown, Janine Pukazhenthi, Budhan TI EJACULATE TRAITS AND SEMINAL PLASMA CHEMISTRY OF GOOD VERSUS POOR QUALITY EJACULATES IN ASIAN ELEPHANTS (ELEPHAS MAXIMUS) SO JOURNAL OF ANDROLOGY LA English DT Meeting Abstract CT 34th Annual Meeting of the American-Society-of-Andrology CY APR 04-07, 2009 CL Philadelphia, PA SP Amer Soc Androl C1 [Kiso, Wendy; Brown, Janine; Pukazhenthi, Budhan] Smithsonian Natl Zool Pk, Front Royal, VA 65804 USA. [Schmitt, Dennis] Missouri State Univ, Springfield, MO USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER SOC ANDROLOGY, INC PI LAWRENCE PA C/O ALLEN PRESS, INC PO BOX 368, LAWRENCE, KS 66044 USA SN 0196-3635 J9 J ANDROL JI J. Androl. PD MAR-APR PY 2009 MA 30 BP 43 EP 43 PG 1 WC Andrology SC Endocrinology & Metabolism GA 414FQ UT WOS:000263849700031 ER PT J AU Pukazhenthi, B Comizzoli, P Padilla, L Songsasen, N Favorretto, S Wildt, D AF Pukazhenthi, Budhan Comizzoli, Pierre Padilla, Luis Songsasen, Nucharin Favorretto, Samantha Wildt, David TI THE RARE ADDRA GAZELLE (GAZELLA DAMA RUFICOLLIS) PRODUCES VIABLE SPERMIC EJACULATES THAT TOLERATE CRYOPRESERVATION SO JOURNAL OF ANDROLOGY LA English DT Meeting Abstract CT 34th Annual Meeting of the American-Society-of-Andrology CY APR 04-07, 2009 CL Philadelphia, PA SP Amer Soc Androl C1 [Pukazhenthi, Budhan; Padilla, Luis; Songsasen, Nucharin; Favorretto, Samantha; Wildt, David] Smithsonian Natl Zool Pk, Front Royal, VA USA. [Comizzoli, Pierre] Smithsonian Natl Zool Pk, Washington, DC USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER SOC ANDROLOGY, INC PI LAWRENCE PA C/O ALLEN PRESS, INC PO BOX 368, LAWRENCE, KS 66044 USA SN 0196-3635 J9 J ANDROL JI J. Androl. PD MAR-APR PY 2009 MA 47 BP 48 EP 48 PG 1 WC Andrology SC Endocrinology & Metabolism GA 414FQ UT WOS:000263849700048 ER PT J AU Zeder, MA AF Zeder, Melinda A. TI The Neolithic Macro-(R)evolution: Macroevolutionary Theory and the Study of Culture Change SO JOURNAL OF ARCHAEOLOGICAL RESEARCH LA English DT Review DE Macroevolution; Evolutionary archaeology; Neolithic; Near East ID BARLEY HORDEUM-VULGARE; GOATS CAPRA-HIRCUS; NEAR-EAST; EVOLUTIONARY ARCHAEOLOGY; PUNCTUATED EQUILIBRIUM; INITIAL DOMESTICATION; WHEAT DOMESTICATION; PIG DOMESTICATION; SOUTHERN LEVANT; FOOD PLANTS AB The macroevolutionary approach in archaeology represents the most recent example in a long tradition of applying principles of biological evolution to the study of culture change. Archaeologists working within this paradigm see macroevolutionary theory as an effective response to the shortcomings of neo-Darwinian biological evolution for studying cultural evolution. Rather than operating at the level of individual traits, macroevolutionary archaeologists emphasize the role of hierarchical processes in culture change. While neo-Darwinian archaeologists disavow any element of human intent in culture change, to macroevolutionary archaeologists human agency is a key component of cultural evolution that allows cultures to respond to pressures more quickly and with greater degree of flexibility and directedness than found in biological evolution. Major culture change, when it happens, is likely to be rapid, even revolutionary, with periods of rapid change separated by periods of relative stasis of actively maintained stability. The emergence of Neolithic cultures has long been recognized as one of two periods of major revolutionary culture change in human prehistory. Here I examine the record for the Near East, tracing the empirical record for the origin of agriculture in this region, as well as other demographic, social, and ideological components of Neolithic emergence. While the empirical record from the Near East subscribes in a general way to basic principles of macroevolutionary theory, cultural evolution cannot be understood through appeal to principles of biological evolution alone, whether based in macroevolutionary theory or neo-Darwinianism. Instead, the key role of human agency in culture change distinguishes cultural evolution from biological evolution and requires a more pluralistic and less doctrinaire appeal to multiple models of change based in both the biological and social sciences. C1 Smithsonian Inst, Natl Museum Nat Hist, Archaeobiol Program, Washington, DC 20013 USA. RP Zeder, MA (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Archaeobiol Program, MRC 112,POB 37012, Washington, DC 20013 USA. EM zederm@si.edu NR 358 TC 47 Z9 47 U1 5 U2 39 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1059-0161 J9 J ARCHAEOL RES JI J. Archaeol. Res. PD MAR PY 2009 VL 17 IS 1 BP 1 EP 63 DI 10.1007/s10814-008-9025-3 PG 63 WC Anthropology; Archaeology SC Anthropology; Archaeology GA 389WH UT WOS:000262124700001 ER PT J AU Tryon, CA Logan, MAV Mouralis, D Kuhn, S Slimak, L Balkan-Atli, N AF Tryon, Christian A. Logan, M. Amelia V. Mouralis, Damase Kuhn, Steve Slimak, Ludovic Balkan-Atli, Nur TI Building a tephrostratigraphic framework for the Paleolithic of Central Anatolia, Turkey SO JOURNAL OF ARCHAEOLOGICAL SCIENCE LA English DT Article DE Tephra correlation; Middle Paleolithic; Lower Paleolithic; Kaletepe Deresi 3 ID STRATOVOLCANO CENTRAL ANATOLIA; TEPHRA DEPOSITS; TURKANA-BASIN; KALETEPE-DERESI-3 TURKEY; NUMERICAL CONSIDERATIONS; GEOCHEMICAL ANALYSIS; DISTAL MICROTEPHRA; QUATERNARY TEPHRAS; VOLCANIC-ROCKS; GLASS SHARDS AB The Central Anatolian Volcanic Province (CAVP) in Turkey preserves widespread deposits of Quaternary tephra, presently associated with a small but growing number of Paleolithic archaeological sites. We use multivariate analyses of the abundances of a Suite of nine major and minor element oxides determined by electron probe microanalysis. From these data, we construct a classificatory model for correlating distal tephra to one of five volcanic edifices or eruptive phases within the CAVP. Application of this model to distal deposits Of primary tephra-fall and reworked tuffaceous sediments from the archaeological sites of Korkuyu and Kaletepe Deresi 3 indicates Late to possibly Early Pleistocene ages for the artifact assemblages there, and provides a fundamental tephrostratigraphic framework to examine spatial and temporal variation in hominin behavior comparable to that of other regions, such as eastern Africa. (C) 2008 Elsevier Ltd. All rights reserved. C1 [Tryon, Christian A.] NYU, Dept Anthropol, New York, NY 10003 USA. [Tryon, Christian A.] Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Human Origins Program, Washington, DC 20560 USA. [Logan, M. Amelia V.] Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. [Mouralis, Damase] Univ Rouen, Dept Geog, F-76821 Mont St Aignan, France. [Mouralis, Damase] CNRS, UMR 6266, F-76821 Mont St Aignan, France. [Kuhn, Steve] Univ Arizona, Dept Anthropol, Tucson, AZ 85721 USA. [Slimak, Ludovic] Univ Toulouse Le Mirail, TRACES, CNRS, UMR 5608, Toulouse, France. [Balkan-Atli, Nur] Istanbul Univ, Fac Letters, Prehist Sect, TR-34134 Istanbul, Turkey. RP Tryon, CA (reprint author), NYU, Dept Anthropol, 25 Waverly Pl, New York, NY 10003 USA. EM christian.tryon@nyu.edu; logana@si.edu; damase.mouralis@univ-rouen.fr; skuhn@email.arizona.edu; slimakl@yahoo.fr; nbalkan@istanbul.edu.tr RI Tryon, Christian/B-1172-2010; OI Tryon, Christian/0000-0002-2354-3273 FU L.S.B. Leakey Foundation; Research Fund of Istanbul University [533/05052006]; French Ministry of Foreign Affairs FX We thank the Department of Cultural Assets and Museums, Ministry of Tourism and Culture of Turkey for permission to conduct research at Kaletepe, and Would like to particularly acknowledge the assistance and encouragement provided by Dr. Fazil Acikgoz, director of the Nigde Museum. Financial support was provided by grants from the L.S.B. Leakey Foundation to Kuhn and from the Research Fund of Istanbul University (project number 533/05052006) and the French Ministry of Foreign Affairs (la mission de Prehistoire Anatolienne) to Balkan-Atl1. Two anonymous readers provided thorough and very valuable reviews that resulted in a substantially improved manuscript. Finally, support and assistance from Rick Potts, Matt Tocheri, and Rhonda Kauffman are greatly appreciated. NR 75 TC 14 Z9 14 U1 0 U2 5 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0305-4403 EI 1095-9238 J9 J ARCHAEOL SCI JI J. Archaeol. Sci. PD MAR PY 2009 VL 36 IS 3 BP 637 EP 652 DI 10.1016/j.jas.2008.10.006 PG 16 WC Anthropology; Archaeology; Geosciences, Multidisciplinary SC Anthropology; Archaeology; Geology GA 407UP UT WOS:000263390100008 ER PT J AU Henry, AG Hudson, HF Piperno, DR AF Henry, Amanda G. Hudson, Holly F. Piperno, Dolores R. TI Changes in starch grain morphologies from cooking SO JOURNAL OF ARCHAEOLOGICAL SCIENCE LA English DT Article DE Cooking; Starch grains; Starch granules; Archaeological residues; Starch database ID STONE ARTIFACTS; TOOL-USE; RESIDUES; MAIZE; IDENTIFICATION; MICROFOSSILS; ECUADOR; PLANTS; TEETH; DIET AB One of the three main plant microfossils, starch grains are increasingly used as markers of diet, plant domestication, tool use and site organization, because their morphology and features provide a means to identify the plant that produced them. However, starch grains are susceptible to damage when they are exposed to hear in the presence of water, as in cooking. We documented the changes that Occur ill the starch grains of 10 domesticated plant species Clue to exposure to different cooking methods, in order to better understand how cooking alters the appearance of the grains, and if these cooking methods might be identifiable in the archaeological record. Our results show that some cooking methods produce unique, identifiable damage oil some types of plant starches. but generally each plant species reacts uniquely to cooking. In order to record the changes for each plant species, we have created a database, available at (http://www.osresearch.net/ similar to hollyf/starchdb/index.cgi), to which registered users call add their own images of cooked starch grains. (C) 2008 Elsevier Ltd. All rights reserved C1 [Henry, Amanda G.] George Washington Univ, Dept Anthropol, Hominid Paleobiol Doctoral Program, Washington, DC 20052 USA. [Henry, Amanda G.; Hudson, Holly F.; Piperno, Dolores R.] Smithsonian Inst, Museum Natl Hist Nat, Dept Anthropol, Archaeobiol Program, Washington, DC 20560 USA. [Piperno, Dolores R.] Smithsonian Trop Res Inst, Balboa, Panama. RP Henry, AG (reprint author), George Washington Univ, Dept Anthropol, Hominid Paleobiol Doctoral Program, 2110 G St NW, Washington, DC 20052 USA. EM ahenry@gwu.edu OI Henry, Amanda/0000-0002-2923-4199 FU NSF IGERT [9987590]; Sigma Xi grant; Smithsonian Institution's National Museum of Natural History FX We Would like to thank Linda Perry for advice and comments, Trammell Hudson for assistance in setting up the database, and finally two anonymous reviewers for their helpful comments. AGH was funded in part by NSF IGERT grant no. 9987590 and a Sigma Xi grant. All three authors were supported by the Smithsonian Institution's National Museum of Natural History. NR 30 TC 62 Z9 66 U1 2 U2 16 PU ACADEMIC PRESS LTD ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0305-4403 J9 J ARCHAEOL SCI JI J. Archaeol. Sci. PD MAR PY 2009 VL 36 IS 3 BP 915 EP 922 DI 10.1016/j.jas.2008.11.008 PG 8 WC Anthropology; Archaeology; Geosciences, Multidisciplinary SC Anthropology; Archaeology; Geology GA 407UP UT WOS:000263390100035 ER PT J AU Vencl, FV Gomez, NE Ploss, K Boland, W AF Vencl, Fredric V. Gomez, Nelida E. Ploss, Kerstin Boland, Wilhelm TI The Chlorophyll Catabolite, Pheophorbide a, Confers Predation Resistance in a Larval Tortoise Beetle Shield Defense SO JOURNAL OF CHEMICAL ECOLOGY LA English DT Article DE Chrysomelidae; Cassidinae; Azteca; Chelymorpha; porphyrin; Merremia; Insect defense ID NATURAL ENEMIES; FECAL SHIELDS; HOST-PLANT; LEPIDOPTERA; BEHAVIOR; FLAVESCENS; APOPTOSIS; INSECTS; ECOLOGY; CELLS AB Larval insect herbivores feeding externally on leaves are vulnerable to numerous and varied enemies. Larvae of the Neotropical herbivore, Chelymorpha alternans (Chrysomelidae:Cassidinae), possess shields made of cast skins and feces, which can be aimed and waved at attacking enemies. Prior work with C. alternans feeding on Merremia umbellata (Convolvulaceae) showed that shields offered protection from generalist predators, and polar compounds were implicated. This study used a ubiquitous ant predator, Azteca lacrymosa, in field bioassays to determine the chemical constitution of the defense. We confirmed that intact shields do protect larvae and that methanol-water leaching significantly reduced shield effectiveness. Liquid chromatography-mass spectrometry (LC-MS) of the methanolic shield extract revealed two peaks at 20.18 min and 21.97 min, both with a molecular ion at m/z 593.4, and a strong UV absorption around 409 nm, suggesting a porphyrin-type compound. LC-MS analysis of a commercial standard confirmed pheophorbide a (Pha) identity. C. alternans shields contained more than 100 mu g Pha per shield. Shields leached with methanol-water did not deter ants. Methanol-water-leached shields enhanced with 3 mu g of Pha were more deterrent than larvae with solvent-leached shields, while those with 5 mu g additional Pha provided slightly less deterrence than larvae with intact shields. Solvent-leached shields with 10 mu g added Pha were comparable to intact shields, even though the Pha concentration was less than 10% of its natural concentration. Our findings are the first to assign an ecological role for a chlorophyll catabolite as a deterrent in an insect defense. C1 [Vencl, Fredric V.] SUNY Stony Brook, Dept Ecol & Evolut, Stony Brook, NY 11794 USA. [Vencl, Fredric V.; Gomez, Nelida E.] Smithsonian Trop Res Inst, Balboa, Panama. [Ploss, Kerstin; Boland, Wilhelm] Max Planck Inst Chem Okol, D-07745 Jena, Germany. RP Vencl, FV (reprint author), SUNY Stony Brook, Dept Ecol & Evolut, Stony Brook, NY 11794 USA. EM fvencl@life.bio.sunysb.edu RI Boland, Wilhelm/K-7762-2012 FU Department of Ecology and Evolution at Stony Brook University; US National Science Foundation [108213] FX We thank N. Rivas, Y. Lakey, and L. Cabilla Rios for laboratory support and technical assistance. An anonymous review and D. Windsor provided many useful insights. Experiments, sample exportation, and specimen collection were done under permits issued by the Authoridad Nacional del Ambiente de Panama ( ANAM). This is contribution # 1165 from the graduate program of the Department of Ecology and Evolution at Stony Brook University. This research was supported by the US National Science Foundation IBN # 108213 to FVV. NR 37 TC 12 Z9 12 U1 0 U2 10 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0098-0331 J9 J CHEM ECOL JI J. Chem. Ecol. PD MAR PY 2009 VL 35 IS 3 BP 281 EP 288 DI 10.1007/s10886-008-9577-1 PG 8 WC Biochemistry & Molecular Biology; Ecology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology GA 418VJ UT WOS:000264177200001 PM 19127385 ER PT J AU Tennent, JM Stanley, JD Hart, PE Bernasconi, MP AF Tennent, Jenny M. Stanley, Jean-Daniel Hart, Patrick E. Bernasconi, Maria Pia TI Coastline Shifts and Probable Ship Landing Site Submerged off Ancient Locri-Epizefiri, Southern Italy SO JOURNAL OF COASTAL RESEARCH LA English DT Article DE Calabria; Calabrian Arc; coastal shift; geoarchaeology; geophysics; Greek; Holocene; Ionian margin; Magna Graecia; marine basin; seismic profiles; ship landing; submergence; uplift; wave-break ID CALABRIA C1 [Tennent, Jenny M.; Stanley, Jean-Daniel] Smithsonian Inst, CUSP, Washington, DC 20013 USA. [Hart, Patrick E.] US Geol Survey, Menlo Pk, CA 94025 USA. [Bernasconi, Maria Pia] Univ Calabria, Dipartimento Sci Terra, I-87036 Cosenza, Italy. RP Stanley, JD (reprint author), Smithsonian Inst, CUSP, Paleo Rm E205 NMNH, Washington, DC 20013 USA. EM stanleyd@si.edu FU NMNH, Smithsonian Institution FX Financial support for the project was provided by the NMNH, Smithsonian Institution. NR 39 TC 2 Z9 2 U1 0 U2 0 PU COASTAL EDUCATION & RESEARCH FOUNDATION PI LAWRENCE PA 810 EAST 10TH STREET, LAWRENCE, KS 66044 USA SN 0749-0208 J9 J COASTAL RES JI J. Coast. Res. PD MAR PY 2009 VL 25 IS 2 BP 488 EP 499 DI 10.2112/08-0014.1 PG 12 WC Environmental Sciences; Geography, Physical; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Physical Geography; Geology GA 432HP UT WOS:000265124400021 ER PT J AU Eberhard, W Rodriguez, RL Polihronakis, M AF Eberhard, W. Rodriguez, R. L. Polihronakis, M. TI Pitfalls in understanding the functional significance of genital allometry SO JOURNAL OF EVOLUTIONARY BIOLOGY LA English DT Review DE allometry; genitalia; sexual selection; stabilizing selection ID BEETLE ONTHOPHAGUS-TAURUS; SEXUAL SIZE DIMORPHISM; MALE FERTILIZATION SUCCESS; STRIDER AQUARIUS-REMIGIS; WATER STRIDER; BODY-SIZE; GEOGRAPHICAL VARIATION; PHYLOGENETIC ANALYSIS; PROLONGED COPULATION; DROSOPHILA-SIMULANS AB The male genitalia of arthropods consistently show negative static allometry (the genitalia of small males of a species are disproportionally large, and those of large males are disproportionally small). We discuss relations between the 'one-size-fits-all' hypothesis to explain this allometry and the regimes of selection that may be acting on genitalia. We focus on the contrasts between directional vs. stabilizing selection, and natural vs. sexual selection. In addition, we point out some common methodological problems in studies of genital allometry. One-size-fits-all types of arguments for negative allometry imply net stabilizing selection, but the effects of stabilizing selection on allometry will be weaker when the correlation between body size and the trait size is weaker. One-size-fits-all arguments can involve natural as well as sexual selection, and negative allometry can also result from directional selection. Several practical problems make direct tests of whether directional or stabilizing selection is acting difficult. One common methodological problem in previous studies has been concentration on absolute rather than relative values of the allometric slopes of genitalia; there are many reasons to doubt the usefulness of comparing absolute slopes with the usual reference value of 1.00. Another problem has been the failure to recognize that size and shape are independent traits of genitalia; rapid divergence in the shape of genitalia is thus not paradoxical with respect to the reduced variation in their sizes that is commonly associated with negative allometric scaling. C1 [Eberhard, W.] Univ Costa Rica, Escuela Biol, Smithsonian Trop Res Inst, San Jose, Costa Rica. [Rodriguez, R. L.] Univ Wisconsin, Dept Biol Sci, Milwaukee, WI 53201 USA. [Polihronakis, M.] Santa Barbara Museum Nat Hist, Santa Barbara, CA USA. RP Eberhard, W (reprint author), Univ Costa Rica, Escuela Biol, Smithsonian Trop Res Inst, San Jose, Costa Rica. EM william.eberhard@gmail.com FU Smithsonian Tropical Research Institute; University of Costa Rica FX We thank John Christy, Kyle Harms, Gerlinde Hobel, William Wcislo, Mary Jane West-Eberhard and two anonymous reviewers for comments on preliminary versions, and the Smithsonian Tropical Research Institute and the University of Costa Rica for financial support. NR 102 TC 48 Z9 49 U1 2 U2 19 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1010-061X J9 J EVOLUTION BIOL JI J. Evol. Biol. PD MAR PY 2009 VL 22 IS 3 BP 435 EP 445 DI 10.1111/j.1420-9101.2008.01654.x PG 11 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 409QM UT WOS:000263520900001 PM 19170826 ER PT J AU Eggert, LS Beadell, JS McClung, A McIntosh, CE Fleischer, RC AF Eggert, Lori S. Beadell, Jon S. McClung, Andrew McIntosh, Carl E. Fleischer, Robert C. TI Evolution of Microsatellite Loci in the Adaptive Radiation of Hawaiian Honeycreepers SO JOURNAL OF HEREDITY LA English DT Article DE ascertainment bias; dinucleotide repeats; genetic distance measures; honeycreepers; microsatellites; phylogenetic inference ID POPULATION SUBDIVISION; MUTATION PROCESSES; GENETIC DISTANCES; PHYLOGENETIC ANALYSIS; SEQUENCE EVOLUTION; ALLELE FREQUENCIES; DNA; DIFFERENTIATION; CONSTRAINTS; DROSOPHILA AB Previous studies have examined germ-line mutations to infer the processes that generate and maintain variability in microsatellite loci. Few studies, however, have examined patterns to infer processes that act on microsatellite loci over evolutionary time. Here, we examine changes in 8 dinucleotide loci across the adaptive radiation of Hawaiian honeycreepers. The loci were found to be highly variable across the radiation, and we did not detect ascertainment bias with respect to allelic diversity or allele size ranges. In examining patterns at the sequence level, we found that changes in flanking regions, repeat motifs, or repeat interruptions were often shared between closely related species and may be phylogenetically informative. Genetic distance measures based on microsatellites were strongly correlated with those based on mitochondrial DNA (mtDNA) sequences as well as with divergence time up to 3 My. Phylogenetic inferences based on microsatellite genetic distances consistently recovered 2 of the 4 honeycreeper clades observed in a tree based on mtDNA sequences but differed from the mtDNA tree in the relationships among clades. Our results confirm that microsatellite loci may be conserved over evolutionary time, making them useful in population-level studies of species that diverged from the species in which they were characterized as long as 5 Ma. Despite this, we found that their use in phylogenetic inference was limited to closely related honeycreeper species. C1 [Eggert, Lori S.] Univ Missouri, Div Biol Sci, Columbia, MO 65211 USA. [Eggert, Lori S.; Beadell, Jon S.; McIntosh, Carl E.; Fleischer, Robert C.] Smithsonian Inst, Natl Zool Pk, Ctr Conservat & Evolutionary Genet, Washington, DC 20008 USA. [Eggert, Lori S.; Beadell, Jon S.; McIntosh, Carl E.; Fleischer, Robert C.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20008 USA. [McClung, Andrew] Univ Hawaii Manoa, Dept Zool, Honolulu, HI 96822 USA. RP Eggert, LS (reprint author), Univ Missouri, Div Biol Sci, 226 Tucker Hall, Columbia, MO 65211 USA. EM eggertl@missouri.edu FU National Science Foundation [DEB-0083944]; Smithsonian Institution; National Institutes of Health [1R01GM063258] FX National Science Foundation (DEB-0083944 to D. Duffy, C. T. Atkinson, S. Jarvi, M. Samuel, and R. C. F.); the Smithsonian Institution Short-term Visitor Program; the National Institutes of Health (1R01GM063258 to R. C. F., D. Fonseca and C. T. Atkinson); Friends of the National Zoo; the Wildlife Program at the US Geological Survey-Biological Resources Division, Pacific Island Ecosystems Research Center (C. T. Atkinson, P. Banko, and T. Pratt, for collection of some blood samples). NR 67 TC 4 Z9 4 U1 4 U2 12 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 0022-1503 EI 1465-7333 J9 J HERED JI J. Hered. PD MAR-APR PY 2009 VL 100 IS 2 BP 137 EP 147 DI 10.1093/jhered/esn111 PG 11 WC Evolutionary Biology; Genetics & Heredity SC Evolutionary Biology; Genetics & Heredity GA 408FD UT WOS:000263420000002 PM 19153085 ER PT J AU Radeka, V Frank, J Geary, JC Gilmore, DK Kotov, I O'Connor, P Takacs, P Tyson, JA AF Radeka, V. Frank, J. Geary, J. C. Gilmore, D. K. Kotov, I. O'Connor, P. Takacs, P. Tyson, J. A. TI LSST sensor requirements and characterization of the prototype LSST CCDs SO JOURNAL OF INSTRUMENTATION LA English DT Article CT PIXEL 2008 International Workshop CY SEP 23-26, 2008 CL Fermilab, Batavia, IL HO Fermilab DE Detectors for UV, visible and IR photons; Optics ID CHARGE DIFFUSION; ELECTRIC-FIELD; SILICON; THICK AB LSST parameters are discussed and requirements on the LSST camera are presented. Characterization methods and results on a number of new devices produced specifically to address LSST's performance goals, including flatness, QE, full well capacity, linearity, dark current, read noise, CTE, and image persistence are presented. The results indicate that commercially produced, thick n-channel over-depleted CCDs can achieve excellent red response, high CTE, low dark current and satisfy LSST requirements with no evidence of persistent image artifacts. We will also report ongoing studies of mosaic assembly techniques to achieve chip-to-chip co-planarity, high fill factor, and thermal stability. C1 [Radeka, V.; Frank, J.; Kotov, I.; O'Connor, P.; Takacs, P.] Brookhaven Natl Lab, Upton, NY 11973 USA. [Geary, J. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gilmore, D. K.] Stanford Linear Accelerator Ctr, Menlo Pk, CA 94025 USA. [Tyson, J. A.] Univ Calif Davis, Davis, CA 95616 USA. RP Kotov, I (reprint author), Brookhaven Natl Lab, Upton, NY 11973 USA. EM kotov@bnl.gov NR 15 TC 16 Z9 16 U1 1 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 1748-0221 J9 J INSTRUM JI J. Instrum. PD MAR PY 2009 VL 4 AR P03002 DI 10.1088/1748-0221/4/03/P03002 PG 14 WC Instruments & Instrumentation SC Instruments & Instrumentation GA 442YU UT WOS:000265878200002 ER PT J AU Hope, WD Aryuthaka, C AF Hope, W. Duane Aryuthaka, Chittima TI A Partial Revision of the Marine Nematode Genus Elzalia (Monhysterida: Xyalidae) with New Characters and Descriptions of Two New Species from Khung Kraben Bay, East Thailand SO JOURNAL OF NEMATOLOGY LA English DT Article DE Elzalia bipectinella; Elzalia tuberculata; Elzalia federici; Elzalia kimae; Elzalia poli; morphology; spicula; gubernaculum; ejaculatory glands; rectal glands ID YELLOW SEA; N-SP AB Elzalia bipectinella(1) n. sp. and E. tuberculata(2) n. sp. from Thailand are described and the males of three species from the Gulf of Mexico, E. federici Castillo-Fernandez and Lambshead (1990), E. kimae Castillo-Fernandez and Lambshead (1990), and E. poli Castillo-Fernandez and Lambshead (1990) are re-described from type and topotype specimens rising light and scanning electron microscopy. New morphological characters are described that include ornamentations at the distal end of the spicula and features of the gubernaculum including the manus with digits, pontis with sensory receptor and accessory process, and the condylus with either conical or foliate projections. Also, ejaculatory and rectal glands are described for the first time for Elzalia. The relevance of the new characters to the taxonomy of Elzalia is discussed. A key to identification of males is provided. A generalized description of females is given, although characters are lacking by which females of each species may be identified. C1 [Hope, W. Duane] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. [Aryuthaka, Chittima] Kasetsart Univ, Fac Fisheries, Dept Marine Sci, Bangkok, Thailand. RP Hope, WD (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. NR 27 TC 4 Z9 4 U1 0 U2 0 PU SOC NEMATOLOGISTS PI MARCELINE PA PO BOX 311, MARCELINE, MO 64658 USA SN 0022-300X J9 J NEMATOL JI J. Nematol. PD MAR PY 2009 VL 41 IS 1 BP 64 EP 83 PG 20 WC Zoology SC Zoology GA 542QD UT WOS:000273508900011 PM 22661779 ER PT J AU Wagner, PJ AF Wagner, Peter J. TI PRESENTATION OF THE 2008 CHARLES SCHUCHERT AWARD OF THE PALEONTOLOGICAL SOCIETY TO JOHN ALROY SO JOURNAL OF PALEONTOLOGY LA English DT Biographical-Item C1 Natl Museum Nat Hist, Smithsonian Inst, Dept Paleobiol, NHB, Washington, DC 20013 USA. RP Wagner, PJ (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Dept Paleobiol, NHB, MRC 121,POB 37012, Washington, DC 20013 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU PALEONTOLOGICAL SOC INC PI LAWRENCE PA 810 EAST 10TH ST, LAWRENCE, KS 66044 USA SN 0022-3360 J9 J PALEONTOL JI J. Paleontol. PD MAR PY 2009 VL 83 IS 2 BP 325 EP 326 PG 2 WC Paleontology SC Paleontology GA 420BQ UT WOS:000264263800018 ER PT J AU Cohen, AN Zabin, CJ AF Cohen, Andrew N. Zabin, Chela J. TI OYSTER SHELLS AS VECTORS FOR EXOTIC ORGANISMS SO JOURNAL OF SHELLFISH RESEARCH LA English DT Article DE oyster shell; exotic organisms; Crassostrea gigas; Crassostrea virginica; Ostrea lurida; Olympia oyster; Perkinsus marinus ID CRASSOSTREA-VIRGINICA; HABITAT; CULTCH; RECRUITMENT; ABUNDANCE; SURVIVAL; SHRIMP; STATES; CRABS; REEFS AB Oyster shell may be taken from one bay and placed in another for a variety of purposes, including the restoration or enhancement of native oysters or other native species. Whereas it is generally appreciated that undesirable organisms call be transferred with live oysters, oyster shells alone call also serve as vectors for the accidental introduction of marine organisms to new locations. We here describe oyster shell plantings made for various purposes, the potential for these plantings to inadvertently transfer live organisms, and biosanitary procedures that could limit these transfers. C1 [Cohen, Andrew N.] Ctr Res Aquat Bioinvas, Richmond, CA 94805 USA. [Zabin, Chela J.] Romberg Tiburon Ctr Environm Studies, Smithsonian Environm Res Ctr, Tiburon, CA 94920 USA. RP Cohen, AN (reprint author), Ctr Res Aquat Bioinvas, 5994 McBryde Ave, Richmond, CA 94805 USA. EM acohen@bioinvasions.com NR 41 TC 14 Z9 14 U1 0 U2 7 PU NATL SHELLFISHERIES ASSOC PI GROTON PA C/O DR. SANDRA E. SHUMWAY, UNIV CONNECTICUT, 1080 SHENNECOSSETT RD, GROTON, CT 06340 USA SN 0730-8000 J9 J SHELLFISH RES JI J. Shellfish Res. PD MAR PY 2009 VL 28 IS 1 BP 163 EP 167 DI 10.2983/035.028.0106 PG 5 WC Fisheries; Marine & Freshwater Biology SC Fisheries; Marine & Freshwater Biology GA 433BA UT WOS:000265177200016 ER PT J AU Hendricks, EA Schubert, WH Taft, RK Wang, HQ Kossin, JP AF Hendricks, Eric A. Schubert, Wayne H. Taft, Richard K. Wang, Huiqun Kossin, James P. TI Life Cycles of Hurricane-Like Vorticity Rings SO JOURNAL OF THE ATMOSPHERIC SCIENCES LA English DT Article ID VORTEX ROSSBY-WAVES; POTENTIAL VORTICITY; TROPICAL CYCLONES; MAXIMUM INTENSITY; KINETIC-ENERGY; SPIRAL BANDS; PART I; EYE; EVOLUTION; MESOVORTICES AB The asymmetric dynamics of potential vorticity mixing in the hurricane inner core are further advanced by examining the end states that result from the unforced evolution of hurricane-like vorticity rings in a non-divergent barotropic model. The results from a sequence of 170 numerical simulations are summarized. The sequence covers a two-dimensional parameter space, with the first parameter defining the hollowness of the vortex (i.e., the ratio of eye to inner-core relative vorticity) and the second parameter defining the thickness of the ring (i.e., the ratio of the inner and outer radii of the ring). In approximately one-half of the cases, the ring becomes barotropically unstable, and there ensues a vigorous vorticity mixing episode between the eye and eyewall. The output of the barotropic model is used to (i) verify that the nonlinear model approximately replicates the linear theory of the fastest-growing azimuthal mode in the early phase of the evolution, and (ii) characterize the end states (defined at t = 48 h) that result from the nonlinear chaotic vorticity advection and mixing. It is found that the linear stability theory is a good guide to the fastest-growing exponential mode in the numerical model. Two additional features are observed in the numerical model results. The first is an azimuthal wavenumber-2 deformation of the vorticity ring that occurs for moderately thick, nearly filled rings. The second is an algebraically growing wavenumber-1 instability (not present in the linear theory because of the assumed solution) that is observed as a wobbling eye (or the trochoidal oscillation for a moving vortex) for thick rings that are stable to all exponentially growing instabilities. Most end states are found to be monopoles. For very hollow and thin rings, persistent mesovortices may exist for more than 15 h before merging to a monopole. For thicker rings, the relaxation to a monopole takes longer (between 48 and 72 h). For moderately thick rings with nearly filled cores, the most likely end state is an elliptical eyewall. In this nondivergent barotropic context, both the minimum central pressure and maximum tangential velocity simultaneously decrease over 48 h during all vorticity mixing events. C1 [Hendricks, Eric A.; Schubert, Wayne H.; Taft, Richard K.] Colorado State Univ, Ft Collins, CO 80523 USA. [Wang, Huiqun] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kossin, James P.] Cooperat Inst Meteorol Satellite Studies, Madison, WI USA. RP Hendricks, EA (reprint author), USN, Res Lab, Monterey, CA 93943 USA. EM eric.hendricks@nrlmry.navy.mil RI Kossin, James/D-3929-2011; Kossin, James/C-2022-2016 OI Kossin, James/0000-0003-0461-9794 FU NASA/TCSP [04-0007-0031]; NSF [ATM-0332197]; Colorado State University FX This research was supported by NASA/TCSP Grant 04-0007-0031, NSF Grant ATM-0332197, and Colorado State University. We thank Paul Ciesielski, Christopher Davis, Richard Johnson, Kevin Mallen, Brian McNoldy, Kate Musgrave, Roger Pielke Sr., Christopher Rozoff, and Jonathan Vigh for their comments and assistance. This manuscript was improved by the helpful comments of two anonymous reviewers. NR 37 TC 23 Z9 23 U1 0 U2 0 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0022-4928 J9 J ATMOS SCI JI J. Atmos. Sci. PD MAR PY 2009 VL 66 IS 3 BP 705 EP 722 DI 10.1175/2008JAS2820.1 PG 18 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 426BB UT WOS:000264681300008 ER PT J AU Paine, CET Harms, KE Ramos, J AF Paine, C. E. Timothy Harms, Kyle E. Ramos, Jesus TI Supplemental irrigation increases seedling performance and diversity in a tropical forest SO JOURNAL OF TROPICAL ECOLOGY LA English DT Article DE diversity; Estacion Biologica Los Amigos; habitat filtering; palms; Peru; precipitation; seasonality; seedling recruitment ID RAIN-FOREST; TREE SEEDLINGS; HABITAT ASSOCIATIONS; SEASONAL DROUGHT; SPECIES RICHNESS; NEOTROPICAL TREE; WOODY-PLANTS; GROWTH; MORTALITY; DYNAMICS AB Diversity is positively correlated with water availability at global, continental and regional scales. With the objective of better understanding the mechanisms that drive these relationships. we investigated the degree to which variation in water availability affects the performance (recruitment, growth a rid survival) of juvenile trees. Precipitation was supplemented throughout two dry seasons in a seasonal moist forest in south-eastern Peru. Supplementing precipitation by 160 mm mo(-1), we increased soil moisture by 17%. To generate seedling communities or known species composition, we sowed 3840 seeds of 12 species. We monitored the fates of the 554 seedlings recruited from the sown seeds. as well as 1856 older non-sown seedlings (10 cm <= height < 50 cm), and 2353 saplings (> 1 m tall). Watering significantly enhanced young seedling growth and survival, increasing stern density and diversity. Watering diminished the recruitment of species associated with upland forests, but increased the survival of both upland- and lowland-associated species. Though supplemental watering increased the growth of older seedlings. their density and diversity were unaffected. Sapling performance was insensitive to watering. We infer that variation in dry-season water availability may affect seedling community structure by differentially affecting recruitment and increasing overall survival. These results suggest that differential seedling recruitment and survival may contribute to the observed relationships between water availability, habitat associations and patterns of tree species richness. C1 [Paine, C. E. Timothy; Harms, Kyle E.] Louisiana State Univ, Dept Biol Sci, Baton Rouge, LA 70803 USA. [Harms, Kyle E.] Smithsonian Trop Res Inst, Balboa 2072, Panama. [Ramos, Jesus] Asociac Conservac Cuenca Amazon, Jiron Cusco 499, Puerto Maldonad, Peru. RP Paine, CET (reprint author), UMR EcoFoG ENGREF, Campus Agron,BP 709, Kourou 97379, French Guiana. EM timothy.paine@ecofog.gf RI Paine, C. E. Timothy/G-9961-2011 FU LSU Board of Regents fellowship; NSF FX Nataly Hidalgo. Patricia Alvarez-Loayza, Christina Georgiou and Cecilia Carrasco helped to set up the watering system and measured multitudes of seedlings and saplings. We thank Nigel Pitman for his unreserved support and productive discussions, and the entire Los Amigos staff for logistical assistance. John Terborgh and Cesar Vela kindly provided unpublished data on adult tree densities. Comments from Liza Comita, Sarahfaye Mahon and three anonymous reviewers greatly strengthened the manuscript. This research was supported by a LSU Board of Regents fellowship to CETP and a NSF grant to KEH.. NR 30 TC 10 Z9 10 U1 4 U2 27 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0266-4674 J9 J TROP ECOL JI J. Trop. Ecol. PD MAR PY 2009 VL 25 BP 171 EP 180 DI 10.1017/S0266467408005798 PG 10 WC Ecology SC Environmental Sciences & Ecology GA 419IH UT WOS:000264212400006 ER PT J AU Matthews, L AF Matthews, Larry TI Internal Affairs SO LANDFALL LA English DT Poetry C1 [Matthews, Larry] Smithsonian Inst, Natl Zool Pk, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU UNIV OTAGO PRESS PI DUNEDIN PA PO BOX 56, DUNEDIN, NEW ZEALAND SN 0023-7930 J9 LANDFALL JI Landfall PD SPR PY 2009 IS 218 BP 99 EP 100 PG 2 WC Literary Reviews SC Literature GA 529GC UT WOS:000272503100034 ER PT J AU Rebbapragada, U Protopapas, P Brodley, CE Alcock, C AF Rebbapragada, Umaa Protopapas, Pavlos Brodley, Carla E. Alcock, Charles TI Finding anomalous periodic time series SO MACHINE LEARNING LA English DT Article DE Anomaly detection; Time series data ID VARIABLE-STARS; LIGHT AB Catalogs of periodic variable stars contain large numbers of periodic light-curves (photometric time series data from the astrophysics domain). Separating anomalous objects from well-known classes is an important step towards the discovery of new classes of astronomical objects. Most anomaly detection methods for time series data assume either a single continuous time series or a set of time series whose periods are aligned. Light-curve data precludes the use of these methods as the periods of any given pair of light-curves may be out of sync. One may use an existing anomaly detection method if, prior to similarity calculation, one performs the costly act of aligning two light-curves, an operation that scales poorly to massive data sets. This paper presents PCAD, an unsupervised anomaly detection method for large sets of unsynchronized periodic time-series data, that outputs a ranked list of both global and local anomalies. It calculates its anomaly score for each light-curve in relation to a set of centroids produced by a modified k-means clustering algorithm. Our method is able to scale to large data sets through the use of sampling. We validate our method on both light-curve data and other time series data sets. We demonstrate its effectiveness at finding known anomalies, and discuss the effect of sample size and number of centroids on our results. We compare our method to naive solutions and existing time series anomaly detection methods for unphased data, and show that PCAD's reported anomalies are comparable to or better than all other methods. Finally, astrophysicists on our team have verified that PCAD finds true anomalies that might be indicative of novel astrophysical phenomena. C1 [Rebbapragada, Umaa; Brodley, Carla E.] Tufts Univ, Dept Comp Sci, Medford, MA 02155 USA. [Protopapas, Pavlos; Alcock, Charles] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Protopapas, Pavlos] Harvard Univ, Cambridge, MA 02138 USA. RP Rebbapragada, U (reprint author), Tufts Univ, Dept Comp Sci, 161 Coll Ave, Medford, MA 02155 USA. EM urebbapr@cs.tufts.edu; pprotopapas@cfa.harvard.edu; brodley@cs.tufts.edu; calcock@cfa.harvard.edu FU NASA [NNX07AV75G]; NSF [IIS0713259] FX The authors would like to acknowledge Dr. Anselm Blumer and Dr. Roni Khardon of Tufts University for their helpful guidance and comments. We also acknowledge Dr. Mark Friedl of Boston University for the donation of the landcover data set, and Dr. David Walt and Matthew Aernecke of Tufts University for the donation of the nose data set. This material is based upon work supported by NASA under Grant No. NNX07AV75G, and the NSF under Grant No. IIS0713259. NR 47 TC 23 Z9 25 U1 0 U2 9 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0885-6125 EI 1573-0565 J9 MACH LEARN JI Mach. Learn. PD MAR PY 2009 VL 74 IS 3 BP 281 EP 313 DI 10.1007/s10994-008-5093-3 PG 33 WC Computer Science, Artificial Intelligence SC Computer Science GA 407RV UT WOS:000263382900003 ER PT J AU Beldade, R Heiser, JB Robertson, DR Gasparini, JL Floeter, SR Bernardi, G AF Beldade, Ricardo Heiser, J. B. Robertson, D. R. Gasparini, J. L. Floeter, S. R. Bernardi, G. TI Historical biogeography and speciation in the Creole wrasses (Labridae, Clepticus) SO MARINE BIOLOGY LA English DT Article ID CORAL-REEF FISH; SPECIES COMPLEX; FAMILY LABRIDAE; ATLANTIC; PHYLOGEOGRAPHY; EVOLUTION; PATTERNS; POPULATIONS; DISPERSAL; INFERENCE AB We tested whether vicariance or dispersal was the likely source of speciation in the genus Clepticus by evaluating the evolutionary timing of the effect of the mid-Atlantic barrier, which separates C. brasiliensis and C. africanus, and the Amazon barrier, which separates C. parrae and C brasiliensis. Genetic data from three mitochondrial genes and one nuclear gene were used. Mitochondrial genes separated Clepticus into three well supported clades corresponding to the three recognized allopatric morpho-species. All analyses provided consistent support for an initial separation (similar to 9.68 to 1.86 mya; 4.84% sequence divergence) of the Caribbean and South Atlantic lineages, followed by a much more recent divergence (similar to 0.60 to 0.12 mya; 0.3% sequence divergence) of the Brazilian and African sister morpho-species. Both these phylogenetic events occurred well after the formation of the two barriers that currently separate those three allopatric populations. The planktonic larval duration of these species (35-49 days) and coastal pelagic habits may have facilitated dispersal by this genus across those dispersal barriers after they formed. C1 [Beldade, Ricardo; Bernardi, G.] Univ Calif Santa Cruz, Dept Ecol & Evolutionary Biol, Santa Cruz, CA 95060 USA. [Heiser, J. B.] Cornell Univ, Dept Ecol & Evolutionary Biol, Ithaca, NY 14853 USA. [Robertson, D. R.] Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. [Gasparini, J. L.] Univ Fed Espirito Santo, Dept Ecol & Recursos Nat, BR-29060900 Vitoria, ES, Brazil. [Floeter, S. R.] Univ Fed Santa Catarina, Dept Ecol & Zool, BR-88010970 Florianopolis, SC, Brazil. RP Beldade, R (reprint author), Univ Calif Santa Cruz, Dept Ecol & Evolutionary Biol, Santa Cruz, CA 95060 USA. EM ricardobeldade@yahoo.com RI Bernardi, Giacomo/F-6346-2011; Floeter, Sergio/B-1438-2012; Beldade, Ricardo/B-3724-2012 OI Bernardi, Giacomo/0000-0002-8249-4678; Beldade, Ricardo/0000-0003-1911-0122 FU Foundation for Science and Technology [SFRH/BPD/26901/2006]; National Geographic Society [7937-05] FX Mills for reviewing the manuscript. R. Beldade was supported by a Foundation for Science and Technology grant (SFRH/BPD/26901/2006) and S. R. Floeter by a National Geographic Society grant (Grant # 7937-05). NR 42 TC 10 Z9 10 U1 0 U2 6 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0025-3162 J9 MAR BIOL JI Mar. Biol. PD MAR PY 2009 VL 156 IS 4 BP 679 EP 687 DI 10.1007/s00227-008-1118-5 PG 9 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 407RA UT WOS:000263380800014 ER PT J AU Hipp, AL Kettenring, KM Feldheim, KA Weber, JA AF Hipp, Andrew L. Kettenring, Karin M. Feldheim, Kevin A. Weber, Jaime A. TI Isolation of 11 polymorphic tri- and tetranucleotide microsatellite loci in a North American sedge (Carex scoparia: Cyperaceae) and cross-species amplification in three additional Carex species SO MOLECULAR ECOLOGY RESOURCES LA English DT Article DE Carex subgenus Vignea; chromosome diversity; Cyperaceae; microsatellite enrichment; sedges AB We report on the isolation and evaluation of 11 microsatellites from a widespread eastern North American wetland sedge, Carex scoparia. Loci exhibit 3-9 alleles over five populations and significant F(IS) (0.204-0.717) in most populations. All primers cross-amplify in at least two other species, and 10 cross-amplify in the more distantly related C. stipata. These markers will be used to examine population genetics and patterns of chromosomal diversification in this ecologically important sedge species and its relatives. C1 [Hipp, Andrew L.; Weber, Jaime A.] Morton Arboretum, Lisle, IL 60532 USA. [Kettenring, Karin M.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Feldheim, Kevin A.] Field Museum, Pritzker Lab Mol Systemat & Evolut, Chicago, IL 60605 USA. RP Hipp, AL (reprint author), Morton Arboretum, 4100 Illinois Route 53, Lisle, IL 60532 USA. EM ahipp@mortonarb.org FU National Fish and Wildlife Foundation [11439]; Chicago Wilderness/Illinois Conservation Foundation [FWS0603] FX Microsatellite enrichment was carried out in the Pritzker Laboratory for Molecular Systematics and Evolution, operated with support from the Pritzker Foundation. K.M.K. and a portion of laboratory expenses were supported by National Fish and Wildlife Foundation Grant 11439 to A.L.H.; field work and additional laboratory expenses were supported by Chicago Wilderness/Illinois Conservation Foundation grant FWS0603 to A.L.H. NR 7 TC 6 Z9 6 U1 0 U2 4 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1755-098X J9 MOL ECOL RESOUR JI Mol. Ecol. Resour. PD MAR PY 2009 VL 9 IS 2 BP 625 EP 627 DI 10.1111/j.1755-0998.2008.02480.x PG 3 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 406ZJ UT WOS:000263333100039 PM 21564711 ER PT J AU Verbruggen, H Ashworth, M LoDuca, ST Vlaeminck, C Cocquyt, E Sauvage, T Zechman, FW Littler, DS Littler, MM Leliaert, F De Clerck, O AF Verbruggen, Heroen Ashworth, Matt LoDuca, Steven T. Vlaeminck, Caroline Cocquyt, Ellen Sauvage, Thomas Zechman, Frederick W. Littler, Diane S. Littler, Mark M. Leliaert, Frederik De Clerck, Olivier TI A multi-locus time-calibrated phylogeny of the siphonous green algae SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article DE Molecular phylogenetics; Relaxed molecular clock; Fossil algae; Bryopsidales; Dasycladales; Ulvophyceae; Chlorophyta ID HALIMEDA BRYOPSIDALES; DASYCLADALES CHLOROPHYTA; UDOTEACEAE BRYOPSIDALES; MAXIMUM-LIKELIHOOD; GENE-SEQUENCES; MOLECULAR-DATA; SOUTH CHINA; 18S RDNA; EVOLUTION; ULVOPHYCEAE AB The siphonous green algae are an assemblage of seaweeds that consist of a single giant cell. They comprise two sister orders, the Bryopsidales and Dasycladales. We infer the phylogenetic relationships among the siphonous green algae based on a five-locus data matrix and analyze temporal aspects of their diversification using relaxed molecular clock methods calibrated with the fossil record. The multi-locus approach resolves much of the previous phylogenetic uncertainty, but the radiation of families belonging to the core Halimedineae remains unresolved. In the Bryopsidales, three main clades were inferred, two of which correspond to previously described suborders (Bryopsidineae and Halimedineae) and a third lineage that contains only the limestone-boring genus Ostreobium. Relaxed molecular clock models indicate a Neoproterozoic origin of the siphonous green algae and a Paleozoic diversification of the orders into their families. The inferred node ages are used to resolve conflicting hypotheses about species ages in the tropical marine alga Halimeda. (C) 2008 Elsevier Inc. All rights reserved. C1 [Verbruggen, Heroen; Vlaeminck, Caroline; Cocquyt, Ellen; Leliaert, Frederik; De Clerck, Olivier] Univ Ghent, Phycol Res Grp, B-9000 Ghent, Belgium. [Verbruggen, Heroen; Vlaeminck, Caroline; Cocquyt, Ellen; Leliaert, Frederik; De Clerck, Olivier] Univ Ghent, Ctr Mol Phylogenet & Evolut, B-9000 Ghent, Belgium. [Ashworth, Matt] Univ Texas Austin, Sect Integrat Biol, Austin, TX 78712 USA. [LoDuca, Steven T.] Eastern Michigan Univ, Dept Geog & Geol, Ypsilanti, MI 48197 USA. [Sauvage, Thomas] Univ Hawaii Manoa, Dept Bot, Honolulu, HI 96822 USA. [Zechman, Frederick W.] Calif State Univ Fresno, Dept Biol, Fresno, CA 93740 USA. [Littler, Diane S.; Littler, Mark M.] Natl Museum Nat Hist, Dept Bot, Smithsonian Inst, Washington, DC 20560 USA. RP Verbruggen, H (reprint author), Univ Ghent, Phycol Res Grp, Krijgslaan 281,Bldg S8, B-9000 Ghent, Belgium. EM heroen.verbruggen@ugent.be; mashworth@mail.utexas.edu; steve.loduca@emich.edu; caroline.vlaeminck@ugent.be; ellene.cocquyt@ugent.be; sauvage@hawaii.edu; zechman@csufresno.edu; littlerd@si.edu; littlerm@si.edu; frederik.leliaert@ugent.be; olivier.declerck@ugent.be RI Leliaert, Frederik/A-9162-2009; Verbruggen, Heroen/C-6951-2009; De Clerck, Olivier/A-9083-2010 OI Leliaert, Frederik/0000-0002-4627-7318; Verbruggen, Heroen/0000-0002-6305-4749; De Clerck, Olivier/0000-0002-3699-8402 NR 80 TC 62 Z9 63 U1 3 U2 31 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 1055-7903 J9 MOL PHYLOGENET EVOL JI Mol. Phylogenet. Evol. PD MAR PY 2009 VL 50 IS 3 BP 642 EP 653 DI 10.1016/j.ympev.2008.12.018 PG 12 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 414RD UT WOS:000263882000020 PM 19141323 ER PT J AU Kimball, RT Braun, EL Barker, FK Bowie, RCK Braun, MJ Chojnowski, JL Hackett, SJ Han, KL Harshman, J Heimer-Torres, V Holznagel, W Huddleston, CJ Marks, BD Miglia, KJ Moore, WS Reddy, S Sheldon, FH Smith, JV Witt, CC Yuri, T AF Kimball, Rebecca T. Braun, Edward L. Barker, F. Keith Bowie, Rauri C. K. Braun, Michael J. Chojnowski, Jena L. Hackett, Shannon J. Han, Kin-Lan Harshman, John Heimer-Torres, Victoria Holznagel, Wallace Huddleston, Christopher J. Marks, Ben D. Miglia, Kathleen J. Moore, William S. Reddy, Sushma Sheldon, Frederick H. Smith, Jordan V. Witt, Christopher C. Yuri, Tamaki TI A well-tested set of primers to amplify regions spread across the avian genome SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article ID GENE TREES; EVOLUTIONARY HISTORY; INTRON VARIATION; SPECIES TREES; BIRDS; MITOCHONDRIAL; PHYLOGENY; SEQUENCE; MARKERS; POLYMORPHISMS C1 [Kimball, Rebecca T.; Braun, Edward L.; Chojnowski, Jena L.; Han, Kin-Lan; Heimer-Torres, Victoria; Smith, Jordan V.; Yuri, Tamaki] Univ Florida, Dept Zool, Gainesville, FL 32611 USA. [Barker, F. Keith] Univ Minnesota, Bell Museum Nat Hist, St Paul, MN 55108 USA. [Bowie, Rauri C. K.; Hackett, Shannon J.; Harshman, John; Reddy, Sushma] Field Museum Nat Hist, Dept Zool, Chicago, IL 60605 USA. [Bowie, Rauri C. K.] Univ Calif Berkeley, Museum Vertebrate Zool, Berkeley, CA 94720 USA. [Bowie, Rauri C. K.] Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. [Bowie, Rauri C. K.] Univ Stellenbosch, Dept Bot & Zool, DST NRF Ctr Excellence, Percy FitzPatrick Inst, ZA-7602 Matieland, South Africa. [Braun, Michael J.; Han, Kin-Lan; Holznagel, Wallace; Huddleston, Christopher J.; Yuri, Tamaki] Smithsonian Inst, Dept Vertebrate Zool, Suitland, MD 20746 USA. [Han, Kin-Lan] Univ Maryland, Behav Ecol Evolut & Systemat Program, College Pk, MD 20742 USA. [Marks, Ben D.; Sheldon, Frederick H.; Witt, Christopher C.] Louisiana State Univ, Museum Nat Sci, Baton Rouge, LA 70803 USA. [Miglia, Kathleen J.; Moore, William S.] Wayne State Univ, Dept Biol Sci, Detroit, MI 48202 USA. [Witt, Christopher C.] Univ New Mexico, Dept Biol, Albuquerque, NM 87131 USA. [Witt, Christopher C.] Univ New Mexico, Museum SW Biol, Albuquerque, NM 87131 USA. RP Kimball, RT (reprint author), Univ Florida, Dept Zool, POB 118525, Gainesville, FL 32611 USA. EM rkimball@ufl.edu RI Han, Kin-Lan/G-7121-2011; Barker, Keith/K-2795-2012; Witt, Christopher/D-8587-2012; Kimball, Rebecca/C-2290-2009; OI Barker, Keith/0000-0001-7488-2470; Witt, Christopher/0000-0003-2781-1543; Kimball, Rebecca/0000-0001-5449-5481; Braun, Edward/0000-0003-1643-5212; Bowie, Rauri/0000-0001-8328-6021 NR 33 TC 99 Z9 99 U1 3 U2 17 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 1055-7903 J9 MOL PHYLOGENET EVOL JI Mol. Phylogenet. Evol. PD MAR PY 2009 VL 50 IS 3 BP 654 EP 660 DI 10.1016/j.ympev.2008.11.018 PG 7 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 414RD UT WOS:000263882000021 PM 19084073 ER PT J AU Vo, TL Mueller, UG Mikheyev, AS AF Vo, Tanya L. Mueller, Ulrich G. Mikheyev, Alexander S. TI Free-living fungal symbionts (Lepiotaceae) of fungus-growing ants (Attini: Formicidae) SO MYCOLOGIA LA English DT Article DE basidiocarp; coevolution; fungus gardening; mutualism; symbiosis ID EVOLUTION; AGRICULTURE; MUTUALISM; ISOPTERA AB Surveys of leucocoprinaceous fungi (Lepiotaceae, Agaricales, Basidiomycota) in the rainforests of Panama and Brazil revealed several free-living counterparts of fungi cultivated by primitive attine ants (the lower Attini, Formicidae, Hymenoptera), adding to two such collections identified in survey by Mueller et al (1998). The accumulated evidence Supports the hypothesis that perhaps all fungi of lower attine ants have close free-living relatives. Free-living Counterparts of ant-cultivated fungi are collected most readily during the early rainy season; in particular these are free-living Mushrooms of fungal counterparts that are cultivated as yeasts in gardens of ants in the Cyphomyrmex rimosus group. Free-living and symbiotic fungi of these yeast-cultivating ant species might represent a promising Study system to compare the biology of sympatric, conspecific fungi existing outside versus inside the attine symbiosis. C1 [Vo, Tanya L.; Mueller, Ulrich G.; Mikheyev, Alexander S.] Univ Texas Austin, Sect Integrat Biol, Patterson Labs, Austin, TX 78712 USA. [Mueller, Ulrich G.] Smithsonian Trop Res Inst, Balboa, Panama. RP Mikheyev, AS (reprint author), Univ Texas Austin, Sect Integrat Biol, Patterson Labs, 1 Univ Stn C0930, Austin, TX 78712 USA. EM mikheyev@mail.utexas.edu RI Mikheyev, Alexander Mikheyev/E-7999-2013; Mikheyev, Alexander/O-7670-2014 OI Mikheyev, Alexander Mikheyev/0000-0003-4369-1019; Mikheyev, Alexander/0000-0003-4369-1019 FU NSF [DEB-9983879]; University of Texas at Austin; US Environmental Protection Agency; US Fulbright grant FX We thank two anonymous reveiwers for their comments on the manuscript. The research was supported by an REU supplement to NSF CAREER award DEB-9983879 and an undergraduate research award to TV from the University of Texas at Austin. ASM was supported by a fellowship from the US Environmental Protection Agency and a US Fulbright grant. We thank the Autoridad Nacional del Ambiente of the Republic of Panama and the Smithsonian Tropical Research Institute for collecting permits, and we thank M. Leone for logistical support. NR 22 TC 36 Z9 36 U1 0 U2 13 PU ALLEN PRESS INC PI LAWRENCE PA 810 E 10TH ST, LAWRENCE, KS 66044 USA SN 0027-5514 J9 MYCOLOGIA JI Mycologia PD MAR-APR PY 2009 VL 101 IS 2 BP 206 EP 210 DI 10.3852/07-055 PG 5 WC Mycology SC Mycology GA 434LH UT WOS:000265275700006 PM 19397193 ER PT J AU Cavender-Bares, J Izzo, A Robinson, R Lovelock, CE AF Cavender-Bares, J. Izzo, A. Robinson, R. Lovelock, C. E. TI Changes in ectomycorrhizal community structure on two containerized oak hosts across an experimental hydrologic gradient SO MYCORRHIZA LA English DT Article DE Ectomycorrhizae; Community assembly; Soil moisture gradient; Quercus montana; Q. palustris; Molecular typing; ITS region ID ARBUSCULAR MYCORRHIZAL FUNGI; CENOCOCCUM-GEOPHILUM; PINUS-MURICATA; NICHE DIFFERENTIATION; PHYTOPHTHORA-QUERCINA; T-RFLP; FOREST; IDENTIFICATION; SOIL; DIVERSITY AB Shifts in ectomycorrhizal (ECM) community structure were examined across an experimental hydrologic gradient on containerized seedlings of two oak species, Quercus montana and Quercus palustris, inoculated from a homogenate of roots from mature oak trees. At the end of one growing season, seedlings were harvested, roots were sorted by morphotype, and proportional colonization of each type was determined. DNA was subsequently extracted from individual root tips for polymerase chain reaction, restriction fragment length polymorphism, and rDNA sequencing of the ITS1/5.8S/ITS2 region to determine identities of fungal morphotypes. Twelve distinct molecular types were identified. Analysis of similarity showed that ECM fungal assemblages shifted significantly in composition across the soil moisture gradient. Taxa within the genus Tuber and the family Thelephoraceae were largely responsible for the changes in fungal assemblages. There were also significant differences in ECM community assemblages between the two oak host species. These results demonstrate that the structure of ECM fungal communities depends on both the abiotic and biotic environments and can shift with changes in soil moisture as well as host plant, even within the same genus. C1 [Cavender-Bares, J.] Univ Minnesota, Dept Ecol Evolut & Behav, St Paul, MN 55108 USA. [Izzo, A.] Univ Calif Berkeley, Plant & Microbial Biol Dept, Berkeley, CA 94720 USA. [Cavender-Bares, J.; Robinson, R.; Lovelock, C. E.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Izzo, A.] Elon Univ, Dept Biol, Elon, NC 27244 USA. [Lovelock, C. E.] Univ Queensland, Sch Integrat Biol, Brisbane, Qld 4072, Australia. [Lovelock, C. E.] Univ Queensland, Ctr Marine Studies, Brisbane, Qld 4072, Australia. RP Cavender-Bares, J (reprint author), Univ Minnesota, Dept Ecol Evolut & Behav, 1987 Upper Buford Circle, St Paul, MN 55108 USA. EM cavender@umn.edu RI Cavender-Bares, Jeannine/K-5716-2013; Lovelock, Catherine/G-7370-2012 OI Lovelock, Catherine/0000-0002-2219-6855 NR 62 TC 23 Z9 25 U1 1 U2 22 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0940-6360 J9 MYCORRHIZA JI Mycorrhiza PD MAR PY 2009 VL 19 IS 3 BP 133 EP 142 DI 10.1007/s00572-008-0220-3 PG 10 WC Mycology SC Mycology GA 424FK UT WOS:000264550700001 PM 19142671 ER PT J AU Davidse, G Soreng, RJ Peterson, PM AF Davidse, Gerrit Soreng, Robert J. Peterson, Paul M. TI Agrostopoa (Poaceae, Pooideae, Poeae, Poinae), a New Genus with Three Species from Colombia SO NOVON LA English DT Article DE Agrostopoa; Colombia; IUCN Red List; Poaceae; Poeae; Poinae; Pooideae; Sierra Nevada del Cocuy; Sierra Nevada de Santa Marta ID CLASSIFICATION AB Agrostopoa Davidse, Soreng & P. M. Peterson, a new genus endemic to the paramos of Colombia, is proposed. The genus includes two new species, A. barclayae Davidse, Soreng & P. M. Peterson and A. woodii Soreng, P. M. Peterson & Davidse, and a third species transferred from Muhlenbergia Schreber, A. wallisii (Mez) P. M. Peterson, Soreng & Davidse (lectotype designated here). A key for determining the species and illustrations of the three species are provided. Agrostopoa is placed in subfamily Pooideae because it has non-Kranz anatomy and lanceolate membranous lodicules, and in tribe Poeae where it differs from Agrostis L. by having carinate lemmas with a terminal awn or mucro, well-developed paleas, and peculiar synflorescences with recurved branches and fragile pedicels. It is classified near Poa L., but differs from that in its single-flowered spikelets that lack rachilla extensions and possess awned or mucronate lemmas. C1 [Davidse, Gerrit] Missouri Bot Garden, St Louis, MO 63166 USA. [Soreng, Robert J.; Peterson, Paul M.] Natl Museum Nat Hist, Smithsonian Inst, Dept Bot, MRC166, Washington, DC 20013 USA. RP Davidse, G (reprint author), Missouri Bot Garden, Pob 299, St Louis, MO 63166 USA. EM gerrit.davidse@mobot.org; sorengr@si.edu; peterson@si.edu NR 11 TC 6 Z9 7 U1 0 U2 2 PU MISSOURI BOTANICAL GARDEN PI ST LOUIS PA 2345 TOWER GROVE AVENUE, ST LOUIS, MO 63110 USA SN 1055-3177 J9 NOVON JI Novon PD MAR PY 2009 VL 19 IS 1 BP 32 EP 40 DI 10.3417/2007132 PG 9 WC Plant Sciences SC Plant Sciences GA 424PD UT WOS:000264577700008 ER PT J AU Wagner, WL Hoch, PC AF Wagner, Warren L. Hoch, Peter C. TI Nomenclatural Corrections in Onagraceae SO NOVON LA English DT Article DE Camissonia; Chylismia; Neoholmgrenia; Oenothera; Onagraceae; Onagroideae AB In this paper, we provide corrections to a recent synoptical revision of the family Onagraceae (Wagner et al., 2007). The first valid publication of subfamily Onagroideae was in 1834 by Eaton, and not in 2007 by Wagner et al. We correct the authorship and place of publication of Camissonia contorta (Douglas) P. H. Raven, Chylismia scapoidea (Torrey & A. Gray) Nuttall ex Raimann, and Camissonia chamaenerioides (A. Gray) P. H. Raven. We correct the authorship and typification of Oenothera suffulta (Engelmann ex A. Gray) W. L. Wagner & Hoch, as well as the typification of Chylismia claviformis subsp. lancifolia (A. Heller) W. L. Wagner & Hoch. Our new genus Holmgrenia W. L. Wagner & Hoch is a later homonym of a name validly published by S. O. Lindberg in 1863. We propose the replacement name of Neoholmgrenia W. L. Wagner & Hoch to correct this problem, and make the two species-level combinations, N. andina (Nuttall) W. L. Wagner & Hoch, and A hilgardii (Greene) W. L. Wagner & Hoch. C1 [Wagner, Warren L.] Smithsonian Inst, MRC 166, Dept Bot, Washington, DC 20013 USA. [Hoch, Peter C.] Missouri Bot Garden, St Louis, MO 63166 USA. RP Wagner, WL (reprint author), Smithsonian Inst, MRC 166, Dept Bot, POB 37012, Washington, DC 20013 USA. EM wagnerw@si.edu; peter.hoch@mobot.org FU U.S. National Science Foundation; National Museum of Natural History of the Smithsonian Institution and the Missouri Botanical Garden FX This research was supported by a Smithsonian Institution Andrew W. Mellon Fellowship in Structure and Evolution of Terrestrial Ecosystems and over many years by the U.S. National Science Foundation. We gratefully acknowledge the continuing support of our home institutions, the National Museum of Natural History of the Smithsonian Institution and the Missouri Botanical Garden. We thank Kanchi Gandhi, A. G. Tiehm, and Jim Zarucchi for bringing some of these problems to our attention, Gandhi and Jim Reveal for productive discussions on various nomenclatural matters, and the staff of the Smithsonian Institution and the Missouri Botanical Garden for assistance with references and specimens. NR 16 TC 0 Z9 0 U1 2 U2 4 PU MISSOURI BOTANICAL GARDEN PI ST LOUIS PA 2345 TOWER GROVE AVENUE, ST LOUIS, MO 63110 USA SN 1055-3177 J9 NOVON JI Novon PD MAR PY 2009 VL 19 IS 1 BP 130 EP 132 DI 10.3417/2008083 PG 3 WC Plant Sciences SC Plant Sciences GA 424PD UT WOS:000264577700025 ER PT J AU Pritchard, JR Pierpaoli, E AF Pritchard, Jonathan R. Pierpaoli, Elena TI Neutrino mass from cosmological 21 cm observations SO NUCLEAR PHYSICS B-PROCEEDINGS SUPPLEMENTS LA English DT Proceedings Paper CT Neutrino Oscillation Workshop CY SEP 06-12, 2008 CL Otranto, ITALY SP Univ Bari, Dipartimento Fis, Dipartimento Fis, Lecce, MIUR, INFN, Univ Salento, European Network Theoret Astroparticle Phys ID HIGH-REDSHIFT AB The best current constraints on the sum of neutrino masses comes from cosmology. Here, we detail the prospects for future mass constraints from cosmological 21 cm observations of the epoch of reionization. We show that future instruments such as SKA and FFTT should be capable of constraining the total mass in neutrinos at the level of the minimum mass allowed by the observed mass splittings. C1 [Pritchard, Jonathan R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Pierpaoli, Elena] Univ So Calif, Los Angeles, CA 90089 USA. RP Pritchard, JR (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jpritchard@cfa.harvard.edu OI Pritchard, Jonathan/0000-0003-4127-5353; Pierpaoli, Elena/0000-0002-7957-8993 NR 9 TC 4 Z9 4 U1 0 U2 0 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0920-5632 J9 NUCL PHYS B-PROC SUP JI Nucl. Phys. B-Proc. Suppl. PD MAR PY 2009 VL 188 BP 31 EP 33 DI 10.1016/j.nuclphysbps.2009.02.005 PG 3 WC Physics, Particles & Fields SC Physics GA 441CB UT WOS:000265745800006 ER PT J AU Sarzetti, LC Labandeira, CC Genise, JF AF Sarzetti, Laura C. Labandeira, Conrad C. Genise, Jorge F. TI MELITTOSPHEX (HYMENOPTERA: MELITTOSPHECIDAE), A PRIMITIVE BEE AND NOT A WASP REPLY SO PALAEONTOLOGY LA English DT Editorial Material C1 [Sarzetti, Laura C.; Genise, Jorge F.] Museo Paleontol Egido Feruglio, CONICET, RA-9100 Trelew, Chubut, Argentina. [Labandeira, Conrad C.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. RP Sarzetti, LC (reprint author), Museo Paleontol Egido Feruglio, CONICET, Ave Fontana 140, RA-9100 Trelew, Chubut, Argentina. EM lsarzetti@mef.org.ar NR 6 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0031-0239 J9 PALAEONTOLOGY JI Paleontology PD MAR PY 2009 VL 52 BP 484 EP 484 PG 1 WC Paleontology SC Paleontology GA 418RF UT WOS:000264165400015 ER PT J AU Dimichele, WA Nelson, WJ Elrjck, S Ames, PR AF Dimichele, William A. Nelson, W. John Elrjck, Scott Ames, Pbtlip R. TI CATASTROPHICALLY BURIED MIDDLE PENNSYLVANIAN SIGILLARIA AND CALAMITEAN SPHENOPSIDS FROM INDIANA, USA: WHAT KIND OF VEGETATION WAS THIS? SO PALAIOS LA English DT Article ID ARBORESCENT LYCOPSIDS; GROWTH ARCHITECTURE; NOVA-SCOTIA; COAL; PALEOECOLOGY; EURAMERICA; FOREST; PEAT; ENVIRONMENTS; REPRODUCTION AB A catastrophically buried stand of calamitean sphenopsids and sigillarian lycopsids is reported from the Middle Pennsylvanian of southwestern Indiana, in the Illinois Basin. The plants were exposed in the highwall of a small surface mine and were rooted in a thin bed of coal (peat), thus representing a flooded and buried swamp surface. Coarse, floodborne silts and sands buried the forest to a depth of <3 m or more, before further incursions of water and sediment truncated the deposit. The rocks are part of the Staunton Formation. Taking up >250 linear meters of exposed highwall surface, the vegetation appears to have been a patchwork of calamitean thickets, with stems perhaps as tall as 3-5 m, within which scattered, but much larger, emergent Sigillaria trees grew, possibly reaching heights of 10-15 m. No ground cover was observed, nor were foliage or reproductive organs attributable to the dominant plants found. The growth of this vegetation in a peat-forming swamp indicates conditions of high water availability, likely in a humid, high-rainfall climate. This kind of plant assemblage, however, cannot be characterized as a rain forest, given that it consisted of medium-height thickets of horsetails with scattered, emergent, and polelike, giant lycopsids, thus lacking a closed upper canopy and possibly only partially shading the ground. C1 [Dimichele, William A.] Natl Museum Nat Hist, Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA. [Nelson, W. John; Elrjck, Scott] Illinois State Geol Survey, Coal Sect, Champaign, IL 61820 USA. [Ames, Pbtlip R.] Black Beauty Coal Co, Evansville, Evansville, IN 47715 USA. RP Dimichele, WA (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA. EM dimichel@si.edu RI DiMichele, William/K-4301-2012 FU Illinois State Geological Survey; Smithsonian Institution FX We thank Black Beauty Coal Company for their cooperation and access to exposures in the Miller Creek Mine. This work was supported in part by the Illinois State Geological Survey and by an Endowment Fund Grant from the Smithsonian Institution. We thank Mary Parrish, Department of Paleobiology, U.S. National Museum of Natural History, Smithsonian Institution, for creating the reconstruction. An earlier draft of this paper was improved significantly by the comments of two anonymous reviewers. NR 52 TC 19 Z9 19 U1 2 U2 8 PU SEPM-SOC SEDIMENTARY GEOLOGY PI TULSA PA 6128 EAST 38TH ST, STE 308, TULSA, OK 74135-5814 USA SN 0883-1351 J9 PALAIOS JI Palaios PD MAR-APR PY 2009 VL 24 IS 3-4 BP 159 EP 166 DI 10.2110/palo.2008.p08-051r PG 8 WC Geology; Paleontology SC Geology; Paleontology GA 422IR UT WOS:000264421500003 ER PT J AU Gomez, AA Jaramillo, CA Parra, M Mora, A AF Gomez, Andres A. Jaramillo, Carlos A. Parra, Mauricio Mora, Andres TI HUESSER HORIZON: A LAKE AND A MARINE INCURSION IN NORTHWESTERN SOUTH AMERICA DURING THE EARLY MIOCENE SO PALAIOS LA English DT Article ID FORELAND BASIN; EASTERN CORDILLERA; TAPHONOMY; COLOMBIA; MODELS; TIME; ORIENTATION; EVOLUTION; PATTERNS; DEPOSITS AB The Cenozoic stratigraphic sequence in the foothills of the Eastern Cordillera of Colombia is mostly fluvial in nature and very thick (similar to 8000 m), but it contains very few mollusk-bearing horizons. Recent fieldwork discovered a well-preserved molluscan assemblage that occurs near the top of the Carbonera Formation (lower Miocene) in the central foothills of the Eastern Cordillera. This level, named the Huesser horizon, is laterally extensive and can be followed for tens of kilometers. The horizon is 10 m thick and was divided into eight levels, five of them highly fossiliferous. Most of the levels are dominated by the freshwater gastropod Sheppardiconcha, with lower abundances of the bivalves Anodondiles and Mytilopsis. The top level is dominated by specimens from the bivalve family Arcidae. The taxonomic composition of the assemblage is similar to that of the Magdalena and Amazonas Basins during the early-to-middle Miocene. Paleoecologic, taphonomic, and palynological analyses indicate that the Huesser accumulated in a freshwater lake system, capped by a marine incursion. The development of a large lake and the subsequent marine event could be related to increasing subsidence coincident with eustatic sea-level rise that has been identified for the basin during the early Miocene. C1 [Parra, Mauricio] Univ Potsdam, Inst Geowissensch, D-14476 Potsdam, Germany. [Mora, Andres] Inst Colombiano Petr, Bucaramanga, Colombia. [Gomez, Andres A.; Jaramillo, Carlos A.] Smithsonian Trop Res Inst, Balboa, Panama. RP Jaramillo, CA (reprint author), POB 0843, Balboa, Ancon, Panama. EM jaramilloc@si.edu RI Parra, Mauricio/B-7497-2013 OI Parra, Mauricio/0000-0002-5955-6105 FU Smithsonian Palcobiology Endowment Fund FX This project was supported by the Smithsonian Palcobiology Endowment Fund. Thanks to M. Zuschin and J. Hartman for detailed reviews of the manuscript. E Wesselingh helped with mollusk taxonomy, and S. Moron, T Gaona, and L. Quiroz helped with fieldwork. N. Atkins improved the readability of the manuscript, Special thanks go to M. I. Barreto for her continuous support and ideas. NR 69 TC 10 Z9 11 U1 0 U2 1 PU SEPM-SOC SEDIMENTARY GEOLOGY PI TULSA PA 6128 EAST 38TH ST, STE 308, TULSA, OK 74135-5814 USA SN 0883-1351 J9 PALAIOS JI Palaios PD MAR-APR PY 2009 VL 24 IS 3-4 BP 199 EP 210 DI 10.2110/palo.2007.p07-074r PG 12 WC Geology; Paleontology SC Geology; Paleontology GA 422IR UT WOS:000264421500007 ER PT J AU Vargas-Soto, JG Andrade, JL Winter, K AF Vargas-Soto, J. G. Andrade, J. L. Winter, K. TI Carbon isotope composition and mode of photosynthesis in Clusia species from Mexico SO PHOTOSYNTHETICA LA English DT Article DE Crassulacean acid metabolism; photosynthetic pathway; species differences; stable carbon isotopes ID CRASSULACEAN ACID METABOLISM; DELTA-C-13 VALUES; MINOR L.; CAM; NITROGEN; LEAVES; PLANTS; PANAMA; DISCRIMINATION; BROMELIACEAE AB The neotropical genus Clusia comprises arborescent species exhibiting Crassulacean Acid Metabolism (CAM) as was first reported for a Mexican species, Clusia lundellii. Here, the occurrence of CAM photosynthesis was studied in 20 species of Clusia, 18 from Mexico, and 2 from Guatemala, using leaf carbon isotopic composition. In most species, samples from individuals collected in different locations were analyzed. CAM was present in at least 11 species, eight of which contained specimens with delta(13)C values less negative than -20.0 aEuro degrees, indicating strong CAM (C. chanekiana, C. flava, C. lundellii, C. mexicana, C. quadrangula, C. rosea, C. suborbicularis, and C. tetra-trianthera). delta(13)C was highly variable in some species, but CAM expression was not correlated to life form (epiphytic, hemiepiphytic, terrestrial) or habitat. CAM specimens were not collected at altitudes above 1 700 m a.s.l. C1 [Vargas-Soto, J. G.; Andrade, J. L.] Ctr Invest Cient Yucatan AC, Unidad Recursos Nat, Merida 97310, Yucatan, Mexico. [Winter, K.] Smithsonian Trop Res Inst, Panama City, Panama. RP Andrade, JL (reprint author), Ctr Invest Cient Yucatan AC, Unidad Recursos Nat, Apartado Postal 87 Cordemex, Merida 97310, Yucatan, Mexico. EM andrade@cicy.mx NR 33 TC 3 Z9 3 U1 11 U2 16 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0300-3604 J9 PHOTOSYNTHETICA JI Photosynthetica PD MAR PY 2009 VL 47 IS 1 BP 33 EP 40 DI 10.1007/s11099-009-0007-6 PG 8 WC Plant Sciences SC Plant Sciences GA 449KS UT WOS:000266330100005 ER PT J AU Soon, WWH AF Soon, Willie W. -H. TI SOLAR ARCTIC-MEDIATED CLIMATE VARIATION ON MULTIDECADAL TO CENTENNIAL TIMESCALES: EMPIRICAL EVIDENCE, MECHANISTIC EXPLANATION, AND TESTABLE CONSEQUENCES SO PHYSICAL GEOGRAPHY LA English DT Review DE solar-Arctic climate connection; total solar irradiance; Atlantic meridional overturning circulation; climate variability ID NORTH-ATLANTIC CLIMATE; SEA-SURFACE TEMPERATURE; SUN-LIKE STARS; MERIDIONAL OVERTURNING CIRCULATION; INTERTROPICAL CONVERGENCE ZONE; EAST-ASIAN MONSOON; FRESH-WATER FLUX; LAST 2000 YEARS; THERMOHALINE CIRCULATION; LATE-HOLOCENE AB Soon (2005) showed that the variable total solar irradiance (TSI) could explain, rather surprisingly, well over 75% of the variance for the decadally smoothed Arctic-wide surface air temperature over the past 130 years. The present paper provides additional empirical evidence for this physical connection, both through several newly published high-resolution paleo-proxy records and through robust climate-process modeling outputs. This paper proposes a mechanistic explanation, involving: (1) the variable strength of the Atlantic meridional overturning circulation (MOC) or thermohaline circulation (THC); (2) the shift and modulation of the Inter-Tropical Convergence Zone (ITCZ) rainbelt and tropical Atlantic ocean conditions; and (3) the intensity of the wind-driven subtropical and subpolar gyre circulation, across both the North Atlantic and North Pacific. A unique test of this proposed solar TSI-Arctic thermal-salinity-cryospheric coupling mechanism is the 5- to 20-year delay effect on the peak Atlantic MOC flow rate centered near 30-35 degrees N, and on sea surface temperature (SST) for the tropical Atlantic. The solar Arctic-mediated climate mechanism on multidecadal to centennial timescales presented here can be compared with and differentiated from both the related solar TSI and UV irradiance forcing on decadal timescales. The ultimate goal of this research is to gain sufficient mechanistic details so that the proposed solar-Arctic climate connection on multidecadal to centennial timescales can be confirmed or falsified. A further incentive is to expand this physical connection to longer, millennial-scale variability as motivated by the multiscale climate interactions shown by Braun et al. (2005), Weng (2005), and Dima and Lohmann (2009). C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Soon, WWH (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 256 TC 21 Z9 21 U1 4 U2 23 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 2-4 PARK SQUARE, MILTON PARK, ABINGDON OR14 4RN, OXON, ENGLAND SN 0272-3646 EI 1930-0557 J9 PHYS GEOGR JI Phys. Geogr. PD MAR-APR PY 2009 VL 30 IS 2 BP 144 EP 184 DI 10.2747/0272-3646.30.2.144 PG 41 WC Environmental Sciences; Geography, Physical; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Physical Geography; Geology; Meteorology & Atmospheric Sciences GA 456HS UT WOS:000266835900004 ER PT J AU Shcherbakov, RV AF Shcherbakov, Roman V. TI Dispersion of waves in relativistic plasmas with isotropic particle distributions SO PHYSICS OF PLASMAS LA English DT Article DE dispersion (wave); plasma Langmuir waves ID ELECTRONS; JETS AB The dispersion laws of Langmuir and transverse waves are calculated in the relativistic nonmagnetized formalism for several isotropic particle distributions: thermal, power law, relativistic Lorentzian kappa, and hybrid beta. For Langmuir waves the parameters of superluminal undamped, subluminal damped principal, and higher modes are determined for a range of distribution parameters. The undamped and principal damped modes are found to match smoothly. Principal damped and second damped modes are found not to match smoothly. The presence of maximum wavenumber is discovered above that no longitudinal modes formally exist. The higher damped modes are discovered to be qualitatively different for thermal and certain nonthermal distributions. Consistently with the known results, the Landau damping is calculated to be stronger for nonthermal power-law-like distributions. The dispersion law is obtained for the single undamped transverse mode. The analytic results for the simplest distributions are provided. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Shcherbakov, RV (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. FU NASA [NNX08AX04H, NNX08AH32G] FX The author is grateful to Ramesh Narayan for fruitful discussions and to anonymous referee, whose comments helped improving this manuscript. This paper was supported by NASA Earth and Space Science Fellowship under Grant No. NNX08AX04H and partially supported by NASA under Grant No. NNX08AH32G. NR 17 TC 2 Z9 2 U1 0 U2 5 PU AMER INST PHYSICS PI MELVILLE PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA SN 1070-664X EI 1089-7674 J9 PHYS PLASMAS JI Phys. Plasmas PD MAR PY 2009 VL 16 IS 3 AR 032104 DI 10.1063/1.3080748 PG 7 WC Physics, Fluids & Plasmas SC Physics GA 427LW UT WOS:000264781800007 ER PT J AU Sprague, AL Hanna, KLD Kozlowski, RWH Helbert, J Maturilli, A Warell, JB Hora, JL AF Sprague, A. L. Hanna, K. L. Donaldson Kozlowski, R. W. H. Helbert, J. Maturilli, A. Warell, J. B. Hora, J. L. TI Spectral emissivity measurements of Mercury's surface indicate Mg- and Ca-rich mineralogy, K-spar, Na-rich plagioclase, rutile, with possible perovskite, and garnet SO PLANETARY AND SPACE SCIENCE LA English DT Article DE Mercury; Mercury's surface composition; Iron-poor mineralogy; Spectroscopy of mercury's surface; Mercury's formation ID THERMAL EMISSION; REFLECTANCE SPECTRA; MU-M; IRRADIANCE CALIBRATION; ANALOG MATERIALS; SPECTROSCOPY; RADAR; ATMOSPHERE; FLYBY; METEORITES AB Mid-infrared 2-D spectroscopic measurements from 8.0 to 12.7 gm of Mercury were taken using Boston University's Mid-Infrared Spectrometer and Imager (MIRSI) mounted on the NASA Infrared Telescope Facility (IRTF) on Mauna Kea, Hawaii, 7-11 April 2006. Measurements reported here cover radar bright region C, a dark plains region west of Caloris Basin, and the interior of Caloris Basin. By use of spectral deconvolution with a large spectral library composed of many mineral compositions and grain size separates, we fitted, or "unmixed", the Mercury spectra. We find mineral suites composed of magnesium-rich orthopyroxene and olivine, Ca-, Mg-, Na-rich clinopyroxene, potassium feldspar, and Na-bearing plagioclase feldspar. Both Ca- and Mg-rich garnet (pyrope and grossular, respectively) are apparently present in small amounts. Opaque minerals are required for spectral matching, with rutile (TiO(2)) repeatedly providing the "best fit". However, in the case of the radar bright region C, perovskite also contributed to a very good fit. Caloris Basin infill is rich in both potassium feldspar and Na-rich plagioclase. There is little or no olivine in the Caloris interior smooth plains. Together with the high alkali content, this indicates that resurfacing magmas were low to intermediate in SiO(2). Data suggest the dark plains exterior to Caloris are highly differentiated low-iron basaltic magmas resulting in material that might be classified as oligorclase basalts. (C) 2009 Elsevier Ltd. All rights reserved C1 [Sprague, A. L.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Hanna, K. L. Donaldson] Brown Univ, Providence, RI 02912 USA. [Kozlowski, R. W. H.] Susquehanna Univ, Selinsgrove, PA 17870 USA. [Helbert, J.; Maturilli, A.] DLR, Inst Planetary Res, D-12489 Berlin, Germany. [Warell, J. B.] Uppsala Univ, Inst Astron Rymfys, Uppsala, Sweden. [Hora, J. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Sprague, AL (reprint author), Univ Arizona, Lunar & Planetary Lab, 1629 E Univ Blvd, Tucson, AZ 85721 USA. EM sprague@lpl.arizona.edu OI Helbert, Jorn/0000-0001-5346-9505; Hora, Joseph/0000-0002-5599-4650 FU NSF [AST-0406796]; Swedish Science foundation FX The authors of this paper were Visiting Astronomers at the NASA Infrared Telescope Facility which is operated by the University of Hawaii under contract from the National Aeronautics and Space Administration. We are especially grateful to Alan Tokunaga and Eric Tollestrop for useful engineering time on the telescope and Don Hunten for helpful discussions. Support for Sprague, Kozlowski, and Donaldson Hanna was provided by NSF Grant AST-0406796. Warell received travel support from the Swedish Science foundation (VR). NR 95 TC 46 Z9 46 U1 1 U2 4 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 MAR PY 2009 VL 57 IS 3 BP 364 EP 383 DI 10.1016/j.pss.2009.01.006 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 426EI UT WOS:000264690400010 ER PT J AU Rick, TC Erlandson, JM Vellanoweth, RL Braje, TJ Collins, PW Guthrie, DA Stafford, TW AF Rick, Torben C. Erlandson, Jon M. Vellanoweth, Rene L. Braje, Todd J. Collins, Paul W. Guthrie, Daniel A. Stafford, Thomas W., Jr. TI Origins and antiquity of the island fox (Urocyon littoralis) on California's Channel Islands SO QUATERNARY RESEARCH LA English DT Article DE Island fox; Urocyon littoralis; Animal translocation; AMS (14)C dating; Island ecology; California Channel Islands ID CARBON ISOTOPE RATIOS; STABLE NITROGEN; BONE-COLLAGEN; HISTORY; MARINE; POPULATIONS; SELECTION; DWARFISM; AMERICA; DEER AB The island fox (Urocyon littoralis) is one of few reportedly endemic terrestrial mammals on California's Channel Islands. Questions remain about how and when foxes first colonized the islands, with researchers speculating on a natural, human-assisted, or combined dispersal during the late Pleistocene and/or Holocene. A natural dispersal of foxes to the northern Channel Islands has been supported by reports of a few fox bones from late Pleistocene paleontological localities. Direct AMS (14)C dating of these "fossil" fox bones produced dates ranging from similar to 6400 to 200 cal yr BP, however, postdating human colonization of the islands by several millennia. Although one of these specimens is the earliest securely dated fox from the islands, these new data support the hypothesis that Native Americans introduced foxes to all the Channel Islands in the early to middle Holocene. However, a natural dispersal for the original island colonization cannot be ruled out until further paleontological, archaeological, and genetic studies (especially aDNA [ancient DNA]) are conducted. Published by University of Washington. C1 [Rick, Torben C.] Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20013 USA. [Erlandson, Jon M.] Univ Oregon, Museum Nat & Cultural Hist, Eugene, OR 97403 USA. [Erlandson, Jon M.] Univ Oregon, Dept Anthropol, Eugene, OR 97403 USA. [Vellanoweth, Rene L.] Calif State Univ Los Angeles, Dept Anthropol, Los Angeles, CA 90032 USA. [Braje, Todd J.] Humboldt State Univ, Dept Anthropol, Arcata, CA 95521 USA. [Collins, Paul W.] Santa Barbara Museum Nat Hist, Dept Vertebrate Zool, Santa Barbara, CA 93105 USA. [Guthrie, Daniel A.] Claremont Coll, Joint Sci Dept, Claremont, CA 91711 USA. [Stafford, Thomas W., Jr.] Stafford Res Inc, Lafayette, CO 80026 USA. RP Rick, TC (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20013 USA. EM rickt@si.edu OI Erlandson, Jon/0000-0002-4705-4319 FU University of Oregon; US Navy; Southern Methodist University FX This project was supported by the University of Oregon, the US Navy, and Southern Methodist University. We thank Ann Huston, Kelly Minas, and Steve Schwartz for supporting our research, and Curtis Marean, Donald Johnson, and Gary Roemer for comments that greatly improved this manuscript. NR 64 TC 23 Z9 25 U1 6 U2 33 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0033-5894 J9 QUATERNARY RES JI Quat. Res. PD MAR PY 2009 VL 71 IS 2 BP 93 EP 98 DI 10.1016/j.yqres.2008.12.003 PG 6 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA 414RS UT WOS:000263883500001 ER PT J AU Clough, GW AF Clough, G. Wayne TI Science, yes! SO SMITHSONIAN LA English DT Editorial Material C1 Smithsonian Inst, Washington, DC 20560 USA. RP Clough, GW (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SMITHSONIAN ASSOC PI WASHINGTON PA 900 JEFFERSON DR, WASHINGTON, DC 20560 USA SN 0037-7333 J9 SMITHSONIAN JI Smithsonian PD MAR PY 2009 VL 39 IS 12 BP 24 EP 24 PG 1 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA 411AH UT WOS:000263619000015 ER PT J AU Mcgowan, R AF Mcgowan, Robert TI IF THERE'S A HELL SO SOUTH DAKOTA REVIEW LA English DT Fiction, Creative Prose C1 [Mcgowan, Robert] Smithsonian Inst, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU UNIV SOUTH DAKOTA PI VERMILLION PA COLLEGE OF ARTS AND SCIENCES DEPT ENGLISH, VERMILLION, SD 57069 USA SN 0038-3368 J9 S DAK REV JI South Dak. Rev. PD SPR PY 2009 VL 47 IS 1 BP 74 EP 77 PG 4 WC Literary Reviews SC Literature GA 529HX UT WOS:000272507800011 ER PT J AU Koutroumpa, D Lallement, R Kharchenko, V Dalgarno, A AF Koutroumpa, Dimitra Lallement, Rosine Kharchenko, Vasili Dalgarno, Alex TI The Solar Wind Charge-eXchange Contribution to the Local Soft X-ray Background SO SPACE SCIENCE REVIEWS LA English DT Review DE SWCX; Heliosphere; SXRB; ISM; Local bubble ID SOUTHERN GALACTIC HEMISPHERE; XMM-NEWTON OBSERVATION; EMISSION; BUBBLE; NEUTRALS; IONS; MAPS AB The major sources of the Soft X-ray Background (SXRB), besides distinct structures as supernovae and superbubbles (e.g. Loop I), are: (i) an absorbed extragalactic emission following a power law, (ii) an absorbed thermal component (similar to 2x10(6) K) from the galactic disk and halo, (iii) an unabsorbed thermal component, supposedly at 10(6) K, attributed to the Local Bubble and (iv) the very recently identified unabsorbed Solar Wind Charge-eXchange (SWCX) emission from the heliosphere and the geocorona. We study the SWCX heliospheric component and its contribution to observed data. In a first part, we apply a SWCX heliospheric simulation to model the oxygen lines (3/4 keV) local intensities during shadowing observations of the MBM 12 molecular cloud and a dense filament in the south galactic hemisphere with Chandra, XMM-Newton, and Suzaku telescopes. In a second part, we present a preliminary comparison of SWCX model results with ROSAT and Wisconsin surveys data in the 1/4 keV band. We conclude that, in the 3/4 keV band, the total local intensity is entirely heliospheric, while in the 1/4 keV band, the heliospheric component seems to contribute significantly to the local SXRB intensity and has potentially a strong influence on the interpretation of the ROSAT and Wisconsin surveys data in terms of Local Bubble hot gas temperature. C1 [Koutroumpa, Dimitra] Univ Versailles St Quentin, Univ Paris 06, CNRS, Serv Aeron,IPSL,UMR 7620, Verrieres Le Buisson, France. [Lallement, Rosine] IPSL, Serv Aeron, UMR 7620, Verrieres Le Buisson, France. [Kharchenko, Vasili; Dalgarno, Alex] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Koutroumpa, D (reprint author), Univ Versailles St Quentin, Univ Paris 06, CNRS, Serv Aeron,IPSL,UMR 7620, Verrieres Le Buisson, France. EM dimitra.koutroumpa@aerov.jussieu.fr RI XRAY, SUZAKU/A-1808-2009 NR 30 TC 25 Z9 25 U1 0 U2 2 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 EI 1572-9672 J9 SPACE SCI REV JI Space Sci. Rev. PD MAR PY 2009 VL 143 IS 1-4 BP 217 EP 230 DI 10.1007/s11214-008-9381-9 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 413NH UT WOS:000263799300017 ER PT J AU Slavin, J AF Slavin, Jonathan D. TI The Origins and Physical Properties of the Complex of Local Interstellar Clouds SO SPACE SCIENCE REVIEWS LA English DT Review DE Interstellar medium: Physical properties; Interstellar medium: Solar neighborhood; Interstellar medium: Atomic processes ID IONIZATION; TEMPERATURES; DENSITIES; DYNAMICS; HELIUM; STARS; FLUX; GAS AB The Complex of Local Interstellar Clouds (CLIC) is a relatively tight grouping of low density, warm, partially ionized clouds within about 30 pc of the Solar System. The Local Interstellar Cloud (LIC) is the cloud observed on most lines of sight and may be the cloud that immediately surrounds our Solar System, the properties of which set the outer boundary conditions of the heliosphere. Using absorption line data toward nearby stars, in situ observations of inflowing interstellar gas from spacecraft in the Solar System, and theoretical modeling of the interstellar radiation field and radiative transfer, we can deduce many characteristics of the LIC. We find that the LIC is partially ionized with modest electron density, n (e) a parts per thousand 0.07 cm(-3). The combination of its temperature and ionization favor photoionization/thermal equilibrium over a non-equilibrium cooling cloud picture. The abundances in the LIC suggest moderate dust destruction for silicate dust but complete destruction of carbonaceous grains. An origin for the LIC as a density enhancement in the ambient medium that has been overrun by a shock seems likely, while its velocity away from the Sco-Cen association points to a possible connection to that region and the Loop I bubble. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Slavin, J (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 83, Cambridge, MA 02138 USA. EM jslavin@cfa.harvard.edu OI Slavin, Jonathan/0000-0002-7597-6935 NR 19 TC 12 Z9 12 U1 0 U2 1 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 EI 1572-9672 J9 SPACE SCI REV JI Space Sci. Rev. PD MAR PY 2009 VL 143 IS 1-4 BP 311 EP 322 DI 10.1007/s11214-008-9342-3 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 413NH UT WOS:000263799300025 ER PT J AU Henderson, RK Baker, A Murphy, KR Hamblya, A Stuetz, RM Khan, SJ AF Henderson, R. K. Baker, A. Murphy, K. R. Hamblya, A. Stuetz, R. M. Khan, S. J. TI Fluorescence as a potential monitoring tool for recycled water systems: A review SO WATER RESEARCH LA English DT Review DE Contamination; Cross-connection; EEM; Matrix effects; Membrane; Monitoring ID DISSOLVED ORGANIC-MATTER; PROTEIN-LIKE FLUORESCENCE; SOIL-AQUIFER TREATMENT; WASTE-WATER; FRESH-WATER; HUMIC SUBSTANCES; RIVER WATER; REVERSE-OSMOSIS; NATURAL-WATERS; METAL-IONS AB A rapid, highly sensitive and selective detector is urgently required to detect contamination events in recycled water systems - for example, cross-connection events in dual reticulation pipes that recycle advanced treated sewage effluent-as existing technologies, including total organic carbon and conductivity monitoring, cannot always provide the sensitivity required. Fluorescence spectroscopy has been suggested as a potential monitoring tool given its high sensitivity and selectivity. A review of recent literature demonstrates that by monitoring the fluorescence of dissolved organic matter (DOM), the ratios of humic-like (Peak C) and protein-like (Peak T) fluorescence peaks can be used to identify trace sewage contamination in river waters and estuaries, a situation analogous to contamination detection in recycled water systems. Additionally, strong correlations have been shown between Peak T and biochemical oxygen demand (BOD) in rivers, which is indicative of water impacted by microbial activity and therefore of sewage impacted systems. Hence, this review concludes that the sensitive detection of contamination events in recycled water systems may be achieved by monitoring Peak T and/or Peak C fluorescence. However, in such systems, effluent is treated to a high standard resulting in much lower DOM concentrations and the impact of these advanced treatment processes on Peaks T and C fluorescence is largely unknown and requires investigation. This review has highlighted that further work is also required to determine (a) the stability and distinctiveness of recycled water fluorescence in relation to the treatment processes utilised, (b) the impact of matrix effects, particularly the impact of oxidation, (c) calibration issues for online monitoring, and (d) the advanced data analytical techniques required, if any, to improve detection of contamination events. (C) 2008 Elsevier Ltd. All rights reserved. C1 [Henderson, R. K.; Baker, A.; Murphy, K. R.; Hamblya, A.; Stuetz, R. M.; Khan, S. J.] Univ New S Wales, Sch Civil & Environm Engn, UNSW Water Res Ctr, Sydney, NSW 2052, Australia. [Baker, A.] Univ Birmingham, Sch Geog Earth & Environm Sci, Birmingham B15 2TT, W Midlands, England. [Murphy, K. R.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Henderson, RK (reprint author), Univ New S Wales, Sch Civil & Environm Engn, UNSW Water Res Ctr, Sydney, NSW 2052, Australia. EM r.henderson@unsw.edu.au RI Murphy, Kathleen/B-8217-2009; Baker, Andy/A-6298-2011; Henderson, Rita/B-2777-2013; Khan, Stuart/E-7523-2012; Hambly, Adam/M-8752-2015 OI Baker, Andy/0000-0002-1552-6166; Murphy, Kathleen/0000-0001-5715-3604; Khan, Stuart/0000-0001-5147-145X; Hambly, Adam/0000-0002-3850-6539 FU Australian Research Council's Linkage Projects [LP0776347]; NERC Knowledge Transfer Network FX This research was supported under Australian Research Council's Linkage Projects funding scheme (project number LP0776347). We acknowledge the support of the NERC Knowledge Transfer Network 'Fluorescence for the Water Sciences'. The Authors thank Assoc. Prof. Jorg Drewes for his helpful comments on the manuscript. NR 160 TC 320 Z9 371 U1 21 U2 248 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0043-1354 J9 WATER RES JI Water Res. PD MAR PY 2009 VL 43 IS 4 BP 863 EP 881 DI 10.1016/j.watres.2008.11.027 PG 19 WC Engineering, Environmental; Environmental Sciences; Water Resources SC Engineering; Environmental Sciences & Ecology; Water Resources GA 420ZV UT WOS:000264328600001 PM 19081598 ER PT J AU Deutsch, J AF Deutsch, James TI Folklore/Cinema: Popular Film as Vernacular Culture SO WESTERN FOLKLORE LA English DT Book Review C1 [Deutsch, James] Smithsonian Inst, Washington, DC 20560 USA. RP Deutsch, J (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 2 TC 0 Z9 0 U1 0 U2 0 PU CALIFORNIA FOLKLORE SOC PI POMONA PA WESTERN FOLKLORE DEPT OF ENGL/FOREIGN LANGUAGES 3801 W.TEMPLE AVENUE, POMONA, CA 91768-4010 USA SN 0043-373X J9 WESTERN FOLKLORE JI West. Folk. PD SPR-SUM PY 2009 VL 68 IS 2-3 BP 328 EP 330 PG 3 WC Folklore SC Arts & Humanities - Other Topics GA 550WT UT WOS:000274164700022 ER PT J AU Sutton-Grier, AE Ho, M Richardson, CJ AF Sutton-Grier, Ariana E. Ho, Mengchi Richardson, Curtis J. TI ORGANIC AMENDMENTS IMPROVE SOIL CONDITIONS AND DENITRIFICATION IN A RESTORED RIPARIAN WETLAND SO WETLANDS LA English DT Article DE compost amendments; denitrification potential (DEA); microbial biomass; plant biomass; plant diversity; soil organic matter (SOM); species richness; wetland restoration ID CENTRAL PENNSYLVANIA; MICROBIAL BIOMASS; CREATED WETLANDS; RESTORATION; MATTER; MARSH; VEGETATION; VIRGINIA; NITROGEN; SURFACE AB Low soil organic matter (SOM) levels can limit nutrient cycling and plant growth in restored wetlands. This study examined how the addition of different amounts of compost Lit a restoration site in Charlotte, North Carolina, affected the development of soil properties, microbial communities, and plant growth and diversity. The stream and wetland restoration was completed in July 2004 and monitored for three years. Available nitrogen (N) and phosphorus (P) increased with increasing SOM. The microbial community responded to organic matter (OM) additions with increases ill both total microbial biomass an(l microbial activity (as measured by denitrification potential). Plant community responses were less consistent. In 2004, leaf % N significantly increased with increasing OM for two species (Pontederia cordata and Sagittaria latifolia) while two other species (Acorus calamus and Schoenoplectus tabernaemontani) showed no relationship; in 2005, however, there was no relationship for any of the species. We also found no relationship between total plant aboveground biomass and % SOM measured in 2006. We found negative relationships between species richness and % SOM in 2004 and 2006, but not in 2005. These results suggest that compost amendments are all effective method for improving soil properties. stimulating microbial communities. and can improve some ecosystem functions, such as nutrient cycling, but may have limited early effects on plant communities. C1 [Sutton-Grier, Ariana E.; Ho, Mengchi; Richardson, Curtis J.] Duke Univ, Nicholas Sch Environm, Durham, NC 27708 USA. RP Sutton-Grier, AE (reprint author), Smithsonian Environm Res Ctr, Box 28, Edgewater, MD 21037 USA. EM sutton-griera@si.edu OI HO, MENGCHI/0000-0001-6876-9666; Sutton-Grier, Ariana/0000-0002-1242-7728 NR 37 TC 26 Z9 30 U1 3 U2 25 PU SOC WETLAND SCIENTISTS PI LAWRENCE PA 810 E TENTH ST, P O BOX 1897, LAWRENCE, KS 66044 USA SN 0277-5212 J9 WETLANDS JI Wetlands PD MAR PY 2009 VL 29 IS 1 BP 343 EP 352 PG 10 WC Ecology; Environmental Sciences SC Environmental Sciences & Ecology GA 434SN UT WOS:000265294500034 ER PT J AU Brito, D Oliveira, LC Oprea, M Mello, MAR AF Brito, Daniel Oliveira, Leonardo C. Oprea, Monik Mello, Marco A. R. TI An overview of Brazilian mammalogy: trends, biases and future directions SO ZOOLOGIA LA English DT Article DE Biomes; meta-analysis; priorities; scientometrics ID BIODIVERSITY HOTSPOTS; CONSERVATION PRIORITIES; ATLANTIC FOREST; EXTINCTION; WILDERNESS; PATTERNS; AMAZON AB Mammals are among the most charismatic and well-studied organisms, and Brazil harbors the largest mammal diversity of the world. The Brazilian Society of Mammalogy was established in 1985, and since 2001 it organizes the Brazilian Congress of Mammalogy. We used the proceedings of all three editions of this congress together with papers indexed in Web of Science and Scielo to evaluate trends in Brazilian mammalogy. All contributions were categorized according to mammalian order, biome, topic of research and state of authors' affiliation, Our results show that mammalian orders with higher species richness receive more attention, but the ranking is different between abstracts and papers. Higher species richness did not translate into more attention for more speciose biomes, and again the ranking was different between papers and abstracts. There are research topics that receive much higher attention than others, and also other important ones, like Taxonomy, that have been neglected. States with greater human populations produce both more papers and abstracts. We conclude that the higher number of publication in the Atlantic Forest is caused by the concentration of mammalogists in the south and southeastern regions of the country. Contrary to what is normally believed, mammalian orders received attention according to their species richness, and not their charisma, probably because richer orders provide more study models. We suggest that additional funding mechanisms should be set in place in order to encourage more research on mammalian orders, topics, and states which have been neglected so far, in order to improve the knowledge on important Brazilian mammal biodiversity. C1 [Brito, Daniel] Univ Fed Goias, Dept Biol Geral, Inst Ciencias Biol, BR-74001970 Goiania, Go, Brazil. [Oliveira, Leonardo C.] Univ Maryland, Dept Biol, College Pk, MD 20740 USA. [Oprea, Monik] Smithsonian Inst, Natl Museum Nat Hist, Div Mammals, Washington, DC 20013 USA. [Mello, Marco A. R.] Univ Fed Sao Carlos, Dept Bot, BR-13565905 Sao Paulo, Brazil. RP Brito, D (reprint author), Univ Fed Goias, Dept Biol Geral, Inst Ciencias Biol, Caixa Postal 131, BR-74001970 Goiania, Go, Brazil. EM brito.dan@gmail.com RI Mello, Marco/B-1095-2008; Oprea, Monik/E-6204-2010; Brito, Daniel/A-4014-2008; Oliveira, Leonardo/G-1290-2012 OI Mello, Marco/0000-0002-9098-9427; Brito, Daniel/0000-0003-1131-4622; Oliveira, Leonardo/0000-0002-1774-0713 NR 34 TC 13 Z9 14 U1 1 U2 6 PU SOC BRASILEIRA ZOOLOGIA, UNIV FEDERAL PARANA PI CURITIBA PA CAIXA POSTAL 19020, CURITIBA, PARANA 81531-980, BRAZIL SN 1984-4670 J9 ZOOLOGIA JI Zoologia PD MAR PY 2009 VL 26 IS 1 BP 67 EP 73 PG 7 WC Zoology SC Zoology GA 453AP UT WOS:000266582600011 ER PT J AU Bennett, MR Harris, JWK Richmond, BG Braun, DR Mbua, E Kiura, P Olago, D Kibunjia, M Omuombo, C Behrensmeyer, AK Huddart, D Gonzalez, S AF Bennett, Matthew R. Harris, John W. K. Richmond, Brian G. Braun, David R. Mbua, Emma Kiura, Purity Olago, Daniel Kibunjia, Mzalendo Omuombo, Christine Behrensmeyer, Anna K. Huddart, David Gonzalez, Silvia TI Early Hominin Foot Morphology Based on 1.5-Million-Year-Old Footprints from Ileret, Kenya SO SCIENCE LA English DT Article ID TURKANA-BASIN; PLIOPLEISTOCENE HOMINIDS; LAKE TURKANA; KOOBI FORA; LAETOLI; AUSTRALOPITHECUS; CHIMPANZEE; BIPEDALISM; ETHIOPIA; WALKING AB Hominin footprints offer evidence about gait and foot shape, but their scarcity, combined with an inadequate hominin fossil record, hampers research on the evolution of the human gait. Here, we report hominin footprints in two sedimentary layers dated at 1.51 to 1.53 million years ago (Ma) at Ileret, Kenya, providing the oldest evidence of an essentially modern human-like foot anatomy, with a relatively adducted hallux, medial longitudinal arch, and medial weight transfer before push-off. The size of the Ileret footprints is consistent with stature and body mass estimates for Homo ergaster/erectus, and these prints are also morphologically distinct from the 3.75-million-year-old footprints at Laetoli, Tanzania. The Ileret prints show that by 1.5 Ma, hominins had evolved an essentially modern human foot function and style of bipedal locomotion. C1 [Bennett, Matthew R.] Bournemouth Univ, Sch Conservat Sci, Poole BH12 5BB, Dorset, England. [Harris, John W. K.] Rutgers State Univ, Dept Anthropol, New Brunswick, NJ 08901 USA. [Richmond, Brian G.] George Washington Univ, Dept Anthropol, Ctr Adv Study Hominid Paleobiol, Washington, DC 20052 USA. [Richmond, Brian G.] Smithsonian Inst, Natl Museum Nat Hist, Human Origins Program, Washington, DC 20013 USA. [Braun, David R.] Univ Cape Town, Dept Archaeol, ZA-7701 Rondebosch, South Africa. [Mbua, Emma; Kiura, Purity; Kibunjia, Mzalendo] Natl Museums Kenya, Nairobi, Kenya. [Olago, Daniel; Omuombo, Christine] Univ Nairobi, Dept Geol, Nairobi, Kenya. [Behrensmeyer, Anna K.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, MRC 121, Washington, DC 20013 USA. [Huddart, David; Gonzalez, Silvia] Liverpool John Moores Univ, Sch Biol & Earth Sci, Liverpool L3 3AF, Merseyside, England. RP Bennett, MR (reprint author), Bournemouth Univ, Sch Conservat Sci, Poole BH12 5BB, Dorset, England. EM mbennett@bmth.ac.uk RI Braun, David/C-9680-2009; OI Omuombo, Christine Atieno/0000-0003-3966-2610; Bennett, Matthew/0000-0002-3063-8844 FU Holt Family Foundation; Wenner-Gren Foundation for Anthropological Research FX This project is part of the Koobi Fora Research and Training Program, which is jointly run by the National Museum of Kenya and Rutgers University and supported by the Holt Family Foundation, M. Weiss, B. Mortenson, G. Noland, C. Chip, and the Wenner-Gren Foundation for Anthropological Research. B. Wood provided valuable comments on a draft of the paper, and the dating was undertaken by F. Brown. The field assistance of H. Manley, S. A. Morse, and M. J. Steele is acknowledged. NR 27 TC 75 Z9 76 U1 9 U2 51 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD FEB 27 PY 2009 VL 323 IS 5918 BP 1197 EP 1201 DI 10.1126/science.1168132 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 411XT UT WOS:000263687600034 PM 19251625 ER PT J AU Lemaitre, R Mclaughlin, PA Sorhannus, U AF Lemaitre, Rafael Mclaughlin, Patsy A. Sorhannus, Ulf TI Phylogenetic relationships within the Pylochelidae (Decapoda: Anomura: Paguroidea): A cladistic analysis based on morphological characters SO ZOOTAXA LA English DT Article DE Decapoda; Anomura; Paguroidea; Pylochelidae; phylogenetic relationships ID HERMIT-CRAB; REPTANTIA; CRUSTACEA; ADULT AB Phylogenetic relationships within the "symmetrical" hermit crab family Pylochelidae were analyzed for 41 of the 45 species and subspecies currently considered valid. In the analyses, 78 morphological characters comprised the data matrix and the outgroup consisted of Thalassina anomala, a member of the Thalassinidae, and Munida quadrispina, a member of the Galatheidae. A poorly resolved strict consensus tree was obtained from a heuristic parsimony analysis of unweighted and unordered characters, which showed the family Pylochelidae and the subfamilies Pylochelinae and Pomatochelinae to be monophyletic taxa - the latter two groups had the highest Bremer support values. Additionally, while the subgenus Pylocheles (Pylocheles) was strongly supported, the subgenera Xylocheles, and Bathycheles were not. More fully resolved trees were obtained when using implied weighting, which recognized the monotypic subfamilies Parapylochelinae, Cancellochelinae and Mixtopagurinae. The subfamily Trizochelinae was found to have four distinct clades and several ambiguously placed taxa. C1 [Lemaitre, Rafael] Natl Museum Nat Hist, Dept Invertebrate Zool, Smithsonian Inst, Washington, DC 20013 USA. [Mclaughlin, Patsy A.] Western Washington Univ, Shannon Point Marine Ctr, Anacortes, WA 98221 USA. [Sorhannus, Ulf] Edinboro Univ Penn, Dept Biol & Hlth Serv, Edinboro, PA 16444 USA. RP Lemaitre, R (reprint author), Natl Museum Nat Hist, Dept Invertebrate Zool, Smithsonian Inst, POB 37012, Washington, DC 20013 USA. EM lemaitrr@si.edu; hermit@fidalgo.net; usorhannus@edinboro.edu NR 53 TC 9 Z9 11 U1 1 U2 1 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD FEB 27 PY 2009 IS 2022 BP 1 EP 14 PG 14 WC Zoology SC Zoology GA 412IS UT WOS:000263719100001 ER PT J AU Lucinda, PHF Vari, RP AF Lucinda, Paulo H. F. Vari, Richard P. TI New Steindachnerina Species (Teleostei: Characiformes: Curimatidae) from the Rio Tocantins Drainage SO COPEIA LA English DT Article AB A new species, Steindachnerina notograptos, Is described from the middle portions of the Rio Tocantins drainage, Brazil. The possession of a small, fleshy, lobulate body situated on each side of the posterior limit of the medial fold of the buccopharyngeal complex is autapomorphic for S. notograptos. The combination of other aspects of the buccopharyngeal complex along with meristic and pigmentation features further distinguish the species from all of its congeners. C1 [Vari, Richard P.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Div Fishes, Washington, DC 20013 USA. [Lucinda, Paulo H. F.] Univ Fed Tocantins, Lab Ictiol Sistemat, BR-77500000 Porto Nacl, Tocantins, Brazil. RP Vari, RP (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Div Fishes, MRC-159,POB 37012, Washington, DC 20013 USA. EM lucinda@uft.edu.br; varir@si.edu RI Lucinda, Paulo /F-1377-2011 OI Lucinda, Paulo /0000-0002-2703-0766 FU Conselho Nacional de Desenvolvimento Cientifico e Tecnologico [304838/2005-5] FX PHFL was partially Supported by a research grant from the Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPq process 304838/2005-5). Support to RPV also provided by the Herbert R. and Evelyn Axelrod Chair in Systematic Ichthyology in the Division of Fishes, National Museum of Natural History, Smithsonian Institution. We thank R. Reis (MCP) and O. Oyakawa (MZUSP) for the loan of specimens and A. Soares, R. Bezerra (both of UNT), and S. Raredon (USNM) for various forms of assistance during this study. NR 9 TC 7 Z9 7 U1 1 U2 2 PU AMER SOC ICHTHYOLOGISTS HERPETOLOGISTS PI CHARLESTON PA UNIV CHARLESTON, GRICE MARINE LABORATORY, 205 FORT JOHNSON RD, CHARLESTON, SC 29412 USA SN 0045-8511 J9 COPEIA JI Copeia PD FEB 23 PY 2009 IS 1 BP 142 EP 147 DI 10.1643/CI-08-076 PG 6 WC Zoology SC Zoology GA 412TV UT WOS:000263748000019 ER PT J AU Fernandez, L Vari, RP AF Fernandez, Luis Vari, Richard P. TI New Species of Trichomycterus from the Andean Cordillera of Argentina (Siluriformes: Trichomycteridae) SO COPEIA LA English DT Article ID TELEOSTEI AB Trichomycterus hualco, new species, is described from an Andean stream In the Provincia de La Rioja, Argentina. The new species Is distinguished from other species of Trichomycterus in the combination of the number of odontodes on the opercle and interopercle, the degree of exposure of the odontodes on the Interopercle, the form of the premaxillary teeth, the presence of papillae-like structures on the body, the number of vertebrae, the position of the first proximal dorsal-fin pteryglophore, the form of the supraorbital canal within the frontal, the length of the lateral-line canal, and various meristic features. C1 [Vari, Richard P.] Natl Museum Nat Hist, Smithsonian Inst, Div Fishes, Washington, DC 20013 USA. [Fernandez, Luis] Amer Museum Nat Hist, Dept Ichthyol, New York, NY 10024 USA. [Fernandez, Luis] Consejo Nacl Invest Cient & Tecn, Inst Fdn Miguel Lillo, Dept Zool, Div Ictiol, RA-4000 San Miguel De Tucuman, Argentina. RP Vari, RP (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Div Fishes, POB 37012,WG-14,MRC-159, Washington, DC 20013 USA. EM luis1813@yahoo.com; varir@si.edu NR 25 TC 16 Z9 16 U1 0 U2 2 PU AMER SOC ICHTHYOLOGISTS HERPETOLOGISTS PI CHARLESTON PA UNIV CHARLESTON, GRICE MARINE LABORATORY, 205 FORT JOHNSON RD, CHARLESTON, SC 29412 USA SN 0045-8511 J9 COPEIA JI Copeia PD FEB 23 PY 2009 IS 1 BP 195 EP 202 DI 10.1643/CI-08-083 PG 8 WC Zoology SC Zoology GA 412TV UT WOS:000263748000025 ER PT J AU Kim, TW Christy, JH Dennenmoser, S Choe, JC AF Kim, Tae Won Christy, John H. Dennenmoser, Stefan Choe, Jae C. TI The strength of a female mate preference increases with predation risk SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE female preference; predation risk; sexual selection; sensory trap; fiddler crab ID CRAB UCA-BEEBEI; MALE FIDDLER-CRABS; SEXUAL SELECTION; RECEIVER BIASES; PILLAR FUNCTION; SENSORY BIAS; CHOICE; COURTSHIP; BEHAVIOR; EVOLUTION AB When females search for mates and their perceived risk of predation increases, they less often express preferences for males that use conspicuous courtship signals, relaxing sexual selection on production of these signals. Here, we report an apparent exception to this general pattern. Courting male fiddler crabs Uca beebei sometimes build pillars of mud at the openings to their burrows in which crabs mate. Females visit several males before they choose a mate by staying and breeding in their burrows, and they preferentially visit males with pillars. Previous studies suggested that this preference is based on a visual orientation behaviour that may reduce females' risk of predation while searching for a mate. We tested this idea by determining whether the female preference for males with pillars increases with perceived predation risk. We attracted avian predators to where crabs were courting and measured the rates that sexually receptive females visited courting males with and without mud pillars. Under elevated risk, females continued to search for mates and they showed a stronger relative preference for males with pillars. Thus, when predation risk is high, females may continue to express preferences that are under natural selection because they help females avoid predation, strengthening sexual selection for use of the preferred signal. C1 [Kim, Tae Won; Choe, Jae C.] Ewha Womans Univ, Div EcoSci, Seoul 120750, South Korea. [Kim, Tae Won] Seoul Natl Univ, Sch Biol Sci, Seoul 151747, South Korea. [Kim, Tae Won; Christy, John H.; Dennenmoser, Stefan] Smithsonian Trop Res Inst, Naos Lab, Panama City, Panama. RP Choe, JC (reprint author), Ewha Womans Univ, Div EcoSci, Seoul 120750, South Korea. EM jaechoe@ewha.ac.kr FU Korea Research Foundation; Korean Government (MOEHRD) [KRF2005-213-D00043, KRF-2006-351-C00044]; Smithsonian Tropical Research Institute; Ewha Womans University Research Grant FX Support was provided by Korea Research Foundation Grants funded by the Korean Government (MOEHRD) (KRF2005-213-D00043 and KRF-2006-351-C00044) and a Special Research Grant from Amore-Pacific Cooperation. Special thanks to Jolyon Faria for field assistance. J.H.C. was supported by the Smithsonian Tropical Research Institute which also provided logistical support for this study. J.C.C. was funded by the Ewha Womans University Research Grant. We thank anonymous reviewers and colleagues of laboratory of Behaviour and Ecology at Ewha Womans University for their helpful comments. NR 40 TC 20 Z9 21 U1 1 U2 17 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 2009 VL 276 IS 1657 BP 775 EP 780 DI 10.1098/rspb.2008.1070 PG 6 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 394BA UT WOS:000262419000022 PM 19019792 ER PT J AU Napolitano, NR Romanowsky, AJ Coccato, L Capaccioli, M Douglas, NG Noordermeer, E Gerhard, O Arnaboldi, M De Lorenzi, F Kuijken, K Merrifield, MR O'Sullivan, E Cortesi, A Das, P Freeman, KC AF Napolitano, N. R. Romanowsky, A. J. Coccato, L. Capaccioli, M. Douglas, N. G. Noordermeer, E. Gerhard, O. Arnaboldi, M. De Lorenzi, F. Kuijken, K. Merrifield, M. R. O'Sullivan, E. Cortesi, A. Das, P. Freeman, K. C. TI The Planetary Nebula Spectrograph elliptical galaxy survey: the dark matter in NGC 4494 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Review DE planetary nebulae: general; galaxies: elliptical and lenticular, cD; galaxies: individual: NGC 4494; galaxies: kinematics and dynamics; galaxies: structure; dark matter ID SIGHT VELOCITY DISTRIBUTIONS; SURFACE BRIGHTNESS GALAXIES; KINEMATICALLY DISTINCT CORES; MODIFIED NEWTONIAN DYNAMICS; SPHERICAL STELLAR-SYSTEMS; EXTENDED ROTATION CURVES; GLOBULAR-CLUSTER SYSTEMS; ABSORPTION-LINE SPECTRA; HUBBLE-SPACE-TELESCOPE; TO-LIGHT RATIO AB We present new Planetary Nebula Spectrograph observations of the ordinary elliptical galaxy NGC 4494, resulting in positions and velocities of 255 planetary nebulae out to seven effective radii (25 kpc). We also present new wide-field surface photometry from MMT/Megacam, and long-slit stellar kinematics from VLT/FORS2. The spatial and kinematical distributions of the planetary nebulae agree with the field stars in the region of overlap. The mean rotation is relatively low, with a possible kinematic axis twist outside 1R(e). The velocity dispersion profile declines with radius, though not very steeply, down to similar to 70 km s(-1) at the last data point. We have constructed spherical dynamical models of the system, including Jeans analyses with multi-component Lambda cold dark matter (CDM) motivated galaxies as well as logarithmic potentials. These models include special attention to orbital anisotropy, which we constrain using fourth-order velocity moments. Given several different sets of modelling methods and assumptions, we find consistent results for the mass profile within the radial range constrained by the data. Some dark matter (DM) is required by the data; our best-fitting solution has a radially anisotropic stellar halo, a plausible stellar mass-to-light ratio and a DM halo with an unexpectedly low central density. We find that this result does not substantially change with a flattened axisymmetric model. Taken together with other results for galaxy halo masses, we find suggestions for a puzzling pattern wherein most intermediate-luminosity galaxies have very low concentration haloes, while some high-mass ellipticals have very high concentrations. C1 [Napolitano, N. R.] INAF Observ Capodimonte, Salita Moiariello 16, I-80131 Naples, Italy. [Romanowsky, A. J.] Univ Calif Santa Cruz, UCO Lick Observ, Santa Cruz, CA 95064 USA. [Romanowsky, A. J.] Univ Concepcion, Dept Fis, Concepcion, Chile. [Coccato, L.; Gerhard, O.; De Lorenzi, F.; Das, P.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Capaccioli, M.] Univ Naples Federico II, Dipartimento Sci Fis, I-80126 Naples, Italy. [Capaccioli, M.] INAF VSTceN, I-80131 Naples, Italy. [Douglas, N. G.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Noordermeer, E.; Merrifield, M. R.; Cortesi, A.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. [Arnaboldi, M.] European So Observ, D-85748 Garching, Germany. [Arnaboldi, M.] Osservatorio Astron Pino Torinese, INAF, I-10025 Pino Torinese, Italy. [Kuijken, K.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [O'Sullivan, E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Freeman, K. C.] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT, Australia. RP Napolitano, NR (reprint author), INAF Observ Capodimonte, Salita Moiariello 16, I-80131 Naples, Italy. EM napolita@na.astro.it; mc@na.infn.it OI Arnaboldi, Magda/0000-0001-7214-3009; O'Sullivan, Ewan/0000-0002-5671-6900; Merrifield, Michael/0000-0002-4202-4727; Napolitano, Nicola Rosario/0000-0003-0911-8884 FU CORDIS within FP6 with aMarie Curie European Reintegration [MERG-FP6-CT-2005-014774]; INAF; National Science Foundation [AST-0507729]; FONDAP Center for Astrophysics CONICYT [15010003]; NASA through Chandra Award [AR5-6012X] FX We would like to thank the Isaac Newton Group staff on La Palma for supporting the PN.S over the years. We thank Gary Mamon for many stimulating discussions on data modelling and comparison with simulations, Ralf Bender, Stacy McGaugh, Thorsten Naab and Jose Onorbe for providing their results in tabular form, Mark Wilkinson for further conversations and the referee for constructive comments. NRN has been funded by CORDIS within FP6 with aMarie Curie European Reintegration Grant, contr. n. MERG-FP6-CT-2005-014774, co-funded by INAF. AJR was supported by the National Science Foundation Grant AST-0507729 and by the FONDAP Center for Astrophysics CONICYT 15010003. EOS acknowledges support from NASA through Chandra Award Number AR5-6012X, and thanks Brian McLeod for his assistance with Megacam data reduction. This research has made use of the NED which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. We acknowledge the usage of the HyperLeda data base (http://leda.univ-lyon1.fr). NR 173 TC 79 Z9 79 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 2009 VL 393 IS 2 BP 329 EP 353 DI 10.1111/j.1365-2966.2008.14053.x PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 406NN UT WOS:000263302300001 ER PT J AU Vikhlinin, A Burenin, RA Ebeling, H Forman, WR Hornstrup, A Jones, C Kravtsov, AV Murray, SS Nagai, D Quintana, H Voevodkin, A AF Vikhlinin, A. Burenin, R. A. Ebeling, H. Forman, W. R. Hornstrup, A. Jones, C. Kravtsov, A. V. Murray, S. S. Nagai, D. Quintana, H. Voevodkin, A. TI CHANDRA CLUSTER COSMOLOGY PROJECT. II. SAMPLES AND X-RAY DATA REDUCTION SO ASTROPHYSICAL JOURNAL LA English DT Article DE catalogs; galaxies: clusters: general; surveys; X-rays: galaxies ID RELAXED GALAXY CLUSTERS; XMM-NEWTON OBSERVATIONS; FLUX-LIMITED SAMPLE; INTRACLUSTER MEDIUM; SCALING RELATIONS; TEMPERATURE PROFILES; MASS FUNCTION; NEARBY CLUSTERS; HIGH-REDSHIFT; PRECISION COSMOLOGY AB We discuss the measurements of the galaxy cluster mass functions at z approximate to 0.05 and z approximate to 0.5 using high-quality Chandra observations of samples derived from the ROSAT PSPC All-Sky and 400 deg(2) surveys. We provide a full reference for the data analysis procedures, present updated calibration of relations between the total cluster mass and its X-ray indicators (T(X), M(gas), and Y(X)) based on a subsample of low-z relaxed clusters, and present a first measurement of the evolving L(X) - M(tot) relation (with M(tot) estimated from Y(X)) obtained from a well defined statistically complete cluster sample and with appropriate corrections for the Malmquist bias applied. Finally, we present the derived cluster mass functions, estimate the systematic uncertainties in this measurement, and discuss the calculation of the likelihood function. We confidently measure the evolution in the cluster comoving number density at a fixed mass threshold, e.g., by a factor of 5.0 +/- 1.2 at M(500) = 2.5 x 10(14) h(-1) M(circle dot) between z = 0 and 0.5. This evolution reflects the growth of density perturbations, and can be used for the cosmological constraints complementing those from the distance-redshift relation. C1 [Vikhlinin, A.; Forman, W. R.; Jones, C.; Murray, S. S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Vikhlinin, A.; Burenin, R. A.; Voevodkin, A.] Space Res Inst IKI, Moscow, Russia. [Ebeling, H.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Hornstrup, A.] Danish Natl Space Ctr, DK-2100 Copenhagen, Denmark. [Kravtsov, A. V.] Univ Chicago, Enrico Fermi Inst, Kavli Inst Cosmol Phys, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Nagai, D.] Yale Univ, Dept Phys, New Haven, CT 06520 USA. [Nagai, D.] Yale Univ, Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA. [Quintana, H.] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 22, Chile. [Voevodkin, A.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. RP Vikhlinin, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 97 TC 354 Z9 354 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2009 VL 692 IS 2 BP 1033 EP 1059 DI 10.1088/0004-637X/692/2/1033 PG 27 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 411TW UT WOS:000263674700008 ER PT J AU Vikhlinin, A Kravtsov, AV Burenin, RA Ebeling, H Forman, WR Hornstrup, A Jones, C Murray, SS Nagai, D Quintana, H Voevodkin, A AF Vikhlinin, A. Kravtsov, A. V. Burenin, R. A. Ebeling, H. Forman, W. R. Hornstrup, A. Jones, C. Murray, S. S. Nagai, D. Quintana, H. Voevodkin, A. TI CHANDRA CLUSTER COSMOLOGY PROJECT III: COSMOLOGICAL PARAMETER CONSTRAINTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmological parameters; cosmology: observations; galaxies: clusters: general; dark matter; surveys ID MASS-TEMPERATURE RELATION; RELAXED GALAXY CLUSTERS; DARK-MATTER HALOES; DIGITAL SKY SURVEY; X-RAY; POWER-SPECTRUM; ACCELERATING UNIVERSE; REDSHIFT SURVEY; LEGACY SURVEY; COSMIC SHEAR AB Chandra observations of large samples of galaxy clusters detected in X-rays by ROSAT provide a new, robust determination of the cluster mass functions at low and high redshifts. Statistical and systematic errors are now sufficiently small, and the redshift leverage sufficiently large for the mass function evolution to be used as a useful growth of a structure-based dark energy probe. In this paper, we present cosmological parameter constraints obtained from Chandra observations of 37 clusters with < z > = 0.55 derived from 400 deg(2) ROSAT serendipitous survey and 49 brightest z approximate to 0.05 clusters detected in the All-Sky Survey. Evolution of the mass function between these redshifts requires Omega(A) > 0 with a similar to 5 sigma significance, and constrains the dark energy equation-of- state parameter to omega(0) = -1.14 +/- 0.21, assuming a constant w and a flat universe. Cluster information also significantly improves constraints when combined with other methods. Fitting our cluster data jointly with the latest supernovae, Wilkinson Microwave Anisotropy Probe, and baryonic acoustic oscillation measurements, we obtain omega(0) = -0.991 +/- 0.045 (stat) +/- 0.039 (sys), a factor of 1.5 reduction in statistical uncertainties, and nearly a factor of 2 improvement in systematics compared with constraints that can be obtained without clusters. The joint analysis of these four data sets puts a conservative upper limit on the masses of light neutrinos Sigma m(v) < 0.33 eV at 95% CL. We also present updated measurements of Omega(M)h and sigma(8) from the low-redshift cluster mass function. C1 [Vikhlinin, A.; Forman, W. R.; Jones, C.; Murray, S. S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kravtsov, A. V.] Univ Chicago, Enrico Fermi Inst, Kavli Inst Cosmol Phys, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Ebeling, H.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Hornstrup, A.] Technol Univ Denmark, Natl Space Inst, DK-2100 Copenhagen, Denmark. [Nagai, D.] Yale Univ, Dept Phys, New Haven, CT 06520 USA. [Nagai, D.] Yale Univ, Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA. [Quintana, H.] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 22, Chile. [Voevodkin, A.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. RP Vikhlinin, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Forman, William/0000-0002-9478-1682 NR 74 TC 588 Z9 591 U1 1 U2 14 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 2009 VL 692 IS 2 BP 1060 EP 1074 DI 10.1088/0004-637X/692/2/1060 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 411TW UT WOS:000263674700009 ER PT J AU Kuraszkiewicz, J Wilkes, BJ Schmidt, G Ghosh, H Smith, PS Cutri, R Hines, D Huff, EM McDowell, JC Nelson, B AF Kuraszkiewicz, Joanna Wilkes, Belinda J. Schmidt, Gary Ghosh, Himel Smith, Paul S. Cutri, Roc Hines, Dean Huff, Eric M. McDowell, Jonathan C. Nelson, Brant TI THE SPECTRAL ENERGY DISTRIBUTIONS OF RED TWO MICRON ALL SKY SURVEY ACTIVE GALACTIC NUCLEI SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; quasars: general ID HUBBLE-SPACE-TELESCOPE; QUASI-STELLAR OBJECTS; EMISSION-LINE PROPERTIES; X-RAY-PROPERTIES; INTERSTELLAR DUST GRAINS; SEYFERT 1 GALAXIES; XMM-NEWTON; OPTICAL SPECTROPOLARIMETRY; STATISTICAL-METHODS; INFRARED GALAXIES AB We present infrared (IR) to X-ray spectral energy distributions (SEDs) for 44 red active galactic nuclei (AGNs) selected from the Two Micron All Sky Survey (2MASS) survey on the basis of their red J-K(S) color (> 2 mag) and later observed by Chandra. In comparison with optically-, radio-, and X-ray-selected AGNs, their median SEDs are red in the optical and near-IR (NIR) with little/no blue bump. Comparison of the various broadband luminosity ratios shows that the main differences lie at the blue end of the optical and in the NIR to far-IR ratios (when available), with the red 2MASS AGNs being redder than the other samples. It thus seems that NIR color selection isolates the reddest subset of AGNs that can be classified optically. The shape of the SEDs is generally consistent with modest absorption by gas (in the X-ray) and dust (in the optical-IR), as demonstrated by comparing the optical and NIR colors with a reddened median SED and observed optical + NIR to intrinsic X-ray ratios. The levels of obscuration, estimated from X-rays, far-IR, and our detailed optical/NIR color modeling, are all consistent implying N(H) <= few x 10(22) cm(-2). We present SED models that show how the AGN optical/NIR colors change due to differing amounts of reddening, AGN to host galaxy ratio, redshift, and scattered light emission, and apply them to the sources in the sample. We find that the 2MASS AGN optical color, B-R, and to a lesser extent the NIR color, J-K(S), are strongly affected by reddening, host galaxy emission, redshift, and in few, highly polarized objects also by scattered AGN light (< 2% of intrinsic AGN light in the R band is scattered; this contribution becomes significant as the direct AGN light is absorbed). The lack of low equivalent widths in the distribution of the [OIII]lambda 5007 emission line implies a predominance of inclined objects in the red 2MASS sample. The obscuration/ inclination of the AGN allows us to see weaker emission components which are generally swamped by the AGN. C1 [Kuraszkiewicz, Joanna; Wilkes, Belinda J.; McDowell, Jonathan C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Schmidt, Gary; Smith, Paul S.; Huff, Eric M.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Ghosh, Himel] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Cutri, Roc; Nelson, Brant] CALTECH, IPAC, Pasadena, CA 91125 USA. [Hines, Dean] Space Sci Inst, Boulder, CO 80301 USA. RP Kuraszkiewicz, J (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Wilkes, Belinda/0000-0003-1809-2364 NR 94 TC 11 Z9 11 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2009 VL 692 IS 2 BP 1143 EP 1179 DI 10.1088/0004-637X/692/2/1143 PG 37 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 411TW UT WOS:000263674700014 ER PT J AU Kuraszkiewicz, J Wilkes, BJ Schmidt, G Smith, PS Cutri, R Czerny, B AF Kuraszkiewicz, Joanna Wilkes, Belinda J. Schmidt, Gary Smith, Paul S. Cutri, Roc Czerny, Bozena TI PRINCIPAL COMPONENT ANALYSIS OF THE SPECTRAL ENERGY DISTRIBUTION AND EMISSION LINE PROPERTIES OF RED 2MASS ACTIVE GALACTIC NUCLEI SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; quasars: general ID X-RAY-PROPERTIES; OPTICALLY SELECTED QUASARS; SEYFERT 1 GALAXIES; CORRELATION SPACE; STELLAR OBJECTS; COMPLETE SAMPLE; RADIO GALAXIES; II EMISSION; SKY-SURVEY; EIGENVECTOR AB We analyze the spectral energy distributions (SEDs) and emission-line properties of the red (J-K(S) > 2) 2MASS active galactic nuclei (AGNs) using principle component analysis (PCA). The sample includes 44 low redshift AGNs with low or moderate obscuration (N(H) < 10(23) cm(-2)) as indicated by X-rays and SED modeling. The obscuration of the AGNs allows us to see weaker emission components (host-galaxy emission, AGN scattered light) which are usually outshone by the AGN. The first four eigenvectors explain 70% of the variance in the sample. Eigenvector 1 (33% variance in the sample) correlates with the ratios of the intrinsic X-ray flux to the observed optical/IR fluxes and the F(2-10 keV)/F([OIII]) ratio. We suggest that it is primarily driven by the L/L(Edd) ratio and strengthened by intrinsic absorption (both circumnuclear and galactic). Eigenvector 2 (18% of variance) correlates with optical/IR colors (B-K(S), B-R, J-K(S)) and optical spectral type and depends on the contribution of the host galaxy relative to the observed AGN emission. Eigenvector 3 (12% of variance) correlates with reddening indicators obtained from the X-rays (hardness ratio, spectral index, N(H)), and the narrow H alpha/H beta emission-line ratio. Their relation suggests a common absorber for the optical/X-rays lying outside the narrow-line region possibly in a moderately inclined host galaxy. Eigenvector 4 (8% of variance) correlates with the degree of polarization and the broad H alpha/H beta ratio, indicating that dust, which scatters the nuclear emission (continuum and the broad-line region emission), also reddens the broad lines. Our analysis shows that, although as suggested by unification schemes, the inclination dependent obscuration (circumnuclear and the host galaxy) is important in determining the AGN SEDs, the L/L(Edd) ratio is the most important factor, followed by host-galaxy emission. C1 [Kuraszkiewicz, Joanna; Wilkes, Belinda J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Schmidt, Gary; Smith, Paul S.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Cutri, Roc] CALTECH, IPAC, Pasadena, CA 91125 USA. [Czerny, Bozena] Nicolaus Copernicus Astron Ctr, Warsaw, Poland. RP Kuraszkiewicz, J (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Czerny, Bozena/A-2363-2015; OI Czerny, Bozena/0000-0001-5848-4333; Wilkes, Belinda/0000-0003-1809-2364 NR 42 TC 16 Z9 16 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2009 VL 692 IS 2 BP 1180 EP 1189 DI 10.1088/0004-637X/692/2/1180 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 411TW UT WOS:000263674700015 ER PT J AU Patel, NA Young, KH Brunken, S Wilson, RW Thaddeus, P Menten, KM Reid, M McCarthy, MC Dinh-V-Trung Gottlieb, CA Hedden, A AF Patel, Nimesh A. Young, Ken H. Bruenken, Sandra Wilson, Robert W. Thaddeus, Patrick Menten, Karl M. Reid, Mark McCarthy, Michael C. Dinh-V-Trung Gottlieb, Carl A. Hedden, Abigail TI SUBMILLIMETER NARROW EMISSION LINES FROM THE INNER ENVELOPE OF IRC+10216 SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; radio lines: stars; stars: individual (IRC+10216); stars: late-type; submillimeter ID CARBON STAR IRC+10216; VIBRATIONALLY EXCITED CS; MOLECULAR-SPECTROSCOPY; COLOGNE DATABASE; EVOLVED STARS; IRC +10216; ABUNDANCES; MILLIMETER; SULFUR; MASER AB A spectral-line survey of IRC+ 10216 in the 345 GHz band has been undertaken with the Submillimeter Array. Although not yet completed, it has already yielded a fairly large sample of narrow molecular emission lines with line widths indicating expansion velocities of similar to 4 km s(-1), less than three times the well known value of the terminal expansion velocity (14.5 km s(-1)) of the outer envelope. Five of these narrow lines have now been identified as rotational transitions in vibrationally excited states of previously detected molecules: the nu = 1, J = 17-16, and J = 19-18 lines of Si(34)S and (29)SiS and the nu = 2, J = 7-6 line of CS. Maps of these lines show that the emission is confined to a region within similar to 60 AU of the star, indicating that the narrow-line emission is probing the region of dust formation where the stellar wind is still being accelerated. C1 [Patel, Nimesh A.; Young, Ken H.; Bruenken, Sandra; Wilson, Robert W.; Thaddeus, Patrick; Reid, Mark; McCarthy, Michael C.; Gottlieb, Carl A.; Hedden, Abigail] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Menten, Karl M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Dinh-V-Trung] Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan. RP Patel, NA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM npatel@cfa.harvard.edu RI Brunken, Sandra/B-1880-2010; OI Brunken, Sandra/0000-0001-7175-4828; Wilson, Robert/0000-0001-5694-6725; McCarthy, Michael/0000-0001-9142-0008 NR 34 TC 22 Z9 22 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2009 VL 692 IS 2 BP 1205 EP 1210 DI 10.1088/0004-637X/692/2/1205 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 411TW UT WOS:000263674700017 ER PT J AU Lee, JY Raymond, JC Ko, YK Kim, KS AF Lee, J. -Y. Raymond, J. C. Ko, Y. -K. Kim, K. -S. TI THREE-DIMENSIONAL STRUCTURE AND ENERGY BALANCE OF A CORONAL MASS EJECTION SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: activity; Sun: corona; Sun: coronal mass ejections (CMEs); Sun: UV radiation ID SOLAR-WIND; FLUX-ROPES; SPECTROMETER; MORPHOLOGY; ENERGETICS; EVOLUTION; GEOMETRY; MODEL; CME AB The Ultraviolet Coronagraph Spectrometer (UVCS) observed Doppler-shifted material of a partial halo coronal mass ejection (CME) on 2001 December 13. The observed ratio of [Ov]/Ov] is a reliable density diagnostic important for assessing the state of the plasma. Earlier UVCS observations of CMEs found evidence that the ejected plasma is heated long after the eruption. We have investigated the heating rates, which represent a significant fraction of the CME energy budget. The parameterized heating and radiative and adiabatic cooling have been used to evaluate the temperature evolution of the CME material with a time-dependent ionization state model. The functional form of a flux-rope model for interplanetary magnetic clouds was also used to parameterize the heating. We find that continuous heating is required to match the UVCS observations. To match the OVI bright knots, a higher heating rate is required such that the heating energy is greater than the kinetic energy. The temperatures for the bright knots in Ly alpha and CIII emission indicate that smaller heating rates are required for those regions. In the context of the flux-rope model, about 75% of the magnetic energy must go into heat in order to match the OVI observations. We derive tighter constraints on the heating than earlier analyses, and we show that thermal conduction with the Spitzer conductivity is not sufficient to account for the heating at large heights. C1 [Lee, J. -Y.; Kim, K. -S.] Kyung Hee Univ, Dept Astron & Space Sci, Yongin 446701, Gyeonggi, South Korea. [Lee, J. -Y.; Raymond, J. C.; Ko, Y. -K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lee, J. -Y.] NW Res Associates Inc, CoRA Div, Boulder, CO 80301 USA. RP Lee, JY (reprint author), Kyung Hee Univ, Dept Astron & Space Sci, Yongin 446701, Gyeonggi, South Korea. FU Korea Research Foundation [ABRL-R14-2002-043-01001-0, KRF-2005-070-C000059]; Smithsonian Astrophysical Observatory [NNG06GG78G]; Astrophysical Research Center for the Structure and Evolution of the Cosmos (ARC-SEC) of Korea Science and Engineering Foundation; [NNM07AA02C] FX We thank G.-S. Choe and Y.-J. Moon for helpful discussion on this paper. This work was supported by the Korea Research Foundation (ABRL-R14-2002-043-01001-0) and Grant NNG06GG78G to the Smithsonian Astrophysical Observatory. J.-Y. Lee acknowledges the support of the Korea Research Foundation (KRF-2005-070-C000059), the Astrophysical Research Center for the Structure and Evolution of the Cosmos (ARC-SEC) of Korea Science and Engineering Foundation through the Science Research Center (SRC) program, and Grant NNM07AA02C to the Smithsonian Astrophysical Observatory. NR 42 TC 23 Z9 23 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 FEB 20 PY 2009 VL 692 IS 2 BP 1271 EP 1286 DI 10.1088/0004-637X/692/2/1271 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 411TW UT WOS:000263674700021 ER PT J AU Caballero-Garcia, MD Miller, JM Trigo, MD Kuulkers, E Fabian, AC Mas-Hesse, JM Steeghs, D van der Klis, M AF Caballero-Garcia, M. D. Miller, J. M. Diaz Trigo, M. Kuulkers, E. Fabian, A. C. Mas-Hesse, J. M. Steeghs, D. van der Klis, M. TI INTEGRAL AND XMM-NEWTON SPECTROSCOPY OF GX 339-4 DURING HARD/SOFT INTERMEDIATE AND HIGH/SOFT STATES IN THE 2007 OUTBURST SO ASTROPHYSICAL JOURNAL LA English DT Review DE accretion, accretion disks; black hole physics; gamma rays: observations; radiation mechanisms: non-thermal; radiation mechanisms: thermal; binaries: close ID BLACK-HOLE CANDIDATE; X-RAY REFLECTION; ACTIVE GALACTIC NUCLEI; PHOTON IMAGING CAMERA; LOW-LUMINOSITY STATES; BROAD-BAND SPECTRUM; LOW/HARD STATE; CYGNUS X-1; MULTIWAVELENGTH OBSERVATIONS; COMPTONIZATION MODELS AB We present simultaneous XMM-Newton and International Gamma-Ray Astrophysics Laboratory (INTEGRAL) observations of the luminous black hole transient and relativistic jet source GX 339-4. GX 339-4 started an outburst on 2006 November and our observations were undertaken from 2007 January to March. We triggered five INTEGRAL and three XMM-Newton Target of Opportunity observations within this period. Our data cover different spectral states, namely hard intermediate, soft intermediate, and high/soft. We performed spectral analysis to the data with both phenomenological and more physical models and found that a nonthermal component seems to be required by the data in all the observations. We find a hardening of the spectrum in the third observation coincident with appearance of a broad and skewed Fe K-alpha line. In all spectral states joint XMM/EPIC-pn, JEM-X, ISGRI, and SPI data were fitted with the hybrid thermal/nonthermal Comptonization EQPAIR model. While this model accounts very well for the high-energy emission observed, it has several drawbacks in the description of the lower-energy channels. Our results imply evolution in the coronal properties, the most important one being the transition from a compact corona in the first observation to the disappearance of coronal material in the second and reappearance in the third. This fact, accompained by the plasma ejection events detected in radio on February 4-18, suggest that the ejected medium is the coronal material responsible for the hard X-ray emission. C1 [Caballero-Garcia, M. D.; Fabian, A. C.] LAEFF INTA, Madrid, Spain. [Miller, J. M.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Diaz Trigo, M.; Kuulkers, E.] ESA ESAC, Madrid, Spain. [Mas-Hesse, J. M.] CAB CSIC INTA, Madrid 28080, Spain. [Steeghs, D.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Steeghs, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [van der Klis, M.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. RP Caballero-Garcia, MD (reprint author), Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. EM mcaballe@ast.cam.ac.uk; jonmm@umich.edu RI Steeghs, Danny/C-5468-2009; Mas-Hesse, J. Miguel /K-6805-2014; Caballero-Garcia, Maria/D-5659-2017 OI Steeghs, Danny/0000-0003-0771-4746; Mas-Hesse, J. Miguel /0000-0002-8823-9723; Caballero-Garcia, Maria/0000-0001-7920-4564 FU NASA FX M. C. G. acknowledges very useful discussion with J. Malzac. This work is based on observations made with INTEGRAL, an ESA science mission with instruments and science data center funded by ESA member states and with the participation of Russia and the USA and on observations with XMM-Newton, an ESAscience mission with instruments and contributions directly funded by ESA member states and the USA (NASA). We thank K. Arnaud for providing part of the EQPAIR code used in this work. We also thank E. Jourdain for the valuable discussions regarding SPI data analysis and the anonymous referee for the very useful comments, which improved greatly the quality of the paper. J. M. M. aknowledges funding from NASA through the INTEGRAL Guest Observer program. M. C. G. was a MEC funded Ph. D. student during the main work of this paper, supported under grants PNE2003-04352 + ESP2005-07714C03- 03. D. S. acknowledges a STFC Advanced Fellowship as well as support through the NASA Guest Observer program. We also acknowledge the Swift/ BAT team for the Swift/ BAT transient monitor results. NR 102 TC 13 Z9 13 U1 2 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2009 VL 692 IS 2 BP 1339 EP 1353 DI 10.1088/0004-637X/692/2/1339 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 411TW UT WOS:000263674700027 ER PT J AU Kelly, BC Vestergaard, M Fan, XH AF Kelly, Brandon C. Vestergaard, Marianne Fan, Xiaohui TI DETERMINING QUASAR BLACK HOLE MASS FUNCTIONS FROM THEIR BROAD EMISSION LINES: APPLICATION TO THE BRIGHT QUASAR SURVEY SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: statistics; methods: data analysis; methods: numerical; methods: statistical ID ACTIVE GALACTIC NUCLEI; DIGITAL-SKY-SURVEY; HIGH-REDSHIFT QUASARS; ESTIMATING LUMINOSITY FUNCTIONS; RADIO-QUIET QUASARS; HOST GALAXIES; VELOCITY DISPERSION; COSMOLOGICAL EVOLUTION; OBSERVATIONAL CONSTRAINTS; COMPLETE SAMPLES AB We describe a Bayesian approach to estimating quasar black hole mass functions (BHMF) using the broad emission lines to estimate black hole mass. We show how using the broad-line mass estimates in combination with statistical techniques developed for luminosity function estimation (e. g., the 1/V(a) correction) leads to statistically biased results. We derive the likelihood function for the BHMF based on the broad-line mass estimates, and derive the posterior distribution for the BHMF, given the observed data. We develop our statistical approach for a flexible model where the BHMF is modeled as a mixture of Gaussian functions. Statistical inference is performed using Markov chain Monte Carlo (MCMC) methods, and we describe a Metropolis-Hastings algorithm to perform the MCMC. The MCMC simulates random draws from the probability distribution of the BHMF parameters, given the data, and we use a simulated data set to show how these random draws may be used to estimate the probability distribution for the BHMF. In addition, we show how the MCMC output may be used to estimate the probability distribution of any quantities derived from the BHMF, such as the peak in the space density of quasars. Our method has the advantage that it is able to constrain the BHMF even beyond the survey detection limits at the adopted confidence level, accounts for measurement errors and the intrinsic uncertainty in broad-line mass estimates, and provides a natural way of estimating the probability distribution of any quantities derived from the BHMF. We conclude by using our method to estimate the local active BHMF using the z < 0.5 Bright Quasar Survey sources. At z similar to 0.2, the quasar BHMF falls off approximately as a power law with slope similar to 2 for M(BH) greater than or similar to 10(8) M(circle dot). Our analysis implies that at a given M(BH), z < 0.5 broad-line quasars have a typical Eddington ratio of similar to 0.4 and a dispersion in Eddington ratio of less than or similar to 0.5 dex. C1 [Kelly, Brandon C.; Fan, Xiaohui] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA. [Kelly, Brandon C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Vestergaard, Marianne] Tufts Univ, Dept Phys & Astron, Medford, MA 02155 USA. RP Kelly, BC (reprint author), Univ Arizona, Dept Astron, Tucson, AZ 85721 USA. EM bckelly@cfa.harvard.edu RI Vestergaard, Marianne/M-5247-2014 OI Vestergaard, Marianne/0000-0001-9191-9837 FU NSF [AST 03-07384, 08-06861]; Packard Fellowship for Science and Engineering; NASA [HF-01220.01]; Space Telescope Science Institute; HST [HST-GO-10417, HST-AR-10691, HST-GO-10833] FX B. C. K., X. F., and M. V. acknowledge support for NSF grants AST 03-07384, 08-06861 and a Packard Fellowship for Science and Engineering. B. C. K. acknowledges support by NASA through Hubble Fellowship grant HF-01220.01 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. We also acknowledge financial support from HST grants HST-GO-10417 (X. F., M. V.), HST-AR-10691 (M. V.), and HST-GO-10833 (M. V.) awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555. NR 90 TC 30 Z9 30 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2009 VL 692 IS 2 BP 1388 EP 1410 DI 10.1088/0004-637X/692/2/1388 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 411TW UT WOS:000263674700032 ER PT J AU Geha, M Willman, B Simon, JD Strigari, LE Kirby, EN Law, DR Strader, J AF Geha, Marla Willman, Beth Simon, Joshua D. Strigari, Louis E. Kirby, Evan N. Law, David R. Strader, Jay TI THE LEAST-LUMINOUS GALAXY: SPECTROSCOPY OF THE MILKY WAY SATELLITE SEGUE 1 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: dwarf; galaxies: individual (Segue 1); galaxies: kinematics and dynamics; Local Group ID SAGITTARIUS DWARF GALAXY; SKY SURVEY VIEW; EXPLORING HALO SUBSTRUCTURE; DARK-MATTER; SPHEROIDAL GALAXY; GLOBULAR-CLUSTERS; GIANT STARS; URSA-MAJOR; VELOCITY DISPERSIONS; LIGHT RATIOS AB We present Keck/DEIMOS spectroscopy of Segue 1, an ultra-low-luminosity (M(V) = -1.5(-0.8)(+0.6)) Milky Way satellite companion. While the combined size and luminosity of Segue 1 are consistent with either a globular cluster or a dwarf galaxy, we present spectroscopic evidence that this object is a dark matter-dominated dwarf galaxy. We identify 24 stars as members of Segue 1 with a mean heliocentric recession velocity of 206 +/- 1.3 km s(-1). Although Segue 1 spatially overlaps the leading arm of the Sagittarius stream, its velocity is 100 km s(-1) different from that predicted for recent Sagittarius tidal debris at this position. We measure an internal velocity dispersion of 4.3 +/- 1.2 km s(-1). Under the assumption that these stars are gravitationally bound and in dynamical equilibrium, we infer a total mass of 4.5(2.5)(+4.7) x 10(5)M(circle dot) in the mass-follow-light case; using a two-component maximum-likelihood model, we determine a mass within 50 pc of 8.7(-5.2)(+13) x 105M(circle dot). These imply mass-to-light (M/L) ratios of ln(M/L(V)) = 7.2(-1.2)(+1.1) (M/L(V) = 1320(-940)(+2680)) and M/L(V) = 2440(-1775)(+1580), respectively. The error distribution of the M/L is nearly lognormal, thus Segue 1 is dark matter-dominated at a high significance. Although we cannot rule out the possibility that Segue 1 has been tidally disrupted, we do not find kinematic evidence supporting tidal effects. Using spectral synthesis modeling, we derive a metallicity for the single red giant branch star in our sample of [Fe/H] = -3.3 +/- 0.2 dex. Finally, we discuss the prospects for detecting gamma rays from annihilation of dark matter particles and show that Segue 1 is the most promising satellite for indirect dark matter detection. We conclude that Segue 1 is the least luminous of the ultra-faint galaxies recently discovered around the Milky Way, and is thus the least-luminous known galaxy. C1 [Geha, Marla] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Willman, Beth] Haverford Coll, Dept Phys, Haverford, PA 19041 USA. [Simon, Joshua D.; Law, David R.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Strigari, Louis E.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, Stanford, CA 94305 USA. [Kirby, Evan N.] Univ Calif Santa Cruz, Lick Observ, UCO, Santa Cruz, CA 95064 USA. [Strader, Jay] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02144 USA. RP Geha, M (reprint author), Yale Univ, Dept Astron, New Haven, CT 06520 USA. EM marla.geha@yale.edu OI Strigari, Louis/0000-0001-5672-6079; Kirby, Evan/0000-0001-6196-5162 FU NSF; NASA [HF-01225.01]; Space Telescope Science Institute FX We acknowledge and appreciate conversations regarding this work with James Bullock, Raja Guhathakurta, Manoj Kaplinghat, Shane Walsh, and Adi Zolotov. E. N. K. acknowledges the support of an NSF Graduate Research Fellowship. J. D. S. gratefully acknowledges the support of a Millikan Fellowship provided by Caltech. L. E. S. by NASA through Hubble Fellowship grant HF-01225.01 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. NR 67 TC 145 Z9 146 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2009 VL 692 IS 2 BP 1464 EP 1475 DI 10.1088/0004-637X/692/2/1464 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 411TW UT WOS:000263674700037 ER PT J AU Li, J van Ballegooijen, AA Mickey, D AF Li, Jing van Ballegooijen, A. A. Mickey, Don TI VECTOR MAGNETIC FIELDS AND ELECTRIC CURRENTS FROM THE IMAGING VECTOR MAGNETOGRAPH SO ASTROPHYSICAL JOURNAL LA English DT Article DE methods: data analysis; Sun: magnetic fields ID SOLAR ACTIVE REGIONS; ADVANCED STOKES POLARIMETER; 2002 JULY 15; FORCE-FREE; FLARE PHENOMENA; 180-DEGREES AMBIGUITY; TRANSITION REGION; FARADAY-ROTATION; PROFILE ANALYSIS; CURRENT HELICITY AB First, we describe a general procedure to produce high-quality vector magnetograms using the Imaging Vector Magnetograph (IVM) at Mees Solar Observatory. Two IVM effects are newly discussed and taken into account: (1) the central wavelength of the Fabry-Perot is found to drift with time as a result of undiagnosed thermal or mechanical instabilities in the instrument; (2) the Stokes V-sign convention built into the IVM is found to be opposite to the conventional definition used in the study of radiative transfer of polarized radiation. At the spatial resolution 2 '' x 2 '', the Stokes Q, U, V uncertainty reaches similar to 1 x 10(-3) to 5 x 10(-4) in time-averaged data over 1 hr in the quiet Sun. When vector magnetic fields are inferred from the time-averaged Stokes spectral images of FeI 6302.5 angstrom, the resulting uncertainties are on the order of 10 G for the longitudinal fields (B(parallel to)), 40 G for the transverse field strength (B(perpendicular to)) and similar to 9 degrees for the magnetic azimuth (phi). The magnetic field inversion used in this work is the "Triplet" code, which was developed and implemented in the IVM software package by the late B. J. LaBonte. The inversion code is described in detail in the Appendix. Second, we solve for the absolute value of the vertical electric current density, vertical bar J(z)vertical bar, accounting for the above IVM problems, for two different active regions. One is a single sunspot region (NOAA 10001 observed on 2002 June 20) while the other is a more complex, quadrupolar region (NOAA10030 observed on 2002 July 15). We use a calculation that does not require disambiguation of 180 degrees in the transverse field directions. The vertical bar J(z)vertical bar uncertainty is on the order of similar to 7.0 mA m(-2). The vertical current density increases with increasing vertical magnetic field. The rate of increase is about 1-2 times as large in the quadrupolar NOAA 10030 region as in the simple NOAA 10001, and it is more spatially variable over NOAA 10030 than over NOAA 10001. C1 [Li, Jing; Mickey, Don] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [van Ballegooijen, A. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Li, J (reprint author), Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA. EM jing@ifa.hawaii.edu; vanballe@cfa.harvard.edu; mickey@ifa.hawaii.edu OI van Ballegooijen, Adriaan/0000-0002-5622-3540 NR 87 TC 5 Z9 5 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2009 VL 692 IS 2 BP 1543 EP 1560 DI 10.1088/0004-637X/692/2/1543 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 411TW UT WOS:000263674700044 ER PT J AU Webb, TMA Yamada, T Huang, JS Ashby, MLN Matsuda, Y Egami, E Gonzalez, M Hayashimo, T AF Webb, T. M. A. Yamada, T. Huang, J. -S. Ashby, M. L. N. Matsuda, Y. Egami, E. Gonzalez, M. Hayashimo, T. TI SPITZER OBSERVATIONS OF EXTENDED LYMAN-alpha CLOUDS IN THE SSA22 FIELD SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; galaxies: active; galaxies: formation; galaxies: high-redshift; galaxies: starburst; infrared: galaxies ID ACTIVE GALACTIC NUCLEI; ULTRALUMINOUS INFRARED GALAXIES; MULTIBAND IMAGING PHOTOMETER; LARGE-SCALE STRUCTURE; HIGH-REDSHIFT; SUBMILLIMETER GALAXIES; BREAK GALAXIES; SPACE-TELESCOPE; PROTOCLUSTER REGION; LUMINOUS GALAXIES AB We present the results of a Spitzer IRAC and MIPS 24 mu m study of extended Lyman-alpha clouds (or Lyman-alpha Blobs, LABs) within the SSA22 filamentary structure at z = 3.09. We detect 6/26 LABs in all IRAC filters, four of which are also detected at 24 mu m, and find good correspondence with the 850 mu m measurements of Geach et al. An analysis of the rest-frame ultraviolet, optical, near-and mid-infrared colors reveals that these six systems exhibit signs of nuclear activity (active galactic nucleus (AGN)) and/or extreme star formation. Notably, they have properties that bridge galaxies dominated by star formation (Lyman-break galaxies (LBGs)) and those with AGNs (LBGs classified as QSOs). The LAB systems not detected in all four IRAC bands, on the other hand, are, as a group, consistent with pure star-forming systems, similar to the majority of the LBGs within the filament. These results indicate that the galaxies within LABs do not comprise a homogeneous population, though they are also consistent with scenarios in which the gas halos are ionized through a common mechanism such as galaxy-scale winds driven by the galaxies within them, or gravitational heating of the collapsing cloud itself. C1 [Webb, T. M. A.; Gonzalez, M.] McGill Univ, Dept Phys, Montreal, PQ H2A 2T8, Canada. [Yamada, T.] Tohoku Univ, Astron Inst, Grad Sch Sci, Aoba Ku, Sendai, Miyagi 9808578, Japan. [Huang, J. -S.; Ashby, M. L. N.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Matsuda, Y.] Kyoto Univ, Dept Astron, Grad Sch Sci, Kyoto 6068502, Japan. [Matsuda, Y.] Natl Astron Observ Japan, Div Opt & Infrared Astron, Tokyo 1818588, Japan. [Egami, E.] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA. [Hayashimo, T.] Tohoku Univ, Res Ctr Neutrino Sci, Grad Sch Sci, Sendai, Miyagi 9808578, Japan. RP Webb, TMA (reprint author), McGill Univ, Dept Phys, 3600 Rue Univ, Montreal, PQ H2A 2T8, Canada. EM webb@physics.mcgill.ca NR 54 TC 32 Z9 32 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2009 VL 692 IS 2 BP 1561 EP 1570 DI 10.1088/0004-637X/692/2/1561 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 411TW UT WOS:000263674700045 ER PT J AU Massaro, F Chiaberge, M Grandi, P Giovannini, G O'Dea, CP Macchetto, FD Baum, SA Gilli, R Capetti, A Bonafede, A Liuzzo, E AF Massaro, F. Chiaberge, M. Grandi, P. Giovannini, G. O'Dea, C. P. Macchetto, F. D. Baum, S. A. Gilli, R. Capetti, A. Bonafede, A. Liuzzo, E. TI EXTENDED X-RAY EMISSION IN RADIO GALAXIES: THE PECULIAR CASE OF 3C 305 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: active; galaxies: individual (3C 305); radiation mechanisms: thermal; radio continuum: galaxies; X-rays: general ID STEEP-SPECTRUM SOURCES; FAST SHOCKS; CHANDRA; SIGNATURES; NGC-1068; 3C-305; ABSORPTION; VIEW; HI AB Extended X-ray structures are common in active galactic nuclei. Here, we present the first case of a compact steep spectrum radio galaxy, 3C 305, in which the X-ray radiation appears to be associated with the optical emission line region, dominated by the [O III] 5007. On the basis of a morphological study performed using a comparison between the X-rays, the optical, and the radio bands, we argue that the high-energy emission has a thermal nature and it is not directly linked to the radio jet and hotspots of this source. Finally, we discuss the origin of the extended X-ray structure connected with the optical emission line region following two different interpretations: as due to the interaction between matter outflows and shock-heated environment gas, or as due to gas photoionized by nuclear emission. C1 [Massaro, F.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Chiaberge, M.; Macchetto, F. D.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Grandi, P.] IASF Ist Astrofis Spaziale & Fis Cosm Bologna, INAF, I-40129 Bologna, Italy. [Chiaberge, M.; Giovannini, G.; Bonafede, A.; Liuzzo, E.] Ist Radioastron Bologna, INAF, I-40129 Bologna, Italy. [Giovannini, G.; Bonafede, A.; Liuzzo, E.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. [O'Dea, C. P.] Rochester Inst Technol, Dept Phys, Carlson Ctr Imaging Sci 76 3144, Rochester, NY 14623 USA. [Capetti, A.] Osserv Astron Torino, INAF, I-10025 Pino Torinese, Italy. [Gilli, R.] Osservatorio Astron Bologna, INAF, I-40127 Bologna, Italy. RP Massaro, F (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. RI Gilli, Roberto/P-1110-2015; Massaro, Francesco/L-9102-2016; OI Gilli, Roberto/0000-0001-8121-6177; Massaro, Francesco/0000-0002-1704-9850; capetti, alessandro/0000-0003-3684-4275; Grandi, Paola/0000-0003-1848-6013; Giovannini, Gabriele/0000-0003-4916-6362 FU National Aeronautics and Space Administration [GO8-9114A]; National Science Foundation FX We thank D.E. Harris for his suggestions and for several comments and G. Privon for the HST images. F.M. is grateful to S. Bianchi for his suggestions, to M. Murgia for discussions on radio reduction, and to A. Siemiginowska for comments on X-ray data analysis. F.M., A.B., and E.L. thank E. Bressert for his help in presenting the image of 3C 305 at the "NRAO image contest 2008" (2nd prize). Finally, we thank our referee for several comments which were helpful toward improving our presentation. This research has made use of NASA's Astrophysics Data System and SAOImage DS9, developed by the Smithsonian Astrophysical Observatory and the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. The National Radio Astronomy Observatory is operated by Associated Universities, Inc., under contract with the National Science Foundation. The work at SAO is supported by NASA grant GO8-9114A. NR 37 TC 17 Z9 17 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD FEB 20 PY 2009 VL 692 IS 2 BP L123 EP L126 DI 10.1088/0004-637X/692/2/L123 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 404JZ UT WOS:000263149100014 ER PT J AU Xiao, YH AF Xiao, Yanhong TI SPECTRAL LINE NARROWING IN ELECTROMAGNETICALLY INDUCED TRANSPARENCY SO MODERN PHYSICS LETTERS B LA English DT Review DE Electromagnetically induced transparency; decoherence; linewidth; buffer gas; wall-coated cell; Ramsey narrowing; Dicke narrowing; motional averaging; density narrowing ID ZEEMAN RESONANCE LINESHAPES; COHERENT MEDIA; BUFFER-GAS; ATOMIC ENSEMBLES; OPTICS; STATES; LIGHT; SPECTROSCOPY; DIFFUSION; CELLS AB Electromagnetically induced transparency (EIT) can make an otherwise opaque medium transparent by utilizing quantum coherence. EIT has attracted great interest since the 1990s for its wide applications in metrology, nonlinear and quantum optics, and quantum information science. We present a review on spectral line narrowing mechanisms in EIT-related systems, accounting for linewidths much narrower than expected from the standard mechanisms of Doppler broadening, transit time broadening, magnetic field inhomogeneity and power broadening. Topics covered include Dicke narrowing, atomic-motion-induced Ramsey narrowing, motional narrowing, density narrowing, laser induced narrowing and power-broadening-free resonance. Intuitive pictures are provided to describe the essential physics of each mechanism. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Xiao, YH (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,Mail Stop 59, Cambridge, MA 02138 USA. EM yxiao@cfa.harvard.edu NR 73 TC 9 Z9 9 U1 5 U2 29 PU WORLD SCIENTIFIC PUBL CO PTE LTD PI SINGAPORE PA 5 TOH TUCK LINK, SINGAPORE 596224, SINGAPORE SN 0217-9849 J9 MOD PHYS LETT B JI Mod. Phys. Lett. B PD FEB 20 PY 2009 VL 23 IS 5 BP 661 EP 680 PG 20 WC Physics, Applied; Physics, Condensed Matter; Physics, Mathematical SC Physics GA 418HI UT WOS:000264138900001 ER PT J AU Muller-Landau, HC AF Muller-Landau, Helene C. TI CARBON CYCLE Sink in the African jungle SO NATURE LA English DT Editorial Material ID TROPICAL FORESTS C1 [Muller-Landau, Helene C.] Smithsonian Trop Res Inst, Balboa, Panama. RP Muller-Landau, HC (reprint author), Smithsonian Trop Res Inst, Apartado Postal 0843-03092, Balboa, Panama. EM mullerh@si.edu NR 11 TC 24 Z9 28 U1 1 U2 10 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 19 PY 2009 VL 457 IS 7232 BP 969 EP 970 DI 10.1038/457969a PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 408HF UT WOS:000263425400028 PM 19225510 ER PT J AU Lewis, SL Lopez-Gonzalez, G Sonke, B Affum-Baffoe, K Baker, TR Ojo, LO Phillips, OL Reitsma, JM White, L Comiskey, JA Djuikouo, MN Ewango, CEN Feldpausch, TR Hamilton, AC Gloor, M Hart, T Hladik, A Lloyd, J Lovett, JC Makana, JR Malhi, Y Mbago, FM Ndangalasi, HJ Peacock, J Peh, KSH Sheil, D Sunderland, T Swaine, MD Taplin, J Taylor, D Thomas, SC Votere, R Woll, H AF Lewis, Simon L. Lopez-Gonzalez, Gabriela Sonke, Bonaventure Affum-Baffoe, Kofi Baker, Timothy R. Ojo, Lucas O. Phillips, Oliver L. Reitsma, Jan M. White, Lee Comiskey, James A. Djuikouo K., Marie-Noel Ewango, Corneille E. N. Feldpausch, Ted R. Hamilton, Alan C. Gloor, Manuel Hart, Terese Hladik, Annette Lloyd, Jon Lovett, Jon C. Makana, Jean-Remy Malhi, Yadvinder Mbago, Frank M. Ndangalasi, Henry J. Peacock, Julie Peh, Kelvin S. -H. Sheil, Douglas Sunderland, Terry Swaine, Michael D. Taplin, James Taylor, David Thomas, Sean C. Votere, Raymond Woell, Hannsjoerg TI Increasing carbon storage in intact African tropical forests SO NATURE LA English DT Article ID LONG-TERM PLOTS; ATMOSPHERIC TRANSPORT; RAIN-FOREST; CO2; CLIMATE; BIOMASS; DISTURBANCES; DIOXIDE; IMPACTS; BALANCE AB The response of terrestrial vegetation to a globally changing environment is central to predictions of future levels of atmospheric carbon dioxide(1,2). The role of tropical forests is critical because they are carbon- dense and highly productive(3,4). Inventory plots across Amazonia show that old- growth forests have increased in carbon storage over recent decades(5-7), but the response of one- third of the world's tropical forests in Africa(8) is largely unknown owing to an absence of spatially extensive observation networks(9,10). Here we report data from a ten- country network of long- term monitoring plots in African tropical forests. We find that across 79 plots ( 163 ha) above- ground carbon storage in live trees increased by 0.63 Mg C ha(-1) yr(-1) between 1968 and 2007 ( 95% confidence interval ( CI), 0.22 - 0.94; mean interval, 1987 - 96). Extrapolation to unmeasured forest components ( live roots, small trees, necromass) and scaling to the continent implies a total increase in carbon storage in African tropical forest trees of 0.34 Pg C yr(-1) ( CI, 0.15 - 0.43). These reported changes in carbon storage are similar to those reported for Amazonian forests per unit area(6,7), providing evidence that increasing carbon storage in old- growth forests is a pan- tropical phenomenon. Indeed, combining all standardized inventory data from this study and from tropical America and Asia(5,6,11) together yields a comparable figure of 0.49 Mg C ha(-1) yr(-1) (n = 156; 562 ha; CI, 0.29 - 0.66; mean interval, 1987 - 97). This indicates a carbon sink of 1.3 Pg C yr(-1) ( CI, 0.8 - 1.6) across all tropical forests during recent decades. Taxon- specific analyses of African inventory and other data(12) suggest that widespread changes in resource availability, such as increasing atmospheric carbon dioxide concentrations, may be the cause of the increase in carbon stocks(13), as some theory(14) and models(2,10,15) predict. C1 [Lewis, Simon L.; Lopez-Gonzalez, Gabriela; Baker, Timothy R.; Phillips, Oliver L.; Feldpausch, Ted R.; Gloor, Manuel; Lloyd, Jon; Peacock, Julie; Peh, Kelvin S. -H.] Univ Leeds, Earth & Biosphere Inst, Sch Geog, Leeds LS2 9JT, W Yorkshire, England. [Sonke, Bonaventure; Djuikouo K., Marie-Noel] Univ Yaounde I, Plant Systemat & Ecol Lab, Yaounde, Cameroon. [Affum-Baffoe, Kofi; Votere, Raymond] Forestry Commiss Ghana, Resource Management Support Ctr, Kumasi, Ghana. [Ojo, Lucas O.] Univ Agr, Dept Environm Management & Toxicol, Abeokuta, Ogun, Nigeria. [Reitsma, Jan M.] Bur Waardenburg BV, NL-4100 AJ Culemborg, Netherlands. [White, Lee] IRET, Libreville, Gabon. [Comiskey, James A.; Sunderland, Terry] Smithsonian Inst, SI MAB Biodivers Program, Washington, DC 20560 USA. [Ewango, Corneille E. N.] Univ Wageningen & Res Ctr, Dept Environm Sci, Forest Ecol & Management Grp, NL-6700 Wageningen, Netherlands. [Hamilton, Alan C.] Plantlife Int, Salisbury SP1 1DX, Wilts, England. [Hart, Terese; Makana, Jean-Remy] Wildlife Conservat Soc DRC, Kinshasa, Zaire. [Hladik, Annette] MNHN, Dept Hommes Nat Soc, F-91800 Brunoy, France. [Lovett, Jon C.; Taplin, James] Univ York, Dept Environm, Ctr Ecol Law & Policy, York YO10 5DD, N Yorkshire, England. [Malhi, Yadvinder] Univ Oxford, Environm Change Inst, Sch Geog & Environm, Oxford OX1 3QY, England. [Mbago, Frank M.; Ndangalasi, Henry J.] Univ Dar Es Salaam, Dept Bot, Dar Es Salaam, Tanzania. [Sheil, Douglas] Ctr Int Forestry Res, Bogor 16000, Indonesia. [Swaine, Michael D.] Univ Aberdeen, Dept Plant & Soil Sci, Sch Biol Sci, Aberdeen AB24 3UU, Scotland. [Taylor, David] Univ Dublin Trinity Coll, Sch Nat Sci, Dept Geog, Dublin 2, Ireland. [Thomas, Sean C.] Univ Toronto, Fac Forestry, Toronto, ON M5S 3B3, Canada. RP Lewis, SL (reprint author), Univ Leeds, Earth & Biosphere Inst, Sch Geog, Leeds LS2 9JT, W Yorkshire, England. EM s.l.lewis@leeds.ac.uk RI Lloyd, Jonathan/F-8893-2010; Mitchard, Edward/C-6346-2009; Thomas, Sean/B-6089-2008; Sheil, Douglas/H-1466-2012; Peh, Kelvin/C-3408-2013; Feldpausch, Ted/D-3436-2009; Phillips, Oliver/A-1523-2011; Sheil, Douglas/A-3867-2015 OI Lewis, Simon/0000-0002-8066-6851; Lloyd, Jonathan/0000-0002-5458-9960; Peh, Kelvin/0000-0002-2921-1341; Feldpausch, Ted/0000-0002-6631-7962; Phillips, Oliver/0000-0002-8993-6168; Sheil, Douglas/0000-0002-1166-6591 FU Royal Society and the Natural Environment Research Council (UK) FX We thank the villagers from Oban (Nigeria), Prince Town, Baneekurom and Dadieso (Ghana), Somolomo, Mekas, Lomie and Alat Makay (Cameroon) and Ekobakoba (Gabon) for hosting our fieldwork, and A. Moungazi, S. Mbadinga, H. Bourobou, L. N. Banak, T. Nzebi, K. Jeffery, SEGC/CIRMF/WCS Research Station Lope, K. Ntim, K. Opoku, Forestry Commission of Ghana, T. Tafoek, Federal University of Agriculture, Abeokuta, Nigeria, ECOFAC- Cameroon, Cameroon Ministry Scientific Research and Innovation, Cameroon Ministry of Forests and Fauna (MINFOF), Forest Development Authority (Liberia), S. Grahame, R. Lowe, L. Banin and K. C. Nguembou for field assistance and logistical support. We thank R. Condit for helping access the Edoro and Lenda data sets, C. Chatelain for providing data from the African Flowering Plants database to standardize our species identifications, J. Chave for providing allometric data, L. Poorter for providing gap size- frequency data, B. Nelson for providing large- scale blow- down data, D. Appleyard for assistance with the plot map, and the Network for Vegetation Function (Nation Evolutionary Synthesis Center and ARC-NZ) for providing some wood mass density data. This work was supported by the Royal Society and the Natural Environment Research Council ( UK). NR 30 TC 376 Z9 398 U1 23 U2 211 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD FEB 19 PY 2009 VL 457 IS 7232 BP 1003 EP U3 DI 10.1038/nature07771 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 408HF UT WOS:000263425400040 PM 19225523 ER PT J AU Hirsch, BT AF Hirsch, Ben T. TI SEASONAL VARIATION IN THE DIET OF RING-TAILED COATIS (NASUA NASUA) IN IGUAZU, ARGENTINA SO JOURNAL OF MAMMALOGY LA English DT Article DE coati; fallback foods; foraging behavior; fruit depletion; Procyonidae; socioecology ID FEMALE SOCIAL RELATIONSHIPS; CEBUS-APELLA; HOME-RANGE; SOUTHEASTERN BRAZIL; PRIMATES; FOREST; MODEL; COMPETITION; AGGRESSION; EVOLUTION AB There is widespread evidence that feeding ecology can lead to differences in mammalian social systems. To understand how diet and ecology affect the social behavior of ring-tailed coatis (Nasua nasua), detailed measures of feeding behavior were recorded from 2 well-studied groups over a 2-year period. The proportion of fruit and invertebrates in the diet of ring-tailed coatis in Iguazu, Argentina, was very similar to that in diets of white-nosed coatis (N. narica) and ring-tailed coatis studied at field sites in Brazil. Consumption of vertebrates in Iguazu was exceptionally rare. The proportion of time spent foraging for invertebrates and fruit generally matched seasonal changes in the abundance these foods in the environment. During the winter, when invertebrate and fruit availability was low, coatis spent it large amount of time feeding on 2 exotic fruit species. The presence of exotic fruits provided coatis with food during the lean winter season and may have influenced the high reproduction and survivorship found in this Population. Coatis spent about 44% of-their fruit-foraging time exploiting pindo palm (Syagrus romanzoffianum) fruits and it appeared that this fruit species played a major role in shaping the ranging and feeding, behavior of coati groups. The time spent foraging at fruit trees and the total number of fruits eaten varied depending oil the species of tree. Coati groups spent an average of 2.5-12.5 min feeding oil different species of fruit trees, and coati groups ate an average of 2.6-269.8 fruits per tree species. The quick depletion of fruit trees and high density of foraging individuals, especially when feeding oil pindo, plays an important role in shaping the social system of coatis. C1 [Hirsch, Ben T.] Smithsonian Inst, Natl Museum Nat Hist, Natl Zool Pk, Ctr Conservat & Evolutionary Genet, Washington, DC 20008 USA. RP Hirsch, BT (reprint author), Smithsonian Trop Res Inst, APO, AA 34002 USA. EM hirschb@si.edu FU National Science Foundation [BCS-0314525] FX I thank Y. Di Blanco, S. Escobar, C. Ferrari, F. Silva, and M. Tammone for help and assistance with the fieldwork. I also thank V. Mufioz for her veterinary assistance. I am partiCUlarly grateful to C. Janson for the immeasurable amount ofadvice he gave me during all aspects of this project, and letting me borrow several pieces of much needed field equipment. I also am very thankful for the consistently helpful comments and advice from M. Di Bitetti. This paper has benefited tremendously thanks to comments by M. Gompper, C. Janson, A. Koenig, A. Pokempner, D. Doran-Sheehy, and 2 anonymous reviewers. I thank the Administration de Parques Nacionales for permission to carry out work in Iguazu. This study was funded in part by a National Science Foundation grant (BCS-0314525). NR 30 TC 19 Z9 20 U1 8 U2 51 PU ALLIANCE COMMUNICATIONS GROUP DIVISION ALLEN PRESS PI LAWRENCE PA 810 EAST 10TH STREET, LAWRENCE, KS 66044 USA SN 0022-2372 J9 J MAMMAL JI J. Mammal. PD FEB 18 PY 2009 VL 90 IS 1 BP 136 EP 143 DI 10.1644/08-MAMM-A-050.1 PG 8 WC Zoology SC Zoology GA 413QF UT WOS:000263806900015 ER PT J AU Strait, DS Weber, GW Neubauer, S Chalk, J Richmond, BG Lucas, PW Spencer, MA Schrein, C Dechow, PC Ross, CF Grosse, IR Wright, BW Constantino, P Wood, BA Lawn, B Hylander, WL Wang, Q Byron, C Slice, DE Smith, AL AF Strait, David S. Weber, Gerhard W. Neubauer, Simon Chalk, Janine Richmond, Brian G. Lucas, Peter W. Spencer, Mark A. Schrein, Caitlin Dechow, Paul C. Ross, Callum F. Grosse, Ian R. Wright, Barth W. Constantino, Paul Wood, Bernard A. Lawn, Brian Hylander, William L. Wang, Qian Byron, Craig Slice, Dennis E. Smith, Amanda L. TI The feeding biomechanics and dietary ecology of Australopithecus africanus SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE evolution; face; finite element analysis; hominin; diet ID FINITE-ELEMENT-ANALYSIS; ELASTIC PROPERTIES; ISOTOPIC EVIDENCE; DENTAL MICROWEAR; CORTICAL BONE; SOUTH-AFRICA; EVOLUTION; PARANTHROPUS; HYPOTHESES; HOMININS AB The African Plio-Pleistocene hominins known as australopiths evolved a distinctive craniofacial morphology that traditionally has been viewed as a dietary adaptation for feeding on either small, hard objects or on large volumes of food. A historically influential interpretation of this morphology hypothesizes that loads applied to the premolars during feeding had a profound influence on the evolution of australopith craniofacial form. Here, we test this hypothesis using finite element analysis in conjunction with comparative, imaging, and experimental methods. We find that the facial skeleton of the Australopithecus type species, A. africanus, is well suited to withstand premolar loads. However, we suggest that the mastication of either small objects or large volumes of food is unlikely to fully explain the evolution of facial form in this species. Rather, key aspects of australopith craniofacial morphology are more likely to be related to the ingestion and initial preparation of large, mechanically protected food objects like large nuts and seeds. These foods may have broadened the diet of these hominins, possibly by being critical resources that australopiths relied on during periods when their preferred dietary items were in short supply. Our analysis reconciles apparent discrepancies between dietary reconstructions based on biomechanics, tooth morphology, and dental microwear. C1 [Strait, David S.; Smith, Amanda L.] SUNY Albany, Dept Anthropol, Albany, NY 12222 USA. [Weber, Gerhard W.; Neubauer, Simon; Slice, Dennis E.] Univ Vienna, Dept Anthropol, A-1090 Vienna, Austria. [Neubauer, Simon] Max Planck Inst Evolutionary Anthropol, Dept Human Evolut, D-04103 Leipzig, Germany. [Chalk, Janine; Richmond, Brian G.; Lucas, Peter W.; Constantino, Paul; Wood, Bernard A.] George Washington Univ, Dept Anthropol, Ctr Adv Study Hominid Paleobiol, Washington, DC 20052 USA. [Richmond, Brian G.; Wood, Bernard A.] Smithsonian Inst, Human Origins Program, Natl Museum Nat Hist, Washington, DC 20560 USA. [Spencer, Mark A.; Schrein, Caitlin] Arizona State Univ, Inst Human Origins, Sch Human Evolut & Social Change, Tempe, AZ 85287 USA. [Dechow, Paul C.] Baylor Coll Dent, Dept Biomed Sci, Texas A&M Hlth Sci Ctr, Dallas, TX 75246 USA. [Ross, Callum F.] Univ Chicago, Dept Organismal Biol & Anat, Chicago, IL 60637 USA. [Grosse, Ian R.] Univ Massachusetts, Dept Mech & Ind Engn, Amherst, MA 01003 USA. [Wright, Barth W.] Kansas City Univ Med & Biosci, Dept Anat, Kansas City, MO 64106 USA. [Lawn, Brian] NIST, Gaithersburg, MD 20899 USA. [Hylander, William L.] Duke Univ, Dept Biol Anthropol & Anat, Durham, NC 27708 USA. [Wang, Qian] Mercer Univ, Sch Med, Div Basic Med Sci, Macon, GA 31207 USA. [Byron, Craig] Mercer Univ, Dept Biol, Macon, GA 31207 USA. [Slice, Dennis E.] Florida State Univ, Dept Comp Sci, Dirac Sci Lib, Tallahassee, FL 32306 USA. RP Strait, DS (reprint author), SUNY Albany, Dept Anthropol, 1400 Washington Ave, Albany, NY 12222 USA. EM dstrait@albany.edu RI Weber, Gerhard/F-2583-2010; Neubauer, Simon/D-1317-2010 OI Neubauer, Simon/0000-0001-9113-5063 FU National Science Foundation(NSF) [0725219, 0725183, 0725147, 0725141, 0725136, 0725126, 0725122, 0725078]; European Union FP6 Marie Curie Actions [MRTN-CT-2005-019564] FX We thank Francis Thackeray and Stephanie Potze from the Transvaal Museum, Northern Flagship Institution, Pretoria, South Africa, for access to fossils and the staff of Selby Clark Clinic, Johannesburg, South Africa, and the Little Company of Mary Hospital, Pretoria, South Africa, for the scanning of specimens. We also thank Gary Schwartz, Peter Ungar, and Frederick Grine for constructive discussions about enamel thickness, dental microwear, and diet. This project was funded by grants from the National Science Foundation Physical Anthropology HOMINID program (NSF BCS 0725219, 0725183, 0725147, 0725141, 0725136, 0725126, 0725122, 0725078) and the European Union FP6 Marie Curie Actions MRTN-CT-2005-019564 "EVAN.'' NR 47 TC 125 Z9 126 U1 6 U2 40 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 2009 VL 106 IS 7 BP 2124 EP 2129 DI 10.1073/pnas.0808730106 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 409OQ UT WOS:000263516100011 PM 19188607 ER PT J AU Caldwell, MS McDaniel, JG Warkentin, KM AF Caldwell, Michael S. McDaniel, J. Gregory Warkentin, Karen M. TI Frequency information in the vibration-cued escape hatching of red-eyed treefrogs SO JOURNAL OF EXPERIMENTAL BIOLOGY LA English DT Article DE frequency; cue; decision rule; predator detection; discrimination; Agalychnis; embryo ID SENSITIVE PREDATOR-AVOIDANCE; CUPIENNIUS-SALEI KEYS; WANDERING SPIDER; SIGNALS; RISK; COMMUNICATION; BEHAVIOR; THREAT; LEAFMINER; CRICKETS AB Incidental acoustic and vibrational cues generated by predators are a potential source of information for prey assessing risk. Substrate vibrations should be excited by most predators, and frequency, amplitude or temporal properties could allow prey to distinguish predator from benign-source vibrations. Red-eyed treefrog embryos detect egg predators using vibrations excited during attacks, hatching rapidly and prematurely to escape. We recorded vibrations in egg clutches during attacks by five species of predators and three common types of benign physical disturbance. We analyzed their frequency distributions to assess if and how frequency properties could be used to discriminate between vibration sources and used vibration playbacks to examine the effects of frequency properties on the escape hatching response. Vibrations produced by predators and benign disturbances generally have broad and overlapping frequency distributions, and all frequencies excited by attacks are also excited by benign disturbances. Decision rules based on the frequency distribution of vibrations alone would therefore result in either high levels of hatching in response to benign vibrations (false alarms) or common failures to hatch in response to predators (missed cues). Nevertheless, embryos hatch in response to predator and not benign disturbances in nature, and our playback results show that vibration frequency information is an important component of their hatching decision. Embryos combine frequency with temporal information to refine their hatching response. Moreover, comparing frequency spectra of predator and benign vibrations suggests that the presence of energy in frequencies outside the range characteristic of attacks might serve as an indicator of benign disturbance. C1 [Caldwell, Michael S.; Warkentin, Karen M.] Boston Univ, Dept Biol, Boston, MA 02215 USA. [McDaniel, J. Gregory] Boston Univ, Dept Mech Engn, Boston, MA 02215 USA. [Warkentin, Karen M.] Smithsonian Trop Res Inst, Balboa, Panama. RP Caldwell, MS (reprint author), Boston Univ, Dept Biol, Boston, MA 02215 USA. EM mpod3@bu.edu FU National Science Foundation [IBN-0234439, IOS-0710247]; Boston University; Smithsonian Tropical Research Institute FX We thank M. Hughey, T. Siok, S. Poo and S. Galeano for assistance with recordings and playback experiments, G. Rosenthal for comments on the manuscript, and M. Ryan for advice. This research was funded by the National Science Foundation (IBN-0234439 and IOS-0710247), Boston University and the Smithsonian Tropical Research Institute. NR 60 TC 11 Z9 11 U1 2 U2 13 PU COMPANY OF BIOLOGISTS LTD PI CAMBRIDGE PA BIDDER BUILDING CAMBRIDGE COMMERCIAL PARK COWLEY RD, CAMBRIDGE CB4 4DL, CAMBS, ENGLAND SN 0022-0949 J9 J EXP BIOL JI J. Exp. Biol. PD FEB 15 PY 2009 VL 212 IS 4 BP 566 EP 575 DI 10.1242/jeb.026518 PG 10 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 402RU UT WOS:000263031600021 PM 19181904 ER PT J AU Chakravorty, S Kembhavi, AK Elvis, M Ferland, G AF Chakravorty, Susmita Kembhavi, Ajit K. Elvis, Martin Ferland, Gary TI Properties of warm absorbers in active galaxies: a systematic stability curve analysis SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE ISM: abundances; galaxies: active; quasars: absorption lines; galaxies: Seyfert; X-rays: ISM ID DIELECTRONIC RECOMBINATION DATA; FINITE-DENSITY PLASMAS; SOFT-X-RAY; XMM-NEWTON OBSERVATIONS; ISOELECTRONIC SEQUENCE; GALACTIC NUCLEI; THERMAL-INSTABILITY; IONIZED ABSORBERS; RATE COEFFICIENTS; ABSORPTION-LINES AB Signatures of warm absorbers are seen in soft X-ray spectra of about half of all type 1 Seyfert galaxies observed and in some quasars and blazars. We use the thermal equilibrium curve to study the influence of the shape of the ionizing continuum, density and the chemical composition of the absorbing gas on the existence and nature of the warm absorbers. We describe circumstances in which a stable warm absorber can exist as a multiphase medium or one with continuous variation in pressure. In particular, we find the following results: (i) the warm absorber exists only if the spectral index of the X-ray power-law ionizing continuum alpha > 0.2 and has a multiphase nature if alpha similar to 0.8, which interestingly is the spectral index for most of the observed type 1 Seyfert galaxies; (ii) thermal and ionization states of highly dense warm absorbers are sensitive to their density if the ionizing continuum is sufficiently soft, i. e. dominated by the ultraviolet; (iii) absorbing gas with super-solar metallicity is more likely to have a multiphase nature and (iv) the nature of the warm absorber is significantly influenced by the absence of iron and associated elements which are produced in the later stages of star formation history in Type Ia supernovae. C1 [Chakravorty, Susmita; Kembhavi, Ajit K.] IUCAA, Pune 411007, Maharashtra, India. [Elvis, Martin] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ferland, Gary] Univ Kentucky, Dept Phys & Astron, Lexington, KY 40506 USA. RP Chakravorty, S (reprint author), IUCAA, Post Bag 4, Pune 411007, Maharashtra, India. EM susmita@iucaa.ernet.in; akk@iucaa.ernet.in; elvis@head.cfa.harvard.edu; gary@pa.uky.edu OI Ferland, Gary/0000-0003-4503-6333 NR 74 TC 23 Z9 23 U1 1 U2 1 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB 11 PY 2009 VL 393 IS 1 BP 83 EP 98 DI 10.1111/j.1365-2966.2008.14249.x PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 399EF UT WOS:000262782500021 ER PT J AU Pont, F Gilliland, RL Knutson, H Holman, M Charbonneau, D AF Pont, F. Gilliland, R. L. Knutson, H. Holman, M. Charbonneau, D. TI Transit infrared spectroscopy of the hot Neptune around GJ 436 with the Hubble Space Telescope SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE planetary systems ID M-DWARF GJ-436; EXTRASOLAR PLANET; TIDAL DISSIPATION; MASS PLANET; LIGHT-CURVE; ATMOSPHERE AB The nearby transiting system GJ 436b offers a unique opportunity to probe the structure and atmosphere of an extrasolar 'hot Neptune'. In this Letter, we present the main results of observations covering two transit events with the Near Infrared Camera and Multi Object Spectrograph ( NICMOS) camera on the Hubble Space Telescope ( HST). The data consist in high-cadence time series of grism spectra covering the 1.1-1.9 mu m spectral range. We find R(pl) = 4.04 +/- 0.10 R(circle plus) and R* = 0.446 +/- 0.011 R(circle dot) for the planet and star radius, confirming and improving earlier measurements with a ground-based photometry and a Spitzer light curve at 8 mu m, as opposed to a much higher value obtained with the Fine Guidance Sensor on the HST. We measure no departure from strict periodicity in the transits to the level of similar to 7 s. This strongly disfavours the proposed explanation of the orbital eccentricity of GJ 436b in terms of the perturbation by another close-by planet. We measure a flat transmission spectrum at the level of a few parts per 10 000 in flux, with no significant signal in the 1.4-mu m water band to a level comparable to the maximum amplitude of the effect predicted by planetary atmosphere models. C1 [Pont, F.] Univ Exeter, Exeter EX4 4QJ, Devon, England. [Gilliland, R. L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Knutson, H.; Holman, M.; Charbonneau, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Pont, F (reprint author), Univ Exeter, Queens Dr, Exeter EX4 4QJ, Devon, England. EM fpont@astro.ex.ac.uk NR 26 TC 44 Z9 44 U1 0 U2 2 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB 11 PY 2009 VL 393 IS 1 BP L6 EP L10 DI 10.1111/j.1745-3933.2008.00582.x PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 399EF UT WOS:000262782500002 ER PT J AU Risaliti, G Salvati, M Elvis, M Fabbiano, G Baldi, A Bianchi, S Braito, V Guainazzi, M Matt, G Miniutti, G Reeves, J Soria, R Zezas, A AF Risaliti, G. Salvati, M. Elvis, M. Fabbiano, G. Baldi, A. Bianchi, S. Braito, V. Guainazzi, M. Matt, G. Miniutti, G. Reeves, J. Soria, R. Zezas, A. TI The XMM-Newton long look of NGC 1365: uncovering of the obscured X-ray source SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: individual: NGC 1365 ID ACTIVE GALACTIC NUCLEI; BLACK-HOLES; LUMINOSITY; GALAXIES; NGC-1365; LINES AB We present an analysis of the extreme obscuration variability observed during an XMM-Newton 5-d continuous monitoring of the active galactic nuclei (AGN) in NGC 1365. The source was in a reflection-dominated state in the first similar to 1.5 d, then a strong increase in the 7-10 keV emission was observed in similar to 10 h, followed by a symmetric decrease. The spectral analysis of the different states clearly shows that this variation is due to an uncovering of the X-ray source. From this observation, we estimate a size of the X-ray source D(S) < 10(13) cm, a distance of the obscuring clouds R similar to 10(16) cm and a density n similar to 10(11) cm(-3). These values suggest that the X-ray absorption/reflection originates from the broad-line region clouds. This is also supported by the resolved width of the iron narrow K alpha emission line, consistent with the width of the broad H beta line. C1 [Risaliti, G.; Elvis, M.; Fabbiano, G.; Baldi, A.; Zezas, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Risaliti, G.; Salvati, M.] INAF Osservatorio Arcetri, Florence, Italy. [Bianchi, S.; Matt, G.] Univ Roma Tre, Dipartimento Fis, I-00146 Rome, Italy. [Reeves, J.] Univ Keele, Astrophys Grp, Sch Phys & Geog Sci, Keele ST5 5BG, Staffs, England. [Guainazzi, M.] ESA, European Space Astron Ctr, E-28080 Madrid, Spain. [Miniutti, G.] Lab Astroparticule & Cosmol APC, UMR 7164, F-75205 Paris, France. [Soria, R.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Braito, V.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Braito, V.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. RP Risaliti, G (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM grisaliti@cfa.harvard.edu RI Bianchi, Stefano/B-4804-2010; Miniutti, Giovanni/L-2721-2014; Zezas, Andreas/C-7543-2011; OI Bianchi, Stefano/0000-0002-4622-4240; Miniutti, Giovanni/0000-0003-0707-4531; Zezas, Andreas/0000-0001-8952-676X; Risaliti, Guido/0000-0002-3556-977X; Braito, Valentina/0000-0002-2629-4989 FU NASA [NNX07AR90G] FX We are grateful to the anonymous referee for his/her helpful comments. This work has been funded by NASA Grant NNX07AR90G. NR 19 TC 78 Z9 78 U1 0 U2 0 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB 11 PY 2009 VL 393 IS 1 BP L1 EP L5 DI 10.1111/j.1745-3933.2008.00580.x PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 399EF UT WOS:000262782500001 ER PT J AU Baldwin, CC Mounts, JH Smith, DG Weigt, LA AF Baldwin, Carole C. Mounts, Julie H. Smith, David G. Weigt, Lee A. TI Genetic identification and color descriptions of early life-history stages of Belizean Phaeoptyx and Astrapogon (Teleostei: Apogonidae) with Comments on identification of adult Phaeoptyx SO ZOOTAXA LA English DT Article DE DNA Barcoding; fish larvae; chromatophores; Belize ID ATLANTIC AB Phaeoptyx and Astrapogon are represented in the Caribbean by six species (P. conklini, P. pigmentaria, P. xenus, A. alutus, A. stellatus, and A. puncticulatus). Species identification of larvae and juveniles is problematic because characters used to distinguish adults (e. g., patterns of pigmentation and numbers of gill rakers) are absent, incomplete, or difficult to discern in the young stages. Neighbor-joining trees derived from mitochondrial cytochrome oxidase 1 sequences (DNA Barcoding) were used to match early life stages and adults. Subsequent comparative analysis of preserved voucher specimens from which the DNA was extracted or digital color photographs of those specimens taken prior to preservation yielded sufficient information to separate all early life-history stages of Belizean Phaeoptyx and Astrapogon and provided additional information for field identification of adult Phaeoptyx. Patterns of chromatophores in fresh material, combined with patterns of melanophores, provide the easiest means of separating the life-history stages of Phaeoptyx. Larvae of Astrapogon species are morphologically very similar, and some differences in pigmentation detected among them may reflect different stages of development. Continued implementation of the DNA Barcoding methods and field protocol outlined herein should prove valuable in accurately identifying much more of the ichthyoplankton fauna of the Caribbean. C1 [Baldwin, Carole C.; Mounts, Julie H.; Smith, David G.; Weigt, Lee A.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Baldwin, CC (reprint author), Smithsonian Inst, Natl Museum Nat Hist, POB 37012, Washington, DC 20013 USA. EM baldwinc@si.edu; mountsj@si.edu; smithd@si.edu; weigtl@si.edu FU Caribbean Coral Reef Ecosystems Program (CCRE); Smithsonian Marine Science Network; National Museum of Natural History Small-Grants Program FX We thank A. Driskell, J. Hunt, A. Ormos, K. Shallop, and A. Clack for their work on the DNA Barcoding of our Belizean fishes; M. Carpenter, A. Driskell, C. DeCourley, D. Miller, and R. Murphy for assistance in the field; and K. Ruetzler, the Caribbean Coral Reef Ecosystems Program (CCRE), the Smithsonian Marine Science Network, and the National Museum of Natural History Small-Grants Program for financial support. This is CCRE contribution no. 824. NR 13 TC 33 Z9 33 U1 0 U2 1 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD FEB 11 PY 2009 IS 2008 BP 1 EP 22 PG 22 WC Zoology SC Zoology GA 406WX UT WOS:000263326700001 ER PT J AU Imamura, H Knapp, LW AF Imamura, Hisashi Knapp, Leslie W. TI A new species of the flathead genus Onigocia (Teleostei: Platycephalidae) collected from the Coral and Tasman Seas SO ZOOTAXA LA English DT Article DE Onigocia lacrimalis sp nov.; Platycephalidae; Coral Sea; Tasman Sea ID GRANDISQUAMA REGAN AB A new species of platycephalid, Onigocia lacrimalis, is described on the basis of specimens collected from the Chesterfield Islands (Coral Sea) and Norfolk Ridge (Tasman Sea), at depths of 111-330 m. Onigocia lacrimalis differs from the six congeners of the genus in having 12-13 (usually 12) second dorsal-fin rays, 12 anal-fin rays, 21-25 pectoral-fin rays, 8 branched caudal-fin rays, anterior 2-4 scales of the lateral line with a spine, and a single preocular spine, and in lacking gill rakers on the upper arch, ocular and interopercular flaps, and distinct antrorse lachrymal spines. C1 [Imamura, Hisashi] Hokkaido Univ Museum, Fisheries Sci Ctr, Hakodate, Hokkaido 0418611, Japan. [Knapp, Leslie W.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA. RP Imamura, H (reprint author), Hokkaido Univ Museum, Fisheries Sci Ctr, 3-1-1 Minato Cho, Hakodate, Hokkaido 0418611, Japan. EM imamura@museum.hokudai.ac.jp; knappl@si.edu NR 12 TC 2 Z9 5 U1 0 U2 0 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD FEB 11 PY 2009 IS 2008 BP 23 EP 28 PG 6 WC Zoology SC Zoology GA 406WX UT WOS:000263326700002 ER PT J AU Menten, KM Wilson, RW Leurini, S Schilke, P AF Menten, Karl M. Wilson, Robert W. Leurini, Silvia Schilke, Peter TI MOLECULES IN G1.6-0.025-"HOT" CHEMISTRY IN THE ABSENCE OF STAR FORMATION AT THE PERIPHERY OF THE GALACTIC CENTER REGION SO ASTROPHYSICAL JOURNAL LA English DT Article DE Galaxy: center; ISM: clouds; ISM: molecules; radio lines: ISM ID 1720 MHZ MASERS; H-II REGIONS; METHANOL MASERS; INTERSTELLAR CLOUDS; MASSIVE STARS; OH; SAGITTARIUS; ABSORPTION; EMISSION; AMMONIA AB We present molecular line mapping of the Giant Molecular Cloud G1.6-0.025, which is located at the high-longitude end of the Central Molecular Zone (CMZ) of our Galaxy. We assess the degree of star formation activity in that region using several tracers, and find very little. We made a large-scale, medium (2') resolution map in the J = 2-1 transition of SiO for which we find clumpy emission over a similar to 0 degrees.8 x 0 degrees.3 sized region stretching along the Galactic plane. Toward selected positions we also took spectra in the easy-to-excite J(k) = 2(k) - 1(k) quartet of CH(3)OH and the carbon monosulfide (CS) 2-1 line. Throughout the cloud these CH(3)OH lines are, remarkably, several times stronger than both the CS and the SiO lines. The large widths of all the observed lines, similar to values generally found in the Galactic center, indicate a high degree of turbulence. Several high LSR velocity clumps that have 50-80 km s(-1) higher velocities than the bulk of the molecular cloud appear at the same projected position as "normal" velocity material; this may indicate cloud-cloud collisions. Statistical equilibrium modeling of the CH(3)OH lines observed by us and others yields relatively high densities and moderate temperatures for a representative dual velocity position. We find 8 x 10(4) cm(-3)/30K for material in the G1.6-0.025 cloud and a higher temperature (190 K), but a 50% lower density in a high-velocity clump projected on the same location. Several scenarios are discussed in which shock chemistry might enhance the CH(3)OH and SiO abundances in G1.6-0.025 and elsewhere in the CMZ. C1 [Menten, Karl M.; Schilke, Peter] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Wilson, Robert W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Leurini, Silvia] European So Observ, D-85748 Garching, Germany. RP Menten, KM (reprint author), Max Planck Inst Radioastron, D-53121 Bonn, Germany. EM kmenten@mpifr-bonn.mpg.de; rwilson@cfa.harvard.edu; sleurini@eso.org; pschilke@mpifr-bonn.mpg.de NR 75 TC 10 Z9 10 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2009 VL 692 IS 1 BP 47 EP 60 DI 10.1088/0004-637X/692/1/47 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 410CG UT WOS:000263553000004 ER PT J AU Homan, J Kaplan, DL van den Berg, M Young, AJ AF Homan, Jeroen Kaplan, David L. van den Berg, Maureen Young, Andrew J. TI A VARIABLE NEAR-INFRARED COUNTERPART TO THE NEUTRON-STAR LOW-MASS X-RAY BINARY 4U 1705-440 SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; binaries: close; stars: individual (4U 1705-440); X-rays: stars ID TIMING-EXPLORER; SPECTRAL BEHAVIOR; 2002 OUTBURST; 2 PATTERNS; 4U-1705-44; EMISSION; JET; EXTINCTION; PHOTOMETRY; LIGHT AB We report the discovery of a near-infrared (NIR) counterpart to the persistent neutron-star low-mass X-ray binary 4U 1705-440, at a location consistent with its recently determined Chandra X-ray position. The NIR source is highly variable, with K(s)-band magnitudes varying between 15.2 and 17.3 and additional J- and H- band observations revealing color variations. A comparison with contemporaneous X-ray monitoring observations shows that the NIR brightness correlates well with X-ray flux and X-ray spectral state. We also find possible indications of a change in the slope of the NIR/X-ray flux relation among different X-ray states. We discuss and test various proposed mechanisms for the NIR emission from neutron-star low-mass X-ray binaries and conclude that the NIR emission in 4U 1705-440 is most likely dominated by X-ray heating of the outer accretion disk and the secondary star. C1 [Homan, Jeroen; Kaplan, David L.] MIT Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [van den Berg, Maureen] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Young, Andrew J.] Univ Bristol, Dept Phys, Astrophys Grp, Bristol BS8 1TL, Avon, England. RP Homan, J (reprint author), MIT Kavli Inst Astrophys & Space Res, 70 Vassar St, Cambridge, MA 02139 USA. EM jeroen@space.mit.edu; dkaplan@kitp.ucsb.edu; maureen@head.cfa.harvard.edu; andy.young@bristol.ac.uk FU NASA [01207.01-A]; Space Telescope Science Institute [NAS 5-26555] FX We thank the numerous observers who have helped us obtain data: F. Baganoff, J. A. Blackburne, A. Burgasser, H.W. Chen, D. Erb, S. Laycock, S. Rappaport, P. Schechter, and M. Torres. Partial support for DLK was provided by NASA through Hubble Fellowship grant #01207.01-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. PyRAF is a product of the Space Telescope Science Institute, which is operated by AURA for NASA. This research has made use of data obtained from the High Energy Astrophysics Science Archive Research Center (HEASARC), provided by NASA's Goddard Space Flight Center. NR 39 TC 10 Z9 10 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2009 VL 692 IS 1 BP 73 EP 80 DI 10.1088/0004-637X/692/1/73 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 410CG UT WOS:000263553000006 ER PT J AU Goodman, AA Pineda, JE Schnee, SL AF Goodman, Alyssa A. Pineda, Jaime E. Schnee, Scott L. TI THE "TRUE" COLUMN DENSITY DISTRIBUTION IN STAR-FORMING MOLECULAR CLOUDS SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; ISM: abundances; ISM: individual (Perseus molecular complex); ISM: molecules ID DARK CLOUDS; INTERSTELLAR DUST; EMISSION MAPS; SUPERSONIC TURBULENCE; MAGNETIC-FIELD; PIPE NEBULA; IC 5146; EXTINCTION; PERSEUS; CORE AB We use the COMPLETE Survey's observations of the Perseus star-forming region to assess and intercompare the three methods used for measuring column density in molecular clouds: near-infrared (NIR) extinction mapping; thermal emission mapping in the far-IR; and mapping the intensity of CO isotopologues. Overall, the structures shown by all three tracers are morphologically similar, but important differences exist among the tracers. We find that the dust-based measures (NIR extinction and thermal emission) give similar, log-normal, distributions for the full (similar to 20 pc scale) Perseus region, once careful calibration corrections are made. We also compare dust-and gas-based column density distributions for physically meaningful subregions of Perseus, and we find significant variations in the distributions for those (smaller, similar to few pc scale) regions. Even though we have used (12)CO data to estimate excitation temperatures, and we have corrected for opacity, the (13)CO maps seem unable to give column distributions that consistently resemble those from dust measures. We have edited out the effects of the shell around the B-star HD 278942 from the column density distribution comparisons. In that shell's interior and in the parts where it overlaps the molecular cloud, there appears to be a dearth of (13)CO, which is likely due either to (13)CO not yet having had time to form in this young structure and/or destruction of (13)CO in the molecular cloud by the HD 278942's wind and/or radiation. We conclude that the use of either dust or gas measures of column density without extreme attention to calibration (e. g., of thermal emission zero-levels) and artifacts (e. g., the shell) is more perilous than even experts might normally admit. And, the use of (13)CO data to trace total column density in detail, even after proper calibration, is unavoidably limited in utility due to threshold, depletion, and opacity effects. If one's main aim is to map column density (rather than temperature or kinematics), then dust extinction seems the best probe, up to a limiting extinction caused by a dearth of sufficient background sources. Linear fits among all three tracers' estimates of column density are given, allowing us to quantify the inherent uncertainties in using one tracer, in comparison with the others. C1 [Goodman, Alyssa A.; Pineda, Jaime E.; Schnee, Scott L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Schnee, Scott L.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. RP Goodman, AA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-42, Cambridge, MA 02138 USA. EM agoodman@cfa.harvard.edu; jpineda@cfa.harvard.edu; schnee@phobos.caltech.edu RI Pineda, Jaime/J-7405-2013; Goodman, Alyssa/A-6007-2010 OI Pineda, Jaime/0000-0002-3972-1978; Goodman, Alyssa/0000-0003-1312-0477 FU Association of Universities for Research in Astronomy, Inc [AST-9613615]; Fundacion Andes [C-13442]; National Science Foundation [AST-0407172, AF002, AST 05-40399] FX This paper was originally inspired by a workshop at the Aspen Center for Physics in the Summer of 2004 on "Star Formation in Galaxies," where it seemed that the assembled audience of experts could not agree on the least biased way to measure the " initial conditions" for stars to form from molecular gas. A conversation with Eve Ostriker at that meeting, about how observations and simulations of star-forming molecular gas might best be compared, was particularly important. The quest to offer the most bias- and error-free column density distributions we could publish based on the COMPLETE data in this paper took nearly four years, and it spawned several other papers by our group (Schnee et al. 2006, 2008; Ridge et al. 2006a; Pineda et al. 2008; Foster et al. 2008) The "2007" version of these distributions and their implications were discussed intensively at the KITP Santa Barbara Workshop on " Star Formation Near and Far," and we deeply thank Eve Ostriker, Paolo Padoan and Enrique Vazquez-Semadeni for their comments both at and since that meeting. We thank Joao Alves, Michelle Borkin, Paola Caselli, Jonathan Foster, Jens Kauffmann, Di Li, Marco Lombardi, and Naomi Ridge for their important contributions to the data and results presented in this work. This material is based upon work supported by the National Science Foundation under Grant No. AST-0407172. JEP is supported by the National Science Foundation through grant #AF002 from the Association of Universities for Research in Astronomy, Inc., under NSF cooperative agreement AST-9613615 and by Fundacion Andes under project No. C-13442. Scott Schnee acknowledges support from the Owens Valley Radio Observatory, which is supported by the National Science Foundation through grant AST 05-40399. NR 43 TC 94 Z9 95 U1 1 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2009 VL 692 IS 1 BP 91 EP 103 DI 10.1088/0004-637X/692/1/91 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 410CG UT WOS:000263553000008 ER PT J AU Rodriguez, LF Zapata, LA Ho, PTP AF Rodriguez, Luis F. Zapata, Luis A. Ho, Paul T. P. TI RESOLVING THE STRUCTURE AND KINEMATICS OF THE BN OBJECT AT 0 ''.2 RESOLUTION SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: individual (Orion); radio continuum: ISM; radio lines: ISM ID RADIO RECOMBINATION LINES; ORION-KL; PROPER MOTIONS; CONTINUUM; REGIONS; DISK; CIRCUMSTELLAR; RADIATION; EMISSION; HYDROGEN AB We present sensitive 7 mm observations of the H53 alpha recombination line and adjacent continuum, made toward the Orion BN/KL region. In the continuum we detect the BN object, the radio source I (GMR I) and the radio counterpart of the infrared (IR) source n (Orion-n). Comparing with observations made at similar angular resolutions but lower frequency, we discuss the spectral indices and angular sizes of these sources. In the H53 alpha line, we only detect the BN object. This is the first time that radio recombination lines have been detected from this source. The LSR radial velocity of BN from the H53 alpha line, V(LSR) = 20.1 +/- 2.1 km s(-1), is consistent with that found from previous studies in near-IR lines. While the continuum emission is expected to have considerable optical depth at 7 mm, the observed H53 alpha line emission is consistent with an optically thin nature and we discuss possible explanations for this apparent discrepancy. There is evidence of a velocity gradient, with the NE part of BN being redshifted by similar to 10 km s(-1) with respect to the SW part. This is consistent with the suggestion of Jiang et al. that BN may be driving an ionized outflow along that direction. C1 [Rodriguez, Luis F.] Univ Nacl Autonoma Mexico, Ctr Radioastron & Astrofis, Morelia 58089, Michoacan, Mexico. [Zapata, Luis A.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Zapata, Luis A.; Ho, Paul T. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ho, Paul T. P.] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. RP Rodriguez, LF (reprint author), Univ Nacl Autonoma Mexico, Ctr Radioastron & Astrofis, Morelia 58089, Michoacan, Mexico. EM l.rodriguez@astrosmo.unam.mx; lzapata@mpifr-bonn.mpg.de; pho@asiaa.sinica.edu.tw NR 27 TC 17 Z9 17 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2009 VL 692 IS 1 BP 162 EP 167 DI 10.1088/0004-637X/692/1/162 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 410CG UT WOS:000263553000016 ER PT J AU Nutzman, P Charbonneau, D Winn, JN Knutson, HA Fortney, JJ Holman, MJ Agol, E AF Nutzman, Philip Charbonneau, David Winn, Joshua N. Knutson, Heather A. Fortney, Jonathan J. Holman, Matthew J. Agol, Eric TI A PRECISE ESTIMATE OF THE RADIUS OF THE EXOPLANET HD 149026b FROM SPITZER PHOTOMETRY SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; techniques: photometric ID TRANSITING EXTRASOLAR PLANETS; STELLAR ATMOSPHERE MODELS; LIMB-DARKENING LAW; GIANT PLANETS; SURFACE GRAVITIES; SPACE-TELESCOPE; LIGHT-CURVE; HOT; PARAMETERS; JUPITER AB We present Spitzer 8 mu m transit observations of the extrasolar planet HD 149026b. At this wavelength, transit light curves are weakly affected by stellar limb darkening, allowing for a simpler and more accurate determination of planetary parameters. We measure a planet-star radius ratio of R(p)/R(star) = 0.05158 +/- 0.00077, and in combination with ground-based data and independent constraints on the stellar mass and radius, we derive an orbital inclination of i = 85 degrees.4(-0 degrees.8)(+0 degrees.9) and a planet radius of R(p) = 0.755 +/- 0.040 R(J). These measurements further support models in which the planet is greatly enriched in heavy elements. C1 [Nutzman, Philip; Knutson, Heather A.; Holman, Matthew J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Winn, Joshua N.] MIT, Dept Phys, Cambridge, MA 02139 USA. [Winn, Joshua N.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Fortney, Jonathan J.] Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Agol, Eric] Univ Washington, Dept Astron, Seattle, WA 98195 USA. RP Nutzman, P (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM pnutzman@cfa.harvard.edu RI Agol, Eric/B-8775-2013; OI Agol, Eric/0000-0002-0802-9145; Fortney, Jonathan/0000-0002-9843-4354; Charbonneau, David/0000-0002-9003-484X FU NASA FX We are grateful to F. van Leeuwen for providing parallax data for HD 149026, and to G. Takeda for discussions regarding the spectroscopic determination of stellar properties. We are especially grateful to G. Henry for sharing many seasons of photometric data. We would also like to thank an anonymous referee for specific and helpful recommendations. This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. NR 41 TC 12 Z9 12 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2009 VL 692 IS 1 BP 229 EP 235 DI 10.1088/0004-637X/692/1/229 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 410CG UT WOS:000263553000022 ER PT J AU Valencic, LA Smith, RK Dwek, E Graessle, D Dame, TM AF Valencic, Lynne A. Smith, Randall K. Dwek, Eli Graessle, Dale Dame, T. M. TI EXAMINING DUST GRAIN MODELS USING THE REDDENING AND X-RAY DUST HALO OF TERZAN 2 SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; globular clusters: individual (Terzan 2); X-rays: ISM ID GLOBULAR-CLUSTER TERZAN-2; INTERSTELLAR DUST; INFRARED-EMISSION; GALACTIC-CENTER; MILKY-WAY; H-I; SCATTERING; EXTINCTION; ABSORPTION; PHOTOMETRY AB We use the X-ray dust halo of the low-mass X-ray binary 4U 1724-307, located in the globular cluster Terzan 2, to probe the interstellar medium along this line of sight (LOS). The X-ray dust halo arises from X-rays scattering off of interstellar dust grains. Using a low optical depth sight line to determine the Chandra ACIS point-spread function, we extracted the radial profile as a function of energy and used it to determine the H column density (N(H)) and cloud location along the LOS for several dust grain models, including the commonly-used models of MRN and WD. The resulting N(H) values were used to determine the reddening E(B-V), which was then compared with the average E(B-V) for this sight line found by other workers. We found that for this LOS, only the ZDA BARE-AC-S, BARE-GR-FG, and BARE-GR-S models yield reddenings within 1 sigma of the literature average. C1 [Valencic, Lynne A.; Dwek, Eli] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Valencic, Lynne A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Smith, Randall K.; Graessle, Dale; Dame, T. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Valencic, LA (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM valencic@milkyway.gsfc.nasa.gov RI Dwek, Eli/C-3995-2012 FU NASA FX The authors thank an anonymous referee for many helpful and insightful comments. This research was supported by an appointment to the NASA Postdoctoral Program at the Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA. NR 50 TC 6 Z9 6 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2009 VL 692 IS 1 BP 502 EP 510 DI 10.1088/0004-637X/692/1/502 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 410CG UT WOS:000263553000043 ER PT J AU Owers, MS Nulsen, PEJ Couch, WJ Markevitch, M Poole, GB AF Owers, Matt S. Nulsen, Paul E. J. Couch, Warrick J. Markevitch, Maxim Poole, Gregory B. TI ABELL 1201: THE ANATOMY OF A COLD FRONT CLUSTER FROM COMBINED OPTICAL AND X-RAY DATA SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: individual (Abell 1201); X-rays: galaxies: clusters ID XMM-NEWTON OBSERVATIONS; GALAXY REDSHIFT SURVEY; FIBER-FED SPECTROGRAPH; MULTIWAVELENGTH ANALYSIS; CHANDRA OBSERVATION; INTERNAL DYNAMICS; VELOCITY DISPERSIONS; PERSEUS CLUSTER; RICH CLUSTERS; CORE AB We present a combined X-ray and optical analysis of the cold front cluster Abell 1201 using archival Chandra data and multi-object spectroscopy taken with the 3.9 m Anglo-Australian and 6.5 m Multiple Mirror Telescopes. This paper represents the first in a series presenting a study of a sample of cold front clusters selected from the Chandra archives with the aim of relating cold fronts to merger activity, understanding the dynamics of mergers and their effect on the cluster constituents. The Chandra X-ray imagery of Abell 1201 reveals two conspicuous surface brightness discontinuities that are shown to be cold fronts, and a remnant core structure. Temperature maps reveal a complex multiphase temperature structure with regions of hot gas interspersed with fingers of cold gas. Our optical analysis is based on a sample of 321 confirmed members, whose mean redshift is z = 0.1673 +/- 0.0002 and velocity dispersion is 778 +/- 36 km s(-1). We search for dynamical substructure and find clear evidence for multiple localized velocity substructures coincident with overdensities in the galaxy surface density. Most notably, we find the structure coincident with the remnant X-ray core. Despite the clear evidence for dynamical activity, we find the peculiar velocity distribution does not deviate significantly from Gaussian. We apply two-body dynamical analyses in order to assess which of the substructures are bound, and thus dynamically important in terms of the cluster merger history. We propose that the cold fronts in Abell 1201 are a consequence of its merger with a smaller subunit, which has induced gas motions that gave rise to "sloshing" cold fronts. Abell 1201 illustrates the value of combining multiwavelength data and multiple substructure detection techniques when attempting to ascertain the dynamical state of a cluster. C1 [Owers, Matt S.] Univ New S Wales, Sch Phys, Sydney, NSW 2052, Australia. [Nulsen, Paul E. J.; Markevitch, Maxim] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Couch, Warrick J.; Poole, Gregory B.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. RP Owers, MS (reprint author), Univ New S Wales, Sch Phys, Sydney, NSW 2052, Australia. EM mowers@phys.unsw.edu.au OI Owers, Matt/0000-0002-2879-1663; Nulsen, Paul/0000-0003-0297-4493 FU Australian Research Council; NASA [NAS8-01130] FX M. S. O was supported by an Australian Postgraduate Award, and acknowledges the hospitality of the Harvard-Smithsonian Center for Astrophysics where a portion of this study was undertaken. We acknowledge the financial support of the Australian Research Council (via its Discovery Project Scheme) throughout the course of this work. P.E.J.N. was supported by NASA grant NAS8-01130. NR 62 TC 16 Z9 16 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2009 VL 692 IS 1 BP 702 EP 722 DI 10.1088/0004-637X/692/1/702 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 410CG UT WOS:000263553000060 ER PT J AU Salvesen, G Miller, JM Cackett, E Siemiginowska, A AF Salvesen, G. Miller, J. M. Cackett, E. Siemiginowska, A. TI A DEEP XMM-NEWTON OBSERVATION OF THE QUASAR 3C 287 SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; relativity ID ACTIVE GALACTIC NUCLEI; X-RAY-EMISSION; SPECTRAL ENERGY-DISTRIBUTIONS; GHZ-PEAKED SPECTRUM; RADIO-LOUD AGN; ACCRETION DISKS; GALAXIES; VIEW; EVOLUTION; CHANDRA AB We report on an XMM-Newton observation of the z = 1.055 quasar and Gigahertz Peaked Spectrum (GPS) source 3C 287. Our 62.3 ks observation provides an exceptional X-ray view of a prominent member of this important subclass of active galactic nuclei (AGNs). The X-ray spectra of 3C 287 are consistent with a simple absorbed power law with a spectral index of Gamma = 1.72 +/- 0.02. Our fits imply a bolometric luminosity of L = 5.8 +/- 0.2x10(45) erg s(-1) over the 0.3-10.0 keV band; this gives a mass lower limit of M(BHmin) >= 4.6 x 10(7) M circle dot assuming X-rays contribute 10% of the bolometric luminosity and radiation at the Eddington limit. Iron emission lines are common in the X-ray spectra of many AGNs, but the observed spectra appear to rule out strong emission lines in 3C 287. The simple power-law spectrum and the absence of strong emission lines may support a picture where our line of sight intersects a relativistic jet. Milliarcsecond radio imaging of 3C 287 appears to support this interpretation. We discuss our results in the context of different AGNs subclasses and the possibility that GPS sources harbor newly formed black hole jets. C1 [Salvesen, G.; Miller, J. M.; Cackett, E.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Siemiginowska, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Salvesen, G (reprint author), Univ Michigan, Dept Astron, 500 Church St, Ann Arbor, MI 48109 USA. EM salvesen@umich.edu; jonmm@umich.edu; aneta@head.cfa.harvard.edu FU NASA [GO2-3148A, GO5-6113X, NAS8-39073] FX We thank the anonymous referee for insightful comments that improved the paper. J.M.M. gratefully acknowledges funding from NASA, through the XMM-Newton Guest Observations program. Partial support for this work was provided by NASA through Chandra Award Number GO2-3148A and GO5-6113X and under the contract NAS8-39073. NR 37 TC 1 Z9 1 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2009 VL 692 IS 1 BP 753 EP 757 DI 10.1088/0004-637X/692/1/753 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 410CG UT WOS:000263553000063 ER PT J AU Milisavljevic, D Fesen, RA Kirshner, RP Challis, P AF Milisavljevic, Dan Fesen, Robert A. Kirshner, Robert P. Challis, Peter TI THE EVOLUTION OF LATE-TIME OPTICAL EMISSION FROM SN 1979C SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; supernovae: general; supernovae: individual (SN 1979C); supernova remnants ID SUPER-NOVA 1979C; LIGHT CURVES; II SUPERNOVAE; X-RAY; SPECTRA; RADIO; M100; SPECTROSCOPY; ULTRAVIOLET; RECOVERY AB Optical spectra of the bright Type II-L supernova SN 1979C obtained in April 2008 with the 6.5 m Multiple Mirror Telescope are compared with archival late-time spectra to follow the evolution of its optical emission over the age range of 11-29 years. We estimate an Ha flux decrease of around 35% from 1993 to 2008 but noticeable increases in the strength of blueshifted emission of forbidden oxygen lines. While the maximum expansion of the broad similar to 6700 km s(-1) Ha emission appears largely unchanged from 1993, we find a significant narrowing of the double-peaked emission profiles in the [OI] lambda lambda 6300, 6364 and [OI] lambda lambda 7319, 7330 lines. A comparison of late-time optical spectra of a few other Type II SNe which, like SN 1979C, exhibit bright late-time X-ray, optical, and radio emissions, suggests that blueshifted double-peaked oxygen emission profiles may be a common phenomenon. Finally, detection of a faint, broad emission bump centered around 5800 similar to suggests the presence of WC-type Wolf-Rayet stars in the SN's host star cluster. C1 [Milisavljevic, Dan; Fesen, Robert A.] Dartmouth Coll, Dept Phys & Astron, Wilder Lab 6127, Hanover, NH 03755 USA. [Kirshner, Robert P.; Challis, Peter] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Milisavljevic, D (reprint author), Dartmouth Coll, Dept Phys & Astron, Wilder Lab 6127, Hanover, NH 03755 USA. FU NSF [AST06-06772] FX We thank C. Gerardy for assistance with the MDM observations, and R. Chevalier and P. Massey for helpful comments on an earlier draft. R. P. acknowledges that supernova research at Harvard is supported by NSF Grant AST06-06772, and D. M. thanks NSERC for partial support of this research through a PGS award. NR 37 TC 10 Z9 10 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2009 VL 692 IS 1 BP 839 EP 843 DI 10.1088/0004-637X/692/1/839 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 410CG UT WOS:000263553000069 ER PT J AU Hershler, R Liu, HP AF Hershler, Robert Liu, Hsiu-Ping TI New species and records of Pyrgulopsis (Gastropoda: Hydrobiidae) from the Snake River basin, southeastern Oregon: further delineation of a highly imperiled fauna SO ZOOTAXA LA English DT Article DE springs; Owyhee River; Malheur River; springsnails; mitochondrial DNA; conservation ID AMERICAN NYMPHOPHILINE GASTROPODS; MITOCHONDRIAL-DNA SEQUENCES; GENUS PYRGULOPSIS; UNITED-STATES; GREAT-BASIN; RISSOOIDEA; SNAILS; DIVERSIFICATION; SPRINGSNAIL; CALIFORNIA AB Here we describe two new species from southeastern Oregon based on morphologic and molecular (mtCOI) evidence. Pyrgulopsis fresti n. sp., commonly known as the "Owyhee hot springsnail" and long considered to be distinct and critically imperiled, lives in thermal springs along a short reach of the Owyhee River above Three Forks. This snail differs from other regional species in its squat shell; penial ornament consisting of a large, disc-shaped ventral gland; absence of a seminal receptacle; and mtCOI sequences. Pyrgulopsis owyheensis n. sp. ranges among five disjunct groups of springs in the Owyhee and Malheur river drainages and is occasionally sympatric with P. fresti. This snail is closely similar to another regional congener, P. intermedia (Tryon, 1865), but is smaller and further differentiated by its typically disjunct inner shell lip, longer and narrower penial filament, more distally positioned ventral gland of penis, and mtCOI sequences. The type locality (Owyhee Spring) population of P. owyheensis is genetically differentiated from the other geographical subunits of this species (1.5-1.8% sequence divergence) and should perhaps be managed as a separate conservation unit. New records are provided for P. intermedia which extends the range of this conservation priority species into the lower Owyhee River basin. We also show that the "Malheur springsnail," which has been listed in various conservation-related publications and documents, is the same as P. intermedia. This study provides critical information for the conservation of springsnails in southeastern Oregon and underscores the need for additional field surveys in the region. C1 [Hershler, Robert] Smithsonian Inst, Dept Invertebrate Zool, Washington, DC 20013 USA. [Liu, Hsiu-Ping] Metropolitan State Coll, Dept Biol, Denver, CO 80217 USA. RP Hershler, R (reprint author), Smithsonian Inst, Dept Invertebrate Zool, POB 37012,NHB W-305,MRC 163, Washington, DC 20013 USA. EM hershlerr@si.edu; liu.hsiuping@gmail.com FU Bureau of Land Management, Vale District [HVP060011] FX The first author is grateful for the field assistance and logistical support provided by William H. Clark, Shaney Rockefeller and Cynthia Tait. Specimens were provided by Terry Frest, Daniel Gustafson, David Hopper and Cary Myler. Yolanda Villacampa measured shells and prepared scanning electron micrographs. Molly Ryan assisted with map preparation. Karolyn Darrow photographed type material and prepared anatomical drawings. Fiscal support for this project was provided by the Bureau of Land Management, Vale District (Award Number HVP060011). NR 41 TC 3 Z9 3 U1 0 U2 1 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD FEB 9 PY 2009 IS 2006 BP 1 EP 22 PG 22 WC Zoology SC Zoology GA 406WU UT WOS:000263326400001 ER PT J AU Hosseini, BH Weck, PF Sadeghpour, HR Kirby, K Stancil, PC AF Hosseini, B. H. Weck, P. F. Sadeghpour, H. R. Kirby, K. Stancil, P. C. TI Photodissociation dynamics of lithium chloride: Contribution of interferometric predissociation SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article DE ground states; infrared spectra; lithium compounds; molecule-photon collisions; photodissociation; predissociation; rotational states; Rydberg states; ultraviolet spectra ID CONFIGURATION-INTERACTION; LINE; ATMOSPHERES; OPACITY; DWARFS; STATES; LICL AB Continuum photoabsorption of lithium chloride (LiCl) was investigated using a coupled-channel time-dependent wave packet approach. Photodissociation cross sections for the production of ground-state Li and Cl atoms were computed up to temperatures of 1500 K for a thermal distribution of rotational levels. At such temperatures, LiCl is believed to be the primary Li-bearing gas in cool stellar atmospheres. Narrow Rydberg resonances in the total absorption spectrum are found to dominate the thermally averaged cross section due to the large density of Rydberg states in the predissociation gap. Comparison with measured photoabsorption cross sections, where available, is made. C1 [Hosseini, B. H.; Sadeghpour, H. R.; Kirby, K.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. [Hosseini, B. H.] Fac Biophys Chem, D-69120 Heidelberg, Germany. [Weck, P. F.] Univ Nevada, Harry Reid Ctr Environm Studies, Las Vegas, NV 89154 USA. [Weck, P. F.] Univ Nevada, Dept Chem, Las Vegas, NV 89154 USA. [Stancil, P. C.] Univ Georgia, Dept Phys & Astron, Athens, GA 30602 USA. [Stancil, P. C.] Univ Georgia, Ctr Simulat Phys, Athens, GA 30602 USA. RP Hosseini, BH (reprint author), Harvard Smithsonian Ctr Astrophys, ITAMP, 60 Garden St, Cambridge, MA 02138 USA. EM hadji-hosseini@stud.uni-heidelberg.de; weckp@unlv.nevada.edu; hrs@cfa.harvard.edu; kirby@cfa.harvard.edu; stancil@physast.uga.edu OI , Philippe/0000-0002-7610-2893 FU NASA [NNG04GM59G]; NSF FX B. H. H. was supported by a grant from the Smithsonian Scholarly Studies Program. P. F. W. acknowledges support from NASA (NASA EPSCoR 2008 Proposal Development Award). H. R. S. and K. K. acknowledge support from a NSF grant to ITAMP at Harvard University and Smithsonian Astrophysical Observatory. P. C. S. acknowledges support from NASA Grant No. NNG04GM59G. NR 22 TC 5 Z9 6 U1 0 U2 1 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0021-9606 J9 J CHEM PHYS JI J. Chem. Phys. PD FEB 7 PY 2009 VL 130 IS 5 AR 054308 DI 10.1063/1.3072094 PG 5 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 404QC UT WOS:000263167100026 PM 19206974 ER PT J AU Head, JJ Bloch, JI Hastings, AK Bourque, JR Cadena, EA Herrera, FA Polly, PD Jaramillo, CA AF Head, Jason J. Bloch, Jonathan I. Hastings, Alexander K. Bourque, Jason R. Cadena, Edwin A. Herrera, Fabiany A. Polly, P. David Jaramillo, Carlos A. TI Giant boid snake from the Palaeocene neotropics reveals hotter past equatorial temperatures SO NATURE LA English DT Article ID TERRESTRIAL POIKILOTHERMS; BODY-SIZE; GIGANTISM; CLIMATE; NUCLEAR; GENES; CO2 AB The largest extant snakes live in the tropics of South America and southeast Asia(1-3) where high temperatures facilitate the evolution of large body sizes among air- breathing animals whose body temperatures are dependant on ambient environmental temperatures ( poikilothermy)(4,5). Very little is known about ancient tropical terrestrial ecosystems, limiting our understanding of the evolution of giant snakes and their relationship to climate in the past. Here we describe a boid snake from the oldest known neotropical rainforest fauna from the Cerrejon Formation ( 58 - 60 Myr ago) in northeastern Colombia. We estimate a body length of 13 and a mass of 1,135 kg, making it the largest known snake(6-9). The maximum size of poikilothermic animals at a given temperature is limited by metabolic rate(4), and a snake of this size would require a minimum mean annual temperature of 30 - 34 degrees C to survive. This estimate is consistent with hypotheses of hot Palaeocene neotropics with high concentrations of atmospheric CO(2) based on climate models(10). Comparison of palaeotemperature estimates from the equator to those from South American mid- latitudes indicates a relatively steep temperature gradient during the early Palaeogene greenhouse, similar to that of today. Depositional environments and faunal composition of the Cerrejon Formation indicate an anaconda- like ecology for the giant snake, and an earliest Cenozoic origin of neotropical vertebrate faunas. C1 [Head, Jason J.] Univ Toronto, Dept Biol, Mississauga, ON L5L 1C6, Canada. [Bloch, Jonathan I.; Hastings, Alexander K.; Bourque, Jason R.; Cadena, Edwin A.; Herrera, Fabiany A.] Univ Florida, Florida Museum Nat Hist, Gainesville, FL 32611 USA. [Cadena, Edwin A.; Herrera, Fabiany A.; Jaramillo, Carlos A.] Smithsonian Trop Res Inst, Balboa, Panama. [Polly, P. David] Indiana Univ, Dept Geol Sci, Bloomington, IN 47405 USA. RP Head, JJ (reprint author), Univ Toronto, Dept Biol, Mississauga, ON L5L 1C6, Canada. EM jason.head@utoronto.ca OI Bloch, Jonathan/0000-0003-1484-6931; Head, Jason/0000-0002-2237-6901; Polly, P. David/0000-0001-7338-8526 FU National Science Foundation; Fondo para Investigaciones del Banco de la Republica de Colombia; Smithsonian Tropical Research Institute Paleobiology Fund; Florida Museum of Natural History; Geological Society of America Graduate Student Research Grant; National Sciences and Engineering Research Council of Canada Discovery Grant FX We thank C. Bell, R. Ghent, E. Kowalski, A. M. Lawing, B. MacFadden, R. Reisz and S. Wing for advice and discussion, K. Seymour, K. Krysko, K. deQueiroz and G. Zug for access to comparative specimens, A. Rincon and M. Carvalho for fieldwork, J. Mason, K. Church, J. Mathis and J. Nestler for fossil preparation, and K. Krysko and J. Nestler for photographic assistance. We thank Carbones del Cerrejon, L. Teicher, F. Chavez, C. Montes and G. Hernandez for logistical support and access to the Cerrejon mine. This research was funded by the National Science Foundation, Fondo para Investigaciones del Banco de la Republica de Colombia, Smithsonian Tropical Research Institute Paleobiology Fund, the Florida Museum of Natural History, a Geological Society of America Graduate Student Research Grant to A.K.H., and a National Sciences and Engineering Research Council of Canada Discovery Grant to J. J. H. NR 30 TC 89 Z9 92 U1 0 U2 28 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD FEB 5 PY 2009 VL 457 IS 7230 BP 715 EP U4 DI 10.1038/nature07671 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 403EA UT WOS:000263064700039 PM 19194448 ER PT J AU Scarbrough, AG Perez-Gelabert, DE AF Scarbrough, Aubrey G. Perez-Gelabert, Daniel E. TI Review of the West Indian species of Efferia Coquillett (Diptera: Asilidae) with 13 new species and checklist: Part II. Hispaniola, Puerto Rico, and Lesser Antilles including Tobago and Trinidad SO ZOOTAXA LA English DT Article DE Diptera; Asilidae; West Indies; Efferia; revision ID ISLAND AB The species of Efferia from Hispaniola, Puerto Rico, and the Lesser Antilles are reviewed. Twenty species are recognized including 12 new species from the Dominican Republic: E. alia sp. nov., E. angusta sp. nov., E. bullata sp. nov., E. clava sp. nov., E. exacta sp. nov., E. incisura sp. nov., E. picea sp. nov., E. serrula sp. nov., E. sinuosa sp. nov., E. suspiciosa sp. nov., E. spinula sp. nov., and E. woodleyi sp. nov., and 1 from Puerto Rico: E. montensis sp. nov. Seven previously described West Indian species are recognized: E. forbesi (Curran, 1931), E. fortis (Walker, 1855), E. fulvibarbis (Macquart, 1848), E. haitensis (Macquart, 1848), E. nigrimystacea (Macquart, 1847), E. portoricensis (Curran, 1919), and E. stylata (Fabricius, 1775). An unresolved species from Tobago and Trinidad is also reported. All of these belong to the aestuans species group. New synonyms include: E. pachychaetus (Bromley, 1928) = E. fulvibarbis (Macquart, 1848), syn. nov.; E. tortola (Curran, 1928) = E. stylata (Fabricius, 1775), syn. nov.; and Phoneus flavotibius Bigot, 1878, = E. fortis (Walker, 1855), syn. nov. Efferia haitensis (Macquart, 1848) is removed from synonymy with E. stylata (Fabricius, 1775). The male of E. stylata is discovered and described. Lectotypes are designated for E. haitensis and E. nigrimystacea. The species is removed from the list of species from Hispaniola. Endemism is high with most species limited to single islands. Only E. stylata and E. forbesi occurring in Puerto Rico and the Virgin Islands and E. nigrimystacea in the Lesser Antilles are more widespread. Hispaniola has the greatest diversity with 15 species whereas Puerto Rico, the British and US Virgin Islands, and the Lesser Antilles have 5. Keys, illustrations of the left wing of selected males, and terminalia of all known species are included. A check-list of the West Indian species of Efferia, including an unresolved species from Tobago and Trinidad, is also provided. C1 [Perez-Gelabert, Daniel E.] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20013 USA. RP Scarbrough, AG (reprint author), Univ Arizona, Dept Entomol, Tucson, AZ 85741 USA. EM saubrey05@q.com; perezd@si.edu FU National Science Foundation [DEB-0103042]; S. W. Williston Diptera Research Fund; Smithsonian Institution FX We thank the curators and colleagues who collected numerous specimens and made them available to us during this study; R. Bastardo, Universidad Autonoma de Santo Domingo (IIBZ); C. Young, J. Rawlins (CMNH); N. Woodley (Systematic Entomology Laboratory, PSI, ARS, USDA, National Museum of Natural History, Smithsonian Institution NMNH); M. Ivie, Montana State University (MAIC), and R. Woodruff (FSCA). We are especially grateful to the curators for the loan and/or access of type material: N. Johnson (OSUC); D. Grimaldi (AMNH); D. Mann (OUMNH); E. McAlister (BMNH); and F. C. Thompson (NMNH). Thanks are extended to C. Young, G. Steck, (FSCA), F. C. Thompson, and D. Grimaldi for their assistance and suggestions when visiting the collections under their care. We thank R. E. Castillo, Fundacion Progressio, Inc., for access to the Reserva Cient fica Ebano Verde. M. Mota, R. O. Sanchez, B. Hierro, and J. R. Albaine, Direccion Nacional de Parques and Departamento de Vida Silvestre, Santo Domingo, assisted with collecting and export permits. Field work by DEPG in the Dominican Republic was supported by National Science Foundation grant DEB-0103042 and grants from the S. W. Williston Diptera Research Fund, Smithsonian Institution. Lastly, we thank the anonymous reviewers for reading the manuscript and providing valuable comments. NR 39 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 FEB 4 PY 2009 IS 1994 BP 1 EP 66 PG 66 WC Zoology SC Zoology GA 403SH UT WOS:000263101800001 ER PT J AU Hinde, K Power, ML Oftedal, LT AF Hinde, Katherine Power, Michael L. Oftedal, Lav T. TI Rhesus Macaque Milk: Magnitude, Sources, and Consequences of Individual Variation Over Lactation SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Article DE milk composition and yield; parity; infant growth; maternal effects; life history ID CERVUS-ELAPHUS-HISPANICUS; MARMOSETS CALLITHRIX-JACCHUS; MACACA-MULATTA; MATERNAL INVESTMENT; SUCKLING BEHAVIOR; ENERGY-INTAKE; REPRODUCTIVE SUCCESS; NUTRIENT DEPOSITION; NIPPLE PREFERENCE; CALF GROWTH AB Lactation represents the greatest postnatal energetic expenditure for mammalian mothers, and a mother's ability to sustain the costs of lactation is influenced by her physical condition. Mothers in good condition may produce infants who weigh more, grow faster, and are more likely to survive than the infants of mothers in poor condition. These effects may be partially mediated through the quantity and quality of milk that mothers produce during lactation. However, we know relatively little about the relationships between maternal condition, milk composition, milk yield, and infant outcomes. Here, we present the first systematic investigation of the magnitude, sources, and consequences of individual variation in milk for an Old World monkey. Rhesus macaques produce dilute milk typical of the primate order, but there was substantial variation among mothers in the composition and amount of milk they produced and thus in the milk energy available to infants. Relative milk yield value (MYV), the grams of milk obtained by mammary evacuation after 3.5-4 h of maternal-infant separation, increased with maternal parity and was positively associated with infant weight. Both milk gross energy (GE) and MYV increased during lactation as infants aged. There was, however, a trade-off; those mothers with greater increases in GE had smaller increases in MYV, and their infants grew more slowly. These results from a well-fed captive population demonstrate that differences between mothers can have important implications for milk synthesis and infant outcome. Am J Phys Anthropol 138:148-157, 2009. (C) 2008 Wiley-Liss. Inc. C1 [Hinde, Katherine] Univ Calif Los Angeles, Dept Anthropol, Los Angeles, CA 90095 USA. [Hinde, Katherine] Calif Natl Primate Res Ctr, Davis, CA USA. [Power, Michael L.] Amer Coll Obstetricians & Gynecologists, Res Dept, Washington, DC 20024 USA. [Power, Michael L.; Oftedal, Lav T.] Smithsonian Natl Zool Pk, Nutr Lab, Washington, DC USA. RP Hinde, K (reprint author), Univ Calif Los Angeles, Dept Anthropol, 341 Haines Hall,Box 951553, Los Angeles, CA 90095 USA. EM kjhinde@ucla.edu OI Power, Michael/0000-0002-6120-3528; Hinde, Katie/0000-0002-0528-866X FU NSF [DDIG 0525025]; NIH [RR019970, RR000169]; California National Primate Research Center [DK77639]; American Society of Primatologists awarded FX Grant sponsor: NSF; Grant number: DDIG 0525025 awarded to K.H. and Joan Silk; Grant sponsor: NIH; Grant numbers: RR019970, RR000169 awarded to John Capitanio and the California National Primate Research Center, DK77639 awarded to MLP; Grant sponsor: American Society of Primatologists awarded to K.H. NR 80 TC 51 Z9 51 U1 0 U2 20 PU WILEY-LISS PI HOBOKEN PA DIV JOHN WILEY & SONS INC, 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PD FEB PY 2009 VL 138 IS 2 BP 148 EP 157 DI 10.1002/ajpa.20911 PG 10 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 395QD UT WOS:000262537700003 PM 18711734 ER PT J AU Reudink, MW Marra, PP Boag, PT Ratcliffe, LM AF Reudink, Matthew W. Marra, Peter P. Boag, Peter T. Ratcliffe, Laurene M. TI Plumage coloration predicts paternity and polygyny in the American redstart SO ANIMAL BEHAVIOUR LA English DT Article DE American redstart; carotenoid; extrapair paternity; polygyny; plumage; Setophaga ruticilla ID MULTIPLE SEXUAL ORNAMENTS; BLACK-CAPPED CHICKADEES; SPARROW PASSER-DOMESTICUS; MALE MATING SUCCESS; FEMALE CHOICE; BADGE SIZE; REPRODUCTIVE SUCCESS; EXTRAPAIR PATERNITY; COMMON YELLOWTHROAT; SETOPHAGA-RUTICILLA AB Many animals display multiple signals that can be used by conspecifics to gather information about the condition or quality of potential mates or competitors. Different signals can indicate different aspects of individual quality or function in spatially or temporally separated periods. However, for long-distance migratory birds, it is unclear if signals, such as plumage traits, function in different phases of the annual cycle. We investigated the potential role of carotenoid-based tail and flank plumage, and bib size, in relation to extrapair paternity and polygyny in the American redstart, Setophaga ruticilla. This work complements our previous research suggesting tail feather brightness acts as a status signal, mediating territory acquisition during the nonbreeding season in Jamaica. Here, we show that tail feather brightness also serves as an important signal during the breeding season. Specifically, our results indicate that polygyny, a behaviour highly dependent on obtaining and defending multiple territories, is significantly predicted by tail brightness. Interestingly, flank redness best predicted whether individuals secured paternity at their nest and the proportion of within-pair offspring sired. We suggest that by expanding the study of plumage function in long-distance migrants to events occurring throughout the annual cycle, we gain a critical perspective on the function and evolution of ornamental traits. 2008 The Association for the Study of Animal Behaviour. Published by Elsevier Ltd. C1 [Reudink, Matthew W.; Marra, Peter P.] Smithsonian Migratory Bird Ctr, Natl Zool Pk, Washington, DC 20008 USA. [Reudink, Matthew W.; Boag, Peter T.; Ratcliffe, Laurene M.] Queens Univ, Dept Biol, Kingston, ON K7L 3N6, Canada. RP Reudink, MW (reprint author), Smithsonian Migratory Bird Ctr, Natl Zool Pk, 3001 Connecticut Ave NW, Washington, DC 20008 USA. EM mattreudink@gmail.com RI Boag, Peter/B-2907-2014; OI Boag, Peter/0000-0003-0050-2089; Reudink, Matthew/0000-0001-8956-5849 FU Natural Sciences and Engineering Research Council of Canada; Canadian Foundation for Innovation; National Science Foundation [0085965]; Smithsonian Institution; Queen's University; Ontario Innovation Trust; Sigma Xi; American Ornithologists' Union; Society of Canadian Ornithologists; American Museum of Natural History FX We gratefully acknowledge the hard work of the many field assistants that contributed to this study. R. Reudink, R. Germain, T. Murphy, B. Ballentine, M. Osmond and C. Studds provided insightful discussion and comments on earlier versions of this manuscript. We thank R. Montgomerie for the use of his colour analysis equipment, software and expertise. We thank C. Scott for molecular assistance. Funding was provided by the Natural Sciences and Engineering Research Council of Canada, the Canadian Foundation for Innovation, the National Science Foundation grant to P. P. M. (0085965), the Smithsonian Institution, Queen's University, Ontario Innovation Trust, Sigma Xi, the American Ornithologists' Union, the Society of Canadian Ornithologists and the American Museum of Natural History. NR 62 TC 25 Z9 25 U1 3 U2 20 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0003-3472 J9 ANIM BEHAV JI Anim. Behav. PD FEB PY 2009 VL 77 IS 2 BP 495 EP 501 DI 10.1016/j.anbehav.2008.11.005 PG 7 WC Behavioral Sciences; Zoology SC Behavioral Sciences; Zoology GA 398CP UT WOS:000262709400028 ER PT J AU Winkler, U Zotz, G AF Winkler, Uwe Zotz, Gerhard TI Highly efficient uptake of phosphorus in epiphytic bromeliads SO ANNALS OF BOTANY LA English DT Article ID VASCULAR EPIPHYTES; MINERAL-NUTRITION; PHOSPHATE-UPTAKE; MONTANE FOREST; NITROGEN; GROWTH; LEAVES; PLANT; ACID; ROOT AB Vascular epiphytes which can be abundant in tree crowns of tropical forests have to cope with low and highly intermittent water and nutrient supply from rainwater, throughfall and stem flow. Phosphorus rather than nitrogen has been suggested as the most limiting nutrient element, but, unlike nitrogen, this element has received little attention in physiological studies. This motivated the present report, in which phosphate uptake kinetics by leaves and roots, the subsequent distribution within plants and the metabolic fate of phosphate were studied as a step towards an improved understanding of physiological adaptations to the conditions of tree canopies. Radioactively labelled [(32)P]phosphate was used to study uptake kinetics and plant distribution of phosphorus absorbed from bromeliad tanks. The metabolism of low molecular phosphorus metabolites was analysed by thin-layer chromatography followed by autoradiography. Uptake of phosphate from tanks is an ATP-dependent process. The kinetics of phosphorus uptake suggest that epiphytes possess effective phosphate transporters. The K(m) value of 1.05 mu m determined for leaves of the bromeliad Aechmea fasciata is comparable with values obtained for the high affinity phosphate transporters in roots of terrestrial plants. In this species, young leaves are the main sink for phosphate absorbed from tank water. Within these leaves, phosphate is then allocated from the basal uptake zone into distal sections of the leaves. More than 80 % of the phosphate incorporated into leaves is not used in metabolism but stored as phytin. Tank epiphytes are adapted to low and intermittent nutrient supply by different mechanisms. They possess an effective mechanism to take up phosphate, minimizing dilution and loss of phosphorus captured in the tank. Available phosphorus is taken up from the tank solution almost quantitatively, and the surplus not needed for current metabolism is accumulated in reserves, i.e. plants show luxury consumption. Young, developing leaves are preferentially supplied with this nutrient element. Taken together, these features allow epiphytes the efficient use of scarce and variable nutrient supplies. C1 [Winkler, Uwe; Zotz, Gerhard] Carl von Ossietzky Univ Oldenburg, Funct Ecol Grp, D-26111 Oldenburg, Germany. [Zotz, Gerhard] Smithsonian Trop Res Inst, Balboa, Panama. RP Winkler, U (reprint author), Carl von Ossietzky Univ Oldenburg, Funct Ecol Grp, D-26111 Oldenburg, Germany. EM u.winkler@uni-oldenburg.de NR 35 TC 31 Z9 31 U1 1 U2 24 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0305-7364 J9 ANN BOT-LONDON JI Ann. Bot. PD FEB PY 2009 VL 103 IS 3 BP 477 EP 484 DI 10.1093/aob/mcn231 PG 8 WC Plant Sciences SC Plant Sciences GA 398FK UT WOS:000262717800008 PM 19033287 ER PT J AU Vijh, UP Meixner, M Babler, B Block, M Bracker, S Engelbracht, CW For, B Gordon, K Hora, J Indebetouw, R Leitherer, C Meade, M Misselt, K Sewilo, M Srinivasan, S Whitney, B AF Vijh, Uma P. Meixner, M. Babler, B. Block, M. Bracker, S. Engelbracht, C. W. For, B. Gordon, K. Hora, J. Indebetouw, R. Leitherer, C. Meade, M. Misselt, K. Sewilo, M. Srinivasan, S. Whitney, B. TI VARIABLE EVOLVED STARS AND YOUNG STELLAR OBJECTS DISCOVERED IN THE LARGE MAGELLANIC CLOUD USING THE SAGE SURVEY SO ASTRONOMICAL JOURNAL LA English DT Article DE infrared: stars; galaxies: individual (LMC); stars: AGB and post-AGB; stars: formation; stars: mass loss; stars: variables: other ID SPITZER-SPACE-TELESCOPE; FU-ORIONIS OBJECTS; GALACTIC BULGE; INFRARED VARIABILITY; AGB STARS; MASS-LOSS; 2MASS; EVOLUTION; MACHO; LMC AB We present initial results and source lists of variable sources in the Large Magellanic Cloud (LMC) for which we detect thermal infrared variability from the Surveying the Agents of a Galaxy's Evolution (SAGE) survey, which had two epochs of photometry separated by 3 months. The SAGE survey mapped a 7 degrees x 7 degrees region of the LMC using the Infrared Array Camera (IRAC) and the MIPS instruments on board Spitzer. Variable sources are identified using a combination of the IRAC 3.6, 4.5, 5.8, 8.0 mu m bands and the MIPS 24 mu m bands. An error-weighted flux difference between the two epochs is used to assess the variability. Of the similar to 3 million sources detected at both epochs, we find similar to 2000 variable sources for which we provide electronic catalogs. Most of the variable sources can be classified as asymptotic giant branch (AGB) stars. A large fraction (> 66%) of the extreme AGB stars are variable and only smaller fractions of carbon-rich (6.1%) and oxygen-rich (2.0%) stars are detected as variable sources. We also detect a population of variable young stellar object candidates. C1 [Vijh, Uma P.; Meixner, M.; Gordon, K.; Leitherer, C.; Sewilo, M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Babler, B.; Bracker, S.; Meade, M.] Univ Wisconsin, Madison, WI 53706 USA. [Block, M.; Engelbracht, C. W.; For, B.; Misselt, K.] Univ Arizona, Tucson, AZ 85719 USA. [Hora, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Indebetouw, R.] Univ Virginia, Charlottesville, VA 22903 USA. [Srinivasan, S.] Johns Hopkins Univ, Baltimore, MD 21218 USA. [Whitney, B.] Space Sci Inst, Madison, WI 53716 USA. RP Vijh, UP (reprint author), Univ Toledo, Rittter Astrophys Res Ctr, 2801 W Bancroft St, Toledo, OH 43606 USA. FU NASA/Spitzer [1275598]; NASA [NAG5-12595] FX The SAGE Project is supported by NASA/Spitzer grant 1275598 and NASA NAG5-12595. We appreciate the support of B. Shiao, the STScI database programmer, for his support. Facilities: Spitzer (IRAC), Spitzer (MIPS) NR 24 TC 42 Z9 42 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD FEB PY 2009 VL 137 IS 2 BP 3139 EP 3148 DI 10.1088/0004-6256/137/2/3139 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 400WV UT WOS:000262901000013 ER PT J AU Kinman, TD Morrison, HL Brown, WR AF Kinman, T. D. Morrison, Heather L. Brown, Warren R. TI DO THE NEARBY BLUE HORIZONTAL BRANCH STARS BELONG TO THE THICK DISK OR THE HALO? SO ASTRONOMICAL JOURNAL LA English DT Article DE Galaxy: halo; Galaxy: structure; stars: horizontal-branch ID RR-LYRAE VARIABLES; METAL-POOR STARS; SOLAR NEIGHBORHOOD; MILKY-WAY; GALACTIC HALO; HIGH-VELOCITY; KINEMATICS; FIELD; METALLICITY; CATALOG AB We study the Milky Way region (vertical bar Z vertical bar < 3.0 kpc) where the thick disk and inner halo overlap by using the kinematics of local blue horizontal branch (BHB) stars (within 1 kpc) and new samples of BHB stars and A-type stars from the Century Survey. We derive Galactic U, V, and W velocities for these BHB and A-type star samples using proper motions from the NOMAD catalog. The mean velocities and the velocity dispersions of the BHB samples (vertical bar Z vertical bar < 3 kpc) are characteristic of the halo, while those of the Century Survey A-type stars are characteristic of the thick disk. There is no evidence from our samples that the BHB stars rotate with the thick disk in the region vertical bar Z vertical bar < 3 kpc. Nearly a third of the nearby local RR Lyrae stars have disk kinematics and are more metal rich than [Fe/H]similar to-1. Only a few percent of the Century Survey BHB (CBHB) stars have these properties. Only one nearby BHB star (HD 130201) is likely to be such a disk star but selection based on high proper motions will have tended to exclude such stars from the local sample. The scale height derived from a sample of local RR Lyrae stars agrees with that of the CBHB stars. The local samples of BHB stars and metal-weak red giants are too incomplete for a similar comparison. C1 [Kinman, T. D.] Natl Opt Astron Observ, Tucson, AZ 85726 USA. [Morrison, Heather L.] Case Western Reserve Univ, Dept Astron, Cleveland, OH 44106 USA. [Brown, Warren R.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Kinman, TD (reprint author), Natl Opt Astron Observ, POB 26732, Tucson, AZ 85726 USA. NR 45 TC 13 Z9 13 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD FEB PY 2009 VL 137 IS 2 BP 3198 EP 3209 DI 10.1088/0004-6256/137/2/3198 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 400WV UT WOS:000262901000019 ER PT J AU Currie, T Evans, NR Spitzbart, BD Irwin, J Wolk, SJ Hernandez, J Kenyon, SJ Pasachoff, JM AF Currie, Thayne Evans, Nancy Remage Spitzbart, Brad D. Irwin, Jonathan Wolk, Scott J. Hernandez, Jesus Kenyon, Scott J. Pasachoff, Jay M. TI THE X-RAY ENVIRONMENT DURING THE EPOCH OF TERRESTRIAL PLANET FORMATION: CHANDRA OBSERVATIONS OF h PERSEI SO ASTRONOMICAL JOURNAL LA English DT Article DE open clusters and associations: individual (NGC 869); planetary systems: formation; stars: pre-main sequence; X-rays: stars ID MAIN-SEQUENCE EVOLUTION; ORION ULTRADEEP PROJECT; YOUNG OPEN CLUSTERS; M-CIRCLE-DOT; CHI-PERSEI; MOLECULAR CLOUD; MONITOR PROJECT; MASS FUNCTION; ALPHA-PERSEI; DEBRIS DISKS AB We describe Chandra/ACIS-I observations of the massive similar to 13-14 Myr-old cluster, h Persei, part of the famous Double Cluster (h and. Persei) in Perseus. Combining the list of Chandra-detected sources with new optical/IR photometry and optical spectroscopy reveals similar to 165 X-ray bright stars with V less than or similar to 23. Roughly 142 have optical magnitudes and colors consistent with cluster membership. The observed distribution of L(x) peaks at L(x) similar to 1030.3 erg s(-1) and likely traces the bright edge of a far larger population of approximate to 0.4-2 M(circle dot) X-ray active stars. From a short list of X-ray active stars with IRAC 8 mu m excess from warm, terrestrial zone dust, we derive a maximum X-ray flux incident on forming terrestrial planets. Although there is no correlation between X-ray activity and IRAC excess, the fractional X-ray luminosity correlates with optical colors and spectral type. By comparing the distribution of L(x)/L(star) versus spectral type and V-I in h Per with results for other 1-100 Myr-old clusters, we show that stars slightly more massive than the Sun (greater than or similar to 1.5M(circle dot)) fall out of X-ray saturation by approximate to 10-15 Myr. Changes in stellar structure for greater than or similar to 1.5M(circle dot) stars likely play an important role in this decline of X-ray emission. C1 [Currie, Thayne; Evans, Nancy Remage; Spitzbart, Brad D.; Irwin, Jonathan; Wolk, Scott J.; Kenyon, Scott J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hernandez, Jesus] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Hernandez, Jesus] Williams Coll, Dept Astron, Williamstown, MA 01267 USA. [Pasachoff, Jay M.] Ctr Invest Astron, Merida 5101A, Venezuela. RP Currie, T (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM tcurrie@cfa.harvard.edu OI Kenyon, Scott/0000-0003-0214-609X; Wolk, Scott/0000-0002-0826-9261 FU NASA Astrophysics Theory [t NAG513278]; Spitzer GO [1320379]; NASA TPF Foundation Science [NNG06GH25]; SAO Predoctoral Fellowship; NASA [NAS8-03060, G06007A] FX We thank Leslie Hebb and Simon Hodgkin for KPNO observing and Nelson Caldwell, Susan Tokarz, Perry Berlind, and Mike Calkins for scheduling, taking, and reducing the Hectospec spectra. We also thank Tom Barnes and Rebecca Cover for early work on this project. Comments from the referee, Leisa Townsley, greatly improved the manuscript. This work is supported by NASA Astrophysics Theory grant NAG513278, Spitzer GO grant 1320379, and NASA TPF Foundation Science grant NNG06GH25G. T. C. received support from a SAO Predoctoral Fellowship. N. R. E., B. D. S, and S. J. W. are supported by NASA contract numbers NAS8-03060 and G06007A. NR 73 TC 12 Z9 12 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD FEB PY 2009 VL 137 IS 2 BP 3210 EP 3221 DI 10.1088/0004-6256/137/2/3210 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 400WV UT WOS:000262901000020 ER PT J AU Edmonds, R Wagg, J Momjian, E Carilli, CL Wilner, DJ Humphreys, EML Menten, KM Hughes, DH AF Edmonds, R. Wagg, J. Momjian, E. Carilli, C. L. Wilner, D. J. Humphreys, E. M. L. Menten, K. M. Hughes, D. H. TI AN EXPANDED VERY LARGE ARRAY SEARCH FOR WATER MEGAMASER EMISSION IN THE SUBMM GALAXY SMM J16359+6612 AT z=2.5 SO ASTRONOMICAL JOURNAL LA English DT Article DE cosmology: observations; galaxies: starburst; gravitational lensing; masers ID DEEP SUBMILLIMETER SURVEY; STAR-FORMING GALAXIES; FIR BRIGHT GALAXIES; HIGH-REDSHIFT; H2O MASERS; MILLIMETER SOURCES; SPECTRAL INDEX; MOLECULAR GAS; FIELD-NORTH; RADIO AB Using the Expanded Very Large Array, we have conducted a search for 22.2 GHz H(2)O megamaser emission in the strongly lensed submm galaxy, SMM J16359+6612 at z = 2.517. This object is lensed into three components, and after a correction for magnification is applied to its submm-wavelength flux density, it is typical of the bulk of the high-redshift, submm galaxy population responsible for the 850 mu m extragalactic background (S850 mu m similar to 1 mJy). We do not detect any H(2)O megamaser emission, but the lensing allows us to place an interesting constraint on the luminosity of any megamasers present, L(H2O) < 5305 L(circle dot) for an assumed linewidth of 80 km s(-1). Because the far-infrared luminosity in submm galaxies is mainly powered by star formation, and very luminous H(2)O megamasers are more commonly associated with quasar activity, it could be that blind searches for H(2)O megamasers will not be an effective means of determining redshifts for less-luminous members of the submm galaxy population. C1 [Edmonds, R.; Wagg, J.; Momjian, E.; Carilli, C. L.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Wilner, D. J.; Humphreys, E. M. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Menten, K. M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Hughes, D. H.] INAOE, Puebla, Mexico. RP Edmonds, R (reprint author), Natl Radio Astron Observ, POB 0, Socorro, NM 87801 USA. EM jwagg@aoc.nrao.edu NR 45 TC 3 Z9 3 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD FEB PY 2009 VL 137 IS 2 BP 3293 EP 3296 DI 10.1088/0004-6256/137/2/3293 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 400WV UT WOS:000262901000027 ER PT J AU Ness, JU Drake, JJ Starrfield, S Bode, MF O'Brien, TJ Evans, A Eyres, SPS Helton, LA Osborne, JP Page, KL Schneider, C Woodward, CE AF Ness, J. -U. Drake, J. J. Starrfield, S. Bode, M. F. O'Brien, T. J. Evans, A. Eyres, S. P. S. Helton, L. A. Osborne, J. P. Page, K. L. Schneider, C. Woodward, C. E. TI HIGH-RESOLUTION X-RAY SPECTROSCOPY OF THE EVOLVING SHOCK IN THE 2006 OUTBURST OF RS OPHIUCHI SO ASTRONOMICAL JOURNAL LA English DT Article DE binaries: symbiotic; methods: data analysis; novae, cataclysmic variables; shock waves; stars: individual (RSOph); X-rays: stars ID HELIUM-LIKE IONS; K-ALPHA COMPLEX; HE-LIKE IRON; CLASSICAL NOVAE; SYMBIOTIC STARS; RECURRENT NOVAE; RED GIANTS; INFRARED-SPECTROSCOPY; CHEMICAL-COMPOSITION; INTERSTELLAR-MEDIUM AB The evolution of the 2006 outburst of the recurrent nova RS Ophiuchi was followed with 12 X-ray grating observations with Chandra and XMM-Newton. We present detailed spectral analyses using two independent approaches. From the best data set, taken on day 13.8 after outburst, we reconstruct the temperature distribution and derive elemental abundances. We find evidence for at least two distinct temperature components on day 13.8 and a reduction of temperature with time. The X-ray flux decreases as a power-law, and the index changes from -5/3 to -8/3 around day 70 after outburst. This can be explained by different decay mechanisms for the hot and cool components. The decay of the hot component and the decrease in temperature are consistent with radiative cooling, while the decay of the cool component can be explained by the expansion of the ejecta. We find overabundances of N and of alpha elements, which could either represent the composition of the secondary that provides the accreted material or that of the ejecta. The N overabundance indicates CNO-cycled material. From comparisons to abundances for the secondary taken from the literature, we conclude that 20%-40% of the observed nitrogen could originate from the outburst. The overabundance of the a elements is not typical for stars of the spectral type of the secondary in the RS Oph system, and white dwarf material might have been mixed into the ejecta. However, no direct measurements of the alpha elements in the secondary are available, and the continuous accretion may have changed the observable surface composition. C1 [Ness, J. -U.; Starrfield, S.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Drake, J. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bode, M. F.] Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England. [O'Brien, T. J.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Observ, Macclesfield SK11 9DL, Cheshire, England. [Evans, A.] Univ Keele, Astrophys Grp, Keele ST5 5BG, Staffs, England. [Eyres, S. P. S.] Univ Cent Lancashire, Sch Comp Engn & Phys Sci, Ctr Astrophys, Preston PR1 2HE, Lancs, England. [Helton, L. A.; Woodward, C. E.] Univ Minnesota, Sch Phys & Astron, Dept Astron, Minneapolis, MN 55455 USA. [Osborne, J. P.; Page, K. L.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Schneider, C.] Hamburger Sternwarte, D-21029 Hamburg, Germany. RP Ness, JU (reprint author), Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. EM juness@sciop.esa.int NR 75 TC 28 Z9 28 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD FEB PY 2009 VL 137 IS 2 BP 3414 EP 3436 DI 10.1088/0004-6256/137/2/3414 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 400WV UT WOS:000262901000038 ER PT J AU Ascenso, J Alves, J Lago, MTVT AF Ascenso, J. Alves, J. Lago, M. T. V. T. TI No evidence of mass segregation in massive young clusters SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE open clusters and associations: general; methods: statistical ID ORION NEBULA CLUSTER; STAR-CLUSTERS; LUMINOSITY FUNCTION; STELLAR POPULATION; MAGELLANIC-CLOUD; ARCHES CLUSTER; STARBURST; EVOLUTION; MOTION AB Aims. We investigate the validity of the mass segregation indicators commonly used in analysing young stellar clusters. Methods. We simulate observations by constructing synthetic seeing-limited images of a 1000 massive clusters (10(4) M(circle dot)) with a standard IMF and a King-density distribution function. Results. We find that commonly used indicators are highly sensitive to sample incompleteness in observational data and that radial completeness determinations do not provide satisfactory corrections, rendering the studies of radial properties highly uncertain. On the other hand, we find that, under certain conditions, the global completeness can be estimated accurately, allowing for the correction of the global luminosity and mass functions of the cluster. Conclusions. We argue that there is currently no observational evidence of mass segregation in young compact clusters since there is no robust way to differentiate between true mass segregation and sample incompleteness effects. Caution should then be exercised when interpreting results from observations as evidence of mass segregation. C1 [Ascenso, J.; Lago, M. T. V. T.] Univ Porto, Ctr Astrofis, P-4150762 Oporto, Portugal. [Ascenso, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Alves, J.] Ctr Astronom Hispano Aleman, Calar Alto Observ, Almeria 04004, Spain. [Lago, M. T. V. T.] Univ Porto, Fac Ciencias, Dept Matemat Aplicada, P-4169007 Oporto, Portugal. RP Ascenso, J (reprint author), Univ Porto, Ctr Astrofis, Rua Estrelas, P-4150762 Oporto, Portugal. EM jascenso@astro.up.pt OI Alves, Joao/0000-0002-4355-0921 FU FCT, Portugal [SFRH/BD/13355/2003, POCTI/CFEAST/55691/2004] FX J. Ascenso acknowledges financial support from FCT, Portugal (grant SFRH/BD/13355/2003 and project POCTI/CFEAST/55691/2004) and is grateful to the Calar Alto Observatory for hosting a very important part of the work. A special thanks also to Jarle Brinchmann and Prof. Pedro Lago for the helpful discussions of statistics. We also thank the anonymous referee for the constructive comments that contributed to improving this work. NR 24 TC 42 Z9 42 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD FEB PY 2009 VL 495 IS 1 BP 147 EP 155 DI 10.1051/0004-6361/200809886 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 410BL UT WOS:000263550000013 ER PT J AU Cappelluti, N Ajello, M Rebusco, P Komossa, S Bongiorno, A Clemens, C Salvato, M Esquej, P Aldcroft, T Greiner, J Quintana, H AF Cappelluti, N. Ajello, M. Rebusco, P. Komossa, S. Bongiorno, A. Clemens, C. Salvato, M. Esquej, P. Aldcroft, T. Greiner, J. Quintana, H. TI A candidate tidal disruption event in the Galaxy cluster Abell 3571 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE X-rays: galaxies; galaxies: clusters: individual: Abell 3571; galaxies: nuclei; X-rays: bursts; galaxies: active ID SUPERMASSIVE BLACK-HOLES; X-RAY OUTBURSTS; GALACTIC NUCLEI; XMM-NEWTON; STAR; LUMINOSITY; CENTERS; OBJECTS; NEARBY; FLARE AB Context. Tidal disruption events are possible sources of temporary nuclear activity in galactic nuclei and can be considered as good indicators of the existence of supermassive black holes in the centers of galaxies. Aims. A new X-ray source has been detected serendipitously with ROSAT in a PSPC pointed observation of the galaxy cluster A3571. Given the strong flux decay of the object in subsequent detections, the tidal disruption scenario is investigated as a possible explanation of the event. Methods. We followed the evolution of the X-ray transient with ROSAT, XMM-Newton and Chandra for a total period of similar to 13 years. We also obtained 7-band optical/NIR photometry with GROND at the ESO/MPI 2.2 m telescope. Results. We report a very large decay of the X-ray flux of the ROSAT source identified with the galaxy LEDA 095953, a member of the cluster Abell 3571. We measured a maximum 0.3-2.4 keV luminosity Log (L(X)) = 42.8 erg s(-1). The high state of the source lasted at least 150 ks; afterwards L(X) declined as similar to t(-2). The spectrum of the brightest epoch is consistent with a black body with temperature kT similar to 0.12 keV. Conclusions. The total energy released by this event in 10 yr was estimated to be Delta E > 2 x 10(50) erg. We interpret this event as a tidal disruption of a solar type star by the central supermassive black hole (i.e. similar to 10(7) M(circle dot)) of the galaxy. C1 [Cappelluti, N.; Komossa, S.; Bongiorno, A.; Clemens, C.; Esquej, P.; Greiner, J.] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. [Cappelluti, N.] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA. [Ajello, M.] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA. [Ajello, M.] KIPAC, Menlo Pk, CA 94025 USA. [Rebusco, P.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Salvato, M.] CALTECH, Pasadena, CA 91125 USA. [Esquej, P.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Aldcroft, T.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Quintana, H.] Pontificia Univ Catolica Chile, Dept Astron & Astrophys, Santiago, Chile. RP Cappelluti, N (reprint author), Max Planck Inst Extraterr Phys, Postfach 1312, D-85741 Garching, Germany. EM cap@mpe.mpg.de OI Bongiorno, Angela/0000-0002-0101-6624; Cappelluti, Nico/0000-0002-1697-186X FU Pappalardo fellowship; FONDAP Centro de Astrofisica FX The XMM-Newton, Chandra and ROSAT archival systems and the full GROND team are acknowledged. P. R. is supported by the Pappalardo fellowship at MIT. H. Q. thanks partial support from the FONDAP Centro de Astrofisica. NR 34 TC 42 Z9 42 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD FEB PY 2009 VL 495 IS 2 BP L9 EP L12 DI 10.1051/0004-6361/200811479 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 413EM UT WOS:000263775700002 ER PT J AU Cornelisse, R D'Avanzo, P Munoz-Darias, T Campana, S Casares, J Charles, PA Steeghs, D Israel, G Stella, L AF Cornelisse, R. D'Avanzo, P. Munoz-Darias, T. Campana, S. Casares, J. Charles, P. A. Steeghs, D. Israel, G. Stella, L. TI Phase-resolved spectroscopy of the accreting millisecond X-ray pulsar SAX J1808.4-3658 during the 2008 outburst SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE accretion, accretion disks; X-rays: binaries; stars: individual: SAXJ1808.4-3658 ID DONOR; STAR; LMXBS; ORBIT; DISKS AB Aims. We obtained phase-resolved spectroscopy of the accreting millisecond X-ray pulsar SAX J1808.4-3658 during its outburst in 2008 to find a signature of the donor star, constrain its radial velocity semi-amplitude (K(2)), and derive estimates for the pulsar mass. Methods. Using Doppler images of the Bowen region, we find a significant (>= 8 sigma) compact spot at a position where the donor star is expected. If this is a signature of the donor star, we measure K(em) = 248 +/- 20 km s(-1) (1 sigma confidence), which represents a strict lower limit to K(2). Also, the Doppler map of He II lambda 4686 shows the characteristic signature of the accretion disc, and there is a hint of enhanced emission that may be a result of tidal distortions in the accretion disc that are expected in very low mass-ratio interacting binaries. Results. The lower limit on K(2) leads to a lower limit on the mass function of f (M(1)) >= 0.10 M(circle dot). Applying the maximum K-correction gives 228 < K(2) < 322 km s(-1) and a mass ratio of 0.051 < q < 0.072. Conclusions. Despite the limited S/N of the data, we were able to detect a signature of the donor star in SAXJ1808.4-3658, although future observations during a new outburst are still needed to confirm this. If the derived K(em) is correct, the largest uncertainty in determining of the mass of the neutron star in SAXJ1808.4-3658 using dynamical studies lies with the poorly known inclination. C1 [Cornelisse, R.; Munoz-Darias, T.; Casares, J.] Inst Astrofis Canarias, San Cristobal la Laguna 3805, Spain. [D'Avanzo, P.; Campana, S.] INAF, Osservatorio Astron Brera, I-23807 Merate, Italy. [Charles, P. A.] S African Astron Observ, ZA-7935 Cape Town, South Africa. [Charles, P. A.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Steeghs, D.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Steeghs, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Israel, G.; Stella, L.] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy. RP Cornelisse, R (reprint author), Inst Astrofis Canarias, Calle Via Lactea S-N, San Cristobal la Laguna 3805, Spain. EM corneli@iac.es RI Steeghs, Danny/C-5468-2009; OI Steeghs, Danny/0000-0003-0771-4746; Campana, Sergio/0000-0001-6278-1576; Israel, GianLuca/0000-0001-5480-6438 FU STFC Advanced Fellowship; Spanish MCYT [AYA2007-66887]; Spanish MEC [CSD2006-00070] FX We cordially thank the director of the European Southern Observatory for granting Director's Discretionary Time (ID 281.D-5060(A). We would like to thank the referee, Craig Heinke, for the careful and helpful comments which have improved this paper. R. C. acknowledges a Ramon y Cajal fellowship (RYC-2007-01046). R. C. acknowledges Katrien Uytterhoeven for useful discussions of different analysis techniques. P. D. A. and S. C. thank S. Covino for useful discussions. D. S. acknowledges an STFC Advanced Fellowship. J. C. acknowledges support by the Spanish MCYT GRANT AYA2007-66887. Partially funded by the Spanish MEC under the Consolider-Ingenio 2010 Program grant CSD2006-00070: First Science with the GTC. NR 19 TC 3 Z9 3 U1 0 U2 2 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD FEB PY 2009 VL 495 IS 1 BP L1 EP L4 DI 10.1051/0004-6361:200811396 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 410BL UT WOS:000263550000001 ER PT J AU Perina, S Barmby, P Beasley, MA Bellazzini, M Brodie, JP Burstein, D Cohen, JG Federici, L Pecci, FF Galleti, S Hodge, PW Huchra, JP Kissler-Patig, M Puzia, TH Strader, J AF Perina, S. Barmby, P. Beasley, M. A. Bellazzini, M. Brodie, J. P. Burstein, D. Cohen, J. G. Federici, L. Pecci, F. Fusi Galleti, S. Hodge, P. W. Huchra, J. P. Kissler-Patig, M. Puzia, T. H. Strader, J. TI An HST/WFPC2 survey of bright young clusters in M31 I. VdB0, a massive star cluster seen at t similar or equal to 25 Myr SO ASTRONOMY & ASTROPHYSICS LA English DT Review DE galaxies: star clusters; galaxies: individual: M31; stars: supergiants; stars: evolution ID LARGE-MAGELLANIC-CLOUD; COLOR-MAGNITUDE DIAGRAMS; EXTRAGALACTIC GLOBULAR-CLUSTERS; RESOLVED STELLAR POPULATIONS; TELESCOPE WFPC2 PHOTOMETRY; LOCAL GROUP GALAXIES; MILKY-WAY; LUMINOSITY FUNCTION; STRUCTURAL PARAMETERS; EVOLUTION DATABASE AB Aims. We introduce our imaging survey of possible young massive globular clusters in M31 performed with the Wide Field and Planetary Camera 2 (WFPC2) on the Hubble Space Telescope (HST). We obtained shallow (to B similar to 25) photometry of individual stars in 20 candidate clusters. We present here details of the data reduction pipeline that is being applied to all the survey data and describe its application to the brightest among our targets, van den Bergh 0 (VdB0), taken as a test case. Methods. Point spread function fitting photometry of individual stars was obtained for all the WFPC2 images of VdB0 and the completeness of the final samples was estimated using an extensive set of artificial stars experiments. The reddening, the age and the metallicity of the cluster were estimated by comparing the observed color magnitude diagram (CMD) with theoretical isochrones. Structural parameters were obtained from model-fitting to the intensity profiles measured within circular apertures on the WFPC2 images. Results. Under the most conservative assumptions, the stellar mass of VdB0 is M > 2.4 x 10(4) M(circle dot), but our best estimates lie in the range similar or equal to 4-9 x 10(4) M(circle dot). The CMD of VdB0 is best reproduced by models having solar metallicity and age similar or equal to 25 Myr. Ages less than similar or equal to 12 Myr and greater than similar or equal to 60 Myr are clearly ruled out by the available data. The cluster has a remarkable number of red super giants (greater than or similar to 18) and a CMD very similar to Large Magellanic Cloud clusters usually classified as young globulars such as NGC 1850, for example. Conclusions. VdB0 is significantly brighter (greater than or similar to 1 mag) than Galactic open clusters of similar age. Its present-day mass and half-light radius (r(h) = 7.4 pc) are more typical of faint globular clusters than of open clusters. However, given its position within the disk of M31, it is expected to be destroyed by dynamical effects, in particular by encounters with giant molecular clouds, within the next similar to 4 Gyr. C1 [Perina, S.; Bellazzini, M.; Federici, L.; Pecci, F. Fusi; Galleti, S.] Osservatorio Astron Bologna, INAF, I-40127 Bologna, Italy. [Perina, S.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. [Barmby, P.] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada. [Beasley, M. A.; Brodie, J. P.] Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Santa Cruz, CA 95064 USA. [Beasley, M. A.] Inst Astrofis Canarias, E-38200 San Cristobal la Laguna, Canary Islands, Spain. [Burstein, D.] Arizona State Univ, Dept Phys & Astron, Tempe, AZ 85287 USA. [Cohen, J. G.] CALTECH, Palomar Observ, Pasadena, CA 91125 USA. [Hodge, P. W.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Huchra, J. P.; Strader, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kissler-Patig, M.] European So Observ, D-85748 Garching, Germany. [Puzia, T. H.] Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. RP Perina, S (reprint author), Osservatorio Astron Bologna, INAF, Via Ranzani 1, I-40127 Bologna, Italy. EM sibilla.perina2@unibo.it; michele.bellazzini@oabo.inaf.it; jlc@astro.caltech.edu RI Bellazzini , Michele/O-9373-2015; Barmby, Pauline/I-7194-2016 OI Bellazzini , Michele/0000-0001-8200-810X; Barmby, Pauline/0000-0003-2767-0090 FU INAF [CRA 1.06.10.04]; Natural Sciences and Engineering Research Council of Canada; STcI [HST-GO-10818.01-A]; Plaskett Fellowship at the Herzberg institute of Astrophysics in Victoria; NASA through an Hubble Fellowship FX S. P. and M. B. acknowledge the financial support of INAF through the PRIN 2007 grant CRA 1.06.10.04 "The local route to galaxy formation ...". P. B. acknowledges research support through a Discovery Grant from the Natural Sciences and Engineering Research Council of Canada. J.G.C. is grateful for partial support through grant HST-GO-10818.01-A from the STcI. T. H. P. gratefully acknowledges support in form of a Plaskett Fellowship at the Herzberg institute of Astrophysics in Victoria, BC. J.S. was supported by NASA through an Hubble Fellowship, administered by STScI. We are grateful to S. van den Bergh for having pointed out some errors in the historical reconstruction of the discovery of VdB0 that were reported in a previous version of the paper. NR 101 TC 27 Z9 27 U1 1 U2 2 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD FEB PY 2009 VL 494 IS 3 BP 933 EP 948 DI 10.1051/0004-6361:200810725 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 406SP UT WOS:000263315500013 ER PT J AU Zwintz, K Kallinger, T Guenther, DB Gruberbauer, M Huber, D Rowe, J Kuschnig, R Weiss, WW Matthews, JM Moffat, AFJ Rucinski, SM Sasselov, D Walker, GAH Casey, MP AF Zwintz, K. Kallinger, T. Guenther, D. B. Gruberbauer, M. Huber, D. Rowe, J. Kuschnig, R. Weiss, W. W. Matthews, J. M. Moffat, A. F. J. Rucinski, S. M. Sasselov, D. Walker, G. A. H. Casey, M. P. TI MOST photometry of the enigmatic PMS pulsator HD 142666 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: pre-main sequence; stars: variables: delta Sct; stars: individual: HD 142666; techniques: photometric ID PRE-MAIN-SEQUENCE; STANDARD SOLAR MODEL; TIME-SERIES DATA; INSTABILITY STRIP; FOURIER SPACE; STARS; OPACITIES; SEISMOLOGY; REDUCTION; EVOLUTION AB Context. Modeling of pre-main sequence (PMS) stars through asteroseismology of PMS p-mode pulsators has only recently become possible, and spacebased photometry is one of the important sources of data for these efforts. We present precise photometry of the pulsating Herbig Ae star HD 142666 obtained in two consecutive years with the MOST (Microvariability & Oscilations of STars) satellite. Aims. Previously, only a single pulsation period was known for HD 142666. The MOST photometry reveals that HD 142666 is multiperiodic. However, the unique identification of pulsation frequencies is complicated by the presence of irregular variability caused by the star's circumstellar dust disk. The two light curves obtained with MOST in 2006 and 2007 provided data of unprecedented quality to study the pulsations in HD 142666 and also to monitor the circumstellar variability. Methods. Frequency analysis was performed using the routine SIGSPEC and the results from the 2006 and 2007 campaigns were then compared to each other with the software CINDERELLA to identify frequencies common to both light curves. The correlated frequencies were then submitted to an asteroseismic analysis. Results. We attribute 12 frequencies to pulsation. Model fits to the three frequencies with the highest amplitudes lie well outside the uncertainty box for the star's position in the HR diagram based on published values. Some of the frequencies appear to be rotationally split modes. Conclusions. The models suggest that either (1) the published estimate of the luminosity of HD 142666, based on a relation between circumstellar disk radius and stellar luminosity, is too high and/or (2) additional physics such as mass accretion may be needed in our models to accurately fit both the observed frequencies and HD 142666's position in the HR diagram. C1 [Zwintz, K.; Kallinger, T.; Gruberbauer, M.; Huber, D.; Kuschnig, R.; Weiss, W. W.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria. [Guenther, D. B.; Casey, M. P.] St Marys Univ, Dept Phys & Astron, Halifax, NS B3H 3C3, Canada. [Rowe, J.; Kuschnig, R.; Matthews, J. M.; Walker, G. A. H.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Rowe, J.] NASA, Moffett Field, CA 94035 USA. [Moffat, A. F. J.] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada. [Rucinski, S. M.] Univ Toronto, David Dunlap Observ, Richmond Hill, ON L4C 4Y6, Canada. [Sasselov, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Huber, D.] Univ Sydney, Sch Phys, Inst Astron, Sydney, NSW 2006, Australia. RP Zwintz, K (reprint author), Univ Vienna, Inst Astron, Turkenschanzstr 17, A-1180 Vienna, Austria. EM zwintz@astro.univie.ac.at; kallinger@astro.univie.ac.at; guenther@ap.smu.ca; Gruberbauer@astro.univie.ac.at; dhuber@physics.usyd.edu.au; rowe@phas.ubc.ca; kuschnig@astro.ubc.ca; Weiss@astro.univie.ac.at; matthews@astro.ubc.ca; moffat@astro.umontreal.ca; rucinski@astro.utoronto.ca; sasselov@cfa.harvard.edu; gordonwa@uvic.ca; mcasey@astro.univie.ac.at OI Kallinger, Thomas/0000-0003-3627-2561; Zwintz, Konstanze/0000-0001-9229-8315 FU Austrian Fonds zur Forderung der wissenschaftlichen Forschung [T335-N16P17580]; The Natural Sciences and Engineering Research Council of Canada; FQRT (Quebec); Canadian Space Agency FX K. Z., T. K., M. G., R. K. and W. W. W. acknowledge support by the Austrian Fonds zur Forderung der wissenschaftlichen Forschung (KZ: project T335-N16; TK, MG, RK and WWW: project P17580). The Natural Sciences and Engineering Research Council of Canada supports the research of D. B. G., J. M. M., A. F. J. M., S. M. R. and M. P. C; A. F. J. M. is also supported by FQRT (Quebec), and R. K. is also supported by the Canadian Space Agency. Special thanks goes to Gregg Wade and Jason Grunhunt who provided the newest values for Teff. NR 40 TC 8 Z9 8 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD FEB PY 2009 VL 494 IS 3 BP 1031 EP 1040 DI 10.1051/0004-6361:200811116 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 406SP UT WOS:000263315500022 ER PT J AU Temim, T Slane, P Gaensler, BM Hughes, JP Van Der Swaluw, E AF Temim, Tea Slane, Patrick Gaensler, B. M. Hughes, John P. Van Der Swaluw, Eric TI CHANDRA AND XMM OBSERVATIONS OF THE COMPOSITE SUPERNOVA REMNANT G327.1-1.1 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: individual (G327.1-1.1); pulsars: general; supernova remnants; X-rays: ISM ID PULSAR WIND NEBULAE; X-RAY; EMISSION; MODEL AB We present new X-ray imaging and spectroscopy of a composite supernova remnant G327.1-1.1 using the Chandra and XMM-Newton X-ray observatories. G327.1-1.1 has an unusual morphology consisting of a symmetric radio shell and an off center nonthermal component that indicates the presence of a pulsar wind nebula (PWN). Radio observations show a narrow finger of emission extending from the PWN structure toward the northwest. X-ray studies with ASCA, ROSAT, and BeppoSAX revealed elongated extended emission and a compact source at the tip of the finger that may be coincident with the actual pulsar. The high resolution Chandra observations provide new insight into the structure of the inner region of the remnant. The images show a compact source embedded in a cometary structure from which a trail of X-ray emission extends in the southeast direction. The Chandra images also reveal two prong-like structures that appear to originate from the vicinity of the compact source and extend into a large bubble that is oriented in the northwest direction, opposite from the bright radio PWN. The emission from the entire radio shell is detected in the XMM data and can be characterized by a thermal plasma model with a temperature of similar to 0.3 keV, which we use to estimate the physical properties of the remnant. The peculiar morphology of G327.1-1.1 may be explained by the emission from a moving pulsar and a relic PWN that has been disrupted by the reverse shock. C1 [Temim, Tea; Slane, Patrick] CfA, Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA. [Temim, Tea] Univ Minnesota, Sch Phys & Astron, Dept Astron, Minneapolis, MN 55455 USA. [Gaensler, B. M.] Univ Sydney, Sch Phys, Inst Astron, Sydney, NSW 2006, Australia. [Hughes, John P.] Rutgers State Univ, Piscataway, NJ USA. [Van Der Swaluw, Eric] Royal Netherlands Meteorol Inst KNMI, De Bilt, Netherlands. RP Temim, T (reprint author), CfA, Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA. RI Gaensler, Bryan/F-8655-2010; OI Gaensler, Bryan/0000-0002-3382-9558; Temim, Tea/0000-0001-7380-3144 FU NASA [GO6-7053X, NAS8-03060]; Australian Research Council [FF0561298] FX Declination Support for this work is provided by NASA Grant GO6-7053X. B.M.G. acknowledges support from the Australian Research Council through a Federation Fellowship (grant FF0561298). P.O.S. acknowledges support from NASA contract NAS8-03060. NR 25 TC 12 Z9 12 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2009 VL 691 IS 2 BP 895 EP 906 DI 10.1088/0004-637X/691/2/895 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 406OH UT WOS:000263304300001 ER PT J AU Chung, SM Gonzalez, AH Clowe, D Zaritsky, D Markevitch, M Jones, C AF Chung, Sun Mi Gonzalez, Anthony H. Clowe, Douglas Zaritsky, Dennis Markevitch, Maxim Jones, Christine TI IMPACTS OF A SUPERSONIC SHOCK FRONT ON STAR FORMATION IN THE BULLET CLUSTER SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: individual (1E0657-56, The Bullet Cluster); galaxies: evolution ID POLYCYCLIC AROMATIC-HYDROCARBONS; NEED ULTRAVIOLET EXCITATION; SPITZER-SPACE-TELESCOPE; ACTIVE GALACTIC NUCLEI; RAM-PRESSURE; EMISSION FEATURES; VIRGO CLUSTER; DARK-MATTER; SPECTROSCOPIC SURVEY; SPIRAL GALAXIES AB We use the Bullet Cluster (1E0657-56) to investigate the extent to which star formation in cluster galaxies is influenced by ram pressure from supersonic gas (Mach 3) during a cluster merger. While the effects of ram pressure have been studied for individual galaxies infalling into galaxy clusters, this system provides a unique opportunity to investigate the impact of dramatic merger events on the cluster galaxy population. In this analysis, we use Spitzer IRAC data to study star formation. At the redshift of the cluster, the 6.2 mu m PAH feature is redshifted into the 8 mu m band, enabling use of the m(4.5) - m(8) color as a proxy for specific star formation rate. We find that the color distribution on the two sides of the shock differs by less than 2 sigma, and conclude that ram pressure from the shock front has no dramatic, immediate impact on the star formation of cluster galaxies in the Bullet Cluster. C1 [Chung, Sun Mi; Gonzalez, Anthony H.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Clowe, Douglas] Ohio Univ, Dept Phys & Astron, Clippinger Lab 251B, Athens, OH 45701 USA. [Zaritsky, Dennis] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Markevitch, Maxim; Jones, Christine] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Chung, SM (reprint author), Univ Florida, Dept Astron, Gainesville, FL 32611 USA. EM schung@astro.ufl.edu FU NASA/Spitzer [1319141]; NASA [NAS8-39073]; Chandra [GO8-9128X]; Spitzer [1265584] FX The authors thank Rafael Barrena for sharing his redshift data with us. We also acknowledge support for this work from NASA/Spitzer grant 1319141. M.M. was supported by NASA contract NAS8-39073 and Chandra grant GO8-9128X. C.J. acknowledges support from Spitzer Contract 1265584. NR 52 TC 14 Z9 14 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2009 VL 691 IS 2 BP 963 EP 970 DI 10.1088/0004-637X/691/2/963 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 406OH UT WOS:000263304300005 ER PT J AU Johannsen, T Psaltis, D McClintock, JE AF Johannsen, Tim Psaltis, Dimitrios McClintock, Jeffrey E. TI CONSTRAINTS ON THE SIZE OF EXTRA DIMENSIONS FROM THE ORBITAL EVOLUTION OF BLACK-HOLE X-RAY BINARIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; gravitation; stars: individual (A0620-00); X-rays: binaries; X-rays: stars ID MAGNETIC BRAKING; ACCRETION DISC; A0620-00; MASS; MILLIMETER; GRAVITY; PULSARS AB One of the plausible unification schemes in physics considers the observable universe to be a four-dimensional surface (the "brane") embedded in a higher dimensional curved spacetime (the "bulk"). In such braneworld gravity models with infinitely large extra dimensions, black holes evaporate fast through the emission of the additional gravitational degrees of freedom, resulting in lifetimes of stellar-mass black holes that are significantly smaller than the Hubble time. We show that the predicted evaporation rate leads to a change in the orbital period of X-ray binaries harboring black holes that is observable with current instruments. We obtain an upper limit on the rate of change of the orbital period of the binary A0620-00 and use it to constrain the asymptotic curvature radius of the extra dimension to a value comparable to the one obtained by table-top experiments. Furthermore, we argue that any measurement of a period increase for low-mass X-ray binaries with a high mass ratio is evidence for new physics beyond general relativity and the standard model. C1 [Johannsen, Tim] Univ Arizona, Dept Phys, Tucson, AZ 85721 USA. [Psaltis, Dimitrios] Univ Arizona, Dept Phys & Astron, Tucson, AZ 85721 USA. [McClintock, Jeffrey E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Johannsen, T (reprint author), Univ Arizona, Dept Phys, 1118 E 4th St, Tucson, AZ 85721 USA. EM timj@physics.arizona.edu; dpsaltis@physics.arizona.edu; jem@head.cfa.harvard.edu FU NSF CAREER [NSF 0746549] FX We thank Nemanja Kaloper and Keith Dienes for fruitful discussions as well as Jack Steiner for his help with the IDL curvefit calculations. We also thank Saul Rappaport for his input on issues of black hole binary evolution. This work was supported in part by the NSF CAREER award NSF 0746549. NR 32 TC 30 Z9 30 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2009 VL 691 IS 2 BP 997 EP 1004 DI 10.1088/0004-637X/691/2/997 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 406OH UT WOS:000263304300008 ER PT J AU Heinke, CO Jonker, PG Wijnands, R Deloye, CJ Taam, RE AF Heinke, C. O. Jonker, P. G. Wijnands, R. Deloye, C. J. Taam, R. E. TI FURTHER CONSTRAINTS ON THERMAL QUIESCENT X-RAY EMISSION FROM SAX J1808.4-3658 SO ASTROPHYSICAL JOURNAL LA English DT Article DE dense matter; pulsars: general; stars: neutron; X-rays: binaries ID ACCRETING MILLISECOND PULSAR; XMM-NEWTON OBSERVATIONS; PHOTON IMAGING CAMERA; NEUTRON-STAR; IGR J00291+5934; CHANDRA OBSERVATIONS; GLOBULAR-CLUSTER-47 TUCANAE; TRANSIENT 1H-1905+000; DISCOVERY; OUTBURST AB We observed SAX J1808.4-3658 (1808), the first accreting millisecond pulsar, in deep quiescence with XMM-Newton and (near simultaneously) Gemini-South. The X-ray spectrum of 1808 is similar to that observed in quiescence in 2001 and 2006, describable by an absorbed power law with photon index 1.74 +/- 0.11 and unabsorbed X-ray luminosity L(X) = 7.9 +/- 0.7 x 10(31) ergs s(-1), for N(H) = 1.3 x 10(21) cm(-2). Fitting all the quiescent XMM-Newton X-ray spectra with a power law, we constrain any thermally emitting neutron star (NS) with a hydrogen atmosphere to have a temperature less than 30 eV and L(NS) (0.01-10 keV) 6.2 x 10(30) ergs s(-1). A thermal plasma model also gives an acceptable fit to the continuum. Adding an NS component to the plasma model produces less stringent constraints on the NS; a temperature of 36(-8)(+4) eV and L(NS) (0.01-10 keV) = 1.3(-0.8)(+0.6) x 10(31) ergs s(-1). In the framework of the current theory of NS heating and cooling, the constraints on the thermal luminosity of 1808 and 1H 1905+000 require strongly enhanced cooling in the cores of these NSs. We compile data from the literature on the mass transfer rates and quiescent thermal flux of the largest possible sample of transient NS low-mass X-ray binaries. We identify a thermal component in the quiescent spectrum of the accreting millisecond pulsar IGR J00291+5934, which is consistent with the standard cooling model. The contrast between the cooling rates of IGR J00291+5934 and 1808 suggests that 1808 may have a significantly larger mass. This can be interpreted as arising from differences in the binary evolution history or initial NS mass in these otherwise similar systems. C1 [Heinke, C. O.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2G7, Canada. [Heinke, C. O.] Univ Virginia, Dept Astron, Charlottesville, VA 22902 USA. [Heinke, C. O.; Deloye, C. J.; Taam, R. E.] Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA. [Jonker, P. G.] SRON, Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands. [Jonker, P. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Wijnands, R.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. [Taam, R. E.] ASIAA Natl Tsing Hua Univ, Hsinchu, Taiwan. RP Heinke, CO (reprint author), Univ Alberta, Dept Phys, 11322-89 Ave, Edmonton, AB T6G 2G7, Canada. EM cheinke@phys.ualberta.ca OI Heinke, Craig/0000-0003-3944-6109 FU Lindheimer Postdoctoral Fellowship at Northwestern University; NASA Chandra [G07-8078X, G08-9053X, G08-9085X, TM7-8007X]; NASA XMM-Newton [NNX06AE78G, NNX06AH62G.]; Netherlands Organization; Theoretical Institute for Advanced Research in Astrophysics (TIARA); National Science Council Excellence Projects program in Taiwan [NSC 96-2752-M-007-007-PAE] FX We thank M. Prakash, D. Page, K. Levenfish, D. Blaschke, and S. Campana for discussions, and the anonymous referee for a useful report. C.O.H. acknowledges support from the Lindheimer Postdoctoral Fellowship at Northwestern University, NASA Chandra grants G07-8078X, G08-9053X, and G08-9085X, and NASA XMM-Newton grants NNX06AE78G and NNX06AH62G. C.J.D. acknowledges support from NASA XMM-Newton grant NXX06AH62G and Chandra grant TM7-8007X. P.G.J. acknowledges support from the Netherlands Organization for Scientific Research. Support for this work is provided in part by the Theoretical Institute for Advanced Research in Astrophysics (TIARA) operated under Academia Sinica and the National Science Council Excellence Projects program in Taiwan administered through grant number NSC 96-2752-M-007-007-PAE. NR 56 TC 61 Z9 61 U1 1 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2009 VL 691 IS 2 BP 1035 EP 1041 DI 10.1088/0004-637X/691/2/1035 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 406OH UT WOS:000263304300011 ER PT J AU Osten, RA Wolk, SJ AF Osten, Rachel A. Wolk, Scott J. TI MULTIWAVELENGTH SIGNATURES OF MAGNETIC ACTIVITY FROM YOUNG STELLAR OBJECTS IN THE LkH alpha 101 CLUSTER SO ASTROPHYSICAL JOURNAL LA English DT Article DE radio continuum: stars; stars: activity; stars: coronae; stars: pre-main sequence; X-rays: stars ID T-TAURI STARS; LOW-MASS STARS; POINT-SOURCE IDENTIFICATION; X-RAY; RADIO-EMISSION; CHROMOSPHERIC EVAPORATION; CORONET CLUSTER; BINARY-SYSTEM; BROWN DWARFS; LARGE ARRAY AB We describe the results of our multiwavelength observing campaign on the young stellar objects in the LkH alpha 101 cluster. Our simultaneous X-ray and multifrequency radio observations are unique in providing simultaneous constraints on short-timescale variability at both wavelengths as well as constraints on the thermal or nonthermal nature of radio emission from young stars. Focussing on radio-emitting objects and the multiwavelength data obtained for them, we find that multifrequency radio data indicate nonthermal emission even in objects with infrared evidence for disks. We find radio variability on timescales of decades, days, and hours. About half of the objects with X-ray and radio detections were variable at X-ray wavelengths, despite lacking large-scale flares or large variations. Variability appears to be a bigger factor affecting radio emission than X-ray emission. A star with infrared evidence for a disk, [BW88] 3, was observed in the decay phase of radio flare. In this object and another ([BW88] 1), we find an inverse correlation between radio flux and spectral index, which contrasts with behavior seen in the Sun and active stars. We interpret this behavior as the repopulation of the hardest energy electrons due to particle acceleration. A radio and X-ray source lacking an infrared counterpart, [BW88] 1, may be near the substellar limit; its radio properties are similar to other cluster members, but its much higher radio to X-ray luminosity ratio is reminiscent of behavior in nearby very low-mass stars/brown dwarfs. We find no correspondence between signatures of particle acceleration and those of plasma heating, both time-averaged and time-variable. The lack of correlated temporal variability in multiwavelength behavior, the breakdown of multiwavelength correlations of time-averaged luminosities, and the optical thickness of X-ray emitting material at radio wavelengths support the idea that radio and X-ray emission on young stars are physically and/or energetically distinct. C1 [Osten, Rachel A.] Univ Maryland, Dept Astron, College Pk, MD 20720 USA. [Wolk, Scott J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Osten, RA (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. EM osten@stsci.edu; swolk@cfa.harvard.edu FU National Aeronautics and Space Administration; National Science Foundation; NASA through Hubble Fellowship [HF-01189.01, NAS5-26555, NAS8-03060]; Space Telescope Science Institute; [GO5-6018X] FX We especially thank Tyler Bourke, Rob Gutermuth, and Brad Spitzbart-coauthors on Paper II upon whose results we are building. Thanks to Jan Forbrich for an advance copy of Forbrich et al. (2007). Thanks also to the referee, Marc Gagne, for constructive comments on improving this paper. This publication makes use of data products from the 2MASS, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center, funded by the National Aeronautics and Space Administration and the National Science Foundation. Support for this work was provided by NASA through Hubble Fellowship grant #HF-01189.01 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc. for NASA, under contract NAS5-26555. The CXC guest investigator program supported this work through grant GO5-6018X. S.J.W. was supported by NASA contract NAS8-03060. This represents the results of VLA program S60872. NR 61 TC 16 Z9 16 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2009 VL 691 IS 2 BP 1128 EP 1144 DI 10.1088/0004-637X/691/2/1128 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 406OH UT WOS:000263304300019 ER PT J AU Sozzetti, A Torres, G Charbonneau, D Winn, JN Korzennik, SG Holman, MJ Latham, DW Laird, JB Fernandez, J O'Donovan, FT Mandushev, G Dunham, E Everett, ME Esquerdo, GA Rabus, M Belmonte, JA Deeg, HJ Brown, TN Hidas, MG Baliber, N AF Sozzetti, Alessandro Torres, Guillermo Charbonneau, David Winn, Joshua N. Korzennik, Sylvain G. Holman, Matthew J. Latham, David W. Laird, John B. Fernandez, Jose O'Donovan, Francis T. Mandushev, Georgi Dunham, Edward Everett, Mark E. Esquerdo, Gilbert A. Rabus, Markus Belmonte, Juan A. Deeg, Hans J. Brown, Timothy N. Hidas, Marton G. Baliber, Nairn TI NEW SPECTROSCOPIC AND PHOTOMETRIC ANALYSIS OF THE TRANSITING PLANET SYSTEMS TrES-3 AND TrES-4 SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars: abundances; stars: fundamental parameters; stars: individual (TrES-3, TrES-4); planetary systems ID LIGHT-CURVE PROJECT; LINE-DEPTH RATIOS; RADIAL-VELOCITY TECHNIQUES; SOLAR-TYPE STARS; EXTRASOLAR PLANETS; PARENT STARS; HOT JUPITERS; LITHIUM ABUNDANCES; MAGNETIC ACTIVITY; OBLIQUITY TIDES AB We report new spectroscopic and photometric observations of the parent stars of the recently discovered transiting planets TrES-3 and TrES-4. A detailed abundance analysis based on high-resolution spectra yields [ Fe/H] = -0.19 +/- 0.08, T(eff) = 5650 +/- 75 K, and log g = 4.4 +/- 0.1 for TrES-3, and [Fe/H] = +0.14 +/- 0.09, T(eff) = 6200 +/- 75 K, and log g = 4.0 +/- 0.1 for TrES-4. The accuracy of the effective temperatures is supported by a number of independent consistency checks. The spectroscopic orbital solution for TrES-3 is improved with our new radial velocity measurements of that system, as are the light-curve parameters for both systems based on newly acquired photometry for TrES-3 and a reanalysis of existing photometry for TrES-4. We have redetermined the stellar parameters taking advantage of the strong constraint provided by the light curves in the form of the normalized separation a/R(star) (related to the stellar density) in conjunction with our new temperatures and metallicities. The masses and radii we derive are M(star) = 0.928(-0.048)(+0.028) M(circle dot), R(star) = 0.829(-0.022)(+0.015) R(circle dot), and M(star) = 1.404(-0.134)(+0.066) M(circle dot), R(star) = 1.846(-0.087)(+0.096) R(circle dot) for TrES-3 and TrES-4, respectively. With these revised stellar parameters, we obtain improved values for the planetary masses and radii. We find M(p) = 1.910(-0.080)(+0.075) M(Jup), R(p) = 1.336(-0.036)(+0.031) R(Jup) for TrES-3, and M(p) = 0.925 +/- 0.082 M(Jup), R(p) = 1.783(-0.086)(+0.093) R(Jup) for TrES-4. We confirm TrES-4 as the planet with the largest radius among the currently known transiting hot Jupiters. C1 [Sozzetti, Alessandro; Torres, Guillermo; Charbonneau, David; Korzennik, Sylvain G.; Holman, Matthew J.; Latham, David W.; Fernandez, Jose; Esquerdo, Gilbert A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Sozzetti, Alessandro] INAF Osservatorio Astron Torino, I-10025 Pino Torinese, Italy. [Winn, Joshua N.] MIT, Dept Phys, Cambridge, MA 02139 USA. [Winn, Joshua N.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Laird, John B.] Bowling Green State Univ, Dept Phys & Astron, Bowling Green, OH 43403 USA. [O'Donovan, Francis T.] CALTECH, Pasadena, CA 91125 USA. [Mandushev, Georgi; Dunham, Edward] Lowell Observ, Flagstaff, AZ 86001 USA. [Everett, Mark E.] Planetary Sci Inst, Tucson, AZ 85719 USA. [Rabus, Markus; Belmonte, Juan A.; Deeg, Hans J.] Inst Astrofis Canarias, Tenerife 38200, Spain. [Brown, Timothy N.; Hidas, Marton G.; Baliber, Nairn] Las Cumbres Observ Global Telescope, Goleta, CA 93117 USA. [Brown, Timothy N.; Hidas, Marton G.; Baliber, Nairn] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. RP Sozzetti, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM asozzett@cfa.harvard.edu RI Rabus, Markus/B-8029-2009; O'Donovan, Francis/I-2423-2014; OI Sozzetti, Alessandro/0000-0002-7504-365X; Hidas, Marton/0000-0002-4027-9240; O'Donovan, Francis/0000-0002-4858-6106; Charbonneau, David/0000-0002-9003-484X FU NASA [NCC 2-1390, NNG04LG89G, NNG05GJ29G]; NSF [AST-0307340]; W. M. Keck Foundation FX AS gratefully acknowledges the Kepler mission for partial support under NASA Cooperative Agreement NCC 2-1390. G.T. acknowledges partial support for this work from NASA Origins grant NNG04LG89G. D. C. is supported in part by NASA Origins grant NNG05GJ29G. F.T.O.D. acknowledges partial support for this work provided through the NASA Postdoctoral Program at the Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA. J.B.L. gratefully acknowledges support from NSF grant AST-0307340. 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. This research has made use of NASA's Astrophysics Data System Abstract Service and of the SIMBAD database, operated at CDS, Strasbourg, France. NR 82 TC 65 Z9 66 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2009 VL 691 IS 2 BP 1145 EP 1158 DI 10.1088/0004-637X/691/2/1145 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 406OH UT WOS:000263304300020 ER PT J AU Hopkins, PF Cox, TJ Younger, JD Hernquist, L AF Hopkins, Philip F. Cox, Thomas J. Younger, Joshua D. Hernquist, Lars TI HOW DO DISKS SURVIVE MERGERS? SO ASTROPHYSICAL JOURNAL LA English DT Review DE galaxies: active; galaxies: evolution; cosmology: theory ID SUPERMASSIVE BLACK-HOLES; EARLY-TYPE GALAXIES; COLD DARK-MATTER; SMOOTHED PARTICLE HYDRODYNAMICS; TULLY-FISHER RELATION; ULTRALUMINOUS INFRARED GALAXIES; QUASAR LUMINOSITY FUNCTION; HUBBLE-SPACE-TELESCOPE; TRIGGERED STAR-FORMATION; ANGULAR-MOMENTUM PROBLEM AB We develop a general physical model for how galactic disks survive and/or are destroyed in mergers and interactions. Based on simple dynamical arguments, we show that gas primarily loses angular momentum to internal torques in a merger, induced by the gravity of the secondary. Gas within some characteristic radius, determined by the efficiency of this angular momentum loss (itself a function of the orbital parameters, mass ratio, and gas fraction of the merging galaxies), will quickly lose angular momentum to the stars sharing the perturbed host disk, fall to the center, and be consumed in a starburst. We use a similar analysis to determine where violent relaxation of the premerger stellar disks is efficient on final coalescence. Our model describes both the dissipational and dissipationless components of the merger, and allows us to predict, for a given arbitrary encounter, the stellar and gas content of the material that will survive (without significant angular momentum loss or violent relaxation) to re-form a disk in the merger remnant, versus being dissipationlessly and violently relaxed or dissipationally losing angular momentum and forming a compact central starburst. We test these predictions with a large library of hydrodynamic merger simulations, and show that they agree well (with small scatter) with the properties of simulated merger remnants as a function of merger mass ratio, orbital parameters, and gas distributions in simulations which span a wide range of parameter space in these properties as well as prescriptions for gas physics, stellar and active galactic nucleus (AGN) feedback, halo and initial disk structural properties, redshift, and galaxy masses. We show that, in an immediate (short-term) sense, the amount of stellar or gaseous disk that survives or re-forms following a given interaction can be understood purely in terms of simple, well understood gravitational physics, independent of the details of the interstellar medium gas physics or stellar and AGN feedback. This allows us to demonstrate and quantify how these physics are in fact important, in an indirect sense, to enable disks to survive mergers by lowering star formation efficiencies in low-mass systems (allowing them to retain large gas fractions) and distributing the gas to large radii. The efficiency of disk destruction in mergers is a strong function of gas content-our model allows us to explicitly predict and demonstrate how, in sufficiently gas-rich mergers (with quite general orbital parameters), even 1: 1 mass-ratio mergers can yield disk-dominated remnants, and more realistic 1: 3-1: 4 mass-ratio major mergers can yield systems with < 20% of their mass in bulges. We discuss a number of implications of this modeling for the abundance and morphology of bulges as a function of mass and redshift, and provide simple prescriptions for the implementation of our results in analytic or semianalytic models of galaxy formation. C1 [Hopkins, Philip F.; Cox, Thomas J.; Younger, Joshua D.; Hernquist, Lars] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Hopkins, PF (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. FU NSF [ACI 96-19019, AST 00-71019, AST 02-06299, AST 03-07690]; NASA ATP [NAG5-12140, NAG5-13292, NAG5-13381]; W. M. Keck Foundation FX We thank Shardha Jogee and Rachel Somerville for helpful discussions, and thank the anonymous referee for helpful suggestions and clarification. This work was supported in part by NSF grants ACI 96-19019, AST 00-71019, AST 02-06299, and AST 03-07690, and NASA ATP grants NAG5-12140, NAG5-13292, and NAG5-13381. Support for T.J.C. was provided by the W. M. Keck Foundation. NR 210 TC 259 Z9 259 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2009 VL 691 IS 2 BP 1168 EP 1201 DI 10.1088/0004-637X/691/2/1168 PG 34 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 406OH UT WOS:000263304300022 ER PT J AU Goddi, C Greenhill, LJ Humphreys, EML Matthews, LD Tan, JC Chandler, J AF Goddi, C. Greenhill, L. J. Humphreys, E. M. L. Matthews, L. D. Tan, Jonathan C. Chandler, J. TI A 42.3-43.6 GHz SPECTRAL SURVEY OF ORION BN/KL: FIRST DETECTION OF THE nu=0 J=1-0 LINE FROM THE ISOTOPOLOGUES (SiO)-Si-29 AND (SiO)-Si-30 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: individual (Orion BN/KL); ISM: molecules; radio lines: ISM; surveys ID MASER EMISSION; LABORATORY ASSIGNMENTS; SUBMILLIMETER ARRAY; OBSERVATIONAL DATA; SILICON MONOXIDE; MOLECULAR CLOUD; STAR-FORMATION; MASSIVE STARS; KLEINMANN-LOW; GROUND-STATE AB We have surveyed molecular line emission from Orion BN/KL from 42.3 to 43.6 GHz with the Green Bank Telescope. Sixty-seven lines were identified and ascribed to 13 different molecular species. The spectrum at 7 mm is dominated by SiO, SO2, CH3OCH3, and C2H5CN. Five transitions have been detected from the SiO isotopologues (SiO)-Si-28, (SiO)-Si-29, and (SiO)-Si-30. We report here for the first time the spectra of the (SiO)-Si-29 and (SiO)-Si-30 nu = 0 J = 1-0 emission in Orion BN/KL, and show that they have double- peaked profiles with velocity extents similar to the main isotopologue. The main motivation for the survey was the search of high-velocity (100-1000 km s(-1)) outflows in the BN/KL region as traced by SiO Doppler components. Some of the unidentified lines in principle could be high-velocity SiO features, but without imaging data their location cannot be established. Wings of emission are present in the v = 0 (SiO)-Si-28, (SiO)-Si-29, and (SiO)-Si-30 profiles, and we suggest that the v = 0 emission from the three isotopologues might trace a moderately high-velocity (similar to 30-50 km s(-1)) component of the flows around the high-mass protostar Source I in the Orion BN/KL region. We also confirm the 7 mm detection of a complex oxygen-bearing species, acetone (CH3COCH3), which has been recently observed toward the hot core at 3 mm, and have found further indications of the presence of long cyanopolyynes (HC5N and HC7N) in the quiescent cold gas of the extended ridge. C1 [Goddi, C.; Greenhill, L. J.; Humphreys, E. M. L.; Matthews, L. D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Tan, Jonathan C.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Chandler, J.] Natl Radio Astron Observ, Socorro, NM 87801 USA. RP Goddi, C (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. FU National Science Foundation [NSF AST 0507478] FX This material is based upon the work supported by the National Science Foundation under Grant No. NSF AST 0507478. NR 64 TC 16 Z9 16 U1 1 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2009 VL 691 IS 2 BP 1254 EP 1264 DI 10.1088/0004-637X/691/2/1254 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 406OH UT WOS:000263304300028 ER PT J AU Luhman, KL Mamajek, EE Allen, PR Muench, AA Finkbeiner, DP AF Luhman, K. L. Mamajek, E. E. Allen, P. R. Muench, A. A. Finkbeiner, D. P. TI DISCOVERY OF A WIDE BINARY BROWN DWARF BORN IN ISOLATION SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: visual; planetary systems: protoplanetary disks; stars: formation; stars: low-mass, brown dwarfs; stars: pre-main sequence ID DIGITAL SKY SURVEY; SPITZER-SPACE-TELESCOPE; INITIAL MASS FUNCTION; STAR-FORMING REGION; MAIN-SEQUENCE STARS; NEAR-INFRARED SPECTRA; DATA RELEASE; SUBSTELLAR OBJECTS; EVOLUTIONARY MODELS; STELLAR POPULATION AB During a survey for stars with disks in the Taurus star-forming region using the Spitzer Space Telescope, we have discovered a pair of young brown dwarfs, FU Tau A and B, in the Barnard 215 dark cloud. They have a projected angular separation of 5 ''.7, corresponding to 800 AU at the distance of Taurus. To assess the nature of these two objects, we have obtained spectra of them and constructed spectral energy distributions. Both sources are young (similar to 1 Myr) according to their Ha emission, gravity-sensitive spectral features, and mid-infrared excess emission. The proper motion of FU Tau A provides additional evidence of its membership in Taurus. We measure spectral types of M7.25 and M9.25 for FU Tau A and B, respectively, which correspond to masses of similar to 0.05 and similar to 0.015 M-circle dot according to the evolutionary models of Chabrier and Baraffe. FU Tau A is significantly overluminous relative to an isochrone passing through FU Tau B and relative to other members of Taurus near its spectral type, which may indicate that it is an unresolved binary. FU Tau A and B are likely to be components of a binary system based on the low probability (similar to 3 x 10(-4)) that Taurus would produce two unrelated brown dwarfs with a projected separation of a <= 6 ''. Barnard 215 contains only one other young star and is in a remote area of Taurus, making FU Tau A and B the first spectroscopically confirmed brown dwarfs discovered forming in isolation rather than in a stellar cluster or aggregate. Because they were born in isolation and comprise a weakly bound binary, dynamical interactions with stars could not have played a role in their formation, and thus are not essential for the birth of brown dwarfs. C1 [Luhman, K. L.; Allen, P. R.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Mamajek, E. E.] Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. [Muench, A. A.; Finkbeiner, D. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Luhman, KL (reprint author), Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. EM kluhman@astro.psu.edu NR 96 TC 39 Z9 39 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 1 PY 2009 VL 691 IS 2 BP 1265 EP 1275 DI 10.1088/0004-637X/691/2/1265 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 406OH UT WOS:000263304300029 ER PT J AU Archontis, V Hood, AW Savcheva, A Golub, L Deluca, E AF Archontis, V. Hood, A. W. Savcheva, A. Golub, L. Deluca, E. TI ON THE STRUCTURE AND EVOLUTION OF COMPLEXITY IN SIGMOIDS: A FLUX EMERGENCE MODEL SO ASTROPHYSICAL JOURNAL LA English DT Article DE MHD; Sun: activity; Sun: corona; Sun: magnetic fields ID X-RAY TELESCOPE; MAGNETIC-FLUX; KINK INSTABILITY; SOLAR-FLARES; CORONA; TUBE; EQUILIBRIUM; SIMULATIONS; ERUPTION; ROPES AB Sigmoids are structures with a forward or inverse S-shape, generally observed in the solar corona in soft X-ray emission. It is believed that the appearance of a sigmoid in an active region is an important factor in eruptive activity. The association of sigmoids with dynamic phenomena such as flares and coronal mass ejections (CMEs) make the study of sigmoids important. Recent observations of a coronal sigmoid, obtained with the X-Ray Telescope (XRT) on board Hinode, showed the formation and eruption phase with high spatial resolution. These observations revealed that the topological structure of the sigmoid is complex: it consists of many differently oriented loops that all together form two opposite J-like bundles or an overall S-shaped structure. A series of theoretical and numerical models have been proposed, over the past years, to explain the nature of sigmoids but there is no explanation on how the aforementioned complexity in sigmoids is built up. In this paper, we present a flux emergence model that leads to the formation of a sigmoid, whose structure and evolution of complexity are in good qualitative agreement with the recent observations. For the initial state of the experiment a twisted flux tube is placed below the photosphere. A density deficit along the axis of the tube makes the system buoyant in the middle and it adopts an O-shape as it rises toward the outer atmosphere. During the evolution of the system, expanding field lines that touch the photosphere at bald-patches (BPs) form two seperatrix surfaces where dissipation is enhanced and current sheets are formed. Originally, each of the BP seperatrix surfaces has a J-like shape. Each one of the J's consist of reconnected field lines with different shapes and different relative orientation. The further dynamical evolution of the emerging flux tube results in the occurrence of many sites that resemble rotational discontinuities. Thus, additional current layers are formed inside the rising magnetized volume increasing the complexity of the system. The reconnected field lines along these layers form an overall S-shaped structure. The reconnection process continues to occur leading to the formation of another current concentration in the middle of the sigmoid where a flaring episode occurs. This central brightening is accompanied by the eruption of a flux rope from the central area of the sigmoid and the appearance of "post-flare" loops underneath the current structure. C1 [Archontis, V.; Hood, A. W.] Univ St Andrews, Sch Math & Stat, St Andrews KY16 9SS, Fife, Scotland. [Savcheva, A.; Golub, L.; Deluca, E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02139 USA. RP Archontis, V (reprint author), Univ St Andrews, Sch Math & Stat, St Andrews KY16 9SS, Fife, Scotland. RI DeLuca, Edward/L-7534-2013 OI DeLuca, Edward/0000-0001-7416-2895 FU NASA [NNM07AB07C] FX Hinode is a Japanese mission developed and launched by ISAS/JAXA, with NAOJ as domestic partner and NASA and STFC (UK) as international partners. It is operated by these agencies in cooperation with ESA and the NSC (Norway). A. S., L. G., and E. D. were supported by NASA contract NNM07AB07C. NR 38 TC 38 Z9 38 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2009 VL 691 IS 2 BP 1276 EP 1291 DI 10.1088/0004-637X/691/2/1276 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 406OH UT WOS:000263304300030 ER PT J AU Morales, JC Ribas, I Jordi, C Torres, G Gallardo, J Guinan, EF Charbonneau, D Wolf, M Latham, DW Anglada-Escude, G Bradstreet, DH Everett, ME O'Donovan, FT Mandushev, G Mathieu, RD AF Carlos Morales, Juan Ribas, Ignasi Jordi, Carme Torres, Guillermo Gallardo, Jose Guinan, Edward F. Charbonneau, David Wolf, Marek Latham, David W. Anglada-Escude, Guillem Bradstreet, David H. Everett, Mark E. O'Donovan, Francis T. Mandushev, Georgi Mathieu, Robert D. TI ABSOLUTE PROPERTIES OF THE LOW-MASS ECLIPSING BINARY CM DRACONIS SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: eclipsing; binaries: spectroscopic; stars: late type; stars: fundamental parameters; stars: individual (CM Dra) ID TRANSITING HOT JUPITER; APSIDAL MOTION; MAIN-SEQUENCE; EVOLUTIONARY MODELS; INFRARED COLORS; WHITE-DWARFS; STARS; METALLICITY; PLANET; RADII AB Spectroscopic and eclipsing binary systems offer the best means for determining accurate physical properties of stars, including their masses and radii. The data available for low-mass stars have yielded firm evidence that stellar structure models predict smaller radii and higher effective temperatures than observed, but the number of systems with detailed analyses is still small. In this paper, we present a complete reanalysis of one of such eclipsing systems, CM Dra, composed of two dM4.5 stars. New and existing light curves as well as a radial velocity curve are modeled to measure the physical properties of both components. The masses and radii determined for the components of CM Dra are M(1) = 0.2310 +/- 0.0009 M(circle dot), M(2) = 0.2141 +/- 0.0010 M(circle dot), R(1) = 0.2534 +/- 0.0019 R(circle dot), and R(2) = 0.2396 +/- 0.0015 R(circle dot). With relative uncertainties well below the 1% level, these values constitute the most accurate properties to date for fully convective stars. This makes CM Dra a valuable benchmark for testing theoretical models. In comparing our measurements with theory, we confirm the discrepancies previously reported for other low-mass eclipsing binaries. These discrepancies seem likely to be due to the effects of magnetic activity. We find that the orbit of this system is slightly eccentric, and we have made use of eclipse timings spanning three decades to infer the apsidal motion and other related properties. C1 [Carlos Morales, Juan; Ribas, Ignasi; Jordi, Carme] IEEC, Barcelona 08034, Spain. [Ribas, Ignasi] CSIC, Inst Ciencies Espai, Fac Ciencies, Bellaterra 08193, Spain. [Jordi, Carme] Univ Barcelona, Inst Ciencies Cosmos, Dept Astron & Meteorol, Barcelona 08028, Spain. [Torres, Guillermo; Charbonneau, David; Latham, David W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gallardo, Jose] Univ Chile, Dept Astron, Santiago, Chile. [Guinan, Edward F.] Villanova Univ, Dept Astron & Astrophys, Villanova, PA 19085 USA. [Wolf, Marek] Charles Univ Prague, Astron Inst, CZ-18000 Prague 8, Czech Republic. [Anglada-Escude, Guillem] Carnegie Inst Washington, Washington, DC 20015 USA. [Bradstreet, David H.] Eastern Coll, Dept Phys & Astron, St Davids, PA 19087 USA. [Everett, Mark E.] Planetary Sci Inst, Tucson, AZ 85719 USA. [Mandushev, Georgi] Lowell Observ, Flagstaff, AZ 86001 USA. [Mathieu, Robert D.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. RP Morales, JC (reprint author), IEEC, Edif Nexus,C Gran Capita 2-4, Barcelona 08034, Spain. EM morales@ieec.uab.es RI Jordi, Carme/L-3051-2014; Ribas, Ignasi/M-2134-2014; Morales, Juan Carlos/H-5548-2015; O'Donovan, Francis/I-2423-2014; OI Jordi, Carme/0000-0001-5495-9602; Ribas, Ignasi/0000-0002-6689-0312; Morales, Juan Carlos/0000-0003-0061-518X; O'Donovan, Francis/0000-0002-4858-6106; Anglada Escude, Guillem/0000-0002-3645-5977; Charbonneau, David/0000-0002-9003-484X FU Spanish Ministerio de Educacion y Ciencia [AYA2006-15623-C02-01, AYA2006-15623-C02-02]; NSF [AST-0708229]; NASA's MASSIF SIM Key Project [BLF57-04]; NSF/RUI [AST05-07536]; National Aeronautics and Space Administration [NNG05GJ29G]; Grant Agency of the Czech Republic [205/06/0217] FX We are grateful to J. Kreiner for help with the compilation of eclipse timings. J. C. M., I. R., and C. J. acknowledge support from the Spanish Ministerio de Educacion y Ciencia via grants AYA2006-15623-C02-01 and AYA2006-15623-C02-02. G. T. acknowledges partial support for this work from NSF grant AST-0708229 and NASA's MASSIF SIM Key Project (BLF57-04). E. F. G. acknowledges support for the FCAPT research under NSF/RUI grant AST05-07536. D. C. and F.T.O.D. acknowledge support for the Sleuth Observatory work by the National Aeronautics and Space Administration under grant NNG05GJ29G issued through the Origins of Solar Systems Program. F.T.O.D. also acknowledges partial support for this work provided through the NASA Postdoctoral Program at the Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA. The investigation of M. W. was supported by the Grant Agency of the Czech Republic under grant No. 205/06/0217. NR 60 TC 87 Z9 89 U1 1 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2009 VL 691 IS 2 BP 1400 EP 1411 DI 10.1088/0004-637X/691/2/1400 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 406OH UT WOS:000263304300041 ER PT J AU Hopkins, PF Hernquist, L Cox, TJ Keres, D Wuyts, S AF Hopkins, Philip F. Hernquist, Lars Cox, Thomas J. Keres, Dusan Wuyts, Stijn TI DISSIPATION AND EXTRA LIGHT IN GALACTIC NUCLEI. IV. EVOLUTION IN THE SCALING RELATIONS SO ASTROPHYSICAL JOURNAL LA English DT Review DE cosmology: theory; galaxies: elliptical and lenticular, cD; galaxies: evolution; galaxies: formation; galaxies: nuclei; galaxies: structure ID EARLY-TYPE GALAXIES; SUPERMASSIVE BLACK-HOLES; STAR-FORMING GALAXIES; HALO OCCUPATION DISTRIBUTION; TULLY-FISHER RELATION; DIGITAL SKY SURVEY; DARK-MATTER HALOES; BRIGHTEST CLUSTER GALAXIES; QUASAR LUMINOSITY FUNCTION; MASSIVE ELLIPTIC GALAXIES AB We develop a model for the physical origin and redshift evolution of spheroid scaling relations. We consider spheroid sizes, velocity dispersions, dynamical masses, profile shapes (Sersic indices), stellar and supermassive black hole (BH) masses, and their related scalings. Our approach combines advantages of prior observational constraints in halo occupation models and libraries of high-resolution hydrodynamic simulations of galaxy mergers. This allows us to separate the relative roles of dissipation, dry mergers, formation time, and evolution in progenitor properties, and identify their impact on observed scalings at each redshift. We show that, at all redshifts, dissipation is the most important factor determining spheroid sizes and fundamental plane scalings, and can account (at z = 0) for the observed fundamental plane tilt and differences between observed disk and spheroid scaling relations. Because disks (spheroid progenitors) at high redshift have characteristically larger gas fractions, this predicts more dissipation in mergers, yielding systematically more compact, smaller spheroids. In detail, this gives rise to a mass-dependent evolution in the sizes of spheroids of a given mass, which agrees well with observations. This relates to a subtle weakening of the tilt of the early-type fundamental plane with redshift, important for a number of studies that assume a nonevolving stellar mass fundamental plane. This also predicts evolution in the BH-host mass relations, toward more massive BHs at higher redshifts. Dry mergers are also significant, but only for large systems which form early-they originate as compact systems, but undergo a number of drymergers (consistent with observations) such that they have sizes at any later observed redshift similar to systems of the same mass formed more recently. Most of the observed, compact high-redshift ellipticals will become the cores of present brightest cluster galaxies, and we show how their sizes, velocity dispersions, and BH masses evolve to become consistent with observations. We also predict what fraction might survive intact from early formation and identify their characteristic z = 0 properties. We make predictions for residual correlations as well, e. g., the correlation of size and fundamental plane residuals with formation time of a given elliptical, that can be used as additional tests of these models. C1 [Hopkins, Philip F.; Hernquist, Lars; Cox, Thomas J.; Keres, Dusan; Wuyts, Stijn] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Hopkins, PF (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 216 TC 158 Z9 158 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 2009 VL 691 IS 2 BP 1424 EP 1458 DI 10.1088/0004-637X/691/2/1424 PG 35 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 406OH UT WOS:000263304300043 ER PT J AU Templeton, MR Karovska, M AF Templeton, Matthew R. Karovska, Margarita TI LONG-PERIOD VARIABILITY IN o CETI SO ASTROPHYSICAL JOURNAL LA English DT Article DE convection; stars: AGB and post-AGB; stars: individual (o Cet, Mira); stars: oscillations; stars: variables: other ID SECONDARY PERIODS; PULSATION MODES; MIRA VARIABLES; TIME-SERIES; RED GIANTS; STARS; CONVECTION; SPECTRUM; EVOLUTION AB We carried out a new and sensitive search for long-period variability in the prototype of the Mira class of long-period pulsating variables, o Ceti (Mira A), the closest and brightest Mira variable. We conducted this search using an unbroken light curve from 1902 to the present, assembled from the visual data archives of five major variable star observing organizations from around the world. We applied several time-series analysis techniques to search for two specific kinds of variability: long secondary periods (LSPs) longer than the dominant pulsation period of similar to 333 days, and long-term period variation in the dominant pulsation period itself. The data quality is sufficient to detect coherent periodic variations with photometric amplitudes of 0.05 mag or less. We do not find evidence for coherent LSPs in o Ceti to a limit of 0.1 mag, where the amplitude limit is set by intrinsic, stochastic, low-frequency variability of approximately 0.1 mag. We marginally detect a slight modulation of the pulsation period similar in timescale to that observed in the Miras with meandering periods, but with a much lower period amplitude of +/- 2 days. However, we do find clear evidence of a low-frequency power-law component in the Fourier spectrum of o Ceti's long-term light curve. The amplitude of this stochastic variability is approximately 0.1 mag at a period of 1000 days, and it exhibits a turnover for periods longer than this. This spectrum is similar to the red noise spectra observed in red supergiants. C1 [Templeton, Matthew R.] Amer Assoc Variable Star Observers, Cambridge, MA 02138 USA. [Karovska, Margarita] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Templeton, MR (reprint author), Amer Assoc Variable Star Observers, 49 Bay State Rd, Cambridge, MA 02138 USA. NR 41 TC 9 Z9 9 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2009 VL 691 IS 2 BP 1470 EP 1478 DI 10.1088/0004-637X/691/2/1470 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 406OH UT WOS:000263304300045 ER PT J AU Gupta, H Gottlieb, CA McCarthy, MC Thaddeus, P AF Gupta, H. Gottlieb, C. A. McCarthy, M. C. Thaddeus, P. TI A SURVEY OF C4H, C6H, AND C6H- WITH THE GREEN BANK TELESCOPE SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: molecules; molecular data; molecular processes; radio lines: ISM ID DENSE INTERSTELLAR CLOUDS; MASS PROTOSTAR IRAS-04368+2557; MOLECULAR LINE OBSERVATIONS; EVOLVED STARLESS CORE; IONIZATION FRACTION; NEGATIVE-IONS; ASTRONOMICAL DETECTION; DARK CLOUDS; IRC+10 216; CHEMISTRY AB A survey of the carbon chain negative ion C6H- and the structurally similar radicals C4H and C6H has been done with the 100 m Green Bank Telescope toward 24 galactic molecular sources. The most readily observed molecular anion to date, C6H- was detected in two new sources: the dark clouds L1544 and L1521F, where it was found to be present at the level of 2.5% +/- 0.8% and 4% +/- 1%, respectively relative to neutral C6H. C4H was detected in nearly all dark clouds surveyed ( in six for the first time), and C6H was detected in five dark clouds and one translucent cloud. The observed C6H-/C6H( 1%-4%) and C6H/C4H(0.2%-1%) ratios in these sources suggest that C6H- may be close to detection in many other dark clouds. The fractional ionization derived from the C6H-/C6H ratio in L1544 and L1521F of 10(-8) to 10(-7) is comparable to earlier estimates from positive molecular ions. C1 [Gupta, H.; Gottlieb, C. A.; McCarthy, M. C.; Thaddeus, P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gupta, H.; Gottlieb, C. A.; McCarthy, M. C.; Thaddeus, P.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA. [Gupta, H.] Univ Texas Austin, Inst Theoret Chem, Dept Chem, Austin, TX 78712 USA. [Gupta, H.] Univ Texas Austin, Inst Theoret Chem, Dept Biochem, Austin, TX 78712 USA. RP Gupta, H (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI McCarthy, Michael/0000-0001-9142-0008 NR 62 TC 41 Z9 41 U1 1 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2009 VL 691 IS 2 BP 1494 EP 1500 DI 10.1088/0004-637X/691/2/1494 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 406OH UT WOS:000263304300047 ER PT J AU Schnee, S Rosolowsky, E Foster, J Enoch, M Sargent, A AF Schnee, S. Rosolowsky, E. Foster, J. Enoch, M. Sargent, A. TI THE GAS TEMPERATURE OF STARLESS CORES IN PERSEUS SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars: formation; ISM: molecules ID CARLO RADIATIVE-TRANSFER; MOLECULAR CLOUD CORES; SPITZER C2D SURVEY; PRE-STELLAR CORES; PRESTELLAR CORES; DENSE CORES; SUBMILLIMETER EMISSION; INTERSTELLAR CLOUDS; INITIAL CONDITIONS; FORMING REGIONS AB In this paper, we study the determinants of starless core temperatures in the Perseus molecular cloud. We use NH(3) (1,1) and (2,2) observations to derive core temperatures (T(kin)) and data from the COMPLETE Survey of Star-Forming Regions and the c2d Spitzer Legacy Survey for observations of the other core and molecular cloud properties. The kinetic temperature distribution probed by NH(3) is in the fairly narrow range of similar to 9-15 K. We find that cores within the clusters IC348 and NGC1333 are significantly warmer than "field" starless cores, and T(kin) is higher within regions of larger extinction-derived column density. Starless cores in the field are warmer when they are closer to Class 0/I protostars, but this effect is not seen for those cores in clusters. For field starless cores, T(kin) is higher in regions in which the (13)CO line width and the 1.1 mm flux from the core are larger, and T(kin) is lower when the the peak column density within the core and average volume density of the core are larger. There is no correlation between T(kin) and (13)CO line width, 1.1 mm flux, density, or peak column density for those cores in clusters. The temperature of the cloud material along the line of sight to the core, as measured by CO or far-infrared emission from dust, is positively correlated with core temperature when considering the collection of cores in the field and in clusters, but this effect is not apparent when the two subsamples of cores are considered separately. C1 [Schnee, S.; Sargent, A.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. [Rosolowsky, E.; Foster, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Rosolowsky, E.] Univ British Columbia Okanagan, Kelowna, BC V1V 1V7, Canada. [Enoch, M.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. RP Schnee, S (reprint author), CALTECH, Div Phys Math & Astron, 770 S Wilson Ave, Pasadena, CA 91125 USA. EM schnee@astro.caltech.edu FU National Science Foundation [AST 05-40399]; NSF Astronomy and Astrophysics Postdoctoral Fellowship [AST-0502605]; NSERC of Canada; NRAO Student Observing Support [GSSP06-0015]; Spitzer Space Telescope Fellowship Program FX We thank the anonymous referee for comments that have improved this paper. S. S. acknowledges support from the Owens Valley Radio Observatory, which is supported by the National Science Foundation through grant AST 05-40399. E. R. was supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship (AST-0502605) and a Discovery Grant from NSERC of Canada. J.B.F. was supported by a grant from the NRAO Student Observing Support Program (GSSP06-0015). Support was provided to M. L. E. by NASA through the Spitzer Space Telescope Fellowship Program. NR 42 TC 17 Z9 17 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2009 VL 691 IS 2 BP 1754 EP 1763 DI 10.1088/0004-637X/691/2/1754 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 406OH UT WOS:000263304300068 ER PT J AU Tyler, KD Le Floc'h, E Rieke, GH Dey, A Desai, V Brand, K Borys, C Jannuzi, BT Armus, L Dole, H Papovich, C Brown, MJI Blaylock, M Higdon, SJU Higdon, JL Charmandaris, V Ashby, MLN Smith, HA AF Tyler, Krystal D. Le Floc'h, Emeric Rieke, George H. Dey, Arjun Desai, Vandana Brand, Kate Borys, Colin Jannuzi, Buell T. Armus, Lee Dole, Herve Papovich, Casey Brown, Michael J. I. Blaylock, Myra Higdon, Sarah J. U. Higdon, James L. Charmandaris, Vassilis Ashby, Matthew L. N. Smith, Howard A. TI SPITZER 70/160 mu m OBSERVATIONS OF HIGH-REDSHIFT ULIRGs AND HyLIRGs IN THE BOOTES FIELD SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; galaxies: active; galaxies: high-redshift; galaxies: photometry; galaxies: starburst; infrared: galaxies ID ULTRALUMINOUS INFRARED GALAXIES; ACTIVE GALACTIC NUCLEI; SPECTRAL ENERGY-DISTRIBUTIONS; MULTIBAND IMAGING PHOTOMETER; STAR-FORMATION HISTORY; SPACE-TELESCOPE; LUMINOUS GALAXIES; MIDINFRARED SPECTROSCOPY; SUBMILLIMETER GALAXIES; ABSOLUTE CALIBRATION AB We present new 70 and 160 mu m observations of a sample of extremely red (R-[ 24] greater than or similar to 15 mag), midinfrared bright, high-redshift (1.7 less than or similar to z less than or similar to 2.8) galaxies. All targets detected in the far-infrared exhibit rising spectral energy distributions (SEDs) consistent with dust emission from obscured active galactic nuclei (AGNs) and/or star-forming regions in luminous IR galaxies (LIRGs). We find that the SEDs of the high-redshift sources are more similar to canonical AGN-dominated local ultraluminous IR galaxies (ULIRGs) with significant warm dust components than to typical local star-forming ULIRGs. The inferred IR (8-1000 mu m) bolometric luminosities are found to be L-bol similar to 4 x 10(12) L-circle dot to similar to 3 x 10(13) L-circle dot (ULIRGs/hyperluminous IR galaxies (HyLIRGs)), representing the first robust constraints on Lbol for this class of object. C1 [Tyler, Krystal D.; Le Floc'h, Emeric; Rieke, George H.; Papovich, Casey; Blaylock, Myra] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Le Floc'h, Emeric] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Dey, Arjun; Jannuzi, Buell T.; Armus, Lee] Natl Opt Astron Observ, Tucson, AZ 85726 USA. [Desai, Vandana] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. [Brand, Kate] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Dole, Herve] Univ Paris 11, Inst Astrophys Spatiale, F-91405 Orsay, France. [Papovich, Casey] Texas A&M Univ, Dept Phys, College Stn, TX 77843 USA. [Brown, Michael J. I.] Monash Univ, Sch Phys, Clayton, Vic 3800, Australia. [Higdon, Sarah J. U.; Higdon, James L.] Georgia So Univ, Dept Phys, Statesboro, GA 30460 USA. [Charmandaris, Vassilis] Fdn Res & Technol Hellas, IESL, GR-71110 Iraklion, Greece. [Charmandaris, Vassilis] Observ Paris, Chercheur Assoc, F-75014 Paris, France. [Ashby, Matthew L. N.; Smith, Howard A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Tyler, KD (reprint author), Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA. RI Charmandaris, Vassilis/A-7196-2008; Brown, Michael/B-1181-2015 OI Charmandaris, Vassilis/0000-0002-2688-1956; Brown, Michael/0000-0002-1207-9137 FU NASA [1255094, 1276199]; NOAO; EU ToK [39965] FX We thank all of our MIPS, IRS, and Bootes collaborators for their discussion and input, as well as Jason Marshall for supplying us with the NGC7714 template and the referee for useful comments and suggestions. This work is based on observations made with the Spitzer Space Telescope, which is operated by NASA/JPL/Caltech. We thank NASA for financial support through contracts 1255094 and 1276199. E. L. F. and C. P. acknowledge support by NASA through the Spitzer Space Telescope Fellowship Program. The research activities of A. D. and B.T.J. are supported by NOAO, which is operated by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. V. C. acknowledges partial support from the EU ToK grant 39965. NR 74 TC 11 Z9 11 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 2009 VL 691 IS 2 BP 1846 EP 1853 DI 10.1088/0004-637X/691/2/1846 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 406OH UT WOS:000263304300075 ER PT J AU Machacek, M Ashby, MLN Jones, C Forman, WR Bastian, N AF Machacek, M. Ashby, M. L. N. Jones, C. Forman, W. R. Bastian, N. TI A MULTIWAVELENGTH VIEW OF STAR FORMATION IN INTERACTING GALAXIES IN THE PAVO GROUP SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: general; galaxies: individual (NGC 6872, NGC 6876, NGC 6877); galaxies: interactions; infrared: galaxies; X-rays: galaxies ID SPITZER-SPACE-TELESCOPE; X-RAY SOURCES; INFRARED ARRAY CAMERA; MEDIUM-SENSITIVITY SURVEY; REDSHIFT SURVEY; SPATIAL-DISTRIBUTION; ANTENNAE GALAXIES; NEARBY GALAXIES; DISK GALAXIES; CLOSE PAIRS AB We combine Spitzer Infrared Array Camera mid-infrared and Chandra X-ray observations of the dominant galaxies NGC 6872 and NGC 6876 in the Pavo group with archival optical and Hi data to study interaction-induced star formation. In the spiral galaxy NGC 6872, 8.0 mu m and 5.8 mu m nonstellar emission having colors consistent with polycyclic aromatic hydrocarbons (PAHs) is concentrated primarily in clumps in three regions: in a 5 kpc radius outer ring about the center of the spiral galaxy, in a bridge of emission connecting NGC 6872's northern spiral arm to IC 4970, and along the full extent of both NGC 6872's tidal arms. PAH emission is correlated with young star clusters and dense Hi regions. We find no strong differences in the mid-infrared colors of the star-forming regions in the spiral galaxy NGC 6872 as a function of position relative to the tidally interacting companion galaxy IC 4970. We find 11 very luminous X-ray sources (greater than or similar to (0.5-5) x 10(39) erg s(-1)) clustered to the southwest in NGC 6872, near bright star-forming regions. In NGC 6872's tidal features, young star clusters form at the boundaries of diffuse X-ray gas, suggesting that stars form as gas stripped by the interactions cools. The nucleus of NGC 6872 is a weak X-ray point source with 0.5-8 keV luminosity of 8.5 x 1039 erg s(-1), but there is little evidence in the inner 1 kpc of NGC 6872 for PAH emission from recent star formation or nuclear activity. However, a 4 kpc "stream," leading from the outer ring of NGC 6872 to the nucleus, may signal the transport of interstellar matter into NGC 6872's nuclear region. Nonstellar emission, consistent with PAH emission, is also found in the central region of elliptical galaxy NGC 6877, companion to the dominant Pavo group elliptical galaxy NGC 6876. However, in the central region of NGC 6876, the dust emission is more likely due to silicate emission from old asymptotic giant branch stars. C1 [Machacek, M.; Ashby, M. L. N.; Jones, C.; Forman, W. R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bastian, N.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. RP Machacek, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mmachacek@cfa.harvard.edu FU National Aeronautics and Space Administration (NASA) through Chandra Award [GO6-7068X, NAS8-03060]; Smithsonian Institution; National Science Foundation FX Support for this work was provided, in part, by the National Aeronautics and Space Administration (NASA) through Chandra Award Number GO6-7068X 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, by NASA through an award issued by JPL/Caltech, and by the Smithsonian Institution. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. This work made use of the IRAC post-BCD processing software "IRACProc" developed by M. Schuster, M. Marengo, and B. Patten at the Smithsonian Astrophysical Observatory, and also data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Data Analysis and Processing Center/California Institute of Technology, funded by NASA and the National Science Foundation. The NASA/IPAC Extragalactic Database (NED), which is operated by JPL/Caltech, under contract with NASA has also been used. We especially thank M. Marengo for help with IRACProc, and C. Horellou and B. Koribalski for use of their Hi maps of NGC 6872. NR 65 TC 3 Z9 3 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2009 VL 691 IS 2 BP 1921 EP 1935 DI 10.1088/0004-637X/691/2/1921 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 406OH UT WOS:000263304300081 ER PT J AU Mora, A Gaona, T Kley, J Montoya, D Parra, M Quiroz, LI Reyes, G Strecker, MR AF Mora, Andres Gaona, Tatiana Kley, Jonas Montoya, Diana Parra, Mauricio Quiroz, Luis Ignacio Reyes, German Strecker, Manfred R. TI The role of inherited extensional fault segmentation and linkage in contractional orogenesis: a reconstruction of Lower Cretaceous inverted rift basins in the Eastern Cordillera of Colombia SO BASIN RESEARCH LA English DT Article ID GERMAN BASIN; NORTHWESTERN ARGENTINA; INVERSION STRUCTURES; TECTONIC INVERSION; SALTA RIFT; EVOLUTION; SYSTEMS; FACIES; GROWTH; QUANTIFICATION AB Lower Cretaceous early syn-rift facies along the eastern flank of the Eastern Cordillera of Colombia, their provenance, and structural context, reveal the complex interactions between Cretaceous extension, spatio-temporal trends in associated sedimentation, and subsequent inversion of the Cretaceous Guatiquia paleo-rift. South of 4 degrees 30'N lat, early syn-rift alluvial sequences in former extensional footwall areas were contemporaneous with fan-delta deposits in shallow marine environments in adjacent hanging-wall areas. In general, footwall erosion was more pronounced in the southern part of the paleorift. In contrast, early syn-rift sequences in former footwall areas in the northern rift sectors mainly comprise shallow marine supratidal sabkha to intertidal strata, whereas hanging-wall units display rapid transitions to open-sea shales. In comparison with the southern paleo-rift sector, fan-delta deposits in the north are scarce, and provenance suggests negligible footwall erosion. The southern graben segment had longer, and less numerous normal faults, whereas the northern graben segment was characterized by shorter, rectilinear faults. To the east, the graben system was bounded by major basin-margin faults with protracted activity and greater throw as compared with intrabasinal faults to the west. Intrabasinal structures grew through segment linkage and probably interacted kinematically with basin-margin faults. Basin-margin faults constitute a coherent fault system that was conditioned by pre-existing basement fabrics. Structural mapping, analysis of present-day topography, and balanced cross sections indicate that positive inversion of extensional structures was focused along basin-bounding faults, whereas intrabasinal faults remained unaffected and were passively transported by motion along the basin-bounding faults. Thus, zones of maximum subsidence in extension accommodated maximum elevation in contraction, and former topographic highs remained as elevated areas. This documents the role of basin-bounding faults as multiphased, long-lived features conditioned by basement discontinuities. Inversion of basin-bounding faults was more efficient in the southern than in the northern graben segment, possibly documenting the inheritance and pivotal role of fault-displacement gradients. Our observations highlight similarities between inversion features in orogenic belts and intra-plate basins, emphasizing the importance of the observed phenomena as predictive tools in the spatiotemporal analysis of inversion histories in orogens, as well as in hydrocarbon and mineral deposits exploration. C1 [Mora, Andres; Parra, Mauricio; Strecker, Manfred R.] Univ Potsdam, Inst Geowissensch, Golm, Germany. [Kley, Jonas] Univ Jena, Inst Geowissensch, Jena, Germany. [Quiroz, Luis Ignacio] Smithsonian Trop Res Inst, Balboa, Panama. [Gaona, Tatiana; Montoya, Diana; Reyes, German] Ingeominas, Bogota, Colombia. RP Mora, A (reprint author), Univ Potsdam, Inst Geowissensch, Karl Liebnecht Str 24, D-14476 Potsdam, Germany. EM andres.mora@geo.uni-potsdam.de RI Kley, Jonas/A-3925-2008; Parra, Mauricio/B-7497-2013 OI Parra, Mauricio/0000-0002-5955-6105 FU Leibniz funds [DFG STR373/16-1]; Geological Survey of Colombia FX The authors are indebted to Arndt Peterhansel, Estelle Mortimer, Gabriela Marcano, Cornelius Uba and Jessica Zamagni for interesting discussions that improved the ideas in this paper. Cornelius Uba and Jessica Zamagni graciously read an earlier version of this paper. Careful reviews by Nestor Cardozo, William Cavazza and Brian Horton improved the final version of this manuscript. Funding for field work came from Leibniz funds to M. Strecker (DFG STR373/16-1) and the Geological Survey of Colombia (Ingeominas, project Cinturones Esmeraldiferos de la Cordillera Oriental). A. Mora and M. Parra are grateful to the DAAD for funding their stay at the Geosciences Departament at the University of Potsdam. Birgit Fabian made Figs 2 and 11. Dr Fernando Etayo-Serna (Ingeominas) determined the relative ages of the ammonites available in our profile locations. Oscar Fernandez from Midland Valley provided a 2dMove license for balancing our cross sections. Sara n and Jaime Corredor assisted our work in the field. NR 85 TC 39 Z9 41 U1 0 U2 11 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0950-091X J9 BASIN RES JI Basin Res. PD FEB PY 2009 VL 21 IS 1 BP 111 EP 137 DI 10.1111/j.1365-2117.2008.00367.x PG 27 WC Geosciences, Multidisciplinary SC Geology GA 397LW UT WOS:000262665200007 ER PT J AU Raja, HA Schmit, JP Shearer, CA AF Raja, Huzefa A. Schmit, John Paul Shearer, Carol A. TI Latitudinal, habitat and substrate distribution patterns of freshwater ascomycetes in the Florida Peninsula SO BIODIVERSITY AND CONSERVATION LA English DT Review DE Aquatic habitats; Biogeography; Freshwater fungi ID AQUATIC HYPHOMYCETE SPORA; WOOD-INHABITING FUNGI; SUBMERGED WOOD; HONG-KONG; LONGITUDINAL DISTRIBUTION; GEOGRAPHICAL RANGE; SPECIES RICHNESS; NORTH QUEENSLAND; SP-NOV; STREAM AB Freshwater ascomycetes are important decomposers of dead woody and herbaceous debris in aquatic habitats. Despite evidence of their ecological importance, latitudinal, habitat and substrate distributional patterns of freshwater ascomycetes are poorly understood. In this study, we examined the latitudinal and habitat distributional patterns, and substrate recurrences of freshwater ascomycetes by collecting dead submerged woody and herbaceous debris in lentic and lotic habitats at five selected sites along a north-central-south, temperate-subtropical latitudinal ecotone in Florida. One hundred and thirty-two fungal taxa were collected during the study. Seventy-four were meiosporic and 56 were mitosporic ascomycetes, while two species were basidiomycetes. Canonical analyses of principal coordinates (CAP) and Sorenson's similarity index of species based on presence/absence data revealed a high turnover in species composition between the northern and southern sites, indicating a change in species composition along the temperate-subtropical latitudinal ecotone of the Florida Peninsula. Results from the ordination analysis indicated that freshwater ascomycete community composition is not significantly different between lentic and lotic habitats in Florida. The geographically broadly distributed species and species commonly found in Florida occurred in both habitats, whereas a number of new or rare species occurred in either lentic or lotic habitats, but not both. The same freshwater ascomycete species did not necessarily occur on both woody and herbaceous debris; of the 132 taxa collected, 100 were reported only on woody debris; 14 species occurred exclusively on herbaceous debris; and 18 species were found on both woody and herbaceous debris in lentic or lotic habitats. Implications of data from this study to the conservation and knowledge of biodiversity for freshwater ascomycetes is discussed. C1 [Raja, Huzefa A.; Shearer, Carol A.] Univ Illinois, Dept Plant Biol, Urbana, IL 61801 USA. [Schmit, John Paul] Smithsonian Environm Res Ctr, Smithsonian Inst, Edgewater, MD 21037 USA. RP Raja, HA (reprint author), Univ Illinois, Dept Plant Biol, 265 Morrill Hall,505 S Goodwin Ave, Urbana, IL 61801 USA. EM raja@illinois.edu RI Raja, Huzefa /J-4794-2015 OI Raja, Huzefa /0000-0002-0824-9463 FU National Science Foundation (NSF) [DEB 03-16496]; National Institutes of Health (NIH) [R01GM-60600]; Integrative Biology, UIUC; Mycological Society of America Graduate Fellowship Award FX We thank Dr. Andrew N. Miller, Christopher Brown, and Dr. J.L. Crane for their assistance with collecting. Appreciation is expressed to the rangers at Blackwater River State Forest, Apalachicola National Forest and Ocala National Forest, for permission to collect within the forests. We are grateful to the Superintendent of Big Cypress National Preserve and Everglades National Park for providing permits to collect aquatic fungi. Financial support of this study by the National Science Foundation (NSF Grant No. DEB 03-16496) and the National Institutes of Health (NIH Grant No. R01GM-60600), Clark Research Grant from Integrative Biology, UIUC, and The Mycological Society of America Graduate Fellowship Award are gratefully acknowledged. Any opinions, findings, and conclusions or recommendations expressed in this publication are those of the authors and do not necessarily reflect the views of the National Science Foundation and National Institutes of Health. This work represents a portion of a thesis in partial fulfillment of the requirements for the doctoral degree at the Graduate College of the University of Illinois at Urbana-Champaign. NR 140 TC 38 Z9 39 U1 0 U2 12 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0960-3115 J9 BIODIVERS CONSERV JI Biodivers. Conserv. PD FEB PY 2009 VL 18 IS 2 BP 419 EP 455 DI 10.1007/s10531-008-9500-7 PG 37 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 401TN UT WOS:000262965400011 ER PT J AU Baeza, JA Schubart, CD Zillner, P Fuentes, S Bauer, RT AF Baeza, J. Antonio Schubart, Christoph D. Zillner, Petra Fuentes, Soledad Bauer, Raymond T. TI Molecular phylogeny of shrimps from the genus Lysmata (Caridea: Hippolytidae): the evolutionary origins of protandric simultaneous hermaphroditism and social monogamy SO BIOLOGICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Article DE 16s rRNA; hermaphrodite; mitochondrial DNA ID MARINE SHRIMP; SEX ALLOCATION; WURDEMANNI CARIDEA; CRUSTACEA; SYSTEM; REPRODUCTION; DECAPODA; MODEL AB Shrimps from the genus Lysmata are known because of their wide diversity of lifestyles, mating systems, symbiotic partnerships, and conspicuous coloration. They can occur in crowds (large aggregations), in small groups, or as socially monogamous pairs. Shrimps from this genus are rare, if not unique among crustaceans, because of their unusual sexual system. To date, the sexual system of all species investigated comprises a protandric simultaneous hermaphroditism: shrimps initially mature and reproduce as males and later in life turn into functional simultaneous hermaphrodites. The evolutionary relationships of the species within the genus are unsettled. A molecular phylogeny of the group may shed light on the evolutionary origins of the peculiar sexual and social systems of these shrimps and help resolve standing taxonomic questions long overdue. Using a 647-bp alignment of the 16S rRNA mitochondrial DNA, we examined the phylogenetic relationship of 21 species of shrimps from the genus Lysmata from several biogeographical regions; the Atlantic, Pacific, and Indo-Pacific. The resulting phylogeny indicates that the genus is paraphyletic and includes the genus Exhippolysmata. The constituent species are subdivided into three well supported clades: one group exclusively composed of neotropical species; a second clade comprising the Indo-Pacific and Atlantic symbiotic fish cleaner shrimps; and a third clade including tropical and temperate species from the Atlantic and Pacific. The molecular phylogeny presented here does not support a historical contingency hypothesis, previously proposed to explain the origins of protandric simultaneous hermaphroditism within the genus. Furthermore, the present study shows that monogamous pair-living is restricted to one monophyletic group of shrimps and therefore probably evolved only once. (C) 2009 The Linnean Society of London, Biological Journal of the Linnean Society, 2009, 96, 415-424. C1 [Baeza, J. Antonio] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Baeza, J. Antonio] Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL 34949 USA. [Schubart, Christoph D.; Zillner, Petra] Univ Regensburg, D-93040 Regensburg, Germany. [Fuentes, Soledad; Bauer, Raymond T.] Univ Louisiana Lafayette, Dept Biol, Lafayette, LA 70504 USA. RP Baeza, JA (reprint author), Smithsonian Trop Res Inst, Apartado Postal 0843-03092, Balboa, Ancon, Panama. EM baezaa@si.edu RI Schubart, Christoph/B-5595-2012; OI Baeza, Juan Antonio/0000-0002-2573-6773 NR 49 TC 40 Z9 43 U1 1 U2 11 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0024-4066 J9 BIOL J LINN SOC JI Biol. J. Linnean Soc. PD FEB PY 2009 VL 96 IS 2 BP 415 EP 424 DI 10.1111/j.1095-8312.2008.01133.x PG 10 WC Evolutionary Biology SC Evolutionary Biology GA 397AU UT WOS:000262635000015 ER PT J AU Wcislo, WT Tierney, SM AF Wcislo, William T. Tierney, Simon M. TI Behavioural environments and niche construction: the evolution of dim-light foraging in bees SO BIOLOGICAL REVIEWS LA English DT Review DE foraging behavior; nocturnal; crepuscular; matinal; vespertine; evolution; niche shifts; niche construction; neurobiology of night vision; Apoidea ID FLYING SWEAT BEES; HIMALAYAN HONEY BEE; NOCTURNAL BEE; MEGALOPTA-GENALIS; EYE SIZE; HYMENOPTERA APOIDEA; POLLINATION ECOLOGY; APIS-LABORIOSA; EL-NINO; HETEROPHRAGMA-QUADRILOCULARE AB Most bees forage for floral resources during the day, but temporal patterns of foraging activity vary extensively, and foraging in dim-light environments has evolved repeatedly. Facultative dim-light foraging behaviour is known in five of nine families of bees, while obligate behaviour is known in four families and evolved independently at least 19 times. The light intensity under which bees forage varies by a factor of 10(8), and therefore the evolution of dim-light foraging represents the invasion of a new, extreme niche. The repeated evolution of dim-light foraging behaviour in bees allows tests of the hypothesis that behaviour acts as an evolutionary pacemaker. With the exception of one species of Apis, facultative dim-light foragers show no external structural traits that are thought to enable visually mediated flight behaviour in low-light environments. By contrast, most obligate dim-light foragers show a suite of convergent optical traits such as enlarged ocelli and compound eyes. In one intensively studied species (Megalopta genalis) these optical changes are associated with neurobiological changes to enhance photon capture. The available ecological evidence suggests that an escape from competition for pollen and nectar resources and avoidance of natural enemies are driving factors in the evolution of obligate dim-light foraging. C1 [Wcislo, William T.; Tierney, Simon M.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Wcislo, WT (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Ancon, Panama. EM WcisloW@si.edu RI Tierney, Simon/H-2410-2015 OI Tierney, Simon/0000-0002-8812-6753 FU Smithsonian Tropical Research Institute (STRI); National Geographic Society Committee on Research and Exploration FX We thank Paola Galgani for help with preparing the bibliography and compiling information on body size; Karen Kapheim, Adam Smith and two anonymous reviewers for providing comments on earlier drafts of this manuscript, and Doug Yanega who also provided much helpful information. S. M. T. received financial support from an Earl S. Tupper Fellowship from the Smithsonian Tropical Research Institute (STRI), and WTW received general research funds from STRI. Associated fieldwork was supported by the National Geographic Society Committee on Research and Exploration and STRI. NR 209 TC 26 Z9 27 U1 5 U2 36 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 2009 VL 84 IS 1 BP 19 EP 37 DI 10.1111/j.1469-185X.2008.00059.x PG 19 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 400OV UT WOS:000262878800002 PM 19046401 ER PT J AU Dechmann, DKN Safi, K AF Dechmann, Dina K. N. . Safi, Kamran TI Comparative studies of brain evolution: a critical insight from the Chiroptera SO BIOLOGICAL REVIEWS LA English DT Review DE Chiroptera; encephalisation; expensive tissue; hippocampus; mating system; mosaic evolution; neocortex; neuroecology; niche adaptation; phylogeny ID PHYLOGENETICALLY INDEPENDENT CONTRASTS; SIZE DIMORPHIC BRAINS; CORRELATED EVOLUTION; MAMMALIAN BRAINS; NEOCORTEX SIZE; TEMPERATURE REGULATION; DISCRETE CHARACTERS; LARGER HIPPOCAMPUS; TESTING HYPOTHESES; DNA-HYBRIDIZATION AB Comparative studies of brain size have a long history and contributed much to our understanding of the evolution and function of the brain and its parts. Recently, bats have been used increasingly as model organisms for such studies because of their large number of species, high diversity of life-history strategies, and a comparatively detailed knowledge of their neuroanatomy. Here, we draw attention to inherent problems of comparative brain size studies, highlighting limitations but also suggesting alternative approaches. We argue that the complexity and diversity of neurological tasks that the brain and its functional regions (subdivisions) must solve cannot be explained by a single or few variables representing selective pressures. Using an example we show that by adding a single relevant variable, morphological adaptation to foraging strategy, to a previous analysis a correlation between brain and testes mass disappears completely and changes entirely the interpretation of the study. Future studies should not only look for novel determinants of brain size but also include known correlates in order to add to our current knowledge. We believe that comparisons at more detailed anatomical, taxonomic, and geographical levels will continue to contribute to our understanding of the function and evolution of mammalian brains. C1 [Safi, Kamran] Zool Soc London, Inst Zool, London NW1 4RY, England. [Dechmann, Dina K. N. .] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Dechmann, Dina K. N. .] Leibniz Inst Zoo & Wildlife Res, D-10315 Berlin, Germany. RP Safi, K (reprint author), Zool Soc London, Inst Zool, Regents Pk, London NW1 4RY, England. EM kamran.safi@ioz.ac.uk RI Dechmann, Dina/A-1827-2010; Safi, Kamran/B-2079-2008 OI Safi, Kamran/0000-0002-8418-6759 FU SNSF [PBZHA-118824]; German Science Foundation [DFG, Vo. 890] FX We would like to thank C. Voigt, J. Scharlemann, K. Jones, J. Niven and an anonymous reviewer for valuable comments on the manuscript. K.S. was supported by the SNSF grant PBZHA-118824. D.K.N.D. was supported by a grant of the German Science Foundation (DFG, Vo. 890). NR 127 TC 33 Z9 33 U1 0 U2 32 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1464-7931 J9 BIOL REV JI Biol. Rev. PD FEB PY 2009 VL 84 IS 1 BP 161 EP 172 DI 10.1111/j.1469-185X.2008.00067.x PG 12 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 400OV UT WOS:000262878800010 PM 19183335 ER PT J AU Lackey, JA AF Lackey, James A. TI Cotyledon areoles in Bobgunnia (Fabaceae: Swartzieae) SO BOTANICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Article DE endosperm; Fabaceae; galactomannan; Leguminosae; seed; Swartzia ID PHYLOGENETIC-RELATIONSHIPS; LEGUMINOSAE; PAPILIONOIDEAE; SEEDS; GENUS; PITS AB Cotyledon areoles, a seed character unique to papilionoid legumes, are reported for the first time in the legume tribe Swartzieae, an anomalous group sometimes considered to be intermediate between subfamilies Caesalpinioideae and Papilionoideae. Bobgunnia madagascariensis has a linear, slightly branched cotyledon areole on the abaxial surface of each cotyledon. Previous reports of other papilionoid seed features in this species are confirmed and extended. These highly distinctive papilionoid seed structures, and recent reports from floral ontogeny and molecular systematics which show Bobgunnia to be closely related to Swartzia and several other genera of Swartzieae, add further evidence to assertions that Swartzia seed structures are derived by simplification from a papilionoid seed, and not by retention of less specialized caesalpinioid seed features. The function and evolutionary advantage of cotyledon areoles are unknown and need investigation. (C) 2009 The Linnean Society of London, Botanical Journal of the Linnean Society, 2009, 159, 287-291. C1 Smithsonian Inst, Dept Bot, Washington, DC 20013 USA. RP Lackey, JA (reprint author), Smithsonian Inst, Dept Bot, NMNH MRC-166,Box 37012, Washington, DC 20013 USA. EM lackeyj@si.edu NR 30 TC 3 Z9 5 U1 0 U2 1 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0024-4074 J9 BOT J LINN SOC JI Bot. J. Linnean Soc. PD FEB PY 2009 VL 159 IS 2 BP 287 EP 291 DI 10.1111/j.1095-8339.2008.00929.x PG 5 WC Plant Sciences SC Plant Sciences GA 412SU UT WOS:000263745300010 ER PT J AU Uemura, Y Takahashi, S Senda, A Fukuda, K Saito, T Oftedal, OT Urashima, T AF Uemura, Yusuke Takahashi, Shunji Senda, Akitsugu Fukuda, Kenji Saito, Tadao Oftedal, Olav T. Urashima, Tadasu TI Chemical characterization of milk oligosaccharides of a spotted hyena (Crocuta crocuta) SO COMPARATIVE BIOCHEMISTRY AND PHYSIOLOGY A-MOLECULAR & INTEGRATIVE PHYSIOLOGY LA English DT Article DE Hyena; Milk oligosaccharide; Carnivora; Hyaenidae; (1)H NMR spectrometry ID STRUCTURAL DETERMINATION; POLAR BEAR; COLOSTRUM; SAMPLE AB The Carnivora include the superfamilies Canoidea and Feloidea. In species of Canoidea other than Canidae, the milk contains only traces of lactose and much larger concentrations of oligosaccharides. In this study, the following oligosaccharides were characterized in the milk of a spotted hyena, which is a species of Feloidea species: Neu5Ac(alpha 2-3)Gal(beta 1-4)Glc, Gal(alpha 1-3)[Fuc(alpha 1-2)]Gal(beta 1-4)Glc, Gal(alpha 1-3)Gal(beta 1-4)Glc and Fuc (alpha 1-2)Gal(beta 1-4)Glc. Lactose was found to be the predominant saccharide; in this respect, the hyena milk is markedly different from the milks of most species of Canoidea species. The sole presence of 3'-SL in the spotted hyena milk is interesting, because the co-presence of 3'-SL and 6'-SL has been reported in the milk or colostrum of many mammalian species. (C) 2008 Elsevier Inc. All rights reserved. C1 [Senda, Akitsugu; Fukuda, Kenji; Urashima, Tadasu] Obihiro Univ Agr & Vet Med, Grad Sch Food Hyg, Obihiro, Hokkaido 0808555, Japan. [Uemura, Yusuke] Iwate Univ, Course Sci Bioresources, United Grad Sch Agr Sci, Morioka, Iwate 0208550, Japan. [Takahashi, Shunji] Obihiro Univ Agr & Vet Med, Dept Bioresource Chem, Obihiro, Hokkaido 0808555, Japan. [Saito, Tadao] Tohoku Univ, Grad Sch Agr Sci, Aoba Ku, Sendai, Miyagi 9818555, Japan. [Oftedal, Olav T.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Urashima, T (reprint author), Obihiro Univ Agr & Vet Med, Grad Sch Food Hyg, Obihiro, Hokkaido 0808555, Japan. EM urashima@obihiro.ac.jp FU University of California (UC), Berkeley FX We thank Lawrence Frank at the Field Station for the Study of Behavior, Ecology, and Reproduction at the University of California (UC), Berkeley for providing the sample of spotted hyena milk. We also thank Michael Jakubasz for assistance in initial processing of the sample. NR 27 TC 11 Z9 11 U1 1 U2 6 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 1095-6433 J9 COMP BIOCHEM PHYS A JI Comp. Biochem. Physiol. A-Mol. Integr. Physiol. PD FEB PY 2009 VL 152 IS 2 BP 158 EP 161 DI 10.1016/j.cbpa.2008.09.013 PG 4 WC Biochemistry & Molecular Biology; Physiology; Zoology SC Biochemistry & Molecular Biology; Physiology; Zoology GA 400MU UT WOS:000262873100004 PM 18840538 ER PT J AU Hagedorn, M Ricker, J McCarthy, M Meyers, SA Tiersch, TR Varga, ZM Kleinhans, FW AF Hagedorn, M. Ricker, J. McCarthy, M. Meyers, S. A. Tiersch, T. R. Varga, Z. M. Kleinhans, F. W. TI Biophysics of zebrafish (Danio rerio) sperm SO CRYOBIOLOGY LA English DT Article DE Coulter; Fourier transform infrared spectroscopy; Permeability; Cell membrane; Lipid; Cryopreservation; Freeze damage; Osmotic pressure; Zebrafish; Danio rerio ID LIPID PHASE-TRANSITIONS; SWORDTAIL XIPHOPHORUS-HELLERI; MACACA-MULATTA SPERMATOZOA; WATER PERMEABILITY; OSMOTIC TOLERANCE; FREEZING RESPONSE; HIGH-THROUGHPUT; CRYOPRESERVATION; CELLS; FISH AB In the past two decades, laboratories around the world have produced thousands of mutant, transgenic, and wild-type zebrafish lines for biomedical research. Although slow-freezing cryopreservation of zebrafish sperm has been available for 30 years, current protocols lack standardization and yield inconsistent post-thaw fertilization rates. Cell cryopreservation cannot be improved without basic physiological knowledge, which was lacking for zebrafish sperm. The first goal was to define basic cryobiological values for wild-type zebrafish sperm and to evaluate how modern physiological methods could aid in developing improved cryopreservation protocols. Coulter counting methods measured an osmotically inactive water fraction (Vb) of 0.37 +/- 0.02 (SEM), an isosmotic cell volume (V(o)) of 12.1 +/- 0.2 mu m(3) (SEM), a water permeability (L(p)) in 10% dimethyl sulfoxide of 0.021 +/- 0.001 (SEM) mu m/min/atm, and a cryoprotectant permeability (P(s)) of 0.10 +/- 0.01 (SEM) X 10(-3) cm/min. Fourier transform infrared spectroscopy indicated that sperm membranes frozen without cryoprotectant showed damage and lipid reorganization, while those exposed to 10% glycerol demonstrated decreased lipid phase transition temperatures, which would stabilize the cells during cooling. The second goal was to determine the practicality and viability of shipping cooled zebrafish sperm overnight through the mail. Flow cytometry demonstrated that chilled fresh sperm can be maintained at 92% viability for 24 h at 0 degrees C, suggesting that it can be shipped and exchanged between laboratories. Additional methods will be necessary to analyze and improve cryopreservation techniques and post-thaw fertility of zebrafish sperm. The present study is a first step to explore such techniques. Published by Elsevier Inc. C1 [Hagedorn, M.] Smithsonian Natl Zool Park, Dept Reprod Sci, Washington, DC 20008 USA. [Hagedorn, M.] Univ Hawaii, Smithsonian Inst, Kaneohe, HI 96744 USA. [Hagedorn, M.] Univ Hawaii, Hawaii Inst Marine Biol, Kaneohe, HI 96744 USA. [Ricker, J.; McCarthy, M.; Meyers, S. A.] Univ Calif Davis, Dept Anat Physiol & Cell Biol, Davis, CA 95616 USA. [Tiersch, T. R.] Louisiana State Univ, Ctr Agr, Louisiana Agr Expt Stn, Aquaculture Res Stn, Baton Rouge, LA 70803 USA. [Varga, Z. M.] Univ Oregon, Zebrafish Int Resource Ctr, Eugene, OR 97403 USA. [Kleinhans, F. W.] Indiana Univ Purdue Univ, Dept Phys, Indianapolis, IN 46202 USA. RP Hagedorn, M (reprint author), Univ Hawaii, Smithsonian Inst, POB 1346, Kaneohe, HI 96744 USA. EM hagedornm@si.edu FU National Institutes of Health [RR016581, P40 RR012546] FX This work supported by Grants from the National Institutes of Health (R01 RR016581) to S.M. and (P40 RR012546) to Z.M.V. NR 32 TC 11 Z9 11 U1 0 U2 12 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0011-2240 J9 CRYOBIOLOGY JI Cryobiology PD FEB PY 2009 VL 58 IS 1 BP 12 EP 19 DI 10.1016/j.cryobiol.2008.09.013 PG 8 WC Biology; Physiology SC Life Sciences & Biomedicine - Other Topics; Physiology GA 401WZ UT WOS:000262974700002 PM 18951888 ER PT J AU Potvin, C Dutilleul, P AF Potvin, Catherine Dutilleul, Pierre TI Neighborhood effects and size-asymmetric competition in a tree plantation varying in diversity SO ECOLOGY LA English DT Article DE biodiversity and ecosystem functioning; neighborhood; Sardinilla; Panama; size-asymmetric competition; tropical-tree plantations ID COSTA-RICA; ECOSYSTEM FUNCTION; SPECIES-DIVERSITY; HUMID TROPICS; RAIN-FOREST; PRODUCTIVITY; COMMUNITIES; BIOMASS; GROWTH; LIGHT AB A plantation of native trees was established in Panama in 2001 to study the relationship between biodiversity and ecosystem functioning. Five years later, mixed-species plots had experienced enhanced tree growth compared with monocultures. Searching for underlying mechanisms, we developed a neighborhood model isolating size and identity effects. We found that the size of neighbors is, by far, the largest source of variation in individual-tree diameter and height. Size-asymmetric competition appears as a structuring factor in the plantation. The relative growth rate of small trees was significantly lower than that of large trees, and their height and basal diameter were most variable. The 50 smallest trees of the plantation suffered a disproportionate amount of death, and the proportion of small trees was highest in monoculture. Increased biomass allocation to branches for trees growing in three-species plots suggests that competition for light might be taking place. Clearly, local neighborhood plays a central role in determining productivity, suggesting that scale needs to be incorporated in the theoretical development and analysis of biodiversity and ecosystem functioning. C1 [Potvin, Catherine] McGill Univ, Dept Biol, Montreal, PQ H3A 1B1, Canada. [Potvin, Catherine] Smithsonian Trop Res Inst, Panama City, Panama. [Dutilleul, Pierre] McGill Univ, Dept Plant Sci, Quebec City, PQ H9X 3V9, Canada. RP Potvin, C (reprint author), McGill Univ, Dept Biol, 1205 Dr Penfield, Montreal, PQ H3A 1B1, Canada. EM Catherine.potvin@mcgill.ca FU Smithsonian Tropical Research Institute; NSERC Individual Discovery FX The data collection was supervised by Jose Monteza, whose help in the field has been invaluable. We are grateful to Jose Bonilla, Benjamin Wadham-Gagnon, and Diane Sharpe, who harvested and weighed the trees in 2006, and to Chrystal Healey, who organized the biomass data from 2001 to 2005. Constructive comments on different versions of the manuscript by Frederic Guichard, Johanne Pelletier, Peter Stoll, and two anonymous reviewers were greatly appreciated. Financial support to the plantation by the Smithsonian Tropical Research Institute made this project feasible. Each author acknowledges an NSERC Individual Discovery grant. NR 37 TC 45 Z9 45 U1 4 U2 34 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA SN 0012-9658 J9 ECOLOGY JI Ecology PD FEB PY 2009 VL 90 IS 2 BP 321 EP 327 DI 10.1890/08-0353.1 PG 7 WC Ecology SC Environmental Sciences & Ecology GA 410IN UT WOS:000263570800005 PM 19323214 ER PT J AU Comita, LS Hubbell, SP AF Comita, Liza S. Hubbell, Stephen P. TI Local neighborhood and species' shade tolerance influence survival in a diverse seedling bank SO ECOLOGY LA English DT Article DE Barro Colorado Island; Panama; community compensatory trend; forest dynamics plot; regeneration; seedling bank; spatial autocorrelation; species coexistence; tropical forest ID TROPICAL TREE; DENSITY-DEPENDENCE; RAIN-FOREST; NEOTROPICAL FOREST; SPATIAL-PATTERN; COEXISTENCE; GROWTH; RECRUITMENT; MORTALITY; COMPETITION AB Accumulating evidence suggests that negative density dependence, particularly at early life stages, is widespread in plant communities. We hypothesized that survival in forest seedling banks declines with increasing density of conspecific neighbors and that local-scale effects cause a negative correlation between seedling survival and tree species abundance in the community. We tested these hypotheses using data on 48 956 established seedlings of 235 species over three years in a 50-ha plot in Panama. For all species combined, we found a significant negative effect of conspecific seedling and adult neighbors within 10 m. In species-level analyses, neighbor density affected survival for 45 of 59 species, with effects of conspecifics different from heterospecifics for 29 species. Despite negative effects of local conspecific neighbors, seedling survival tended to be positively correlated with species abundance at the 50-ha scale. However, when accounting for species' shade tolerance, we found a significant negative relationship between seedling survival and species' basal area, but not density, in the 50-ha plot. Our findings indicate that attempts to quantify the contribution of density dependence to tropical tree species coexistence must integrate effects of neighbors across multiple life stages and should also take into account variation in life history strategy. C1 [Comita, Liza S.; Hubbell, Stephen P.] Univ Georgia, Dept Plant Biol, Athens, GA 30602 USA. [Hubbell, Stephen P.] Smithsonian Trop Res Inst, Balboa Ancon, Panama. RP Comita, LS (reprint author), Columbia Univ, Dept Ecol Evolut & Environm Biol, New York, NY 10027 USA. EM lsc2125@columbia.edu FU Mellon Foundation; National Science Foundation [DEB-0075102]; Center for Tropical Forest Science; Smithsonian Tropical Research Institute FX We thank the dozens of assistants who helped collect data on trees and seedlings in the BCI plot over the past 25 years. In particular, we thank S. Aguilar and R. Perez for species identifications and S. Lao for database management. Funding was provided by the Mellon Foundation and National Science Foundation (DEB-0075102). L. S. Comita acknowledges the support of an NSF Graduate Research Fellowship and a University of Georgia Presidential Fellowship. Logistical support was provided by the Center for Tropical Forest Science and the Smithsonian Tropical Research Institute. We thank R. Condit for valuable statistical advice and S. Queenborough, R. Pulliam, C. Peterson, J. Hamrick, and D. Porter for critical comments on the manuscript. NR 32 TC 84 Z9 99 U1 7 U2 59 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA SN 0012-9658 J9 ECOLOGY JI Ecology PD FEB PY 2009 VL 90 IS 2 BP 328 EP 334 DI 10.1890/08-0451.1 PG 7 WC Ecology SC Environmental Sciences & Ecology GA 410IN UT WOS:000263570800006 PM 19323215 ER PT J AU Kellner, JR Clark, DB Hubbell, SP AF Kellner, James R. Clark, David B. Hubbell, Stephen P. TI Pervasive canopy dynamics produce short-term stability in a tropical rain forest landscape SO ECOLOGY LETTERS LA English DT Letter DE canopy gap; forest dynamics; global change; light detection and ranging; remote sensing; stability ID RESOLUTION SATELLITE DATA; ABOVEGROUND BIOMASS; GAP DYNAMICS; TREE HEIGHT; COSTA-RICA; LA-SELVA; CARBON; GROWTH; FOOTPRINT; PATTERNS AB A fundamental property of all forest landscapes is the size frequency distribution of canopy gap disturbances. But characterizing forest structure and changes at large spatial scales has been challenging and most of our understanding is from permanent inventory plots. Here we report the first application of light detection and ranging remote sensing to measurements of canopy disturbance and regeneration in an old-growth tropical rain forest landscape. Pervasive local height changes figure prominently in the dynamics of this forest. Although most canopy gaps recruited to higher positions during 8.5 years, size frequency distributions were similar at two points in time and well-predicted by power-laws. At larger spatial scales (hundreds of ha), height increases and decreases occurred with similar frequency and changes to canopy height that were analysed using a height transition matrix suggest that the distribution of canopy height at the beginning of the study was close to the projected steady-state equilibrium under the recent disturbance regime. Taken together, these findings show how widespread local height changes can produce short-term stability in a tropical rain forest landscape. C1 [Kellner, James R.; Hubbell, Stephen P.] Univ Georgia, Dept Plant Pathol, Athens, GA 30602 USA. [Clark, David B.] Univ Missouri, Dept Biol, St Louis, MO 63121 USA. [Hubbell, Stephen P.] Smithsonian Trop Res Inst, Ancon, Panama. RP Kellner, JR (reprint author), Univ Georgia, Dept Plant Pathol, Athens, GA 30602 USA. EM jkellner@stanford.edu NR 48 TC 45 Z9 45 U1 2 U2 23 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1461-023X J9 ECOL LETT JI Ecol. Lett. PD FEB PY 2009 VL 12 IS 2 BP 155 EP 164 DI 10.1111/j.1461-0248.2008.01274.x PG 10 WC Ecology SC Environmental Sciences & Ecology GA 394SR UT WOS:000262468500005 PM 19143827 ER PT J AU Santagata, S Bacela, K Reid, DF Mclean, KA Cohen, JS Cordell, JR Brown, CW Johengen, TH Ruiz, GM AF Santagata, Scott Bacela, Karolina Reid, David F. Mclean, Kevin A. Cohen, Jill S. Cordell, Jeffery R. Brown, Christopher W. Johengen, Thomas H. Ruiz, Gregory M. TI CONCENTRATED SODIUM CHLORIDE BRINE SOLUTIONS AS AN ADDITIONAL TREATMENT FOR PREVENTING THE INTRODUCTION OF NONINDIGENOUS SPECIES IN THE BALLAST TANKS OF SHIPS DECLARING NO BALLAST ON BOARD SO ENVIRONMENTAL TOXICOLOGY AND CHEMISTRY LA English DT Article DE Introduced species; Ballast water; Zooplankton; Great Lakes; Salinity tolerance ID INVERTEBRATE RESTING EGGS; FRESH-WATER INVERTEBRATES; SALINITY TOLERANCE; GREAT-LAKES; RESIDUAL BALLAST; CHESAPEAKE BAY; NACL SALINITY; MACROINVERTEBRATES; SEA; ZOOPLANKTON AB Currently, seawater flushing is the only management strategy for reducing the number of viable organisms in residual sediments and water of ballast tanks of vessels declaring no ballast on board (NOBOB) that traffic ports of the eastern United States. Previously, we identified several species of freshwater and brackish-water peracarid crustaceans able to survive the osmotic shock that occurs during open-ocean ballast water exchange and, potentially, to disperse over long distances via ballasted ships and NOBOB vessels. We tested the efficacy of concentrated sodium chloride brine solutions as an additional treatment for eradicating the halotolerant taxa often present in the ballast tanks of NOBOB ships. The lowest brine treatments (30 ppt for 1 h) caused 100% mortality in several species of cladocerans and copepods collected from oligohaline habitats. Several brackish-water peracarid crustaceans, however, including some that can survive in freshwater as well, required higher brine concentrations and longer exposure durations (45-60 ppt for 3-24 h). The most resilient animals were widely introduced peracarid crustaceans that generally prefer mesohaline habitats but do not tolerate freshwater (required brine treatments of 60-110 ppt for 3-24 h). Brine treatments (30 ppt) also required less time to cause 100% mortality for eight taxa compared with treatments using 34 ppt seawater. Based on these experiments and published data, we present treatment strategies for the ballast tank biota often associated with NOBOB vessels entering the Great Lakes region. We estimate the lethal dosage of brine for 95% of the species in our experiments to be 110 ppt (95% confidence interval, 85-192 ppt) when the exposure time is 1 h and 60 ppt (95% confidence interval, 48-98 ppt) when the exposure duration is 6 h or longer. C1 [Santagata, Scott; Mclean, Kevin A.; Cohen, Jill S.; Brown, Christopher W.; Ruiz, Gregory M.] Smithsonian Environm Res Ctr, Marine Invas Lab, Edgewater, MD 21037 USA. [Bacela, Karolina] Univ Lodz, Dept Invertebrate Zool & Hydrobiol, PL-90237 Lodz, Poland. [Reid, David F.] NOAA, Great Lakes Environm Res Lab, Ann Arbor, MI 48105 USA. [Cordell, Jeffery R.] Univ Washington, Sch Aquat & Fishery Sci, Seattle, WA 98195 USA. [Johengen, Thomas H.] Univ Michigan, Cooperat Inst Limnol & Ecosyst Res, Ann Arbor, MI 48109 USA. RP Santagata, S (reprint author), Long Isl Univ, Dept Biol, CW Post Campus,720 No Blvd, Brookville, NY 11548 USA. EM scott.santagata@gmail.com RI Bacela-Spychalska, Karolina/E-4234-2015; OI Bacela-Spychalska, Karolina/0000-0003-4498-5107; Ruiz, Gregory/0000-0003-2499-441X FU National Oceanic and Atmospheric Administration, Aquatic Invasive Species Program; University of Michigan FX We thank the following institutions and individuals: Z.R. Gasiunaite, Coastal Research and Planning Institute, Klaipeda University, Klaipeda, Lithuania; C. Stepien, Lake Erie Center, University of Toledo; Northwestern Michigan College Great Lakes Water Studies Institute; M. Laterveer, The Rotterdam Zoo/Aquarium; National Oceanographic Atmospheric Administration's laboratories at Alepna and Muskegon, Michigan, USA; and the Romberg Tiburon Center for Environmental Studies, San Francisco State University. Funding was provided by the National Oceanic and Atmospheric Administration, Aquatic Invasive Species Program (National Center for Research on Aquatic Invasive Species), through the Cooperative Institute for Limnology and Ecosystems Research administered by the University of Michigan. Contribution 1476 of the Great Lakes Environmental Research Laboratory. NR 37 TC 7 Z9 7 U1 0 U2 11 PU SETAC PRESS PI PENSACOLA PA 1010 N 12TH AVE, PENSACOLA, FL 32501-3367 USA SN 0730-7268 J9 ENVIRON TOXICOL CHEM JI Environ. Toxicol. Chem. PD FEB PY 2009 VL 28 IS 2 BP 346 EP 353 DI 10.1897/08-140.1 PG 8 WC Environmental Sciences; Toxicology SC Environmental Sciences & Ecology; Toxicology GA 398HN UT WOS:000262723300016 PM 18811222 ER PT J AU Ruczynski, I Kalko, EKV Siemers, BM AF Ruczynski, Ireneusz Kalko, Elisabeth K. V. Siemers, Bjoern M. TI Calls in the Forest: A Comparative Approach to How Bats Find Tree Cavities SO ETHOLOGY LA English DT Article ID BIALOWIEZA-PRIMEVAL-FOREST; FEMALE BECHSTEINS BATS; NYCTALUS-NOCTULA; MYOTIS-NATTERERI; ECHOLOCATION CALLS; ROOST SELECTION; N-LEISLERI; INFORMATION-TRANSFER; INSECTIVOROUS BATS; PLECOTUS-AURITUS AB Although tree cavities are a particularly critical resource for forest bats, how bats search for and find new roosts is still poorly known. Building on a recent study on the sensory basis of roost finding in the noctule (Ruczynski et al. 2007), here we take a comparative approach to how bats find roosts. We tested the hypothesis that species' flight abilities and echolocation call characteristics play important roles in how well and by which cues bats find new tree roosts. We used the very manoeuvrable, faintly echolocating brown long-eared bat (Plecotus auritus) and the less manoeuvrable, louder Daubenton's bat (Myotis daubentonii) as study species. The species are sympatric in European temperate forests and both roost in tree cavities. We trained bats in short-term captivity to find entrances to tree cavities and experimentally manipulated the sensory cues available to them. In both species, cue type influenced the search time for successful cavity detection. Visual, olfactory and temperature cues did not improve the bats' performance over the performance by echolocation alone. Eavesdropping on conspecific echolocation calls played back from inside the cavity decreased search time in Daubenton's bat (M. daubentonii), underlining the double function of echolocation signals - orientation and communication. This was not so in the brown long-eared bat (P. auritus) that has low call amplitudes. The highly manoeuvrable P. auritus found cavities typically from flight and the less manoeuvrable M. daubentonii found more entrances during crawling. Comparison with the noctule data from Ruczynski et al. (2007) indicates that manoeuvrability predicts the mode of cavity search. It further highlights the importance of call amplitude for eavesdropping and cavity detection in bats. C1 [Ruczynski, Ireneusz] Polish Acad Sci, Mammal Res Inst, PL-17230 Bialowieza, Poland. [Kalko, Elisabeth K. V.] Smithsonian Trop Res Inst, Balboa, Panama. [Kalko, Elisabeth K. V.] Univ Ulm, Ulm, Germany. [Siemers, Bjoern M.] Max Planck Inst Ornithol, Sensory Ecol Grp, Seewiesen, Germany. RP Ruczynski, I (reprint author), Polish Acad Sci, Mammal Res Inst, Waszkiewicza 1, PL-17230 Bialowieza, Poland. EM iruczyns@zbs.bialowieza.pl FU Polish Ministry of Science and Higher Education [2 PO4F 040 29]; Max Planck Society FX We are grateful to Joanna Prokopiuk, Anke Hellbach, Ola Szarlik, Anna Nowicki, Ewelina Rogozinska, Marta Wojciech and Katarzyna Walor for assistance during field work, Jerzy Chilecki for helping with technical problems, Dieter Schmidl for drawing the bat pictures and Leonie Baier for help in assembling figures and Klemen Koselj for statistical advice. Paul Racey provided helpful comments and suggestions. We thank two anonymous referees for helpful comments on the manuscript. The study was funded by a grant from the Polish Ministry of Science and Higher Education (2 PO4F 040 29) and supported by the Max Planck Society. NR 56 TC 20 Z9 20 U1 1 U2 26 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0179-1613 J9 ETHOLOGY JI Ethology PD FEB PY 2009 VL 115 IS 2 BP 167 EP 177 DI 10.1111/j.1439-0310.2008.01599.x PG 11 WC Psychology, Biological; Behavioral Sciences; Zoology SC Psychology; Behavioral Sciences; Zoology GA 395FP UT WOS:000262510300007 ER PT J AU Hurt, C Anker, A Knowlton, N AF Hurt, Carla Anker, Arthur Knowlton, Nancy TI A MULTILOCUS TEST OF SIMULTANEOUS DIVERGENCE ACROSS THE ISTHMUS OF PANAMA USING SNAPPING SHRIMP IN THE GENUS ALPHEUS SO EVOLUTION LA English DT Article DE Alpheus; coalescent theory; Isthmus of Panama; molecular evolution; speciation ID SPECIES COMPLEX CRUSTACEA; APPROXIMATE BAYESIAN COMPUTATION; ANCESTRAL POPULATION SIZES; MOLECULAR CLOCK; MITOCHONDRIAL-DNA; EASTERN PACIFIC; MULTIPLE LOCI; ALPHEIDAE; DECAPODA; RATES AB The completion of the Panamanian Isthmus is one of the greatest natural experiments in evolution, sending multiple species pairs from a broad range of taxonomic groups on independent evolutionary trajectories. The resulting transisthmian sister species have been used as model systems for examining consequences that accompany cessation of gene flow in formerly panmictic populations. However, variance in pairwise genetic distances of these "geminates" often exceeds expectations, seemingly conflicting with the assumption that separation of populations was contemporaneous with the final closure of the Isthmus. Multilocus datasets and coalescent-based analytical methods can be used to estimate divergence times while accounting for variance in gene divergence that predates isolation, thus removing the need to invoke unequal divergence times. Here we present results from Bayesian analyses of sequence data from seven nuclear and one mitochondrial marker in eight transisthmian species pairs in the snapping shrimp genus Alpheus. Divergence times in two species pairs were shown to occur much earlier than the Isthmus final closure, but much of the variance in pairwise genetic distances from cytochrome oxidase I (COI) was explained when ancestral polymorphisms were accounted for. Results illustrate how coalescent approaches may be more appropriate for dating recent divergences than for estimating ancient speciation events. C1 [Hurt, Carla] Univ Miami, Dept Biol, Coral Gables, FL 33124 USA. [Anker, Arthur] Univ Florida, Dept Zool, Gainesville, FL 32611 USA. [Knowlton, Nancy] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. RP Hurt, C (reprint author), Univ Miami, Dept Biol, Coral Gables, FL 33124 USA. EM hurtc@bio.miami.edu RI Hurt, Carla/A-3284-2011 NR 48 TC 30 Z9 33 U1 5 U2 42 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 FEB PY 2009 VL 63 IS 2 BP 514 EP 530 DI 10.1111/j.1558-5646.2008.00566.x PG 17 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 405WD UT WOS:000263254000017 PM 19154357 ER PT J AU Mehdiabadi, NJ Kronforst, MR Queller, DC Strassmann, JE AF Mehdiabadi, Natasha J. Kronforst, Marcus R. Queller, David C. Strassmann, Joan E. TI PHYLOGENY, REPRODUCTIVE ISOLATION AND KIN RECOGNITION IN THE SOCIAL AMOEBA DICTYOSTELIUM PURPUREUM SO EVOLUTION LA English DT Article DE Cellular slime molds; cryptic species; macrocysts; population structure; rDNA gene tree; social evolution ID CELLULAR SLIME-MOLDS; GENETICAL EVOLUTION; MATING TYPES; MICROORGANISMS; GIGANTEUM AB Little is known about the population structure of social microorganisms, yet such studies are particularly interesting for the ways that genetic variation impacts their social evolution. Dictyostelium, a eukaryotic microbe widely used as a developmental model, has a social fruiting stage in which some formerly independent individuals die to help others. To assess genetic variation within the social amoeba Dictyostelium purpureum, we sequenced similar to 4000 base pairs of ribosomal DNA ( rDNA) from 37 isolates collected in Texas, Virginia, and Japan. Our analysis showed extensive genetic variation between populations and clear evidence of phylogenetic structure. We identified three major phylogenetic groups that were more different than other accepted species pairs. Tests using pairs of clones showed that both sexual macrocyst and asexual fruiting body formation were influenced by genetic divergence. Macrocysts were less likely to form between pairs of clones from different groups than from the same group. There was also a correlation between the genetic divergence of a pair of clones and their degree of mixing within fruiting bodies. These observations suggest that cryptic species might occur within D. purpureum and, more importantly, reveal how genetic variation impacts social interactions. C1 [Kronforst, Marcus R.] Harvard Univ, FAS Ctr Syst Biol, Cambridge, MA 02138 USA. [Mehdiabadi, Natasha J.; Queller, David C.; Strassmann, Joan E.] Rice Univ, Dept Ecol & Evolutionary Biol, Houston, TX 77005 USA. RP Mehdiabadi, NJ (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, POB 37012, Washington, DC 20013 USA. EM Mehdiabadi@si.edu; mkronforst@cgr.harvard.edu; queller@rice.edu; strassm@rice.edu OI Strassmann, Joan/0000-0003-0638-8440 FU National Science Foundation (NSF) [EF-0626963]; NSF [DBI-0301415]; National Library of Medicine [5T15 LM07093] FX We thank members of the Strassmann-Queller laboratory for help with collecting samples, especially C. Jack, T. Edwards, W. Massie, and S. Rodriguez. We also thank S. Brady for help with phylogenetic analyses; D. Matute for statistical advice; and P. Abbot, J. Coyne, S. Kalla, S. West, and two anonymous reviewers for helpful comments and discussion. This material is based on work supported by the National Science Foundation (NSF) Program under Grant EF-0626963. NJM was supported by an NSF Postdoctoral Fellowship DBI-0301415 in Microbial Biology and a Keck Postdoctoral Fellowship in Computational Biology (National Library of Medicine Grant 5T15 LM07093). NR 28 TC 13 Z9 13 U1 0 U2 6 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0014-3820 J9 EVOLUTION JI Evolution PD FEB PY 2009 VL 63 IS 2 BP 542 EP 548 DI 10.1111/j.1558-5646.2008.00574.x PG 7 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 405WD UT WOS:000263254000020 PM 19215294 ER PT J AU Kursar, TA Engelbrecht, BMJ Burke, A Tyree, MT El Omari, B Giraldo, JP AF Kursar, Thomas A. Engelbrecht, Bettina M. J. Burke, Amy Tyree, Melvin T. El Omari, Bouchra Giraldo, Juan P. TI Tolerance to low leaf water status of tropical tree seedlings is related to drought performance and distribution SO FUNCTIONAL ECOLOGY LA English DT Article DE drought resistance; dry season; hydraulic conductance; rainfall; water potential ID DESICCATION-TOLERANCE; MOIST FOREST; BETA-DIVERSITY; SURVIVAL; CONDUCTANCE; SENSITIVITY; CAVITATION; GRADIENTS; PATTERNS; DIEBACK AB Habitat specialization models predict that adaptations to environmental conditions explain species distributions. In tropical rainforests, the ability of the seedlings to survive during drought has been shown to be a key determinant of species distributions. We hypothesize that differences among species in their tolerance to low tissue water status is the mechanism underlying differences in performance during drought. To test this hypothesis we quantified tolerance to low leaf water status for over 20 species from central Panama in screenhouse experiments using two different experimental approaches. Results from both approaches were highly correlated with each other. We found that tolerance to low leaf water status correlated with species drought performance in the field and with their distribution across a gradient of dry season length, with the more desiccation-tolerant species having higher survival in dry relative to irrigated conditions, and occurring in drier areas. These results support the hypothesis that, in tropical forests, tolerance to low tissue water status governs seedling performance during drought, as well as being a determinant of species distribution patterns. Lower tolerance to low leaf water status was correlated with greater stem hydraulic conductance. In addition, all species tested, including both desiccation-sensitive and desiccation-resistant species, showed similar losses of xylem conductance, about 80%, when near death. These results suggest that a principal mechanism by which desiccation leads to plant mortality is the loss of xylem conductivity. C1 [Kursar, Thomas A.] Univ Utah, Dept Biol, Salt Lake City, UT 84112 USA. [Kursar, Thomas A.; Engelbrecht, Bettina M. J.; Burke, Amy; Tyree, Melvin T.; El Omari, Bouchra; Giraldo, Juan P.] Smithsonian Trop Res Inst, Panama City, Panama. [Engelbrecht, Bettina M. J.] Univ Kaiserslautern, Dept Plant Ecol & Systemat, D-67663 Kaiserslautern, Germany. [Tyree, Melvin T.] USDA Forest Serv, No Res Stn, S Burlington, VT 05403 USA. [Tyree, Melvin T.] Univ Alberta, Dept Renewable Resources, Edmonton, AB T6G 2E3, Canada. RP Kursar, TA (reprint author), Univ Utah, Dept Biol, Salt Lake City, UT 84112 USA. EM kursar@biology.utah.edu RI Engelbrecht, Bettina/E-9914-2012 FU Andrew W. Mellon Foundation; USDA Forest Service FX Authors thank N. Anaya, M. Rios, G. Rivas, R. Perez, S. Aguilar, and T. Brenes-Arguedas for assistance with determining species distributions, D. Feener for statistical advice, J. Sperry for comments on the text and the Autoridad Nacional del Ambiente of Panama for research and collection permits. The project was funded by the Andrew W. Mellon Foundation and the USDA Forest Service. NR 36 TC 78 Z9 81 U1 6 U2 71 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0269-8463 J9 FUNCT ECOL JI Funct. Ecol. PD FEB PY 2009 VL 23 IS 1 BP 93 EP 102 DI 10.1111/j.1365-2435.2008.01483.x PG 10 WC Ecology SC Environmental Sciences & Ecology GA 395FQ UT WOS:000262510400010 ER PT J AU Miller, W Drautz, DI Janecka, JE Lesk, AM Ratan, A Tomsho, LP Packard, M Zhang, Y McClellan, LR Qi, J Zhao, F Gilbert, MTP Dalen, L Arsuaga, JL Ericson, PGP Huson, DH Helgen, KM Murphy, WJ Gotherstrom, A Schuster, SC AF Miller, Webb Drautz, Daniela I. Janecka, Jan E. Lesk, Arthur M. Ratan, Aakrosh Tomsho, Lynn P. Packard, Mike Zhang, Yeting McClellan, Lindsay R. Qi, Ji Zhao, Fangqing Gilbert, M. Thomas P. Dalen, Love Arsuaga, Juan Luis Ericson, Per G. P. Huson, Daniel H. Helgen, Kristofer M. Murphy, William J. Gotherstrom, Anders Schuster, Stephan C. TI The mitochondrial genome sequence of the Tasmanian tiger (Thylacinus cynocephalus) SO GENOME RESEARCH LA English DT Article ID MARSUPIAL WOLF; DNA-SEQUENCES; PHYLOGENY; MAMMOTH AB We report the first two complete mitochondrial genome sequences of the thylacine (Thylacinus cynocephalus), or so-called Tasmanian tiger, extinct since 1936. The thylacine's phylogenetic position within australidelphian marsupials has long been debated, and here we provide strong support for the thylacine's basal position in Dasyuromorphia, aided by mitochondrial genome sequence that we generated from the extant numbat (Myrmecobius fasciatus). Surprisingly, both of our thylacine sequences differ by 11%-15% from putative thylacine mitochondrial genes in GenBank, with one of our samples originating from a direct offspring of the previously sequenced individual. Our data sample each mitochondrial nucleotide an average of 50 times, thereby providing the first high-fidelity reference sequence for thylacine population genetics. Our two sequences differ in only five nucleotides out of 15,452, hinting at a very low genetic diversity shortly before extinction. Despite the samples' heavy contamination with bacterial and human DNA and their temperate storage history, we estimate that as much as one-third of the total DNA in each sample is from the thylacine. The microbial content of the two thylacine samples was subjected to metagenomic analysis, and showed striking differences between a wild-captured individual and a born-in-captivity one. This study therefore adds to the growing evidence that extensive sequencing of museum collections is both feasible and desirable, and can yield complete genomes. C1 [Miller, Webb; Drautz, Daniela I.; Lesk, Arthur M.; Ratan, Aakrosh; Tomsho, Lynn P.; Packard, Mike; Zhang, Yeting; McClellan, Lindsay R.; Qi, Ji; Zhao, Fangqing; Schuster, Stephan C.] Penn State Univ, Ctr Comparat Genom & Bioinformat, University Pk, PA 16802 USA. [Janecka, Jan E.; Murphy, William J.] Texas A&M Univ, Coll Vet Med & Biomed Sci, Dept Vet Integrat Biosci, College Stn, TX 77843 USA. [Gilbert, M. Thomas P.] Univ Copenhagen, Ctr Ancient Genet, DK-2100 Copenhagen, Denmark. [Dalen, Love] Univ London, Sch Biol Sci, Egham TW20 0EX, Surrey, England. [Arsuaga, Juan Luis] ISCIII Evoluc & Comportamiento Humanos, Ctr Mixto UCM, Pabellon 28029, Spain. [Ericson, Per G. P.] Swedish Museum Nat Hist, Dept Vertebrate Zool, S-10405 Stockholm, Sweden. [Huson, Daniel H.] Univ Tubingen, Ctr Bioinformat Tubingen, D-72076 Tubingen, Germany. [Helgen, Kristofer M.] Smithsonian Inst, Natl Museum Nat Hist, Div Mammals, Washington, DC 20013 USA. [Gotherstrom, Anders] Uppsala Univ, Evolutionary Biol Ctr, Dept Evolutionary Biol, S-75236 Uppsala, Sweden. RP Miller, W (reprint author), Penn State Univ, Ctr Comparat Genom & Bioinformat, University Pk, PA 16802 USA. EM webb@bx.psu.edu; scs@bx.psu.edu RI Dalen, Love/A-6686-2008; Zhao, Fangqing/A-9992-2009; Research, NRM-BIG/F-2603-2013; Gilbert, Marcus/A-8936-2013; QI, JI/E-2797-2016; OI Dalen, Love/0000-0001-8270-7613; Gilbert, Marcus/0000-0002-5805-7195; Gotherstrom, Anders/0000-0001-8579-1304 FU National Human Genome Research Institute [HG002238]; Gordon and Betty Moore Foundation; Pennsylvania Department of Health FX We thank Don Wilson, Linda Gordon, Michael Carleton, Helen Kafka, Paul Rhymer, Lauren Helgen, and Christen Wemmer for assistance at the Smithsonian Institution. We also thank Dr. Michael Bunce and Dr. Peter Spencer (Murdoch University), and Peter Mortensen, Olavi Gronwall, and Erik Ahlander (Swedish Museum of Natural History) for assistance with sample collection and data about the thylacine specimens, together with Adrian Wayne (Department of Environment and Conservation, Western Australia) for providing the numbat tissues. We are grateful to the National Museum of Natural History's Photographic Services for the images in Figure 1, and to Cathy Riemer for suggestions about the presentation. Sequencing-by-synthesis costs were covered in part by generous funding from Penn State University. This work was supported by the National Human Genome Research Institute, grant HG002238 (to W. M.), and by the Gordon and Betty Moore Foundation (to J. Q. and S. C. S.). This project was funded, in part, under a grant from the Pennsylvania Department of Health using Tobacco Settlement Funds appropriated by the legislature. NR 27 TC 60 Z9 63 U1 5 U2 38 PU COLD SPRING HARBOR LAB PRESS, PUBLICATIONS DEPT PI WOODBURY PA 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2924 USA SN 1088-9051 J9 GENOME RES JI Genome Res. PD FEB PY 2009 VL 19 IS 2 BP 213 EP 220 DI 10.1101/gr.082628.108 PG 8 WC Biochemistry & Molecular Biology; Biotechnology & Applied Microbiology; Genetics & Heredity SC Biochemistry & Molecular Biology; Biotechnology & Applied Microbiology; Genetics & Heredity GA 404ED UT WOS:000263132600005 PM 19139089 ER PT J AU Mayne, RG McSween, HY McCoy, TJ Gale, A AF Mayne, R. G. McSween, H. Y., Jr. McCoy, T. J. Gale, A. TI Petrology of the unbrecciated eucrites SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article ID HED PARENT BODY; BASALTIC EUCRITES; REFLECTANCE SPECTRA; ELECTRON-MICROPROBE; METAMORPHIC HISTORY; ANTARCTIC EUCRITES; ASTEROID 4-VESTA; OXYGEN-ISOTOPE; SOLAR-SYSTEM; GA AGO AB Twenty-nine unbrecciated eucrites have been thoroughly characterized in terms of the petrologic factors that affect their spectra, such as mineral chemistry, modal adundances, grain sizes, and textures. We have conducted a combined petrologic and spectral Study designed to provide insight into the petrogenesis of the basaltic crust of Vesta and the variety of rock-types that exist within it, as well as aid in the petrologic interpretation of spectra to be collected by the Dawn orbiting spacecraft. This paper details the petrology part of the study. Unbrecciated eucrite samples were selected to avoid the complications of lithologic mixing in the accompanying spectral study. A wide variety of textural types are seen within the basaltic eucrites, encompassing quenched, coarse-grained, and granoblastic samples. Zoned pyroxenes in eucrites and those that preserve a history of initial rapid cooling are rare. Nearly all eucrite samples have been thermally metamorphosed and would commonly be classified as equilibrated; however, this term reflects only the quadrilateral (Mg, Fe, and Ca) compositions of pyroxenes, and considerable variations are seen within the minor elements (Al, Ti, and Cr) in pyroxenes as well as plagioclase compositions. Determination of both pyroxene and plagioclase compositions together with pyroxene geothermometry provides a better estimate for the relative degree of thermal metamorphism a eucrite has experienced. The petrologic differences observed here might allow different eucrites to be distinguished spectrally. This is especially true for the varying pyroxene compositions as the spectra of eucrites are dominated by absorption features attributed to pyroxene. (C) 2008 Elsevier Ltd. All rights reserved. C1 [Mayne, R. G.; McSween, H. Y., Jr.] Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA. [Mayne, R. G.; McCoy, T. J.] Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20560 USA. [Gale, A.] Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA. RP Mayne, RG (reprint author), Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA. EM MayneR@si.edu FU Graduate Fellowship at the Smithsonian; NASA Cosmochemistry [NNG06GG36G] FX Samples analyzed in this study were provided by the Smithsonian National Museum of Natural History. We thank Alan Patchen for all assistance with the electron microprobe and Donald Lindsley for advice in using the QUILF program. We greatly appreciate the constructive reviews given by Akira Yamaguchi, Paul Buchanan, and Allan Treiman and thank Hiroko Nagahara for the editorial handling of this manuscript. This work was supported by a Graduate Fellowship at the Smithsonian to R.G.M. and NASA Cosmochemistry Grant NNG06GG36G to H.Y.M. NR 75 TC 55 Z9 57 U1 3 U2 18 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD FEB 1 PY 2009 VL 73 IS 3 BP 794 EP 819 DI 10.1016/j.gca.2008.10.035 PG 26 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 400OF UT WOS:000262877000012 ER PT J AU Morgan, ME Behrensmeyer, AK Badgley, C Barry, JC Nelson, S Pilbeam, D AF Morgan, Michele E. Behrensmeyer, Anna K. Badgley, Catherine Barry, John C. Nelson, Sherry Pilbeam, David TI Lateral trends in carbon isotope ratios reveal a Miocene vegetation gradient in the Siwaliks of Pakistan SO GEOLOGY LA English DT Article ID NORTHERN PAKISTAN; STABLE-ISOTOPES; PLANTS; PHOTOSYNTHESIS; PALEOECOLOGY; FOREST; MIDDLE AB Isotopic analyses of mammalian tooth enamel from a well-defined, laterally extensive 150 k.y. interval (9.15-9.30 Ma) reveal an ecological gradient in vegetation on the late Miocene sub-Himalayan alluvial plain. Two contemporaneous river systems deposited the sediments of this interval, with a mountain-sourced system (herein, Blue-gray) to the southwest interfingering with a foothill-sourced system (Buff) to the northeast. Fossil mammal teeth collected from a 32 km transect across this fluvial gradient are significantly more depleted in C-13 from northeastern localities than from southwestern localities. This trend occurs in equids, giraffids, suids, sivapithecine hominoids, and anthracotheres. We propose that the Buff fluvial system provided more equably moist substrate conditions and supported more closed-canopy vegetation than the Blue-gray fluvial system. Herbivores living along the paleovegetation gradient thus acquired different carbon isotopic signatures during the period of tooth enamel formation, resulting from higher delta C-13 values in the forage supported by the Blue-gray fluvial system compared with forage associated. with the Buff system. The data also imply that many Siwalik mammalian herbivores displayed marked fidelity in juvenile home ranges and habitats. C1 [Morgan, Michele E.; Barry, John C.; Pilbeam, David] Harvard Univ, Peabody Museum, Cambridge, MA 02138 USA. [Behrensmeyer, Anna K.] Smithsonian Inst, MRC 121, Dept Paleobiol, Washington, DC 20013 USA. [Badgley, Catherine] Univ Michigan, Museum Paleontol, Ann Arbor, MI 48019 USA. [Badgley, Catherine] Univ Michigan, Dept Ecol & Evolutionary Biol, Ann Arbor, MI 48019 USA. [Nelson, Sherry] Univ New Mexico, Dept Anthropol, Albuquerque, NM 87131 USA. RP Morgan, ME (reprint author), Harvard Univ, Peabody Museum, Cambridge, MA 02138 USA. FU National Science Foundation [EAR-0125663]; American School of Prehistoric Research fund of the Peabody Museum, Harvard University FX We thank Naomi Levin and Jared Singer for laboratory assistance and Miriam Belmaker. Thure Cerling, Mikael Fortelius, and Lawrence Flynn for helpful discussions. Andrew Barth, Paul Koch, Henry Fricke, and two anonymous reviewers provided constructive comments. Mary Parrish ably assisted with the figures. Research was supported by National Science Foundation grant EAR-0125663 and the American School of Prehistoric Research fund of the Peabody Museum, Harvard University. NR 29 TC 7 Z9 8 U1 2 U2 12 PU GEOLOGICAL SOC AMER, INC PI BOULDER PA PO BOX 9140, BOULDER, CO 80301-9140 USA SN 0091-7613 J9 GEOLOGY JI Geology PD FEB PY 2009 VL 37 IS 2 BP 103 EP 106 DI 10.1130/G25359A.1 PG 4 WC Geology SC Geology GA 403QK UT WOS:000263096900002 ER PT J AU Seiler, TJ Rasse, DP Li, JH Dijkstra, P Anderson, HP Johnson, DP Powell, TL Hungate, BA Hinkle, CR Drake, BG AF Seiler, Troy J. Rasse, Daniel P. Li, Jiahong Dijkstra, Paul Anderson, Hans P. Johnson, David P. Powell, Thomas L. Hungate, Bruce A. Hinkle, C. Ross Drake, Bert G. TI Disturbance, rainfall and contrasting species responses mediated aboveground biomass response to 11 years of CO2 enrichment in a Florida scrub-oak ecosystem SO GLOBAL CHANGE BIOLOGY LA English DT Article DE aboveground biomass; canopy closure; elevated CO2; long-term stimulation; Quercus geminata; Quercus myrtifolia; resource limitation; scrub-oak; species-specific response ID ELEVATED ATMOSPHERIC CO2; CARBON-DIOXIDE ENRICHMENT; OPEN-TOP CHAMBERS; LONG-TERM; QUERCUS-MYRTIFOLIA; RISING CO2; DECIDUOUS FOREST; NET ECOSYSTEM; TERRESTRIAL ECOSYSTEMS; NUTRIENT AVAILABILITY AB This study reports the aboveground biomass response of a fire-regenerated Florida scrub-oak ecosystem exposed to elevated CO2 (1996-2007), from emergence after fire through canopy closure. Eleven years exposure to elevated CO2 caused a 67% increase in aboveground shoot biomass. Growth stimulation was sustained throughout the experiment; although there was significant variability between years. The absolute stimulation of aboveground biomass generally declined over time, reflecting increasing environmental limitations to long-term growth response. Extensive defoliation caused by hurricanes in September 2004 was followed by a strong increase in shoot density in 2005 that may have resulted from reopening the canopy and relocating nitrogen from leaves to the nutrient-poor soil. Biomass response to elevated CO2 was driven primarily by stimulation of growth of the dominant species, Quercus myrtifolia, while Quercus geminata, the other co-dominant oak, displayed no significant CO2 response. Aboveground growth also displayed interannual variation, which was correlated with total annual rainfall. The rainfall x CO2 interaction was partially masked at the community level by species-specific responses: elevated CO2 had an ameliorating effect on Q. myrtifolia growth under water stress. The results of this long-term study not only show that atmospheric CO2 concentration had a consistent stimulating effect on aboveground biomass production, but also showed that available water is the primary driver of interannual variation in shoot growth and that the long-term response to elevated CO2 may have been caused by other factors such as nutrient limitation and disturbance. C1 [Seiler, Troy J.; Li, Jiahong; Anderson, Hans P.; Johnson, David P.; Powell, Thomas L.; Drake, Bert G.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Rasse, Daniel P.] Norwegian Inst Agr & Environm Sci, As, Norway. [Dijkstra, Paul; Hungate, Bruce A.] No Arizona Univ, Dept Biol Sci, Flagstaff, AZ 86011 USA. [Hinkle, C. Ross] Univ Cent Florida, Dept Biol, Orlando, FL 32816 USA. RP Drake, BG (reprint author), Smithsonian Environm Res Ctr, POB 28,647 Contees Wharf Rd, Edgewater, MD 21037 USA. EM drakeb@si.edu RI Hungate, Bruce/F-8991-2011; Powell, Thomas/F-9877-2016; OI Hungate, Bruce/0000-0002-7337-1887; Powell, Thomas/0000-0002-3516-7164; Daniel, Rasse/0000-0002-5977-3863 FU Department of Energy to the Smithsonian Institution [DE-FG02-95ER61993]; NASA Kennedy Space Center; Dynamac Corp.; US Fish and Wildlife Service; Merritt Island National Wildlife Refuge FX This work was supported by a grant from the Department of Energy to the Smithsonian Institution (DE-FG02-95ER61993). We are grateful to everyone who dedicated hard work and enthusiasm in support of the site over the years. We thank John Erickson and Jessica Hines for their helpful comments on an earlier version of this manuscript. We acknowledge the support and encouragement of NASA Kennedy Space Center, Dynamac Corp., and US Fish and Wildlife Service, Merritt Island National Wildlife Refuge. NR 80 TC 31 Z9 31 U1 2 U2 20 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1354-1013 J9 GLOBAL CHANGE BIOL JI Glob. Change Biol. PD FEB PY 2009 VL 15 IS 2 BP 356 EP 367 DI 10.1111/j.1365-2486.2008.01740.x PG 12 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 395FR UT WOS:000262510500006 ER PT J AU McAlpine, CA Etter, A Fearnside, PM Seabrook, L Laurance, WF AF McAlpine, C. A. Etter, A. Fearnside, P. M. Seabrook, L. Laurance, W. F. TI Increasing world consumption of beef as a driver of regional and global change: A call for policy action based on evidence from Queensland (Australia), Colombia and Brazil SO GLOBAL ENVIRONMENTAL CHANGE-HUMAN AND POLICY DIMENSIONS LA English DT Review DE Beef consumption; Carbon credits; Deforestation; Ecosystem degradation; Exotic grasses; Greenhouse gases; Market forces; New consumers; Regrowth forests; Soybeans ID GREENHOUSE-GAS EMISSIONS; RAIN-FOREST FRAGMENTATION; LAND-USE; TROPICAL DEFORESTATION; SUSTAINABLE DEVELOPMENT; AGRICULTURAL LAND; GRAZING SYSTEMS; CLIMATE-CHANGE; AMAZONIA; SAVANNA AB While the global community is seeking to reduce fossil fuel consumption, a parallel but equally important issue is the environmental impacts of increased world consumption of beef. We provide a comparative analysis and synthesis of the expansion of beef cattle production and its regional and global environmental impacts for Queensland (Australia), Colombia and Brazil. Evidence assembled indicates that rising beef consumption is a major driver of regional and global change, and warrants greater policy attention. We propose four policy imperatives to help mitigate escalating environmental impacts of beef: stop subsidising beef production and promoting beef consumption; control future expansion of soybeans and extensive grazing; protect and restore regrowth forests in grazing lands; and allocate resources to less environmentally damaging alternative land uses. (C) 2008 Elsevier Ltd. All rights reserved. C1 [McAlpine, C. A.; Seabrook, L.] Univ Queensland, Sch Geog Planning & Architecture, Ctr Remote Sensing & Spatial Informat Sci, St Lucia, Qld 4072, Australia. [Etter, A.] Javeriana Univ, Dept Ecol & Terr, Bogota, Colombia. [Fearnside, P. M.] Natl Inst Res Amazon INPA, BR-69011970 Manaus, Amazonas, Brazil. [Laurance, W. F.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP McAlpine, CA (reprint author), Univ Queensland, Sch Geog Planning & Architecture, Ctr Remote Sensing & Spatial Informat Sci, St Lucia, Qld 4072, Australia. EM c.mcalpine@uq.edu.au RI Seabrook, Leonie/D-2992-2009; McAlpine, Clive/A-3907-2010; Etter, Andres/E-1860-2011; Laurance, William/B-2709-2012; Fearnside, Philip/D-6559-2011 OI Seabrook, Leonie/0000-0001-5602-5168; Etter, Andres/0000-0003-0665-9300; Fearnside, Philip/0000-0003-3672-9082 NR 102 TC 84 Z9 88 U1 10 U2 92 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0959-3780 J9 GLOBAL ENVIRON CHANG JI Glob. Environ. Change-Human Policy Dimens. PD FEB PY 2009 VL 19 IS 1 BP 21 EP 33 DI 10.1016/j.gloenvcha.2008.10.008 PG 13 WC Environmental Sciences; Environmental Studies; Geography SC Environmental Sciences & Ecology; Geography GA 425RS UT WOS:000264655400005 ER PT J AU Carter, LM Campbell, BA Watters, TR Phillips, RJ Putzig, NE Safaeinili, A Plaut, JJ Okubo, CH Egan, AF Seu, R Biccari, D Orosei, R AF Carter, Lynn M. Campbell, Bruce A. Watters, Thomas R. Phillips, Roger J. Putzig, Nathaniel E. Safaeinili, Ali Plaut, Jeffrey J. Okubo, Chris H. Egan, Anthony F. Seu, Roberto Biccari, Daniela Orosei, Roberto TI Shallow radar (SHARAD) sounding observations of the Medusae Fossae Formation, Mars SO ICARUS LA English DT Article DE Mars; Mars, surface; Radar observations; Volcanism ID MARTIAN GEOLOGIC RECORD; VOLCANIC GEOLOGY; DEPOSITS; PATERA; REGION; DISPERSAL; ERUPTIONS; THARSIS; ICE AB The SHARAD (shallow radar) sounding radar on the Mars Reconnaissance Orbiter detects subsurface reflections in the eastern and western parts of the Medusae Fossae Formation (MFF). The radar waves penetrate up to 580 in of the MFF and detect clear subsurface interfaces in two locations: west MFF between 150 and 155 degrees E and east MFF between 209 and 213 degrees E. Analysis of SHARAD radargrams suggests that the real part of the permittivity is similar to 3.0, which falls within the range of permittivity values inferred from MARSIS data for thicker parts of the MFF. The SHARAD data cannot uniquely determine the composition of the MFF material, but the low permittivity implies that the upper few hundred meters of the MFF material has a high porosity. One possibility is that the MFF is comprised of low-density welded or interlocked pyroclastic deposits that are capable Of Sustaining the steep-sided yardangs and ridges seen in imagery. The SHARAD surface echo power across the MFF is low relative to typical martian plains, and completely disappears in parts of the east MFF that correspond to the radar-dark Stealth region. These areas are extremely rough at centimeter to meter scales, and the lack of echo power is most likely due to a combination of surface roughness and a low near-surface permittivity that reduces the echo strength from any locally flat regions, There is also no radar evidence for internal layering in any of the SHARAD data for the MFF, despite the fact that tens-of-meters scale layering is apparent in infrared and visible wavelength images of nearby areas. These interfaces may not be detected in SHARAD data if their permittivity contrasts are low, or if the layers are discontinuous. The lack of closely spaced internal radar reflectors suggests that the MFF is not an equatorial analog to the current martian polar deposits, which show clear evidence of multiple internal layers in SHARAD data. (c) 2008 Elsevier Inc. All rights reserved. C1 [Carter, Lynn M.; Campbell, Bruce A.; Watters, Thomas R.] Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20013 USA. [Phillips, Roger J.; Putzig, Nathaniel E.; Egan, Anthony F.] SW Res Inst, Boulder, CO 80302 USA. [Safaeinili, Ali; Plaut, Jeffrey J.] Jet Prop Lab, Pasadena, CA 91109 USA. [Okubo, Chris H.] US Geol Survey, Flagstaff, AZ 86001 USA. [Seu, Roberto; Biccari, Daniela] Univ Roma La Sapienza, Dipartimento INFOCOM, I-00184 Rome, Italy. [Orosei, Roberto] Inst Nazl Astrofis, Ist Astrofis Spaziale & Fis Cosm, I-00133 Rome, Italy. RP Carter, LM (reprint author), Smithsonian Inst, Ctr Earth & Planetary Studies, MRC 135,POB 37012, Washington, DC 20013 USA. EM carterl@si.edu RI Carter, Lynn/D-2937-2012 FU NASA MRO FX We thank the SHARAD Operations Center team, including Emanuele Gjacomoni, Federica Russo, Marco Cutigni, Oreste Fuga, and Riccardo Mecozzi for their assistance with targeting, calibration, and data processing. We thank the HIRISE and MRO engineering and operations teams for their work in designing, building, and operating the equipment. We are grateful to Fabrizio Bernardini for assistance with SHARAD data processing. Lionel Wilson and an anonymous reviewer provided helpful comments. The Shallow Subsurface Radar (SHARAD) was provided by the Italian Space Agency through a contract with Thales Alenia Space Italia, and it is operated by the INFOCOM Department, University of Rome "La Sapienza." This work was partially supported through a NASA MRO Participating Scientist grant to L.M. Carter. NR 31 TC 41 Z9 42 U1 2 U2 4 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 FEB PY 2009 VL 199 IS 2 BP 295 EP 302 DI 10.1016/j.icarus.2008.10.007 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 405UV UT WOS:000263250600007 ER PT J AU Ryabchun, S Tong, CYE Blundell, R Gol'tsman, G AF Ryabchun, Sergey Tong, Cheuk-Yu Edward Blundell, Raymond Gol'tsman, Gregory TI Stabilization Scheme for Hot-Electron Bolometer Receivers Using Microwave Radiation SO IEEE TRANSACTIONS ON APPLIED SUPERCONDUCTIVITY LA English DT Article DE Allan variance; hot-electron bolometer (HEB) mixer; radiometer equation; terahertz receivers AB We present the results of a stabilization scheme for terahertz receivers based on NbN hot-electron bolometer (HEB) mixers that uses microwave radiation with a frequency much lower than the gap frequency. of NbN to compensate for mixer current fluctuations. A feedback control loop, which actively controls the power level of the injected microwave radiation, has successfully been implemented to stabilize the operating point of the HEB mixer. This allows us to increase the receiver Allan time to 10 s and also improve the temperature resolution of the receiver by about 30% in the total power mode of operation. C1 [Ryabchun, Sergey; Tong, Cheuk-Yu Edward; Blundell, Raymond] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ryabchun, Sergey; Gol'tsman, Gregory] Moscow State Pedag Univ, Dept Phys & Informat Technol, Moscow 119992, Russia. RP Ryabchun, S (reprint author), Moscow State Pedag Univ, Dept Phys & Informat Technol, Moscow 119992, Russia. EM sryabchun@rplab.ru; etong@cfa.harvard.edu; rblundell@cfa.harvard.edu; goltsman@rplab.ru OI Tong, Edward/0000-0002-7736-4203 NR 26 TC 6 Z9 6 U1 2 U2 8 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 1051-8223 J9 IEEE T APPL SUPERCON JI IEEE Trans. Appl. Supercond. PD FEB PY 2009 VL 19 IS 1 BP 14 EP 19 DI 10.1109/TASC.2008.2008398 PG 6 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA 404NZ UT WOS:000263161300002 ER PT J AU Basset, Y Hawkins, BA Leather, SR AF Basset, Yves Hawkins, Bradford A. Leather, Simon R. TI Visions for insect conservation and diversity: spanning the gap between practice and theory SO INSECT CONSERVATION AND DIVERSITY LA English DT Editorial Material ID TROPICAL RAIN-FORESTS; CLIMATE-CHANGE; ARTHROPOD ASSEMBLAGES; SPATIAL-DISTRIBUTION; DISTRIBUTION MODELS; BIODIVERSITY; MANAGEMENT; ABUNDANCE; COMMUNITIES; ROUNDABOUTS C1 [Leather, Simon R.] Univ London Imperial Coll Sci Technol & Med, Div Biol, Ascot, Berks, England. [Basset, Yves] Smithsonian Trop Res Inst, Panama City, Panama. [Hawkins, Bradford A.] Univ Calif Irvine, Dept Ecol & Evolut Biol, Irvine, CA 92717 USA. RP Leather, SR (reprint author), Univ London Imperial Coll Sci Technol & Med, Div Biol, Silwood Pk Campus, Ascot, Berks, England. EM s.leather@imperial.ac.uk RI Hawkins, Bradford/A-3510-2011; Basset, Yves/B-6642-2014 NR 56 TC 6 Z9 7 U1 1 U2 10 PU WILEY-LISS PI HOBOKEN PA DIV JOHN WILEY & SONS INC, 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 1752-458X J9 INSECT CONSERV DIVER JI Insect. Conserv. Divers. PD FEB PY 2009 VL 2 IS 1 BP 1 EP 4 DI 10.1111/j.1752-4598.2008.00042.x PG 4 WC Biodiversity Conservation; Entomology SC Biodiversity & Conservation; Entomology GA 398VK UT WOS:000262759400001 ER PT J AU Berke, SK Cruz, V AF Berke, Sarah K. Cruz, Veronica TI Sublethal predation in an ecosystem engineering polychaete SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology CY JAN 03-07, 2009 CL Boston, MA SP Soc Integrat & Comparat Biol C1 [Berke, Sarah K.; Cruz, Veronica] Florida State Univ, Smithsonian Environm Res Ctr, Tallahassee, FL 32306 USA. EM skberke@gmail.com NR 0 TC 0 Z9 0 U1 0 U2 1 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD FEB PY 2009 VL 49 BP E14 EP E14 PG 1 WC Zoology SC Zoology GA 481KL UT WOS:000268808800054 ER PT J AU Brady, SG Danforth, BN Cardinal, S AF Brady, S. G. Danforth, B. N. Cardinal, S. TI Phylogeny and evolution of eusocial insects: a comparison of origins and losses in ants and bees SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology CY JAN 03-07, 2009 CL Boston, MA SP Soc Integrat & Comparat Biol C1 [Brady, S. G.; Danforth, B. N.; Cardinal, S.] Cornell Univ, Smithsonian Inst, Ithaca, NY 14853 USA. EM bradys@si.edu NR 0 TC 0 Z9 0 U1 1 U2 7 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD FEB PY 2009 VL 49 BP E20 EP E20 PG 1 WC Zoology SC Zoology GA 481KL UT WOS:000268808800080 ER PT J AU Craft, JD Paul, VJ Sotka, EE AF Craft, J. D. Paul, V. J. Sotka, E. E. TI A coevolutionary arms-race between macroalgae and herbivores: are tropical herbivores more tolerant of lipophilic secondary metabolites than temperate herbivores? SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology CY JAN 03-07, 2009 CL Boston, MA SP Soc Integrat & Comparat Biol C1 [Craft, J. D.; Paul, V. J.; Sotka, E. E.] Smithsonian Marine Stn, Coll Charleston, Charleston, SC USA. EM craftjd@gmail.com NR 0 TC 0 Z9 0 U1 0 U2 3 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD FEB PY 2009 VL 49 BP E40 EP E40 PG 1 WC Zoology SC Zoology GA 481KL UT WOS:000268808800157 ER PT J AU Douglass, JK Tobin, WF Wcislo, WT AF Douglass, J. K. Tobin, W. F. Wcislo, W. T. TI A Portable Microvolumeter for Studies of Invertebrate Brain-body Scaling SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology CY JAN 03-07, 2009 CL Boston, MA SP Soc Integrat & Comparat Biol C1 Smithsonian Trop Res Inst, Panama City, Panama. Univ Calif Santa Cruz, Santa Cruz, CA 95064 USA. EM douglassj@si.edu NR 0 TC 0 Z9 0 U1 0 U2 0 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD FEB PY 2009 VL 49 BP E223 EP E223 PG 1 WC Zoology SC Zoology GA 481KL UT WOS:000268808800887 ER PT J AU Hoang, LK Mccoy, KA St Mary, CM Guillette, LJ AF Hoang, L. K. Mccoy, K. A. St Mary, C. M. Guillette, L. J. TI Renal pathologies in giant toads (Bufo marinus) vary across land-use practices SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology CY JAN 03-07, 2009 CL Boston, MA SP Soc Integrat & Comparat Biol C1 [Hoang, L. K.; Mccoy, K. A.; St Mary, C. M.; Guillette, L. J.] Univ Florida, Smithsonian Trop Res Inst, Gainesville, FL 32611 USA. EM kristam@ufl.edu NR 0 TC 0 Z9 0 U1 0 U2 2 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD FEB PY 2009 VL 49 BP E243 EP E243 PG 1 WC Zoology SC Zoology GA 481KL UT WOS:000268808800968 ER PT J AU Javonillo, R Malabarba, LR Weitzman, SH Burns, JR AF Javonillo, R. Malabarba, L. R. Weitzman, S. H. Burns, J. R. TI Evolution of sexually dimorphic novelties and reproductive strategies in fishes of the family Characidae (Teleostei: Ostariophysi) SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology CY JAN 03-07, 2009 CL Boston, MA SP Soc Integrat & Comparat Biol C1 George Washington Univ, Washington, DC 20052 USA. Univ Fed Rio Grande do Sul, Porto Alegre, RS, Brazil. Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. EM rjavonil@gwu.edu RI Malabarba, Luiz/I-3225-2012 NR 0 TC 0 Z9 0 U1 0 U2 2 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD FEB PY 2009 VL 49 BP E84 EP E84 PG 1 WC Zoology SC Zoology GA 481KL UT WOS:000268808800336 ER PT J AU Muscedere, ML Seid, M Johnson, N Willey, T Gillis, B Traniello, JFA AF Muscedere, M. L. Seid, M. Johnson, N. Willey, T. Gillis, B. Traniello, J. F. A. TI Brains, neurotransmitters, nursing, and foraging in the ant Pheidole dentata SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology CY JAN 03-07, 2009 CL Boston, MA SP Soc Integrat & Comparat Biol C1 [Muscedere, M. L.; Seid, M.; Johnson, N.; Willey, T.; Gillis, B.; Traniello, J. F. A.] Northwestern Univ, Boston Univ, Smithsonian Trop Res Inst, Chicago, IL 60611 USA. EM mario@bu.edu NR 0 TC 1 Z9 1 U1 0 U2 3 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD FEB PY 2009 VL 49 BP E122 EP E122 PG 1 WC Zoology SC Zoology GA 481KL UT WOS:000268808800484 ER PT J AU Olson, JR Swanson, DL Cooper, SJ Braun, MJ Williams, JB AF Olson, J. R. Swanson, D. L. Cooper, S. J. Braun, M. J. Williams, J. B. TI Metabolic performance and latitudinal distribution of Black-capped and Carolina Chickadees SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology CY JAN 03-07, 2009 CL Boston, MA SP Soc Integrat & Comparat Biol C1 Ohio State Univ, Columbus, OH 43210 USA. Univ S Dakota, Vermillion, SD 57069 USA. Univ Wisconsin Oshkosh, Smithsonian Inst, Suitland, MD USA. EM olson.133@osu.edu NR 0 TC 0 Z9 0 U1 1 U2 2 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD FEB PY 2009 VL 49 BP E284 EP E284 PG 1 WC Zoology SC Zoology GA 481KL UT WOS:000268808801131 ER PT J AU Schwartz, ML Norenburg, JL AF Schwartz, M. L. Norenburg, J. L. TI Molecular phylogenetics and taxonomy of pilidiophoran nemerteans: tackling a can of worms SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology CY JAN 03-07, 2009 CL Boston, MA SP Soc Integrat & Comparat Biol C1 Seattle Univ, Seattle, WA USA. Smithsonian Inst, Washington, DC 20560 USA. EM norenburgj@si.edu RI Norenburg, Jon/K-3481-2015 OI Norenburg, Jon/0000-0001-7776-1527 NR 0 TC 0 Z9 0 U1 1 U2 1 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD FEB PY 2009 VL 49 BP E153 EP E153 PG 1 WC Zoology SC Zoology GA 481KL UT WOS:000268808800609 ER PT J AU Walters, LJ Turner, T Kuffner, IB Paul, VJ Ritson-Williams, R Grablow, K Settar, C Rivera, G Hickey, TD AF Walters, L. J. Turner, T. Kuffner, I. B. Paul, V. J. Ritson-Williams, R. Grablow, K. Settar, C. Rivera, G. Hickey, T. D. TI Coral-Algal-Urchin Interactions in Caribbean Waters SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology CY JAN 03-07, 2009 CL Boston, MA SP Soc Integrat & Comparat Biol C1 Univ Cent Florida, Orlando, FL 32816 USA. Univ Virgin Isl, St Thomas, VI USA. Smithsonian Inst, Washington, DC 20560 USA. EM ljwalter@pegasus.cc.ucf.edu NR 0 TC 0 Z9 0 U1 0 U2 3 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD FEB PY 2009 VL 49 BP E321 EP E321 PG 1 WC Zoology SC Zoology GA 481KL UT WOS:000268808801279 ER PT J AU Chaney, DS Mamay, SH DiMichele, WA Kerp, H AF Chaney, Dan S. Mamay, Sergius H. DiMichele, William A. Kerp, Hans TI AURITIFOLIA GEN. NOV., PROBABLE SEED PLANT FOLIAGE WITH COMIOID AFFINITIES FROM THE EARLY PERMIAN OF TEXAS, USA SO INTERNATIONAL JOURNAL OF PLANT SCIENCES LA English DT Article DE peltasperm; Permian; Texas; Comia ID NORTH-CENTRAL TEXAS; WEST TEXAS; PALEOBOTANY; PALYNOLOGY; MORPHOLOGY; ANATOMY; KANSAS AB Auritifolia waggoneri gen. et sp. nov. has compound leaves and is possibly a peltasperm, with venation similar to Comia Zalessky. The frond is once pinnate, >40 cm in length, with a short petiole, subopposite pinnae, increasing in size distally, terminating in two elongate pinnae. The petiole base is swollen. Fronds probably abscised upon senescence. Venation is three ordered, each higher order of progressively smaller diameter. Pinna midveins arise from the main rachis and give rise to secondary veins. Two types of tertiary veins are present. One type arises from the secondaries and forms fascicles; the other type is interfascicular and arises directly from pinna midveins. All tertiaries are of the same diameter. Tertiary veins dichotomize, anastomose, and may terminate in blind endings, so not all extend to the laminar margin. Laminae are amphistomatic. Monocyclic stoma are surrounded by five to six subsidiary cells. Epidermis and palisade parenchyma are uniseriate. Auritifolia is most similar to Comia in which the tertiaries lack anastomoses and blind endings and terminate at the laminar margin. The leaf architecture of Auritifolia differs significantly from that of Comia. (Russian and Chinese translations of this abstract are available in the online edition of International Journal of Plant Sciences.) C1 [Chaney, Dan S.; DiMichele, William A.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. [Kerp, Hans] Univ Munster, Forschungsstelle Palaobot, D-48143 Munster, Germany. RP Chaney, DS (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, MRC 121,POB 37012, Washington, DC 20013 USA. EM chaneyd@si.edu RI DiMichele, William/K-4301-2012 NR 47 TC 13 Z9 13 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 1058-5893 J9 INT J PLANT SCI JI Int. J. Plant Sci. PD FEB PY 2009 VL 170 IS 2 BP 247 EP 266 DI 10.1086/595293 PG 20 WC Plant Sciences SC Plant Sciences GA 406XP UT WOS:000263328500011 ER PT J AU Mamay, SH Chaney, DS DiMichele, WA AF Mamay, Sergius H. Chaney, Dan S. DiMichele, William A. TI COMIA, A SEED PLANT POSSIBLY OF PELTASPERMOUS AFFINITY: A BRIEF REVIEW OF THE GENUS AND DESCRIPTION OF TWO NEW SPECIES FROM THE EARLY PERMIAN (ARTINSKIAN) OF TEXAS, C-GREGGII SP NOV AND C-CRADDOCKII SP NOV. SO INTERNATIONAL JOURNAL OF PLANT SCIENCES LA English DT Article DE paleobotany; Paleozoic; Clear Fork Formation; Comia; peltasperm ID WEST TEXAS; PALEOBOTANY; PALYNOLOGY; BRONGNIART; COUNTY; PANGEA; FLORA AB Comia is a widespread foliage morphogenus of probable seed plant affinity primarily known from rocks of Late Permian age, in the Angaran and Cathaysian paleobiogeographic regions. It also occurs in the Early Permian of the western Euramerican equatorial paleobiogeographic region. Vegetative features and consistent association with peltaspermous reproductive organs suggest affinity with the Peltaspermales. New material from north-central Texas allows two new species to be attributed to this genus, Comia greggii and Comia craddockii. Both species are uncommon elements of the Early Permian ( Leonardian-Artinskian) flora. They exhibit a diagnostic form of venation typical of Comia and allied forms, in which the tertiary veins form fascicles and interfascicular groups. Ultimate veins extend from their insertion point to the laminar margin, usually with one dichotomy. They neither anastomose nor terminate in blind endings. In gross architecture, C. craddockii is once pinnate. The morphology of the frond of C. greggii is not known. The much wider, more finely veined laminae of C. greggii are clearly distinguishable from the narrow pinnules with coarser venation of C. craddockii. ( Russian and Chinese translations of this abstract are available in the online edition of International Journal of Plant Sciences.) C1 [Mamay, Sergius H.; Chaney, Dan S.; DiMichele, William A.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. RP Chaney, DS (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, MRC 121,POB 37012, Washington, DC 20013 USA. EM chaneyd@si.edu RI DiMichele, William/K-4301-2012 NR 60 TC 6 Z9 6 U1 1 U2 4 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 1058-5893 J9 INT J PLANT SCI JI Int. J. Plant Sci. PD FEB PY 2009 VL 170 IS 2 BP 267 EP 282 DI 10.1086/595294 PG 16 WC Plant Sciences SC Plant Sciences GA 406XP UT WOS:000263328500012 ER PT J AU Crofoot, MC Norton, TM Lessnau, RG Viner, TC Chen, TC Mazzaro, LM Yabsley, MJ AF Crofoot, M. C. Norton, T. M. Lessnau, R. G. Viner, T. C. Chen, T. C. Mazzaro, L. M. Yabsley, M. J. TI Field Anesthesia and Health Assessment of Free-ranging Cebus capucinus in Panama SO INTERNATIONAL JOURNAL OF PRIMATOLOGY LA English DT Article DE Barro Colorado Island; chemical immobilization; darting; disease; hematology; serology; Telazol ID EMERGING INFECTIOUS-DISEASES; BEARS URSUS-MARITIMUS; LEMURS LEMUR-CATTA; BIOMEDICAL EVALUATION; POLAR BEARS; TILETAMINE-HYDROCHLORIDE; ZOLAZEPAM-HYDROCHLORIDE; MALARIA INFECTION; FRENCH-GUIANA; WILDLIFE AB Health and disease are critical factors for understanding primate evolution and for developing effective conservation and management strategies. However, comprehensive health assessments of wild primate populations are rare, in part because of the difficulty and risk of chemically immobilizing subjects to obtain the necessary biological samples. We report here the results of a health assessment, as well as the methods and drug dosages used to capture white-faced capuchins (Cebus capucinus) on Barro Colorado Island, Panama. We captured and measured 24 capuchins as part of an ongoing radiotelemetry study, and collected biological samples from 9 of them for a comprehensive health survey. TelazolA (R) was very effective for immobilizing and capturing capuchins, although the doses we used were higher than those recommended for captive capuchins. High Telazol doses immobilized individuals quickly, ensuring that we were able to find and recover the sedated monkeys. The capuchins were generally in good condition, and had few ecto-, hemo-, or intestinal parasites. However, all but 1 of the adults had substantial dental abnormalities. In addition, 1 juvenile had indeterminate genitalia that we believe to be the result of hypospadias. Seven of the capuchins tested positive for exposure to Herpesvirus tamarinus and all individuals tested positive for exposure to Cebus cytomegalovirus. Hematology, serum chemistry, and plasma mineral levels from the wild individuals were, for the most part, comparable to those recorded for captive Cebus capucinus, and contribute to establishing baseline health values for the species. C1 [Crofoot, M. C.] Smithsonian Trop Res Inst, Panama City, Panama. [Crofoot, M. C.] Max Planck Inst Ornithol, Dept Migrat & Immunoecol, D-78315 Radolfzell am Bodensee, Germany. [Norton, T. M.] St Catherines Isl Fdn, Midway, GA 31320 USA. [Lessnau, R. G.] Detroit Zool Soc, Royal Oak, MI 48067 USA. [Viner, T. C.] Smithsonian Inst, Natl Zool Pk, Dept Pathol, Washington, DC 20008 USA. [Chen, T. C.] Boston Univ, Sch Med, Sect Endocrinol Diabet & Nutr, Boston, MA 02218 USA. [Mazzaro, L. M.] Myst Aquarium & Inst Explorat, Mystic, CT 06355 USA. [Yabsley, M. J.] Univ Georgia, Warnell Sch Forestry & Nat Resources, Athens, GA 30602 USA. [Yabsley, M. J.] Univ Georgia, Coll Vet Med, Dept Populat Hlth, SE Cooperat Wildlife Dis Study, Athens, GA 30602 USA. RP Crofoot, MC (reprint author), Smithsonian Trop Res Inst, Apartado 0843 03092, Panama City, Panama. EM crofootm@si.edu FU Smithsonian Tropical Research Institute (STRI); Automated Radio Telemetry System Initiative; Smithsonian Tropical Research Institute; Frederik Sheldon Travel Grant; American Society of Primatologists Small Research Grant; Department of Biology, Armstrong Atlantic State University; Department of Biological Anthropology; Harvard University; Harvard University IACUC [A-3593-1] FX We thank the Smithsonian Tropical Research Institute (STRI) and the Automated Radio Telemetry System Initiative, especially Oris Acevedo, Martin Wikelski, and Roland Kays for logistical support. We also thank Michelle Brown, Robyn Hoing, Jennifer Booth by, Robert Horan, Vilma Fernandez, George Middleton, Thomas Lambert, and Sheryl Staaden for help with darting; Nicanor Obaldia, DVM and Claudia Brandariz, DVM for veterinary support; Ann Bratthauer and Betty Ackerman for assistance analyzing samples; and Dennis Cote for help understanding the pharmacokinetics of Telazol. We thank Melissa Emery-Thompson, Zarin Machanda, Susy Cote, Linda Taylor, and Richard Wrangham for helpful comments and discussions on a previous draft of this paper. The Smithsonian Tropical Research Institute, the Frederik Sheldon Travel Grant, the American Society of Primatologists Small Research Grant, Sigma Xi, the Department of Biology, Armstrong Atlantic State University, and the Department of Biological Anthropology, Harvard University provided financial support for this work. The research described in this paper received clearance from the Harvard University IACUC (assurance number A-3593-1). NR 49 TC 10 Z9 10 U1 0 U2 15 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0164-0291 J9 INT J PRIMATOL JI Int. J. Primatol. PD FEB PY 2009 VL 30 IS 1 BP 125 EP 141 DI 10.1007/s10764-009-9333-6 PG 17 WC Zoology SC Zoology GA 404GN UT WOS:000263139300008 ER PT J AU Brostoff, LB Gonzalez, JJ Jett, P Russo, RE AF Brostoff, Lynn B. Gonzalez, Jhanis J. Jett, Paul Russo, Richard E. TI Trace element fingerprinting of ancient Chinese gold with femtosecond laser ablation-inductively coupled mass spectrometry SO JOURNAL OF ARCHAEOLOGICAL SCIENCE LA English DT Article DE Femtosecond; LA-ICP-MS; Trace element; Ancient gold ID ICP-MS; PRECIOUS METALS; NANOSECOND; SAMPLES; BRASS AB In this collaborative investigation, femtosecond laser ablation-inductively coupled mass spectrometry (LA-ICP-MS) was applied to the study of a remarkable group of ancient Chinese gold objects in the Smithsonian's Freer Gallery of Art and Arthur M. Sackler Gallery. Taking advantage of the superior ablation characteristics and high precision of a femtosecond 266 nm Ti:sapphire laser at Lawrence Berkeley National Laboratory, major, minor and trace element concentrations in the gold fragments were quantified. Results validate use of femtosecond LA-ICP-MS for revealing "fingerprints" in minute gold samples. These fingerprints allow us to establish patterns based on the association of silver, palladium and platinum that support historical, technical and stylistic relationships, and shed new light on these ancient objects. (C) 2008 Published by Elsevier Ltd. C1 [Brostoff, Lynn B.] Lib Congress, Preservat Res & Testing Div, Washington, DC 20540 USA. [Gonzalez, Jhanis J.; Russo, Richard E.] Univ Calif Berkeley, Lawrence Berkeley Lab, Berkeley, CA 94720 USA. [Jett, Paul] Smithsonian Inst, Freer Gallery Art Arthur M Sackler Museum, Washington, DC 20013 USA. RP Brostoff, LB (reprint author), Lib Congress, Preservat Res & Testing Div, 101 Independence Ave SE, Washington, DC 20540 USA. EM lbrostoff@loc.gov FU Office of Science, Office of Basic Energy Sciences, Chemical Sciences, Geosciences, and Biosciences Division; Deputy Administrator for Defense Nuclear Nonproliferation, Research and Development of the US Department of Energy [DE-AC02-05CH11231] FX The gold objects under study are part of the collection of the Freer Gallery of Art and Arthur M. Sackler Gallery, Smithsonian Institution. The gold foil fragments are part of The Dr Paul Singer Collection of Chinese Art of the Arthur M. Sackler Gallery, Smithsonian Institution; a joint gift of the Arthur M. Sackler Foundation, Paul Singer, the AMS Foundation for the Arts, Sciences, and Humanities, and the Children of Arthur M. Sackler, accession numbers RLS1997.48.4504 A-U. Work at LBNL was supported by the Office of Science, Office of Basic Energy Sciences, Chemical Sciences, Geosciences, and Biosciences Division, and the Deputy Administrator for Defense Nuclear Nonproliferation, Research and Development of the US Department of Energy under Contract No. DE-AC02-05CH11231. LB. also wishes to thank Jeff Speakman for reviewing an earlier draft of this paper. NR 29 TC 17 Z9 17 U1 1 U2 15 PU ACADEMIC PRESS LTD ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0305-4403 J9 J ARCHAEOL SCI JI J. Archaeol. Sci. PD FEB PY 2009 VL 36 IS 2 BP 461 EP 466 DI 10.1016/j.jas.2008.09.037 PG 6 WC Anthropology; Archaeology; Geosciences, Multidisciplinary SC Anthropology; Archaeology; Geology GA 400QX UT WOS:000262884700026 ER PT J AU Harbaugh, DT Wagner, WL Allan, GJ Zimmer, EA AF Harbaugh, Danica T. Wagner, Warren L. Allan, Gerard J. Zimmer, Elizabeth A. TI The Hawaiian Archipelago is a stepping stone for dispersal in the Pacific: an example from the plant genus Melicope (Rutaceae) SO JOURNAL OF BIOGEOGRAPHY LA English DT Article DE Hawaiian Islands; island biogeography; long-distance dispersal; Melicope; molecular phylogeny; Pacific biogeography; Rutaceae; stepping stone ID SILVERSWORD ALLIANCE ASTERACEAE; ILEX L. AQUIFOLIACEAE; NUCLEAR RIBOSOMAL DNA; NORTH-AMERICAN ORIGIN; PHYLOGENETIC-RELATIONSHIPS; CHLOROPLAST DNA; TRNL-F; TETRAMOLOPIUM ASTERACEAE; SANDALWOODS SANTALUM; MOLECULAR PHYLOGENY AB Pacific biogeographical patterns in the widespread plant genus Melicope J.R. Forst. & G. Forst. (Rutaceae) were examined by generating phylogenetic hypotheses based on chloroplast and nuclear ribosomal sequence data. The aims of the study were to identify the number of colonization events of Melicope to the Hawaiian Islands and to reveal the relationship of Hawaiian Melicope to the Hawaiian endemic genus Platydesma H. Mann. The ultimate goal was to determine if the Hawaiian Islands served as a source area for the colonization of Polynesia. Nineteen accessions were sampled in this study, namely eight Melicope species from the Hawaiian Islands, four from the Marquesas Islands, one species each from Tahiti, Australia and Lord Howe Island, two Australian outgroups and two species of the Hawaiian endemic genus Platydesma. To place our results in a broader context, 19 sequences obtained from GenBank were included in an additional analysis, including samples from Australia, Papua New Guinea, New Zealand, Southeast Polynesia and Asia. DNA sequences were generated across 19 accessions for one nuclear ribosomal and three chloroplast gene regions. Maximum parsimony analyses were conducted on separate and combined data sets, and a maximum likelihood analysis was conducted on the combined nuclear ribosomal and chloroplast data set. A broader nuclear ribosomal maximum parsimony analysis using sequences obtained from GenBank was also performed. Geographic areas were mapped onto the combined chloroplast and nuclear ribosomal tree, as well as onto the broader tree, using the parsimony criterion to determine the dispersal patterns. Phylogenetic analyses revealed that Platydesma is nested within Melicope and is sister to the Hawaiian members of Melicope. The Hawaiian Melicope + Platydesma lineage was a result of a single colonization event, probably from the Austral region. Finally, Marquesan Melicope descended from at least one, and possibly two, colonization events from the Hawaiian Islands. These data demonstrate a shifting paradigm of Pacific oceanic island biogeography, in which the patterns of long-distance dispersal and colonization in the Pacific are more dynamic than previously thought, and suggest that the Hawaiian Islands may act as a stepping stone for dispersal throughout the Pacific. C1 [Harbaugh, Danica T.; Wagner, Warren L.; Zimmer, Elizabeth A.] Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, Washington, DC 20013 USA. [Allan, Gerard J.] No Arizona Univ, Dept Biol Sci Environm Genet & Genom Facil, Flagstaff, AZ 86011 USA. RP Harbaugh, DT (reprint author), Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, POB 37012,MRC 166, Washington, DC 20013 USA. EM harbaughd@si.edu RI Zimmer, Elizabeth/G-3890-2011 FU Smithsonian National Museum of Natural History; Department of Botany at the Smithsonian National Museum of Natural History FX The authors thank the editor David Bellwood, Harvey E. Ballard Jr and an anonymous referee for their comments and suggestions for improving the manuscript, and Tom Hartley and Jean-Yves Meyer who contributed plant material for this project. We also thank Andrew G. Medina Moreno, who assisted with the molecular work as a Minority Student Intern at the Smithsonian National Museum of Natural History, and the Department of Botany at the Smithsonian National Museum of Natural History for providing fellowship funding to D.H. NR 84 TC 40 Z9 41 U1 3 U2 13 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0305-0270 J9 J BIOGEOGR JI J. Biogeogr. PD FEB PY 2009 VL 36 IS 2 BP 230 EP 241 DI 10.1111/j.1365-2699.2008.02008.x PG 12 WC Ecology; Geography, Physical SC Environmental Sciences & Ecology; Physical Geography GA 395GA UT WOS:000262511400005 ER PT J AU Makkeasorn, A Chang, NB Li, JH AF Makkeasorn, Ammarin Chang, Ni-Bin Li, Jiahong TI Seasonal change detection of riparian zones with remote sensing images and genetic programming in a semi-arid watershed SO JOURNAL OF ENVIRONMENTAL MANAGEMENT LA English DT Article DE Riparian classification; Soil moisture; RADARSAT-1; LANDSAT; Vegetation index; Ecohydrology; Genetic programming ID GEOGRAPHIC INFORMATION-SYSTEMS; SOIL-MOISTURE; VEGETATION INDEX; NEURAL-NETWORKS; BUFFER STRIPS; NOAA AVHRR; SAR; CLASSIFICATION; CALIBRATION; DELINEATION AB Riparian zones are deemed significant due to their interception capability of non-point Source impacts and the maintenance of ecosystem integrity region wide. To improve classification and change detection of riparian buffers, this paper developed an evolutionary computational, supervised classification method - the Riparian Classification Algorithm (RICAL) - to conduct the seasonal change detection of riparian zones in a vast semi-arid watershed, South Texas. RICAL uniquely demonstrates an integrative effort to incorporate both vegetation indices and soil moisture images derived from LANDSAT 5 TM and RADARSAT-1 satellite images, respectively. First, an estimation of soil moisture based on RADARSAT-1 Synthetic Aperture Radar (SAR) images was conducted via the first-stage genetic programming (GP) practice. Second, for the statistical analyses and image classification, eight vegetation indices were prepared based on reflectance factors that were calculated as the response of the instrument on LANDSAT. These spectral vegetation indices were then independently used for discriminate analysis along With Soil moisture images to classify the riparian zones via the second-stage GP practice. The practical implementation was assessed by a case study in the Choice Canyon Reservoir Watershed (CCRW), South Texas, which is mostly agricultural and range land in a semi-arid coastal environment. To enhance the application potential, a combination of Iterative Self-Organizing Data Analysis Techniques (ISODATA) and maximum likelihood supervised classification was also performed for spectral discrimination and classification of riparian varieties comparatively. Research findings show that the RICAL algorithm may yield around 90% accuracy based on the unseen ground data. But using different vegetation indices Would not significantly improve the final quality of the spectral discrimination and classification. Such practices may lead to the formulation of more effective management strategies for the handling of non-point source Pollution, bird habitat monitoring, and grazing and live stock management in the future. Published by Elsevier Ltd. C1 [Makkeasorn, Ammarin; Chang, Ni-Bin] Univ Cent Florida, Dept Civil & Environm Engn, Orlando, FL 32816 USA. [Li, Jiahong] Smithsonian Environm Res Ctr, Kennedy Space Ctr, FL 32829 USA. RP Chang, NB (reprint author), Univ Cent Florida, Dept Civil & Environm Engn, 4000 Cent Florida Blvd, Orlando, FL 32816 USA. EM nchang@mail.ucf.edu NR 57 TC 21 Z9 25 U1 0 U2 19 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0301-4797 EI 1095-8630 J9 J ENVIRON MANAGE JI J. Environ. Manage. PD FEB PY 2009 VL 90 IS 2 BP 1069 EP 1080 DI 10.1016/j.jenvman.2008.04.004 PG 12 WC Environmental Sciences SC Environmental Sciences & Ecology GA 386PQ UT WOS:000261895500043 PM 18524456 ER PT J AU Missa, O Basset, Y Alonso, A Miller, SE Curletti, G De Meyer, M Eardley, C Mansell, MW Wagner, T AF Missa, Olivier Basset, Yves Alonso, Alfonso Miller, Scott E. Curletti, Gianfranco De Meyer, Marc Eardley, Connal Mansell, Mervyn W. Wagner, Thomas TI Monitoring arthropods in a tropical landscape: relative effects of sampling methods and habitat types on trap catches SO JOURNAL OF INSECT CONSERVATION LA English DT Article DE Africa; Biological monitoring; Gabon; Indicator value index; Insect trap ID RAIN-FOREST; INSECT HERBIVORES; PITFALL TRAPS; BIODIVERSITY; CONSERVATION; ASSEMBLAGES; COMMUNITIES; BUTTERFLIES; GUIDELINES; DIVERSITY AB To discuss the challenge of monitoring multi-species responses of tropical arthropods to disturbance, we considered a large dataset (4 x 10(5) individuals; 1,682 morphospecies representing 22 focal taxa) based on the work of parataxonomists to examine the effects of anthropogenic disturbance on arthropods at Gamba, Gabon. Replication included three sites in each of four different stages of forest succession and land use after logging, surveyed during a whole year with four sampling methods: pitfall, Malaise, flight-interception and yellow pan traps. We compared the suitability of each sampling method for biological monitoring and evaluated statistically their reliability for 118 arthropod families. Our results suggest that a range of sampling methods yields more diverse material than any single method operated with high replication. Multivariate analyses indicated that morphospecies composition in trap catches was more strongly influenced by habitat type than by sampling methods. This implies that for multi-species monitoring, differences in trap efficiency between habitats may be neglected, as far as habitat types remain well contrasted. We conclude that for the purpose of monitoring large arthropod assemblages in the long-term, a protocol based on operating a set of different and non-disruptive traps appears superior in design than summing a series of taxa-specific protocols. C1 [Basset, Yves] Smithsonian Trop Res Inst, Panama City, Panama. [Missa, Olivier] Univ York, Dept Biol, York YO10 5YW, N Yorkshire, England. [Alonso, Alfonso] Smithsonian Inst, Monitoring & Assessment Biodivers Program, Washington, DC 20560 USA. [Miller, Scott E.] Smithsonian Inst, Washington, DC 20013 USA. [Curletti, Gianfranco] Museo Civ Storia Nat, I-10022 Carmagnola, TO, Italy. [De Meyer, Marc] Royal Museum Cent Africa, B-3080 Tervuren, Belgium. [Eardley, Connal] Plant Protect Res Inst, ZA-0121 Pretoria, South Africa. [Mansell, Mervyn W.] Univ Pretoria, Dept Zool & Entomol, ZA-0002 Pretoria, South Africa. [Wagner, Thomas] Univ Koblenz Landau, Inst Integrierte Nat Wissensch Biol, D-56070 Koblenz, Germany. RP Basset, Y (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Panama City, Panama. EM bassety@si.edu RI Missa, Olivier/G-2687-2012; Basset, Yves/B-6642-2014; OI Missa, Olivier/0000-0002-4330-5192; Miller, Scott/0000-0002-4138-1378 FU Smithsonian Institution; National Zoological Park; Shell Foundation and Shell Gabon FX F. Dallmeier, J. Comiskey, M. Lee, J. Mavoungou and J. B. Mikissa helped to implement the project. Parataxonomists B. Amvame, N. Koumba, S. Mboumba Ditona, G. Moussavou, P. Ngoma, J. Syssou, L. Tchignoumba and E. Tobi collected, processed, sorted and data-based most of the insect material with great competence. J. Raymakers and S. Mboumba Ditona provided the vegetational data. M. Foldvari, S. W. Lingafelter and F. C. Thompson helped with pipunculid, cerambycid and syrphid identifications, respectively. V. Novotny commented on an early draft of the manuscript. The project was funded by the Smithsonian Institution, National Zoological Park, Conservation and Research Center/MAB Program through grants from the Shell Foundation and Shell Gabon. This is contribution No. 84 of the Gabon Biodiversity Program. NR 60 TC 26 Z9 27 U1 2 U2 30 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 1366-638X J9 J INSECT CONSERV JI J. Insect Conserv. PD FEB PY 2009 VL 13 IS 1 BP 103 EP 118 DI 10.1007/s10841-007-9130-5 PG 16 WC Biodiversity Conservation; Entomology SC Biodiversity & Conservation; Entomology GA 389WK UT WOS:000262125000011 ER PT J AU Mendoza-Franco, EF Reina, RG Torchin, ME AF Mendoza-Franco, Edgar F. Reina, Ruth G. Torchin, Mark E. TI DACTYLOGYRIDS (MONOGENOIDEA) PARASITIZING THE GILLS OF ASTYANAX SPP. (CHARACIDAE) FROM PANAMA AND SOUTHEAST MEXICO, A NEW SPECIES OF DIAPHOROCLEIDUS AND A PROPOSAL FOR CHARACITHECIUM N. GEN. SO JOURNAL OF PARASITOLOGY LA English DT Article ID FRESH-WATER FISHES; HELMINTH-PARASITES; ANCYROCEPHALINAE; TELEOSTEI; BASIN AB Diaphorocleidus orthodusus n. sp. and Diaphorocleidus kabatai (Molnar. Hanek and Fernando, 1974) Jogunoori, Kritsky, and Venkatanarasaiah, 2004 are detailed from Astyanax orthodus and Astyanax aeneus, respectively. Palombitrema heteroancistrium (Price and Bussing, 1968) is described from specimens collected from A. aeneus, and Urocleidoides strombicirrus (Price and Bussing, 1967) is reported for the first time from A. aeneus and Astyanax fasciatus in Panama. Characithecium costaricensis (Price and Bussing, 1967) n. comb. is detailed based on specimens from A. aeneus. Characithecium costaricensis is characterized by having overlapping gonads, a medioventral vaginal aperture, a copulatory complex consisting of single counterclockwise coil of the copulatory organ that is articulated to the accessory piece, and a haptor having 2 pairs of anchors, dorsal and ventral bars, and 14 hooks. Measurements of body size varied substantially among individual worms, both within and across different host species and locations. However, the morphological differences were insufficient to separate species of Characithecium. This result suggests limited parasite speciation across sympatric species of Astyanax in Mexico and Panama. C1 [Mendoza-Franco, Edgar F.; Reina, Ruth G.; Torchin, Mark E.] Smithsonian Trop Res Inst, Naos Isl Labs, Panama City, Panama. RP Mendoza-Franco, EF (reprint author), BC ASCR, Inst Parasitol, Branisovska 31, Ceske Budejovice 37005, Czech Republic. EM oberon.men@gmail.com FU Smithsonian Tropical Research through a postdoctoral fellowship to EFMF FX We thank C. Schloeder, A. Terrero, and C. Vega from Panama and G. Arjona-Torres and F. Puc-Itza from the Center for Investigation and Advanced Studies, National Polytechnic Institute (CINVESTAV-IPN), Merida, Mexico, for their field assistance during the collection of fish hosts. We also thank 2 anonymous reviewers for their valuable comments and suggestions on the manuscript. Funding was provided by Smithsonian Tropical Research institute through a postdoctoral fellowship to EFMF NR 20 TC 11 Z9 12 U1 0 U2 5 PU AMER SOC PARASITOLOGISTS PI LAWRENCE PA 810 EAST 10TH STREET, LAWRENCE, KS 66044 USA SN 0022-3395 J9 J PARASITOL JI J. Parasitol. PD FEB PY 2009 VL 95 IS 1 BP 46 EP 55 DI 10.1645/GE-1592.1 PG 10 WC Parasitology SC Parasitology GA 414RO UT WOS:000263883100008 PM 19245277 ER PT J AU Wysor, B Freshwater, D Fredericq, S Norris, J AF Wysor, B. Freshwater, D. Fredericq, S. Norris, J. TI A PRELIMINARY ASSESSMENT OF MACROALGAL DIVERSITY IN BOCAS DEL TORO, CARIBBEAN PANAMA SO JOURNAL OF PHYCOLOGY LA English DT Meeting Abstract C1 [Wysor, B.] Roger Williams Univ, Dept Biol Marine Biol & Environm Sci, Bristol, RI 02809 USA. [Freshwater, D.] Univ N Carolina, Ctr Marine Sci, Wilmington, NC 28401 USA. [Fredericq, S.] Univ Louisiana Lafayette, Dept Biol, Lafayette, LA 70504 USA. [Norris, J.] Natl Museum Nat Hist, Dept Bot, Smithsonian Inst, Washington, DC 20560 USA. NR 0 TC 1 Z9 1 U1 1 U2 3 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0022-3646 J9 J PHYCOL JI J. Phycol. PD FEB PY 2009 VL 45 BP 30 EP 30 PG 1 WC Plant Sciences; Marine & Freshwater Biology SC Plant Sciences; Marine & Freshwater Biology GA 415BW UT WOS:000263910300098 ER PT J AU Young, RG Adey, WH Muller, KM AF Young, R. G. Adey, W. H. Mueller, K. M. TI FUCUS (HETROKONTOPHYTA; PHAEOPHYTA) BIOGEOGRAPHY ACROSS NORTH AMERICAN SHORES SO JOURNAL OF PHYCOLOGY LA English DT Meeting Abstract C1 [Young, R. G.; Mueller, K. M.] Univ Waterloo, Waterloo, ON N2L 3G1, Canada. [Adey, W. H.] Smithsonian Inst, Marine Syst Lab, Washington, DC 20560 USA. RI Adey, Walter/G-2858-2011 NR 0 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0022-3646 J9 J PHYCOL JI J. Phycol. PD FEB PY 2009 VL 45 BP 31 EP 31 PG 1 WC Plant Sciences; Marine & Freshwater Biology SC Plant Sciences; Marine & Freshwater Biology GA 415BW UT WOS:000263910300100 ER PT J AU Ramos, R Cipriani, R Guzman, HM Garcia, E AF Ramos, Ruth Cipriani, Roberto Guzman, Hector M. Garcia, Elia TI Chronology of mercury enrichment factors in reef corals from western Venezuela SO MARINE POLLUTION BULLETIN LA English DT Article DE Reef corals; Sclerochronology; Metal pollution; Enrichment factors; Mercury; Petrochemical industry ID HEAVY-METALS; ATMOSPHERIC MERCURY; COASTAL SEDIMENTS; HISTORICAL TRENDS; TRACE-ELEMENTS; RECORD; DEPOSITION; POLLUTION; ESTUARY; LEAD AB Mining and deforestation in the early 20th century, the development of petrochemical industries during the 1950s, and the constant weathering of natural deposits of cinabrium (HgS) have made Golfo Triste, Venezuela, a region impacted by mercury (Hg). We studied the chronology of Hg in coral skeletons of Siderastrea siderea (1 colony, 1900-1996) and Montastraea faveolata (2 colonies, 1930-1999) from Parque Nacional San Esteban. Maximum values of Hg/Ca ratios and standard deviations of Hg enrichment factors occurred in the 1940s, 1960s, and 1980s, and matched maxima of decadal rainfall. Values from the 1950s and 1970s matched periods of abundant but constantly decreasing rainfall and hence were best explained by the combination of runoff and the sudden bioavailability of Hg in the region. This sudden availability likely was associated with activities of the chlorine-caustic soda and fertilizer plants of Moron petrochemical complex, industries that started producing large amounts of Hg in 1958. (C) 2008 Elsevier Ltd. All rights reserved. C1 [Ramos, Ruth; Garcia, Elia] Univ Simon Bolivar, CETOXMAR, Caracas 1080A, Venezuela. [Cipriani, Roberto] Univ Simon Bolivar, Secc Ecol & Evoluc, Dept Estudios Ambientales, Caracas 1080A, Venezuela. [Guzman, Hector M.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Garcia, Elia] Univ Simon Bolivar, Dept Biol Organismos, Caracas 1080A, Venezuela. RP Ramos, R (reprint author), Univ Simon Bolivar, CETOXMAR, AP 89000, Caracas 1080A, Venezuela. EM ruthr@usb.ve FU FONACIT [2001000599]; Smithsonian Tropical Research Institute. FX We would like to thank C. Bastidas, E. Brunneti, A. Croquer for their logistical support while sampling at Golfo Triste; we are also grateful to A. Oliveros for laboratory assistance and to Laboratorio de Desechos Toxicos (USB) for metal analyses. P. Zanders made helpful comments to improve this manuscript. This work was sponsored by FONACIT (Project G-2001000599) and the Smithsonian Tropical Research Institute. NR 51 TC 10 Z9 11 U1 1 U2 13 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0025-326X EI 1879-3363 J9 MAR POLLUT BULL JI Mar. Pollut. Bull. PD FEB PY 2009 VL 58 IS 2 BP 222 EP 229 DI 10.1016/j.marpolbul.2008.09.023 PG 8 WC Environmental Sciences; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 422IQ UT WOS:000264421400018 PM 19012938 ER PT J AU Mathews, LM Anker, A AF Mathews, Lauren M. Anker, Arthur TI Molecular phylogeny reveals extensive ancient and ongoing radiations in a snapping shrimp species complex (Crustacea, Alpheidae, Alpheus armillatus) SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article DE Species complex; Snapping shrimp; Alpheidae; Alpheus armillatus; Cryptic radiation; Western Atlantic; Eastern Pacific; Transisthmian ID POPULATION GENETIC-STRUCTURE; CRYPTIC SPECIATION; MARINE POPULATIONS; MITOCHONDRIAL-DNA; BRACHIDONTES-EXUSTUS; GEOGRAPHIC SCALES; LARVAL DISPERSAL; SCORCHED MUSSEL; RAPID RADIATION; GENUS ALPHEUS AB Tropical marine habitats often harbor high biodiversity, including many cryptic taxa. Though the prevalence of cryptic marine taxa is well known, the evolutionary histories of these groups remain poorly understood. The snapping shrimp genus Alpheus is a good model for such investigations, as cryptic species complexes are very common, indicating widespread genetic diversification with little or no morphological change. Here, we present an extensive phylogeographic investigation of the diversified amphi-American Alpheus armillatus species complex, with geographic sampling in the Caribbean Sea, Gulf of Mexico, Florida, Brazil, and the tropical Eastern Pacific. Sequence data from two mitochondrial genes (16SrRNA and cytochrome oxidase 1) and one nuclear gene (myosin heavy chain) provide strong evidence for division of the species complex into six major clades, with extensive substructure within each clade. Our total data set suggests that the A. armillatus complex includes no less than 19 putative divergent lineages, 11 in the Western Atlantic and 8 in the Eastern Pacific. Estimates of divergence times from Bayesiananalyses indicate that the radiation of the species complex began similar to 10 MYA with the most recent divergences among subclades dating to within the last 3 MY. Furthermore, individuals from the six major clades had broadly overlapping geographic distributions, which may reflect secondary contact among previously isolated lineages, and have apparently undergone several changes in superficial coloration, which is typically the most pronounced phenotypic character distinguishing lineages. In addition, the extensive substructure within clades indicates a great deal of molecular diversification following the rise of the Isthmus of Panama. In summary, this investigation reflects substantial biodiversity concealed by morphological similarity, and suggests that both ancient and ongoing divergences have contributed to the generation of this biodiversity. It also underlines the necessity to work with the most complete data set possible, which includes comprehensive and wide-ranging sampling of taxa. (C) 2008 Elsevier Inc. All rights reserved. C1 [Mathews, Lauren M.] Worcester Polytech Inst, Dept Biol, Worcester, MA 01609 USA. [Anker, Arthur] Smithsonian Trop Res Inst, Naos Unit 0948, APO, AA 34002 USA. RP Mathews, LM (reprint author), Worcester Polytech Inst, Dept Biol, 100 Inst Rd, Worcester, MA 01609 USA. EM lmathews@wpi.edu FU WPI Faculty Advancement in Research; Nancy Knowlton (USNM/STRI) FX We are grateful to the staffs of the Discovery Bay Marine Laboratory, Tropical Research Laboratory, and the Bermuda Biological Station for Research for logistic support. Additionally, we thank the Government of Bermuda (Permit No. SP050601) and to the National Environment and Planning Agency of Jamaica, and the Autoridad Nacional del Ambiente of Panama for granting collection and exportation permits. This research was funded by a WPI Faculty Advancement in Research grant to L.M., and by a postdoctoral fellowship from Nancy Knowlton (USNM/STRI) to A.A. Tim Page (Griffith University, Brisbane) and a second anonymous reviewer made a number of valuable comments considerably improving the overall quality of the manuscript. A.A. thanks Tim Coles and Sammy De Grave for inviting him to participate in the Operation Wallacea invertebrate survey in Utila, Honduras. We also thank Paulo Young (late of MNRJ) and Christoph Schubart (University of Regensburg) for collection of some specimens. NR 95 TC 19 Z9 22 U1 0 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 2009 VL 50 IS 2 BP 268 EP 281 DI 10.1016/j.ympev.2008.10.026 PG 14 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 404MU UT WOS:000263158100005 PM 19041948 ER PT J AU Irwin, J Aigrain, S Bouvier, J Hebb, L Hodgkin, S Irwin, M Moraux, E AF Irwin, Jonathan Aigrain, Suzanne Bouvier, Jerome Hebb, Leslie Hodgkin, Simon Irwin, Mike Moraux, Estelle TI The Monitor project: rotation periods of low-mass stars in M50 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE techniques: photometric; surveys; stars: pre-main-sequence; stars: rotation; open clusters and associations: individual: M50 ID ANGULAR-MOMENTUM EVOLUTION; OPEN CLUSTER NGC-2516; SOLAR-TYPE STARS; PHOTOMETRIC LIGHT CURVES; YOUNG OPEN CLUSTERS; K-DWARFS; LITHIUM DEPLETION; ALPHA-PERSEI; CHI-PERSEI; PLEIADES AB We report on the results of a time-series photometric survey of M50 (NGC 2323), a similar to 130 Myr open cluster, carried out using the Cerro Tololo Inter-American Observatory (CTIO) 4-m Blanco telescope and Mosaic-II detector as part of the Monitor project. Rotation periods were derived for 812 candidate cluster members over the mass range 0.2 less than or similar to M/M circle dot less than or similar to 1.1. The rotation period distributions show a clear mass-dependent morphology, statistically indistinguishable from those in NGC 2516 and M35 taken from the literature. Due to the availability of data from three observing runs separated by similar to 10 and 1 month time-scales, we are able to demonstrate clear evidence for evolution of the photometric amplitudes, and hence spot patterns, over the 10 month gap. We are not able to constrain the time-scales for these effects in detail due to limitations imposed by the large gaps in our sampling, which also prevent the use of the phase information. C1 [Irwin, Jonathan; Hodgkin, Simon; Irwin, Mike] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Irwin, Jonathan] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Aigrain, Suzanne] Univ Exeter, Sch Phys, Astrophys Grp, Exeter EX4 4QL, Devon, England. [Bouvier, Jerome; Moraux, Estelle] Observ Grenoble, Astrophys Lab, F-38041 Grenoble 9, France. [Hebb, Leslie] Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. RP Irwin, J (reprint author), Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. EM jmi@ast.cam.ac.uk NR 54 TC 37 Z9 37 U1 0 U2 1 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB 1 PY 2009 VL 392 IS 4 BP 1456 EP 1466 DI 10.1111/j.1365-2966.2008.14158.x PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 394VK UT WOS:000262479300013 ER PT J AU Joshi, YC Pollacco, D Cameron, AC Skillen, I Simpson, E Steele, I Street, RA Stempels, HC Christian, DJ Hebb, L Bouchy, F Gibson, NP Hebrard, G Keenan, FP Loeillet, B Meaburn, J Moutou, C Smalley, B Todd, I West, RG Anderson, DR Bentley, S Enoch, B Haswell, CA Hellier, C Horne, K Irwin, J Lister, TA McDonald, I Maxted, P Mayor, M Norton, AJ Parley, N Perrier, C Pont, F Queloz, D Ryans, R Smith, AMS Udry, S Wheatley, PJ Wilson, DM AF Joshi, Y. C. Pollacco, D. Cameron, A. Collier Skillen, I. Simpson, E. Steele, I. Street, R. A. Stempels, H. C. Christian, D. J. Hebb, L. Bouchy, F. Gibson, N. P. Hebrard, G. Keenan, F. P. Loeillet, B. Meaburn, J. Moutou, C. Smalley, B. Todd, I. West, R. G. Anderson, D. R. Bentley, S. Enoch, B. Haswell, C. A. Hellier, C. Horne, K. Irwin, J. Lister, T. A. McDonald, I. Maxted, P. Mayor, M. Norton, A. J. Parley, N. Perrier, C. Pont, F. Queloz, D. Ryans, R. Smith, A. M. S. Udry, S. Wheatley, P. J. Wilson, D. M. TI WASP-14b: 7.3 M-J transiting planet in an eccentric orbit SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE techniques: photometric; techniques: radial velocities; stars: individual: GSC 01482-00882 ID EXTRA-SOLAR PLANETS; SPIN-ORBIT; HD 147506B; MASSIVE PLANET; STARS; EVOLUTION; PROJECT; LITHIUM; CANDIDATES; PARAMETERS AB We report the discovery of a 7.3 M-J exoplanet WASP-14b, one of the most massive transiting exoplanets observed to date. The planet orbits the 10th-magnitude F5V star USNO-B1 11118-0262485 with a period of 2.243 752 d and orbital eccentricity e = 0.09. A simultaneous fit of the transit light curve and radial velocity measurements yields a planetary mass of 7.3 +/- 0.5 M-J and a radius of 1.28 +/- 0.08 R-J. This leads to a mean density of about 4.6 g cm(-3) making it the densest transiting exoplanets yet found at an orbital period less than 3 d. We estimate this system to be at a distance of 160 +/- 20 pc. Spectral analysis of the host star reveals a temperature of 6475 +/- 100 K, log g = 4.07 cm s(-2) and v sin i = 4.9 +/- 1.0 km s(-1), and also a high lithium abundance, log N(Li) = 2.84 +/- 0.05. The stellar density, effective temperature and rotation rate suggest an age for the system of about 0.5-1.0 Gyr. C1 [Joshi, Y. C.; Pollacco, D.; Simpson, E.; Christian, D. J.; Gibson, N. P.; Keenan, F. P.; Todd, I.; Ryans, R.] Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland. [Cameron, A. Collier; Stempels, H. C.; Hebb, L.; Horne, K.; Smith, A. M. S.] Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. [Skillen, I.] Isaac Newton Grp Telescopes, E-38700 Tenerife, Spain. [Steele, I.] Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England. [Street, R. A.; Lister, T. A.] Las Cumbres Observ, Santa Barbara, CA 93117 USA. [Bouchy, F.; Hebrard, G.; Loeillet, B.] Univ Paris 06, CNRS, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France. [Loeillet, B.; Moutou, C.] CNRS, Lab Astrophys Marseille, UMR 6110, F-13376 Marseille 12, France. [Smalley, B.; Anderson, D. R.; Bentley, S.; Hellier, C.; McDonald, I.; Maxted, P.; Wilson, D. M.] Keele Univ, Astrophys Grp, Keele ST5 5BG, Staffs, England. [West, R. G.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Enoch, B.; Haswell, C. A.; Norton, A. J.; Parley, N.] Open Univ, Dept Phys & Astron, Milton Keynes MK7 6AA, Bucks, England. [Irwin, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Mayor, M.; Queloz, D.; Udry, S.] Univ Geneva, Observ Geneva, CH-1290 Sauverny, Switzerland. [Perrier, C.] Univ Grenoble 1, Observ Grenoble, Lab Astrophys, F-38041 Grenoble 9, France. [Pont, F.] Univ Bern, Inst Phys, CH-3012 Bern, Switzerland. [Wheatley, P. J.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Meaburn, J.] Univ Manchester, Dept Phys & Astron, Macclesfield SK11 9DL, Cheshire, England. RP Joshi, YC (reprint author), Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Univ Rd, Belfast BT7 1NN, Antrim, North Ireland. EM y.joshi@qub.ac.uk RI Smith, Alexis/J-4757-2012; OI Norton, Andrew/0000-0001-7619-8269; Gibson, Neale/0000-0002-9308-2353 FU Queen's University Belfast; Open University, Isaac Newton Group La Palma and Instituto de Astrof 'isica de Canarias. SuperWASP Cameras; Consortium Universities; UK's Science and Technology Facilities Council; SOPHIE; Optical Infrared Coordination Network FX The SuperWASP Consortium consists of astronomers primarily from the Queen's University Belfast, St Andrews, Keele, Leicester, The Open University, Isaac Newton Group La Palma and Instituto de Astrof 'isica de Canarias. SuperWASP Cameras were constructed and operated with funds made available from Consortium Universities and the UK's Science and Technology Facilities Council. SOPHIE observations have been funded by the Optical Infrared Coordination Network. Data from the Liverpool and NOT telescopes were obtained under the auspices of the International Time of the Canary Islands. We extend our thanks to the staff of the ING and OHP for their continued support of SuperWASP- N and SOPHIE instruments. FPK is grateful to AWE Aldermaston for the award of a William Penney Fellowship. NR 39 TC 68 Z9 68 U1 0 U2 1 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB 1 PY 2009 VL 392 IS 4 BP 1532 EP 1538 DI 10.1111/j.1365-2966.2008.14178.x PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 394VK UT WOS:000262479300018 ER PT J AU Christian, DJ Gibson, NP Simpson, EK Street, RA Skillen, I Pollacco, D Collier Cameron, A Joshi, YC Keenan, FP Stempels, HC Haswell, CA Horne, K Anderson, DR Bentley, S Bouchy, F Clarkson, WI Enoch, B Hebb, L Hebrard, G Hellier, C Irwin, J Kane, SR Lister, TA Loeillet, B Maxted, P Mayor, M McDonald, I Moutou, C Norton, AJ Parley, N Pont, F Queloz, D Ryans, R Smalley, B Smith, AMS Todd, I Udry, S West, RG Wheatley, PJ Wilson, DM AF Christian, D. J. Gibson, N. P. Simpson, E. K. Street, R. A. Skillen, I. Pollacco, D. Collier Cameron, A. Joshi, Y. C. Keenan, F. P. Stempels, H. C. Haswell, C. A. Horne, K. Anderson, D. R. Bentley, S. Bouchy, F. Clarkson, W. I. Enoch, B. Hebb, L. Hebrard, G. Hellier, C. Irwin, J. Kane, S. R. Lister, T. A. Loeillet, B. Maxted, P. Mayor, M. McDonald, I. Moutou, C. Norton, A. J. Parley, N. Pont, F. Queloz, D. Ryans, R. Smalley, B. Smith, A. M. S. Todd, I. Udry, S. West, R. G. Wheatley, P. J. Wilson, D. M. TI WASP-10b: a 3M(J), gas-giant planet transiting a late-type K star SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: data analysis; techniques: photometric; techniques: radial velocities; stars: planetary systems ID TIDAL EVOLUTION; STELLAR; MASS; PHOTOMETRY; CANDIDATES; EXOPLANETS; SUPERWASP; SYSTEMS AB We report the discovery of WASP-10b, a new transiting extrasolar planet (ESP) discovered by the Wide Angle Search for Planets ( WASP) Consortium and confirmed using Nordic Optical Telescope FIbre-fed Echelle Spectrograph and SOPHIE radial velocity data. A 3.09-d period, 29 mmag transit depth and 2.36 h duration are derived for WASP-10b using WASP and high-precision photometric observations. Simultaneous fitting to the photometric and radial velocity data using a Markov Chain Monte Carlo procedure leads to a planet radius of 1.28R(J), a mass of 2.96M(J) and eccentricity of approximate to 0.06. WASP-10b is one of the more massive transiting ESPs, and we compare its characteristics to the current sample of transiting ESP, where there is currently little information for masses greater than approximate to 2M(J) and non-zero eccentricities. WASP-10's host star, GSC 2752-00114 (USNO-B1.0 1214-0586164) is among the fainter stars in the WASP sample, with V = 12.7 and a spectral type of K5. This result shows promise for future late-type dwarf star surveys. C1 [Christian, D. J.; Gibson, N. P.; Simpson, E. K.; Pollacco, D.; Joshi, Y. C.; Keenan, F. P.; Ryans, R.; Todd, I.] Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland. [Christian, D. J.] Calif State Univ Northridge, Dept Phys & Astron, Northridge, CA 91330 USA. [Street, R. A.; Lister, T. A.] Las Cumbres Observ, Santa Barbara, CA 93117 USA. [Skillen, I.] Isaac Newton Grp Telescopes, E-38700 Tenerife, Spain. [Collier Cameron, A.; Stempels, H. C.; Horne, K.; Hebb, L.; Lister, T. A.; Smith, A. M. S.] Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. [Haswell, C. A.; Clarkson, W. I.; Enoch, B.; Norton, A. J.; Parley, N.] Open Univ, Dept Phys & Astron, Milton Keynes MK7 6AA, Bucks, England. [Anderson, D. R.; Bentley, S.; Hellier, C.; Lister, T. A.; Maxted, P.; McDonald, I.; Smalley, B.; Wilson, D. M.] Keele Univ, Astrophys Grp, Keele ST5 5BG, Staffs, England. [Bouchy, F.; Hebrard, G.] Univ Paris 06, CNRS, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France. [Bouchy, F.] Observ Haute Provence, F-04870 St Michel lObservatoire, France. [Clarkson, W. I.] STScI, Baltimore, MD 21218 USA. [Irwin, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kane, S. R.] CALTECH, Michelson Sci Ctr, Pasadena, CA 91125 USA. [Loeillet, B.; Moutou, C.] Lab Astrophys Marseille, F-13376 Marseille 12, France. [Mayor, M.; Pont, F.; Queloz, D.; Udry, S.] Univ Geneva, Observ Geneva, CH-1290 Sauverny, Switzerland. [Pont, F.] Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England. [West, R. G.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Wheatley, P. J.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. RP Christian, DJ (reprint author), Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Univ Rd, Belfast BT7 1NN, Antrim, North Ireland. EM d.christian@qub.ac.uk RI Smith, Alexis/J-4757-2012; Kane, Stephen/B-4798-2013; OI Norton, Andrew/0000-0001-7619-8269; Gibson, Neale/0000-0002-9308-2353 NR 30 TC 54 Z9 54 U1 0 U2 3 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB 1 PY 2009 VL 392 IS 4 BP 1585 EP 1590 DI 10.1111/j.1365-2966.2008.14164.x PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 394VK UT WOS:000262479300021 ER PT J AU Zasche, P Liakos, A Niarchos, P Wolf, M Manimanis, V Gazeas, K AF Zasche, P. Liakos, A. Niarchos, P. Wolf, M. Manimanis, V. Gazeas, K. TI Period changes in six contact binaries: WZ And, V803 Aql, DF Hya, PY Lyr, FZ Ori, and AH Tau SO NEW ASTRONOMY LA English DT Article DE Stars: binaries: eclipsing; Stars: individual: WZ And, V803 Aql, DF; Hya, PY Lyr, FZ Ori, AH Tau; Stars: fundamental parameters ID ECLIPSING BINARIES; CLOSE BINARIES; UMA SYSTEM; RS CVN; ALGOL; COMPONENTS; CURVES; HYDRAE; STARS AB Six contact binaries lacking a period analysis have been chosen to search for the presence of a third body. The O-C diagrams of these binaries were analyzed with the least-squares method by using all available times of minima. Ten new minima times, obtained from our observations, were included in the present research. The Light-Time Effect was adopted for the first time as the main cause for the detailed description of the long-term period changes. Third bodies were found with orbital periods from 49 up to 100 years, and eccentricities from 0.0 to 0.56 for the selected binaries. In one case (WZ And), a fourth-body LITE variation was also applied. The mass functions and the minimal masses of such bodies were also calculated and a possible angular separation and magnitude differences were discussed for a prospective interferometric discovery of these bodies. (C) 2008 Elsevier B.V. All rights reserved. C1 [Zasche, P.; Wolf, M.] Charles Univ Prague, Astron Inst, Fac Math & Phys, CZ-18000 Prague 8, Czech Republic. [Liakos, A.; Niarchos, P.; Manimanis, V.] Univ Athens, Dept Astrophys Astron & Mech, Fac Phys, Athens 11528, Greece. [Gazeas, K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Zasche, P (reprint author), Charles Univ Prague, Astron Inst, Fac Math & Phys, Holesovickach 2, CZ-18000 Prague 8, Czech Republic. EM zasche@sirrah.troja.mff.cuni.cz RI Liakos, Alexios/K-4452-2013 OI Liakos, Alexios/0000-0002-0490-1469 FU Czech-Greek project of collaboration [7-2006-5]; Ministry of Education, Youth and Sport of the Czech Republic; Czech Science Foundation [205/06/0217]; National and Kapodistrian University of Athens, Greece [70/3/8680] FX This investigation was supported for P.Z. and M.W. by the Czech-Greek project of collaboration No. 7-2006-5 Photometry and Spectroscopy of Binaries of Ministry of Education, Youth and Sport of the Czech Republic and by the Czech Science Foundation Grant No. 205/06/0217, and for A.L., P.N., V.M. and K.G. by the Special Account for Research Grants 70/3/8680 of the National and Kapodistrian University of Athens, Greece. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France, and of NASA's Astrophysics Data System Bibliographic Services. NR 47 TC 27 Z9 27 U1 1 U2 1 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 1384-1076 J9 NEW ASTRON JI New Astron. PD FEB PY 2009 VL 14 IS 2 BP 121 EP 128 DI 10.1016/j.newast.2008.06.002 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 374DL UT WOS:000261022700002 ER PT J AU Lehner, MJ Wen, CY Wang, JH Marshall, SL Schwamb, ME Zhang, ZW Bianco, FB Giammarco, J Porrata, R Alcock, C Axelrod, T Byun, YI Chen, WP Cook, KH Dave, R King, SK Lee, T Lin, HC Wang, SY Rice, JA De Pater, I AF Lehner, M. J. Wen, C.-Y. Wang, J.-H. Marshall, S. L. Schwamb, M. E. Zhang, Z.-W. Bianco, F. B. Giammarco, J. Porrata, R. Alcock, C. Axelrod, T. Byun, Y.-I. Chen, W. P. Cook, K. H. Dave, R. King, S.-K. Lee, T. Lin, H.-C. Wang, S.-Y. Rice, J. A. De Pater, I. TI The Taiwanese-American Occultation Survey: The Multi-Telescope Robotic Observatory SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID KUIPER-BELT OBJECTS; STELLAR OCCULTATIONS; OORT CLOUD; SIZE DISTRIBUTION; SOLAR-SYSTEM; BODIES; TAOS; DISCOVERY; ORBITS; SEARCH AB The Taiwanese-American Occultation Survey (TAOS) operates four fully automatic telescopes to search for occultations of stars by Kuiper Belt Objects. It is a versatile facility that is also useful for the study of initial optical GRB afterglows. This paper provides a detailed description of the TAOS multi-telescope system, control software, and high-speed imaging. C1 [Lehner, M. J.; Wen, C.-Y.; Wang, J.-H.; King, S.-K.; Lee, T.; Wang, S.-Y.] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. [Lehner, M. J.; Bianco, F. B.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Lehner, M. J.; Bianco, F. B.; Alcock, C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Wang, J.-H.; Zhang, Z.-W.; Chen, W. P.; Lin, H.-C.] Natl Cent Univ, Inst Astron, Jhongli 320, Taoyuan County, Taiwan. [Marshall, S. L.] Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA. [Marshall, S. L.; Cook, K. H.] Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94550 USA. [Schwamb, M. E.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Giammarco, J.] Eastern Univ, Dept Phys & Astron, St Davids, PA 19087 USA. [Porrata, R.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94270 USA. [Axelrod, T.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Byun, Y.-I.] Yonsei Univ, Dept Astron, Seoul 120749, South Korea. [Dave, R.] Harvard Univ, Initiat Innovat Comp, Cambridge, MA 02138 USA. [Rice, J. A.] Univ Calif Berkeley, Dept Stat, Berkeley, CA 94720 USA. [De Pater, I.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. RP Lehner, MJ (reprint author), Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 106, Taiwan. EM mlehner@asiaa.sinica.edu.tw RI Lee, Typhoon/N-8347-2013; OI Lehner, Matthew/0000-0003-4077-0985; Schwamb, Megan/0000-0003-4365-1455 NR 33 TC 27 Z9 27 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6280 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD FEB PY 2009 VL 121 IS 876 BP 138 EP 152 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 414WA UT WOS:000263894700006 ER PT J AU Olson, SL Hearty, PJ AF Olson, Storrs L. Hearty, Paul J. TI A sustained+21 m sea-level highstand during MIS 11 (400 ka): direct fossil and sedimentary evidence from Bermuda SO QUATERNARY SCIENCE REVIEWS LA English DT Article ID LATE QUATERNARY MEGATSUNAMI; ELEVATED MARINE DEPOSITS; MIDDLE PLEISTOCENE; LAST INTERGLACIATION; CANARY-ISLANDS; ANTARCTIC ICE; MEGA-HIGHSTAND; WARM FUTURE; HISTORY; RECORD AB A small, protected karstic feature exposed in a limestone quarry in Bermuda preserved abundant sedimentary and biogenic materials documenting a transgressive phase, still-stand, and regressive phase of a sea-level in excess of 21.3 m above present during Marine Isotope Stage (MIS) 11 (400 ka) as determined by U/Th dating and amino acid racemization. Cobbles and marine sediments deposited during the high-energy transgressive phase exhibit rim cements indicating a subsequent phreatic environment. This was succeeded stratigraphically by a still-stand deposition of fine calcareous lagoonal sediments containing bioclasts of red algae and benthic and planktonic foraminifera that was intensely burrowed by marine invertebrates, probably upogebiid shrimp, that could not be produced under any condition other than sustained marine submergence. Overlying this were pure carbonate beach sands of a low-energy regressive phase containing abundant remains of terrestrial and marine vertebrates and invertebrates. The considerable diversity of this fauna along with taphonomic evidence from seabird remains indicates deposition by high run-up waves over a minimum duration of months, if not years. The maximum duration has yet to be determined but probably did not exceed one or two thousand years. The most abundant snails in this fauna are two species indicative of brackish water and high-tide line showing that a Ghyben-Herzberg lens must have existed at > + 20 m. The nature of these sediments and fossil accumulation is incompatible with tsunami deposition and, given the absence of evidence for tectonic uplift of the Bermuda pedestal or platform, provide proof that sea-level during MIS 11 exceeded + 20 m, a fact that has widespread ramifications for geologists, biogeographers, and human demographics along the world's coastlines. (C) 2008 Elsevier Ltd. All rights reserved. C1 [Olson, Storrs L.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Div Birds, Washington, DC 20013 USA. [Hearty, Paul J.] Bald Head Isl Conservancy, Bald Head Isl, NC 28461 USA. [Hearty, Paul J.] Univ Wollongong, GeoQuEST Res Ctr, Wollongong, NSW 2522, Australia. RP Olson, SL (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Div Birds, POB 37012, Washington, DC 20013 USA. EM olsons@si.edu; hearty@bhic.org NR 73 TC 52 Z9 52 U1 0 U2 7 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0277-3791 J9 QUATERNARY SCI REV JI Quat. Sci. Rev. PD FEB PY 2009 VL 28 IS 3-4 BP 271 EP 285 DI 10.1016/j.quascirev.2008.11.001 PG 15 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA 416GJ UT WOS:000263993400008 ER PT J AU Clough, GW AF Clough, G. Wayne TI Thinking Ahead SO SMITHSONIAN LA English DT Editorial Material C1 Smithsonian Inst, Washington, DC 20560 USA. RP Clough, GW (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SMITHSONIAN ASSOC PI WASHINGTON PA 900 JEFFERSON DR, WASHINGTON, DC 20560 USA SN 0037-7333 J9 SMITHSONIAN JI Smithsonian PD FEB PY 2009 VL 39 IS 11 BP 28 EP 28 PG 1 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA 398UP UT WOS:000262757300011 ER PT J AU Filippov, B Golub, L Koutchmy, S AF Filippov, Boris Golub, Leon Koutchmy, Serge TI X-Ray Jet Dynamics in a Polar Coronal Hole Region SO SOLAR PHYSICS LA English DT Article DE Coronal holes; Jets; Magnetic fields, models; Magnetic reconnection, observational signatures ID EXTREME-ULTRAVIOLET JETS; H-ALPHA SURGES; MAGNETIC RECONNECTION; SOLAR SPICULES; CHROMOSPHERIC SPICULES; BRIGHT POINTS; HINODE; TELESCOPE; MECHANISM; MODELS AB New X-ray observations of the north polar region taken from the X-ray Telescope (XRT) of the Hinode spacecraft are used to analyze several time sequences showing small loop brightenings with a long ray above. We focus on the formation of the jet and discuss scenarios to explain the main features of the events: the relationship with the expected surface magnetism, the rapid and sudden radial motion, and possibly the heating, based on the assumption that the jet occurs above a null point of the coronal magnetic field. We conclude that 2-D reconnection models should be complemented in order to explain the observational details of these events and suggest that alternative scenarios may exist. C1 [Filippov, Boris] Russian Acad Sci, Pushkov Inst Terr Magnetism Ionosphere & Radio Wa, Troitsk 142190, Moscow Region, Russia. [Golub, Leon] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Filippov, Boris; Koutchmy, Serge] Inst Astrophys Paris, CNRS, F-75014 Paris, France. [Filippov, Boris; Koutchmy, Serge] Univ Paris 06, F-75014 Paris, France. RP Filippov, B (reprint author), Russian Acad Sci, Pushkov Inst Terr Magnetism Ionosphere & Radio Wa, Troitsk 142190, Moscow Region, Russia. EM bfilip@izmiran.troitsk.ru; golub@cfa.harvard.edu; koutchmy@iap.fr RI Filippov, Boris/G-2810-2014; OI Golub, Leon/0000-0001-9638-3082 FU Russian Foundation for Basic Research [06-02-16424]; NATO CRG [940291]; NASA [NNM07AA02C] FX This work was supported in part by the Russian Foundation for Basic Research ( grant 06-02-16424) and in part by the NATO CRG 940291. Hinode is a Japanese mission developed and launched by ISAS/JAXA, with NAOJ as partner and NASA, ESA and STFC (UK) as international partners. It is operated by these agencies in co-operation with ESA and NSC ( Norway). US members of the XRT team are supported by NASA contract NNM07AA02C to SAO. The work is partly completed thanks to exchange visits to the Paris Institut d'Astrophysique. NR 51 TC 44 Z9 44 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 J9 SOL PHYS JI Sol. Phys. PD FEB PY 2009 VL 254 IS 2 BP 259 EP 269 DI 10.1007/s11207-008-9305-6 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 413LG UT WOS:000263794000003 ER PT J AU Introini, GO Magalhaes, CA Fortunato, H Recco-Pimentel, SM AF Introini, G. O. Magalhaes, C. A. Fortunato, H. Recco-Pimentel, S. M. TI Comparison of the spermatozoan morphology of Isognomon bicolor and Isognomon alatus (Mollusca, Bivalvia, Isognomonidae) SO TISSUE & CELL LA English DT Article DE Bivalvia; Isognomonidae; Spermatozoa; Ultrastructure ID SPERM ULTRASTRUCTURE; SPERMATOGENESIS; GAMETOGENESIS; INVAGINATIONS; VENERIDAE; OYSTERS AB In this Study We used transmission and scanning electron microscopy to examine the spermatozoan Structure of Isognomon bicolor and Isognomon alatus. The spermatozoa of both species were of the primitive or ect-aquasperm type. The acrosomal morphologies were essentially similar but the top of the acrosomal vesicle in I. bicolor sperm had a slightly flattened edge whereas the apex of the acrosomal vesicle of. alatus sperm had a rounded outline. This difference Suggested that acrosomal morphology Could be an important character for taxonomic differentiation. In the present work, the results demonstrated that the gamete ultrastructure of the two distinct species I. alatus, from Panama, and I. bicolor, from the southeastern region of Brazil, were similar to the other studied species of the superfamily Pterioidea. (C) 2008 Elsevier Ltd. All rights reserved. C1 [Introini, G. O.; Recco-Pimentel, S. M.] Univ Estadual Campinas, Inst Biol, Dept Biol Celular, BR-13083863 Campinas, SP, Brazil. [Magalhaes, C. A.] Esplanada Minist Blcoc B, Minist Meio Ambiente, Secretaria Mudancas Climat & Qualidade Ambiental, Brasilia, DF, Brazil. [Fortunato, H.] Smithsonian Trop Res Inst, Balboa, Panama. RP Recco-Pimentel, SM (reprint author), Univ Estadual Campinas, Inst Biol, Dept Biol Celular, CP 6109, BR-13083863 Campinas, SP, Brazil. EM shirlei@unicamp.br NR 25 TC 8 Z9 9 U1 0 U2 11 PU CHURCHILL LIVINGSTONE PI EDINBURGH PA JOURNAL PRODUCTION DEPT, ROBERT STEVENSON HOUSE, 1-3 BAXTERS PLACE, LEITH WALK, EDINBURGH EH1 3AF, MIDLOTHIAN, SCOTLAND SN 0040-8166 J9 TISSUE CELL JI Tissue Cell PD FEB PY 2009 VL 41 IS 1 BP 67 EP 74 DI 10.1016/j.tice.2008.07.002 PG 8 WC Anatomy & Morphology; Cell Biology SC Anatomy & Morphology; Cell Biology GA 402LW UT WOS:000263016200007 PM 18790511 ER PT J AU Tsujimoto, M Takei, D Drake, JJ Ness, JU Kitamoto, S AF Tsujimoto, Masahiro Takei, Dai Drake, Jeremy J. Ness, Jan-Uwe Kitamoto, Shunji TI X-Ray Spectroscopy of the Classical Nova V458 Vulpeculae with Suzaku SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN LA English DT Article DE stars: individual (Nova Vulpeculae 2007 number 1, V458 Vulpeculae); stars: novae; X-rays: stars ID INTERSTELLAR-MEDIUM; BOARD SUZAKU; SUPERNOVA REMNANT; HERCULIS 1991; 2006 OUTBURST; RS-OPHIUCHI; EMISSION; NUCLEOSYNTHESIS; MODEL; SAGITTARII AB We conducted a target of opportunity X-ray observation of the classical nova V458 Vulpeculae 88 d after the explosion using the Suzaku satellite. With a similar to 20 ks exposure, the X-ray Imaging Spectrometer detected X-ray emission significantly harder than typical super-soft Source emission. The X-ray spectrum shows K alpha lines from N, Ne, Mg, Si, and S, and L-series emission from Fe in highly ionized states. The spectrum can be described by a single-temperature (similar to 0.64 keV) thin thermal plasma model in collisional equilibrium with a hydrogen-equivalent extinction column density of similar to 3 x 10(21) cm(-2), a flux of similar to 10(-12) erg s(-1) cm(-2), and a luminosity of similar to 6 x 10(34) erg s(-1) in the 0.3-3.0 keV band at an assumed distance of 13 kpc. We found a hint of an enhancement of N and deficiencies of O and Fe relative to other metals. The observed X-ray properties can be interpreted as the emission arising from shocks of ejecta from an ONe-type nova. C1 [Tsujimoto, Masahiro] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Tsujimoto, Masahiro] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan. [Takei, Dai; Kitamoto, Shunji] Rikkyo Univ, Dept Phys, Toshima Ku, Tokyo 1718501, Japan. [Drake, Jeremy J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Ness, Jan-Uwe] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. RP Tsujimoto, M (reprint author), Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA. EM tsujimoto@astro.isas.jaxa.jp RI XRAY, SUZAKU/A-1808-2009 NR 68 TC 7 Z9 7 U1 0 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0004-6264 EI 2053-051X J9 PUBL ASTRON SOC JPN JI Publ. Astron. Soc. Jpn. PD JAN 30 PY 2009 VL 61 SI 1 BP S69 EP S76 DI 10.1093/pasj/61.sp1.S69 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 422HK UT WOS:000264418100006 ER PT J AU Wang, Z Kerkines, ISK Morokuma, K Zhang, P AF Wang, Zhi Kerkines, Ioannis S. K. Morokuma, Keiji Zhang, Peng TI Analytical potential energy surfaces for N-3 low-lying doublet states SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article DE configuration interactions; nitrogen; potential energy surfaces; reaction kinetics theory ID N+N-2 EXCHANGE-REACTION; AB-INITIO; RATE COEFFICIENTS; ELECTRON-AFFINITIES; DIABATIC STATES; GROUND-STATE; N3; QUANTUM; NITROGEN; AZIDE AB Adiabatic potential energy surfaces (PESs) for five low lying doublet states (three (2)A(') states and two (2)A(') states) of N-3 are constructed based on 1504 single point calculations at the MRCISD(Q) level using aug-cc-pVTZ basis set. A new strategy is adopted to obtain the final PESs by combining global fits of individual adiabatic PESs and local simultaneous fits of two adiabatic PESs in several conical intersection regions with switching functions. These global fits employ basis functions that satisfy permutational invariance with respect to like nuclei and have rms errors around 2-3 kcal/mol. The special local two-state fits are performed at the cyclic, bent, and linear N-3 conical intersection regions to take account of intrinsic square root behavior of the potentials and to improve the quality of fitting. Stationary points as well as minima on the concial intersections and seams of crossing are located on these PESs and compared with ab initio results. The agreement is satisfactory in most cases. In addition to the construction of adiabatic PESs, diabatization is performed for the 1 (2)A(') and 2 (2)A(') states around their conical intersection at the N-3 bent region. These two diabatic PESs and the diabatic coupling potential have been constructed and reported. C1 [Wang, Zhi; Kerkines, Ioannis S. K.; Morokuma, Keiji] Emory Univ, Dept Chem, Atlanta, GA 30322 USA. [Wang, Zhi; Kerkines, Ioannis S. K.; Morokuma, Keiji] Emory Univ, Cherry Logan Emerson Ctr Sci Computat, Atlanta, GA 30322 USA. [Zhang, Peng] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Dept Phys, Cambridge, MA 02138 USA. [Zhang, Peng] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom Mol & Opt Phys, Cambridge, MA 02138 USA. RP Wang, Z (reprint author), Emory Univ, Dept Chem, 1515 Dickey Dr, Atlanta, GA 30322 USA. EM morokuma@euch4e.chem.emory.edu FU AFOSR [FA9550-04-1-0080, FA955007-1-0395] FX The authors acknowledge Professor Bastian J. Braams, Professor Joel Bowman and Dr. Zhen Xie for very helpful advices in the use of permutationally invariant fitting procedure. The present research is in part supported by grants from AFOSR (Grant Nos. FA9550-04-1-0080 and FA955007- 1-0395). Computer time was provided by a grant under the DoD-High Performance Computing Program and by the Research Center for Computational Science, Okazaki, Japan as well as by the Cherry Emerson Center for Scientific Computation. NR 49 TC 10 Z9 10 U1 0 U2 9 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0021-9606 J9 J CHEM PHYS JI J. Chem. Phys. PD JAN 28 PY 2009 VL 130 IS 4 AR 044313 DI 10.1063/1.3068742 PG 18 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 401TJ UT WOS:000262965000024 PM 19191391 ER PT J AU Dekel, A Birnboim, Y Engel, G Freundlich, J Goerdt, T Mumcuoglu, M Neistein, E Pichon, C Teyssier, R Zinger, E AF Dekel, A. Birnboim, Y. Engel, G. Freundlich, J. Goerdt, T. Mumcuoglu, M. Neistein, E. Pichon, C. Teyssier, R. Zinger, E. TI Cold streams in early massive hot haloes as the main mode of galaxy formation SO NATURE LA English DT Article ID INTEGRAL FIELD SPECTROSCOPY; SUBMILLIMETER GALAXIES; MAJOR MERGERS; DISK GALAXIES; DARK-MATTER; TO 2; EVOLUTION; ACCRETION; Z-SIMILAR-TO-2.3; SIMULATIONS AB Massive galaxies in the young Universe, ten billion years ago, formed stars at surprising intensities(1,2). Although this is commonly attributed to violent mergers, the properties of many of these galaxies are incompatible with such events, showing gas- rich, clumpy, extended rotating disks not dominated by spheroids(1-5). Cosmological simulations(6) and clustering theory(6,7) are used to explore how these galaxies acquired their gas. Here we report that they are 'stream- fed galaxies', formed from steady, narrow, cold gas streams that penetrate the shock- heated media of massive dark matter haloes(8,9). A comparison with the observed abundance of star- forming galaxies implies that most of the input gas must rapidly convert to stars. One- third of the stream mass is in gas clumps leading to mergers of mass ratio greater than 1: 10, and the rest is in smoother flows. With a merger duty cycle of 0.1, three- quarters of the galaxies forming stars at a given rate are fed by smooth streams. The rarer, submillimetre galaxies that form stars even more intensely(2,12,13) are largely merger- induced starbursts. Unlike destructive mergers, the streams are likely to keep the rotating disk configuration intact, although turbulent and broken into giant star- forming clumps that merge into a central spheroid(4,10,11). This stream- driven scenario for the formation of discs and spheroids is an alternative to the merger picture. C1 [Dekel, A.; Birnboim, Y.; Engel, G.; Freundlich, J.; Goerdt, T.; Mumcuoglu, M.; Neistein, E.; Zinger, E.] Hebrew Univ Jerusalem, Racah Inst Phys, IL-91904 Jerusalem, Israel. [Birnboim, Y.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Freundlich, J.] Ecole Normale Super, Dept Phys, F-75231 Paris, France. [Neistein, E.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Pichon, C.] Inst Astrophys, F-75014 Paris, France. [Pichon, C.] UPMC, F-75014 Paris, France. [Teyssier, R.] CEA Saclay, DSM IRFU, UMR AIM, F-91191 Gif Sur Yvette, France. [Teyssier, R.] Univ Zurich, Inst Theoret Phys, CH-8057 Zurich, Switzerland. RP Dekel, A (reprint author), Hebrew Univ Jerusalem, Racah Inst Phys, IL-91904 Jerusalem, Israel. EM dekel@phys.huji.ac.il OI Birnboim, Yuval/0000-0002-6547-8545 FU France-Israel Teamwork in Sciences; German-Israel Science Foundation; Israel Science Foundation; NASA Theory Program at UCSC; Minerva fellowship FX We acknowledge discussions with N.Bouche, S. M. Faber, R. Genzel, D. Koo, A. Kravtsov, A. Pope, J. R. Primack, J. Prochaska, A. Sternberg and J. Wall. This research was supported by the France-Israel Teamwork in Sciences, the German-Israel Science Foundation, the Israel Science Foundation, a NASA Theory Program at UCSC, and a Minerva fellowship (T.G.). We thank the Barcelona Centro Nacional de Supercomputacion for computer resources and technical support. The simulation is part of the Horizon collaboration. NR 33 TC 750 Z9 751 U1 1 U2 19 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD JAN 22 PY 2009 VL 457 IS 7228 BP 451 EP 454 DI 10.1038/nature07648 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 395JA UT WOS:000262519200040 PM 19158792 ER PT J AU Su, YN van Ballegooijen, A Lites, BW Deluca, EE Golub, L Grigis, PC Huang, GL Ji, HS AF Su, Yingna van Ballegooijen, Adriaan Lites, Bruce W. Deluca, Edward E. Golub, Leon Grigis, Paolo C. Huang, Guangli Ji, Haisheng TI OBSERVATIONS AND NONLINEAR FORCE-FREE FIELD MODELING OF ACTIVE REGION 10953 SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: corona; Sun: filaments; Sun: flares; Sun: magnetic fields; Sun: photosphere; Sun: X-rays, gamma rays ID CORONAL MAGNETIC-FIELDS; STOKES PROFILE ANALYSIS; VECTOR MAGNETOGRAPH DATA; HINODE MISSION; SOLAR CORONA; FLUX ROPES; FLARE; RECONSTRUCTION; CANCELLATION; PHOTOSPHERE AB We present multiwavelength observations of a simple bipolar active region (NOAA 10953), which produced several small flares ( mostly B class and one C8.5 class) and filament activations from April 30 to May 3 in 2007. We also explore nonlinear force-free field (NLFFF) modeling of this region prior to the C8.5 flare on May 2, using magnetograph data from SOHO/MDI and Hinode/SOT. A series of NLFFF models are constructed using the flux-rope insertion method. By comparing the modeled field lines with multiple X-ray loops observed by Hinode/XRT, we find that the axial flux of the flux rope in the best-fit models is ( 7 +/- 2) x 10(20) Mx, while the poloidal flux has a wider range of (0.1-10) x 10(10) Mx cm(-1). The axial flux in the best-fit model is well below the upper limit (similar to 15 x 10(20) Mx) for stable force-free configurations, which is consistent with the fact that no successful full filament eruption occurred in this active region. From multiwavelength observations of the C8.5 flare, we find that the X-ray brightenings ( in both RHESSI and XRT) appeared about 20 minutes earlier than the EUV brightenings seen in TRACE 171 angstrom images and filament activations seen in MLSO H alpha images. This is interpreted as an indication that the X-ray emission may be caused by direct coronal heating due to reconnection, and the energy transported down to the chromosphere may be too low to produce EUV brightenings. This flare started from nearly unsheared flare loop, unlike most two-ribbon flares that begin with highly sheared footpoint brightenings. By comparing with our NLFFF model, we find that the early flare loop is located above the flux rope that has a sharp boundary. We suggest that this flare started near the outer edge of the flux rope, not at the inner side or at the bottom as in the standard two-ribbon flare model. C1 [Su, Yingna; van Ballegooijen, Adriaan; Deluca, Edward E.; Golub, Leon; Grigis, Paolo C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Su, Yingna; Huang, Guangli; Ji, Haisheng] Acad Sinica, Purple Mt Observ, Nanjing 210008, Peoples R China. [Lites, Bruce W.] High Altitude Observ, Boulder, CO 80307 USA. RP Su, YN (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM ynsu@head.cfa.harvard.edu RI Su, Yingna/J-1674-2012; DeLuca, Edward/L-7534-2013; OI DeLuca, Edward/0000-0001-7416-2895; van Ballegooijen, Adriaan/0000-0002-5622-3540 FU NASA [NNM07AB07C, NNG05GK32G]; NSFC [10773032, 10833007] FX We thank the referee for helpful suggestions to improve this paper. Hinode is a Japanese mission developed and launched by ISAS/JAXA, with NAOJ as domestic partner and NASA and STFC (UK) as international partners. It is operated by these agencies in co-operation with ESA and the NSC ( Norway). The authors thank the team of Hinode/XRT, Hinode/SOT, TRACE, RHESSI, SOHO MDI, MLSO, KSO, and GOES for providing valuable data. Y.S. acknowledges Kathy K. Reeves for helpful discussions. U. S. members of the XRT team are supported by NASA contract NNM07AB07C to the Smithsonian Astrophysical Observatory (SAO). The TRACE analysis are supported at SAO by a contract from Lockheed Martin. Y.S. is also supported by the NSFC projects with 10773032 and 10833007. The NLFFF modeling work was supported by NASA/LWS grant NNG05GK32G. NR 47 TC 39 Z9 39 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2009 VL 691 IS 1 BP 105 EP 114 DI 10.1088/0004-637X/691/1/105 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 405BH UT WOS:000263196600011 ER PT J AU Gogarten, SM Dalcanton, JJ Williams, BF Seth, AC Dolphin, A Weisz, D Skillman, E Holtzman, J Cole, A Girardi, L de Jong, RS Karachentsev, ID Olsen, K Rosema, K AF Gogarten, Stephanie M. Dalcanton, Julianne J. Williams, Benjamin F. Seth, Anil C. Dolphin, Andrew Weisz, Daniel Skillman, Evan Holtzman, Jon Cole, Andrew Girardi, Leo de Jong, Roelof S. Karachentsev, Igor D. Olsen, Knut Rosema, Keith TI THE ACS NEARBY GALAXY SURVEY TREASURY. II. YOUNG STARS AND THEIR RELATION TO H alpha AND UV EMISSION TIMESCALES IN THE M81 OUTER DISK SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: individual (M81); galaxies: spiral; galaxies: stellar content; H II regions ID LARGE-MAGELLANIC-CLOUD; EXTENDED ULTRAVIOLET DISK; INITIAL MASS FUNCTIONS; FORMATION HISTORY; STELLAR EVOLUTION; FAR-ULTRAVIOLET; SPIRAL GALAXIES; FORMATION THRESHOLDS; FORMATION RATES; DWARF GALAXIES AB We have obtained resolved stellar photometry from Hubble Space Telescope Advanced Camera for Surveys observations of a field in the outer disk of M81 as part of ANGST. Motivated by the recent discovery of extended UV disks around many nearby spiral galaxies, we use the observed stellar population to derive the recent star formation histories of five similar to 0.5 kpc-sized regions within this field. These regions were selected on the basis of their UV luminosity from GALEX and include two H II regions, two regions that are UV-bright but Ha-faint, and one "control" region faint in both UV and Ha. We estimate our effective star formation rate detection limit at similar to 2 x 10(-4) M(circle dot) yr(-1), which is lower than that of GALEX for regions of this size. As expected, the H II regions contain massive main-sequence stars ( in the mass range 18-27 M(circle dot), based on our best extinction estimates), while similar massive main-sequence stars are lacking in the UV-bright/H alpha-faint regions. The observations are consistent with stellar ages less than or similar to 10 Myr in the H II regions, and greater than or similar to 16 Myr in the UV-bright/H alpha-faint regions. All regions but the control have formed similar to 10(4) M(circle dot) of stars over the past similar to 65 Myr. Thus, our results, for at least one small area in the outer disk of M81, are consistent with an age difference being sufficient to explain the observed discrepancy between star forming regions detected in H alpha and those detected exclusively in UV. However, our data cannot conclusively rule out other explanations, such as a strongly truncated initial mass function. C1 [Gogarten, Stephanie M.; Dalcanton, Julianne J.; Williams, Benjamin F.; Rosema, Keith] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Seth, Anil C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Dolphin, Andrew] Raytheon Co, Tucson, AZ 85706 USA. [Weisz, Daniel; Skillman, Evan] Univ Minnesota, Dept Astron, Minneapolis, MN 55455 USA. [Holtzman, Jon] New Mexico State Univ, Dept Astron, Las Cruces, NM 88003 USA. [Cole, Andrew] Univ Tasmania, Sch Math & Phys, Hobart, Tas, Australia. [Girardi, Leo] Osserv Astron Padova, I-35122 Padua, Italy. [de Jong, Roelof S.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Karachentsev, Igor D.] Special Astrophys Observ, N Arkhyz, Kchr, Russia. [Olsen, Knut] Natl Opt Astron Observ, Tucson, AZ 85719 USA. RP Gogarten, SM (reprint author), Univ Washington, Dept Astron, Box 351580, Seattle, WA 98195 USA. EM stephanie@astro.washington.edu OI Gogarten, Stephanie/0000-0002-7231-9745 FU NASA [GO-10915, NAS5-26555]; JPL/Caltech FX We thank Janice Lee and her collaborators for generously providing an Ha image of our M81 Deep Field, and for many helpful discussions. We also thank the anonymous referee for constructive comments, which improved the paper. Support for this work was provided by NASA through grant GO-10915 from the Space Telescopes Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. J.J.D. was partially supported as a Wycoff Fellow. GALEX ( Galaxy Evolution Explorer) is a NASA Small Explorer, launched in April 2003. The Spitzer Space Telescope is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by JPL/Caltech, under contract with NASA. NR 65 TC 36 Z9 36 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2009 VL 691 IS 1 BP 115 EP 130 DI 10.1088/0004-637X/691/1/115 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 405BH UT WOS:000263196600012 ER PT J AU Yang, Y Wilson, AS Matt, G Terashima, Y Greenhill, LJ AF Yang, Y. Wilson, A. S. Matt, G. Terashima, Y. Greenhill, L. J. TI SUZAKU OBSERVATIONS OF THE CIRCINUS GALAXY SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: individual (Circinus); galaxies: Seyfert; X-rays: galaxies ID X-RAY SPECTROSCOPY; SEYFERT 2 GALAXIES; GALACTIC RIDGE; CHANDRA; NGC-4945; EMISSION; SPECTRUM; BEPPOSAX; REGION; AGN AB We report Suzaku observations of the active, Compton-thick Circinus galaxy. Observations were obtained with both the X-ray imaging spectrometer (XIS) and the hard X-ray detector (HXD). Below 10 keV, the nuclear spectrum is dominated by radiation reflected from cold dense gas of high column density, while above 13 keV the radiation is directly transmitted nuclear emission seen through a column density of similar or equal to 4 x 10(24) cm(-2). In the 0.2-10 keV band, the XIS spectrum is contaminated at 5% level by the brightest off-nuclear source in Circinus, but drops to 1% in the 5-10 keV band and is negligible at higher energies. We find no significant evidence for variability in the hard (> 12 keV) emission. Circinus is marginally detected with the HXD/GSO in the 50-100 keV band at 2.5 sigma level. We model the 3-70 keV band XIS+PIN spectra with four components: the Compton transmitted nuclear emission, the reflected nuclear emission, a soft power law(representing a combination of scattered nuclear emission, extended emission, and contamination by sources in the galaxy below a few keV), and emission lines. The hard nuclear power law is found to have a photon index Gamma(h) similar or equal to 1.6, very similar to the soft power law. The high-energy cutoff is E-C similar or equal to 49 keV. These results agree with those from BeppoSAX. An extrapolation of this model up to the GSO band shows good agreement with the GSO spectrum and supports our detection of Circinus up to similar or equal to 100 keV. C1 [Yang, Y.; Wilson, A. S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Matt, G.] Univ Roma Tre, Dipartimento Fis, I-100046 Rome, Italy. [Terashima, Y.] Ehime Univ, Fac Sci, Dept Phys, Matsuyama, Ehime 7908577, Japan. [Greenhill, L. J.] Ctr Astrophys, Smithsonian Astron Observ, Cambridge, MA 02138 USA. RP Yang, Y (reprint author), Univ Illinois, Dept Astron, 1002 W Green St, Urbana, IL 61801 USA. RI XRAY, SUZAKU/A-1808-2009 FU NASA through LTSA [NAG 513065]; University of Maryland [NMX06AI34G] FX Y. Yang would like to thank Richard Mushotzky for discussions on the XIS spectra. We thank Koji Mukai, Illana Harrus, and Kenji Hamaguchi at Suzaku GOF for help with issues related to data reduction and calibration. We thank an anonymous referee for suggestions that improved this paper. This work is supported by NASA through LTSA grant NAG 513065 and Suzaku NMX06AI34G granted to the University of Maryland. NR 31 TC 19 Z9 19 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 2009 VL 691 IS 1 BP 131 EP 139 DI 10.1088/0004-637X/691/1/131 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 405BH UT WOS:000263196600013 ER PT J AU Zapata, LA Menten, K Reid, M Beuther, H AF Zapata, Luis A. Menten, Karl Reid, Mark Beuther, Henrik TI AN EXTENSIVE, SENSITIVE SEARCH FOR SiO MASERS IN HIGH- AND INTERMEDIATE-MASS STAR-FORMING REGIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: molecules; radio continuum: ISM; radio lines: ISM; techniques: interferometric; techniques: spectroscopic ID YOUNG STELLAR OBJECTS; H-II REGIONS; EXCITED SILICON MONOXIDE; COMPACT RADIO-EMISSION; SAGITTARIUS B2 MAIN; MILLIMETER CONTINUUM; HII-REGIONS; ORION-KL; INTERFEROMETRIC OBSERVATIONS; PROTOSTELLAR CANDIDATES AB We present sensitive Very Large Array observations with an angular resolution of a few arcseconds of the J = 1-0 line of SiO in the v = 1 and 2 vibrationally excited states toward a sample of 60 Galactic regions in which stars of high or intermediate mass are currently forming and/or have recently formed. We report the detection of SiO maser emission in both vibrationally excited transitions toward only three very luminous regions: Orion-KL, W51N, and Sgr B2(M). Toward all three, SiO maser emission had previously been reported, in Orion-KL in both lines, in W51N only in the v = 2 line and in Sgr B2(M) only in the v = 1 line. Our work confirms that SiO maser emission in star-forming regions is a rare phenomenon, indeed, that requires special, probably extreme, physical and chemical conditions not commonly found. In addition to this SiO maser survey, we also present images of the simultaneously observed 7 mm continuum emission from a subset of our sample of star-forming regions where such emission was detected. This is, in most cases, likely to be free-free emission from compact and ultracompact H II regions. C1 [Zapata, Luis A.; Menten, Karl] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Reid, Mark] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Beuther, Henrik] Max Planck Inst Astron, D-69117 Heidelberg, Germany. RP Zapata, LA (reprint author), Max Planck Inst Radioastron, Auf Hugel 69, D-53121 Bonn, Germany. EM lzapata@mpifr-bonn.mpg.de; kmenten@mpifr-bonn.mpg.de; reid@cfa.harvard.edu; beuther@mpia-hd.mpg.de NR 94 TC 29 Z9 29 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2009 VL 691 IS 1 BP 332 EP 341 DI 10.1088/0004-637X/691/1/332 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 405BH UT WOS:000263196600027 ER PT J AU Hartman, JD Gaudi, BS Pinsonneault, MH Stanek, KZ Holman, MJ McLeod, BA Meibom, S Barranco, JA Kalirai, JS AF Hartman, J. D. Gaudi, B. S. Pinsonneault, M. H. Stanek, K. Z. Holman, M. J. McLeod, B. A. Meibom, S. Barranco, J. A. Kalirai, J. S. TI DEEP MMT TRANSIT SURVEY OF THE OPEN CLUSTER M37. III. STELLAR ROTATION AT 550 Myr SO ASTROPHYSICAL JOURNAL LA English DT Review DE open clusters and associations: individual (M37); stars: low-mass, brown dwarfs; stars: rotation; stars: spots; stars: variables: other ID LOW-MASS STARS; ALPHA-PERSEI CLUSTER; MAIN-SEQUENCE STARS; SOLAR-TYPE STARS; ANGULAR-MOMENTUM EVOLUTION; PHOTOMETRIC LIGHT CURVES; NGC 1039 M34; ECLIPSING BINARY; HYADES CLUSTER; POSSIBLE MEMBERS AB In the course of conducting a deep (14.5 less than or similar to r less than or similar to 23), 20 night survey for transiting planets in the rich similar to 550 Myr old open cluster M37, we have measured the rotation periods of 575 stars, which lie near the cluster main sequence, with masses 0.2 M(circle dot) less than or similar to M less than or similar to 1.3 M(circle dot). This is the largest sample of rotation periods for a cluster older than 500 Myr. Using this rich sample we investigate a number of relations between rotation period, color, and the amplitude of photometric variability. Stars with M greater than or similar to 0.8 M(circle dot) show a tight correlation between period and mass with heavier stars rotating more rapidly. There is a group of four stars with P > 15 days that fall well above this relation, which, if real, would present a significant challenge to theories of stellar angular momentum evolution. Below 0.8 M(circle dot), the stars continue to follow the period-mass correlation but with a broad tail of rapid rotators that expands to shorter periods with decreasing mass. We combine these results with observations of other open clusters to test the standard theory of lower main-sequence stellar angular momentum evolution. We find that the model reproduces the observations for solar-mass stars, but discrepancies are apparent for stars with 0.6 less than or similar to M less than or similar to 1.0 M(circle dot). We also find that for late K through early M dwarf stars in this cluster, rapid rotators tend to be bluer than slow rotators in B - V but redder than slow rotators in V - I(C). This result supports the hypothesis that the significant discrepancy between the observed and predicted temperatures and radii of low-mass main-sequence stars is due to stellar activity. C1 [Hartman, J. D.; Holman, M. J.; McLeod, B. A.; Meibom, S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gaudi, B. S.; Pinsonneault, M. H.; Stanek, K. Z.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Barranco, J. A.] San Francisco State Univ, Dept Phys & Astron, San Francisco, CA 94132 USA. [Kalirai, J. S.] Univ Calif Santa Cruz, Lick Observ, Univ Calif Observ, Santa Cruz, CA 95060 USA. RP Hartman, JD (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jhartman@cfa.harvard.edu; gaudi@astronomy.ohio-state.edu; pinsono@astronomy.ohio-state.edu; kstanek@astronomy.ohio-state.edu; mholman@cfa.harvard.edu; bmcleod@cfa.harvard.edu; smeibom@cfa.harvard.edu; barranco@stars.sfsu.edu; jkalirai@ucolick.org RI Gaudi, Bernard/I-7732-2012; OI Barranco, Joseph/0000-0003-2045-677X; Hartman, Joel/0000-0001-8732-6166 FU NSF [AST-0501681]; NASA [NNG06GH69G] FX We are grateful to C. Alcock for providing partial support for this project through his NSF grant (AST-0501681). Funding for M. H. came from NASA Origins grant NNG06GH69G. We would like to thank G. Furesz and A. Szentgyorgyi for help in preparing the Hectochelle observations, S. Barnes, S. Saar, N. Brickhouse, and S. Baliunas for helpful discussions, and the staff of the MMT, without whom this work would not have been possible. We are grateful to the anonymous referee for providing a thoughtful critique which improved the quality of this paper. We would also like to thank the MMT TAC for awarding us a significant amount of telescope time for this project. This research has made use of the WEBDA database, operated at the Institute for Astronomy of the University of Vienna; it has also made use of the SIMBAD database, operated at CDS, Strasbourg, France. NR 145 TC 52 Z9 52 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2009 VL 691 IS 1 BP 342 EP 364 DI 10.1088/0004-637X/691/1/342 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 405BH UT WOS:000263196600028 ER PT J AU Hansen, BMS Shih, HY Currie, T AF Hansen, Brad M. S. Shih, Hsin-Yi Currie, Thayne TI THE PULSAR PLANETS: A TEST CASE OF TERRESTRIAL PLANET ASSEMBLY SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrobiology; planetary systems: formation; pulsars: individual (PSR B1257+12); scattering ID M-CIRCLE-PLUS; MILLISECOND PULSARS; SOLAR-SYSTEM; ORBITAL EVOLUTION; TIDAL INTERACTION; GIANT PLANETS; NEUTRON-STAR; PSR B1257+12; ACCRETION; DISK AB We model the assembly of planets from planetary embryos under the conditions suggested by various scenarios for the formation of the planetary system around the millisecond pulsar B1257+12. We find that the most likely models fall at the low angular momentum end of the proposed range. Models that invoke supernova fallback produce such disks, although we find that a solar composition disk produces a more likely evolution than one composed primarily of heavy elements. Furthermore, we find that dust sedimentation must occur rapidly as the disk cools, in order that the solid material be confined to a sufficiently narrow range of radii. A quantitative comparison between the observations and the best-fit models shows that the simulations can reproduce the observed eccentricities and masses, but have difficulty reproducing the compactness of the pulsar planet system. Finally, we examine the results of similar studies of solar system terrestrial planet accumulation and discuss what can be learned from the comparison. C1 [Hansen, Brad M. S.; Shih, Hsin-Yi; Currie, Thayne] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Hansen, Brad M. S.; Shih, Hsin-Yi; Currie, Thayne] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA. [Currie, Thayne] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02140 USA. RP Hansen, BMS (reprint author), Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. EM hansen@astro.ucla.edu; jennywho@ucla.edu; tcurrie@cfa.harvard.edu FU Sloan Foundation; NASA; Space Interferometry Mission FX B. H. acknowledges support by the Sloan Foundation, the NASA Astrobiology Society and the Space Interferometry Mission. In particular, the computing cluster purchased with Sloan Funds made the calculations presented in this paper considerably less painful than they would otherwise have been. NR 48 TC 16 Z9 16 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2009 VL 691 IS 1 BP 382 EP 393 DI 10.1088/0004-637X/691/1/382 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 405BH UT WOS:000263196600031 ER PT J AU Drake, JJ Laming, JM Ness, JU Orlando, S Starrfield, S Beardmore, AP Bode, MF Evans, A Eyres, SPS Gehrz, RD Goad, MR Gonzalez-Riestra, R Krautter, J O'Brien, TJ Osborne, JP Page, KL Schwarz, G Woodward, CE AF Drake, Jeremy J. Laming, J. M. Ness, J-U Orlando, S. Starrfield, S. Beardmore, A. P. Bode, M. F. Evans, A. Eyres, S. P. S. Gehrz, R. D. Goad, M. R. Gonzalez-Riestra, R. Krautter, J. O'Brien, T. J. Osborne, J. P. Page, K. L. Schwarz, G. Woodward, C. E. TI X-RAY SPECTROSCOPIC DIAGNOSIS OF A WIND-COLLIMATED BLAST WAVE AND METAL-RICH EJECTA FROM THE 2006 EXPLOSION OF RS OPHIUCHI SO ASTROPHYSICAL JOURNAL LA English DT Article DE shock waves; stars: individual (RS Oph); novae, cataclysmic variables; X-rays: binaries; X-rays: stars ID 1985 OUTBURST; SWIFT OBSERVATIONS; ATOMIC DATABASE; SYMBIOTIC STARS; EMISSION-LINES; MASS ACCRETION; SHOCK-WAVE; ABUNDANCES; SYSTEMS; NEBULAE AB Chandra HETG observations of RS Ophiuchi at day 13.9 of the 2006 outburst reveal a rich spectrum of emission lines from abundant ions formed over a wide temperature range (similar to 3 x 10(6) to 60 x 10(6) K) indicative of shock heating of the circumstellar medium by the expanding blast wave. Lines are asymmetric and strongly broadened (v similar to 2400 km s(-1) at zero intensity). Using simple analytical model profiles, we show how the lines are shaped by differential absorption in the red giant wind and explosion ejecta, and that shock heating to multimillion degree temperatures appears to have occurred preferentially in the direction perpendicular to the line of sight. We conclude that the asymmetric nature of the offset 1/r(2) density profile and likely equatorial circumstellar density enhancement in which the explosion occurred are responsible for both the shock collimation and broad range in plasma temperature observed. The ejecta mass deduced from X-ray absorption is more easily reconciled with the expected mass accretion rate for material enhanced in metals by up to an order of magnitude. C1 [Drake, Jeremy J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Laming, J. M.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA. [Ness, J-U; Starrfield, S.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Orlando, S.] Osservatorio Astron Palermo GS Vaiana, I-90134 Palermo, Italy. [Beardmore, A. P.; Goad, M. R.; Osborne, J. P.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Bode, M. F.] Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England. [Evans, A.] Keele Univ, Astrophys Grp, Keele ST5 5BG, Staffs, England. [Eyres, S. P. S.] Univ Cent Lancashire, Ctr Astrophys, Preston PR1 2HE, Lancs, England. [Gehrz, R. D.; Woodward, C. E.] Univ Minnesota, Dept Astron, Sch Phys & Astron, Minneapolis, MN 55455 USA. [Gonzalez-Riestra, R.] ESAC, XMM Sci Operat Ctr, Madrid 28080, Spain. [Krautter, J.] Landessternwarte Konigstuhl, D-69117 Heidelberg, Germany. [O'Brien, T. J.] Univ Manchester, Jodrell Bank Observ, Sch Phys & Astron, Macclesfield SK11 9DL, Cheshire, England. [Schwarz, G.] W Chester Univ, Dept Geol & Astron, W Chester, PA 19383 USA. RP Drake, JJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jdrake@cfa.harvard.edu; Jan-Uwe.Ness@asu.edu; sumner.starrfield@asu.edu OI Orlando, Salvatore/0000-0003-2836-540X FU NASA [NAS8-39073, PF5-60039]; CXC; NSF; PPARC FX We thank the Chandra Director, Harvey Tananbaum, for generous allocation of Discretionary Time to observe RS Oph and the Chandra X-ray Center (CXC) Mission Planning department for fitting the observation into the schedule. J.J.D. was funded by NASA contract NAS8-39073 to the CXC during the course of this research. J.-U.N. gratefully acknowledges support provided by NASA through Chandra Postdoctoral Fellowship grant PF5-60039 awarded by the CXC, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. S. Starrfield received partial support from NSF and NASA grants to ASU. A. P. B., J.P.O., and K. L. P. acknowledge funding from PPARC. Finally, we extend warm thanks to the anonymous referee whose astute report enabled us to significantly clarify and improve the manuscript. NR 41 TC 19 Z9 19 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2009 VL 691 IS 1 BP 418 EP 424 DI 10.1088/0004-637X/691/1/418 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 405BH UT WOS:000263196600034 ER PT J AU Schmelz, JT Nasraoui, K Rightmire, LA Kimble, JA Del Zanna, G Cirtain, JW DeLuca, EE Mason, HE AF Schmelz, J. T. Nasraoui, K. Rightmire, L. A. Kimble, J. A. Del Zanna, G. Cirtain, J. W. DeLuca, E. E. Mason, H. E. TI ARE CORONAL LOOPS ISOTHERMAL OR MULTITHERMAL? SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: corona; Sun: fundamental parameters; Sun: UV radiation ID SOLAR ACTIVE REGIONS; TRANSITION-REGION; TEMPERATURE-MEASUREMENTS; DIAGNOSTIC SPECTROMETER; ATOMIC DATABASE; EMISSION-LINES; TRACE; EXPLORER; WAVELENGTHS; SOHO/CDS AB Surprisingly few solar coronal loops have been observed simultaneously with TRACE and SOHO/Coronal Diagnostics Spectrometer (CDS), and even fewer analyses of these loops have been conducted and published. The SOHO Joint Observing Program 146 was designed in part to provide the simultaneous observations required for in-depth temperature analysis of active region loops and determine whether these loops are isothermal or multithermal. The data analyzed in this paper were taken on 2003 January 17 of AR 10250. We used TRACE filter ratios, emission measure loci, and two methods of differential emission measure analysis to examine the temperature structure of three different loops. TRACE and CDS observations agree that Loop 1 is isothermal with log T = 5.85, both along the line of sight as well as along the length of the loop leg that is visible in the CDS field of view. Loop 2 is hotter than Loop 1. It is multithermal along the line of sight, with significant emission between 6.2 < log T < 6.4, but the loop apex region is out of the CDS field of view so it is not possible to determine the temperature distribution as a function of the loop height. Loop 3 also appears to be multithermal, but a blended loop that is just barely resolved with CDS may be adding cool emission to the Loop 3 intensities and complicating our results. So, are coronal loops isothermal or multithermal? The answer appears to be yes. C1 [Schmelz, J. T.; Nasraoui, K.; Rightmire, L. A.; Kimble, J. A.] Univ Memphis, Dept Phys, Memphis, TN 38152 USA. [Del Zanna, G.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Cirtain, J. W.] NASA, MSFC, NSSTC, Huntsville, AL 35805 USA. [DeLuca, E. E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Mason, H. E.] Ctr Math Sci, DAMTP, Cambridge CB3 OWA, England. RP Schmelz, JT (reprint author), Univ Memphis, Dept Phys, Memphis, TN 38152 USA. EM jschmelz@memphis.edu; G.Del-Zanna@damtp.cam.ac.uk; Jonathan.W.Cirtain@nasa.gov; edeluca@cfa.harvard.edu; H.E.Mason@damtp.cam.ac.uk RI DeLuca, Edward/L-7534-2013 OI DeLuca, Edward/0000-0001-7416-2895 FU NSF [ATM-0402729]; NASA [NNG05GE68]; PPARC FX We thank Harry Warren for the use of his DEM program, Amy Winebarger for installing this program on our computers, and University of Memphis physics students James Andrews and Jennifer Garst for help with analysis. Solar physics research at University of Memphis is supported by NSF ATM-0402729 and NASA NNG05GE68G. H. E. M. and G.D.Z. acknowledge financial support from PPARC. We are grateful to P. R. Young and the entire CDS team for their help in obtaining these observations. We also benefited greatly from discussions at the coronal loops workshops in Paris (2002 November), Palermo (2004 September), and Santorini (2007 June). NR 31 TC 23 Z9 23 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2009 VL 691 IS 1 BP 503 EP 515 DI 10.1088/0004-637X/691/1/503 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 405BH UT WOS:000263196600043 ER PT J AU Gonzalez, AH Clowe, D Bradac, M Zaritsky, D Jones, C Markevitch, M AF Gonzalez, Anthony H. Clowe, Douglas Bradac, Marusa Zaritsky, Dennis Jones, Chirstine Markevitch, Maxim TI A MULTIPLY IMAGED LUMINOUS INFRARED GALAXY BEHIND THE BULLET CLUSTER (1E0657-56) SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: general; galaxies: evolution; galaxies: starburst; gravitational lensing ID STAR-FORMATION HISTORY; INTERACTION CROSS-SECTION; HIGH-REDSHIFT GALAXIES; STELLAR MASS DENSITY; FORMING GALAXIES; DARK-MATTER; SUBMILLIMETER GALAXIES; SPITZER MIPS; X-RAY; CONSTRAINTS AB We present evidence for a Spitzer-selected luminous infrared galaxy (LIRG) behind the Bullet Cluster (1E0657-56). The galaxy, originally identified as a multiply imaged source using Infrared Array Camera (IRAC) photometry, has a spectral energy distribution consistent with a highly extincted (A(V) similar to 3.3), strongly star forming galaxy at z = 2.7. Using our strong gravitational lensing model presented in a previous paper, we find that the magnifications are vertical bar mu vertical bar approximate to 10-50 for the three images of the galaxy. The brightest and faintest images differ by a factor of 3.2 in magnification. The implied infrared luminosity is consistent with the galaxy being a LIRG, with a stellar mass of M(*) similar to 2 x 10(10) M(circle dot) and a star formation rate (SFR) of similar to 90 M(circle dot) yr(-1). With lensed fluxes at 24 mu m of 0.58 mJy and 0.39 mJy in the two brightest images, this galaxy presents a unique opportunity for detailed study of an obscured starburst with a SFR comparable to that of L* galaxies at z > 2. C1 [Gonzalez, Anthony H.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Clowe, Douglas] Ohio Univ, Dept Phys & Astron, Athens, OH 45701 USA. [Bradac, Marusa] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Zaritsky, Dennis] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Jones, Chirstine; Markevitch, Maxim] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Gonzalez, AH (reprint author), Univ Florida, Dept Astron, Gainesville, FL 32611 USA. EM anthony@astro.ufl.edu FU NASA [HST-GO-10200, HST-GO-10863, HST-GO-11099, 1319141]; Space Telescope Science Institute [HST-HF-01206.01] FX A. H. G. thanks R.-R. Chary, A. Dey, J.-P. Kneib, A. Pope, and G. Wilson for constructive discussions related to this work, S. Charlot and G. Bruzual for providing access to the Charlot & Bruzual (2007) models, and the anonymous referee for comments that significantly improved the manuscript. The authors acknowledge support for this work from NASA/HST grants HST-GO-10200, HST-GO-10863, and HST-GO-11099, as well as NASA/Spitzer grant 1319141. M. B. also acknowledges support from NASA through Hubble Fellowship grant # HST-HF-01206.01 awarded by the Space Telescope Science Institute. NR 51 TC 20 Z9 20 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2009 VL 691 IS 1 BP 525 EP 530 DI 10.1088/0004-637X/691/1/525 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 405BH UT WOS:000263196600045 ER PT J AU Tafoya, D Gomez, Y Patel, NA Torrelles, JM Gomez, JF Anglada, G Miranda, LF de Gregorio-Monsalvo, I AF Tafoya, D. Gomez, Y. Patel, N. A. Torrelles, J. M. Gomez, J. F. Anglada, G. Miranda, L. F. de Gregorio-Monsalvo, I. TI A COLLIMATED, IONIZED BIPOLAR STRUCTURE AND A HIGH DENSITY TORUS IN THE PLANETARY NEBULA IRAS 17347-3139 SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary nebulae: general; planetary nebulae: individual (IRAS 17347-3139); radio continuum: stars; stars: AGB and post-AGB; stars: mass loss; stars: winds, outflows ID WATER-MASER EMISSION; PROTOPLANETARY NEBULAE; RADIO-CONTINUUM; STARS; JET; IRAS-17347-3139; KINEMATICS; EVOLUTION; BUBBLES; SHAPES AB We present observations of continuum (lambda = 0.7, 1.3, 3.6, and 18 cm) and OH maser (lambda = 18 cm) emission toward the young planetary nebula IRAS 17347-3139, which is one of the three planetary nebulae that are known to harbor water maser emission. From the continuum observations, we show that the ionized shell of IRAS 17347-3139 consists of two main structures: one extended (size similar to 1 ''.5) with bipolar morphology along P. A.= -30 degrees, elongated in the same direction as the lobes observed in the near-infrared (NIR) images, and a central compact structure (size similar to 0 ''.25) elongated in the direction perpendicular to the bipolar axis, coinciding with the equatorial dark lane observed in the NIR images. Our image at 1.3 cm suggests the presence of dense walls in the ionized bipolar lobes. We estimate for the central compact structure a value of the electron density at least similar to 5 times higher than in the lobes. A high-resolution image of this structure at 0.7 cm shows two peaks separated by about 0 ''.13 (corresponding to 100-780 AU, using a distance range of 0.8-6 kpc). This emission is interpreted as originating in an ionized equatorial torus-like structure, from whose edges the water maser emission might be arising. We have detected weak OH 1612 MHz maser emission at V(LSR) similar to -70 km s(-1) associated with IRAS 17347-3139. We derive a 3 sigma upper limit of < 35% for the percentage of circularly polarized emission. Within our primary beam, we detected additional OH 1612 MHz maser emission in the local standard of rest velocity ranges -5 to -24 and -90 to -123 km s(-1), associated with the sources J17380406-3138387 and OH 356.65-0.15, respectively. C1 [Tafoya, D.; Gomez, Y.] Univ Nacl Autonoma Mexico, Ctr Radioastron & Astrofis, Morelia 58089, Michoacan, Mexico. [Patel, N. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Torrelles, J. M.] Univ Barcelona, Fac Fis, CSIC, Inst Ciencias Espacio,IEEC, E-08028 Barcelona, Spain. [Gomez, J. F.; Anglada, G.; Miranda, L. F.] CSIC, Inst Astrofis Andalucia, E-18008 Granada, Spain. [de Gregorio-Monsalvo, I.] European So Observ, Santiago 19001 19, Chile. RP Tafoya, D (reprint author), Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM dtafoya@cfa.harvard.edu RI Gomez, Jose Francisco/D-8392-2016; OI Gomez, Jose Francisco/0000-0002-7065-542X; Torrelles, Jose Maria/0000-0002-6896-6085 FU DGAPA-UNAM [IN100407]; CONACyT [49947]; MEC (Spain) [AYA2005-08523-C03, AYA2005-01495]; Consejeria de Innovacion; Ciencia y Empresa of Junta de Andalucia. FX D. T. and YG acknowledge support from DGAPA-UNAM grant IN100407 and CONACyT grant 49947. G. A., J. F. G., and J. M. T. acknowledge support from MEC (Spain) grant AYA2005-08523-C03 (co-funded with FEDER funds). L. F. M. is supported by MEC grant AYA2005-01495 (cofunded with FEDER funds). G. A., I. dG., J. F. G., J. M. T., and L. F. M. are also supported by Consejeria de Innovacion, Ciencia y Empresa of Junta de Andalucia. We thank the anonymous referee for constructive comments on the manuscript. NR 42 TC 8 Z9 8 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2009 VL 691 IS 1 BP 611 EP 620 DI 10.1088/0004-637X/691/1/611 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 405BH UT WOS:000263196600052 ER PT J AU Bloom, JS Perley, DA Li, W Butler, NR Miller, AA Kocevski, D Kann, DA Foley, RJ Chen, HW Filippenko, AV Starr, DL Macomber, B Prochaska, JX Chornock, R Poznanski, D Klose, S Skrutskie, MF Lopez, S Hall, P Glazebrook, K Blake, CH AF Bloom, J. S. Perley, D. A. Li, W. Butler, N. R. Miller, A. A. Kocevski, D. Kann, D. A. Foley, R. J. Chen, H. -W. Filippenko, A. V. Starr, D. L. Macomber, B. Prochaska, J. X. Chornock, R. Poznanski, D. Klose, S. Skrutskie, M. F. Lopez, S. Hall, P. Glazebrook, K. Blake, C. H. TI OBSERVATIONS OF THE NAKED-EYE GRB 080319B: IMPLICATIONS OF NATURE'S BRIGHTEST EXPLOSION SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: high-redshift; gamma rays: bursts; gamma rays: observations; supernovae: general ID GAMMA-RAY BURSTS; DIGITAL SKY SURVEY; LIGHT CURVES; MULTIWAVELENGTH OBSERVATIONS; REDSHIFT DISTRIBUTION; OPTICAL FLASHES; DATA RELEASE; AFTERGLOWS; SPECTRA; ENERGY AB The first gamma-ray burst (GRB) confirmed to be bright enough to be seen with the naked eye, GRB 080319B at redshift z = 0.937, allowed for exquisite follow-up observations across the electromagnetic spectrum. We present our detailed optical and infrared (IR) observations of the afterglow, consisting of over 5000 images starting 51 s after the GRB trigger, in concert with our own analysis of the Swift UVOT, Burst Alert Telescope (BAT), and XRT data. The event is extreme not only in observed properties but also intrinsically: it was the most luminous event ever recorded at optical and IR wavelengths and had an exceedingly high isotropic-equivalent energy release in gamma-rays. At early times, the afterglow evolution is broadly consistent with being reverse-shock dominated, but then is subsumed by a forward shock at around 1000 s. The overall spectral energy distribution, spanning from ultraviolet through near-IR wavelengths, shows no evidence for a significant amount of dust extinction in the host frame. The afterglow evolution, however, is highly chromatic: starting at about 1000 s the index shifts blueward before shifting back to the red at late times. In our deepest late-time observations, we find tentative evidence for an optical jet break and a luminous supernova. Finally, we examine the detectability of such events with current and future facilities and find that such an event could be detected in gamma rays by BAT out to z = 10.7 (8 sigma), while the nominal EXIST sensitivity would allow detection to z approximate to 32. At the K band, this source would have been easily detected with meter-class telescopes to z approximate to 17. C1 [Bloom, J. S.; Perley, D. A.; Li, W.; Butler, N. R.; Miller, A. A.; Kocevski, D.; Foley, R. J.; Filippenko, A. V.; Starr, D. L.; Macomber, B.; Chornock, R.; Poznanski, D.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Kann, D. A.; Klose, S.] Thuringer Landessternwarte Tautenburg, D-07778 Tautenburg, Germany. [Chen, H. -W.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Starr, D. L.] Las Cumbres Global Telescope Network, Goleta, CA 93117 USA. [Prochaska, J. X.] Univ Calif Santa Cruz, Lick Observ, Univ Calif Observ, Santa Cruz, CA 95064 USA. [Skrutskie, M. F.] Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA. [Lopez, S.] Univ Chile, Dept Astron, Santiago, Chile. [Glazebrook, K.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Blake, C. H.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Bloom, JS (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. RI Glazebrook, Karl/N-3488-2015; Lopez, Sebastian /I-5657-2016 OI Glazebrook, Karl/0000-0002-3254-9044; Lopez, Sebastian /0000-0003-0389-0902 FU Department of Energy; NASA/Swift [NNG05GF55G]; National Science Foundation (NSF) [AST-0607485]; TABASGO Foundation; NASA/Swift Guest Investigator [NNG05GF35G, NNG06GI86G]; Chilean Centro de Astrofisica FONDAP [15010003]; FONDECYT [1060823] FX Much of this research could not have been undertaken without the work of S. Barthelmy running the GCN Circulars and the Swift team for their extraordinary efforts. N. R. B. was partially supported by a SciDAC grant from the Department of Energy. J. S. B., J. X. P., and H.-W.C. are partially supported by NASA/Swift grant NNG05GF55G. A.V.F.'s group at U. C. Berkeley is supported by National Science Foundation (NSF) grant AST-0607485 and the TABASGO Foundation, as well as by NASA/Swift Guest Investigator grants NNG05GF35G and NNG06GI86G. S. L. was partly supported by the Chilean Centro de Astrofisica FONDAP No. 15010003 and by FONDECYT grant 1060823. We thank J. Brewer of the IFMD Foundation. This publication makes use of data products from the 2MASS, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/CaliforniaInstitute of Technology, funded by NASA and the NSF. KAIT and its ongoing research were made possible by donations from Sun Microsystems, Inc., the Hewlett-Packard Company, AutoScope Corporation, Lick Observatory, the NSF, the University of California, the Sylvia & Jim Katzman Foundation, and the TABASGO Foundation. Partially 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 Science and Technology Facilities Council (United Kingdom), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), Ministrio da Cincia e Tecnologia (Brazil), and SECYT (Argentina). We thank the Gemini Observatory staff for their excellent work in observing GRB 080319B; the assistance of the Lick Observatory staff is also acknowledged. The PAIRITEL is operated by the Smithsonian Astrophysical Observatory (SAO) and was made possible by a grant from the Harvard University Milton Fund, the camera loan from the University of Virginia, and the continued support of the SAO and UC Berkeley. The PAIRITEL project is further supported by NASA/Swift Guest Investigator Grant NNG06GH50G. We are grateful to E. E. Falco and the Mt. Hopkins staff (W. Peters, R. Hutchins, and T. Groner) for their continued assistance with PAIRITEL. NR 90 TC 95 Z9 96 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2009 VL 691 IS 1 BP 723 EP 737 DI 10.1088/0004-637X/691/1/723 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 405BH UT WOS:000263196600062 ER PT J AU Landi, E Cranmer, SR AF Landi, E. Cranmer, S. R. TI ION TEMPERATURES IN THE LOW SOLAR CORONA: POLAR CORONAL HOLES AT SOLAR MINIMUM SO ASTROPHYSICAL JOURNAL LA English DT Article DE line: profiles; Sun: corona; Sun: UV radiation; techniques: spectroscopic; turbulence; waves ID ALFVEN WAVES; CYCLOTRON WAVES; TRANSITION REGION; MAGNETOHYDRODYNAMIC MODE; LINE WIDTHS; MINOR IONS; WIND IONS; ACCELERATION; TURBULENCE; SUMER AB In the present work we use a deep-exposure spectrum taken by the SUMER spectrometer in a polar coronal hole in 1996 to measure the ion temperatures of a large number of ions at many different heights above the limb between 0.03 and 0.17 solar radii. We find that the measured ion temperatures are almost always larger than the electron temperatures and exhibit a nonmonotonic dependence on the charge-to-mass ratio. We use these measurements to provide empirical constraints to a theoretical model of ion heating and acceleration based on gradually replenished ion-cyclotron waves. We compare the wave power required to heat the ions to the observed levels to a prediction based on a model of anisotropic magnetohydrodynamic turbulence. We find that the empirical heating model and the turbulent cascade model agree with one another, and explain the measured ion temperatures, for charge-to-mass ratios smaller than about 0.25. However, ions with charge-to-mass ratios exceeding 0.25 disagree with the model; the wave power that they require to be heated to the measured ion temperatures shows an increase with charge-to-mass ratio (i. e., with increasing frequency) that cannot be explained by a traditional cascade model. We discuss possible additional processes that might be responsible for the inferred surplus of wave power. C1 [Landi, E.] USN, Res Lab, Artep Inc, Washington, DC 20375 USA. [Cranmer, S. R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Landi, E (reprint author), USN, Res Lab, Artep Inc, 4555 Overlook Ave SW, Washington, DC 20375 USA. RI Landi, Enrico/H-4493-2011 FU NASA [NNG06EA14I, NNH06CD24C, NNX06AG95G, NNG04GE77G] FX The work of Enrico Landi is supported by the NNG06EA14I, NNH06CD24C as well as other NASA grants. The work of Steven Cranmer is supported by NASA under grants NNX06AG95G and NNG04GE77G to the Smithsonian Astrophysical Observatory. The authors would like to thank Adriaan van Ballegooijen and Mari Paz Miralles for valuable discussions. NR 59 TC 32 Z9 32 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2009 VL 691 IS 1 BP 794 EP 805 DI 10.1088/0004-637X/691/1/794 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 405BH UT WOS:000263196600068 ER PT J AU Li, LX Narayan, R McClintock, JE AF Li, Li-Xin Narayan, Ramesh McClintock, Jeffrey E. TI INFERRING THE INCLINATION OF A BLACK HOLE ACCRETION DISK FROM OBSERVATIONS OF ITS POLARIZED CONTINUUM RADIATION SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; polarization; radiative transfer; relativity; X-rays: binaries ID MARGINALLY STABLE ORBIT; ACTIVE GALACTIC NUCLEI; X-RAY POLARIZATION; MAGNETIZED ACCRETION; SPECTRAL EVOLUTION; RELATIVISTIC JETS; EMISSION-LINES; CRAB-NEBULA; CYGNUS X-1; SPIN AB Spin parameters of stellar-mass black holes in X-ray binaries are currently being estimated by fitting the X-ray continuum spectra of their accretion disk emission. For this method, it is necessary to know the inclination of the X-ray-producing inner region of the disk. Since the inner disk is expected to be oriented perpendicular to the spin axis of the hole, the usual practice is to assume that the black hole spin is aligned with the orbital angular momentum vector of the binary, and to estimate the inclination of the latter from ellipsoidal modulations in the light curve of the secondary star. We show that the inclination of the disk can be inferred directly if we have both spectral and polarization information on the disk radiation. The predicted degree of polarization varies from 0% to 5% as the disk inclination changes from face-on to edge-on. With current X-ray polarimetric techniques the polarization degree of a typical bright X-ray binary could be measured to an accuracy of 0.1% by observing the source for about 10 days. Such a measurement would constrain the disk inclination to within a degree or two and would significantly improve the reliability of black hole spin estimates. In addition, it would provide new information on the tilt between the black hole spin axis and the orbital rotation axis of the binary, which would constrain any velocity kicks experienced by stellar-mass black holes during their formation. C1 [Li, Li-Xin] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Narayan, Ramesh; McClintock, Jeffrey E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Li, LX (reprint author), Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85741 Garching, Germany. OI Narayan, Ramesh/0000-0002-1919-2730 NR 91 TC 39 Z9 39 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2009 VL 691 IS 1 BP 847 EP 865 DI 10.1088/0004-637X/691/1/847 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 405BH UT WOS:000263196600072 ER PT J AU Knutson, HA Charbonneau, D Burrows, A O'Donovan, FT Mandushev, G AF Knutson, Heather A. Charbonneau, David Burrows, Adam O'Donovan, Francis T. Mandushev, Georgi TI DETECTION OF A TEMPERATURE INVERSION IN THE BROADBAND INFRARED EMISSION SPECTRUM OF TrES-4 SO ASTROPHYSICAL JOURNAL LA English DT Article DE eclipses; planetary systems; stars: individual: (TrES-4); techniques: photometric ID EXTRASOLAR GIANT PLANETS; SPITZER-SPACE-TELESCOPE; EXOPLANET HD 189733B; LIGHT CURVES; THERMAL EMISSION; HOT JUPITERS; THEORETICAL SPECTRA; ARRAY CAMERA; ATMOSPHERES; 209458B AB We estimate the strength of the bandpass-integrated thermal emission from the extrasolar planet TrES-4 at 3.6, 4.5, 5.8, and 8.0 mu m using the Infrared Array Camera on the Spitzer Space Telescope. We find relative eclipse depths of 0.137% +/- 0.011%, 0.148% +/- 0.016%, 0.261% +/- 0.059%, and 0.318% +/- 0.044% in these four bandpasses, respectively. We also place a 2 sigma upper limit of 0.37% on the depth of the secondary eclipse in the 16 mu m IRS peak-up array. These eclipse depths reveal that TrES-4 has an emission spectrum similar to that of HD 209458b, which requires the presence of water emission bands created by a thermal inversion layer high in the atmosphere in order to explain the observed features. TrES-4 receives more radiation from its star than HD 209458b and has a correspondingly higher effective temperature, therefore the presence of a temperature inversion in this planet's atmosphere lends support to the idea that inversions might be correlated with the irradiance received by the planet. We find no evidence for any offset in the timing of the secondary eclipse, and place a 3 sigma upper limit of vertical bar e cos(omega)vertical bar < 0.0058, where e is the planet's orbital eccentricity and omega is the argument of pericenter. From this we conclude that tidal heating from ongoing orbital circularization is unlikely to be the explanation for TrES-4's inflated radius. C1 [Knutson, Heather A.; Charbonneau, David] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Burrows, Adam] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [O'Donovan, Francis T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Mandushev, Georgi] Lowell Observ, Flagstaff, AZ 86001 USA. RP Knutson, HA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM hknutson@cfa.harvard.edu RI O'Donovan, Francis/I-2423-2014; OI O'Donovan, Francis/0000-0002-4858-6106; Charbonneau, David/0000-0002-9003-484X FU NASA through an award issued by JPL/Caltech. [NNX07AG80, G1328902]; National Science Foundation Graduate Research Fellowship; NASA Astrobiology Institute under Cooperative Agreement [CAN-02-OSS-02]; Office of Space Science; Goddard Space Flight Center FX This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract to NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. H. A. K. was supported by a National Science Foundation Graduate Research Fellowship. A. B. acknowledges the support of NASA through grant NNX07AG80G and JPL/Spitzer Agreement no. 1328902 and through the NASA Astrobiology Institute under Cooperative Agreement no. CAN-02-OSS-02 issued through the Office of Space Science. A. B. would also like to acknowledge Laurent Ibgui for checking the model results. F. T. O'D. was supported by an appointment to the NASA Postdoctoral Program at the Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA. NR 47 TC 74 Z9 74 U1 1 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2009 VL 691 IS 1 BP 866 EP 874 DI 10.1088/0004-637X/691/1/866 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 405BH UT WOS:000263196600073 ER PT J AU Donnarumma, I Vittorini, V Vercellone, S Del Monte, E Feroci, M D'Ammando, F Pacciani, L Chen, AW Tavani, M Bulgarelli, A Giuliani, A Longo, F Pucella, G Argan, A Barbiellini, G Boffelli, F Caraveo, P Cattaneo, PW Cocco, V Costa, E De Paris, G Di Cocco, G Evangelista, Y Fiorini, M Froysland, T Frutti, M Fuschino, F Galli, M Gianotti, F Labanti, C Lapshov, I Lazzarotto, F Lipari, P Marisaldi, M Mastropietro, M Mereghetti, S Morelli, E Morselli, A Pellizzoni, A Perotti, F Picozza, P Porrovecchio, G Prest, M Rapisarda, M Rappoldi, A Rubini, A Soffitta, P Trifoglio, M Trois, A Vallazza, E Zambra, A Zanello, D Pittori, C Santolamazza, P Verrecchia, F Giommi, P Colafrancesco, S Salotti, L Villata, M Raiteri, CM Chen, WP Efimova, NV Jordan, B Konstantinova, TS Koptelova, E Kurtanidze, OM Larionov, VM Ros, JA Sadun, AC Anderhub, H Antonelli, LA Antoranz, P Backes, M Baixeras, C Balestra, S Barrio, JA Bartko, H Bastieri, D Gonzalez, JB Becker, JK Bednarek, W Berger, K Bernardini, E Biland, A Bock, RK Bonnoli, G Bordas, P Tridon, DB Bosch-Ramon, V Bretz, T Britvitch, I Camara, M Carmona, E Chilingarian, A Commichau, S Contreras, JL Cortina, J Costado, MT Covino, S Curtef, V Dazzi, F De Angelis, A Del Pozo, ED Reyes, RD De Lotto, B De Maria, M De Sabata, F Mendez, CD Dominguez, A Dorner, D Doro, M Elsaesser, D Errando, M Ferenc, D Fernandez, E Firpo, R Fonseca, MV Font, L Galante, N Lopez, RJG Garczarczyk, M Gaug, M Goebel, F Hadasch, D Hayashida, M Herrero, A Hohne-Monch, D Hose, J Hsu, CC Huber, S Jogler, T Kranich, D La Barbera, A Laille, A Leonardo, E Lindfors, E Lombardi, S Lopez, M Lorenz, E Majumdar, P Maneva, G Mankuzhiyil, N Mannheim, K Maraschi, L Mariotti, M Martinez, M Mazin, D Meucci, M Meyer, M Miranda, JM Mirzoyan, R Moldon, J Moles, M Moralejo, A Nieto, D Nilsson, K Ninkovic, J Oya, I Paoletti, R Paredes, JM Pasanen, M Pascoli, D Pauss, F Pegna, RG Perez-Torres, MA Persic, M Peruzzo, L Prada, F Prandini, E Puchades, N Raymers, A Rhode, W Ribo, M Rico, J Rissi, M Robert, A Rugamer, S Saggion, A Saito, TY Salvati, M Sanchez-Conde, M Sartori, P Satalecka, K Scalzotto, V Scapin, V Schweizer, T Shayduk, M Shinozaki, K Shore, SN Sidro, N Sierpowska-Bartosik, A Sillanpaa, A Sitarek, J Sobczynska, D Spanier, F Stamerra, A Stark, LS Takalo, L Tavecchio, F Temnikov, P Tescaro, D Teshima, M Tluczykont, M Torres, DF Turini, N Vankov, H Venturini, A Vitale, V Wagner, RM Wittek, W Zabalza, V Zandanel, F Zanin, R Zapatero, J Acciari, V Aliu, E Arlen, T Beilicke, M Benbow, W Bradbury, SM Buckley, JH Bugaev, V Butt, Y Byrum, K Cannon, A Cesarini, A Chow, YC Ciupik, L Cogan, P Colin, P Cui, W Daniel, MK Dickherber, R Duke, C Ergin, T Fegan, SJ Finley, JP Finnegan, G Fortin, P Furniss, A Gall, D Gillanders, GH Guenette, R Gyuk, G Grube, J Hanna, D Holder, J Horan, D Hui, CM Humensky, TB Imran, A Kaaret, P Karlsson, N Kertzman, M Kieda, D Kildea, J Konopelko, A Krawczynski, H Krennrich, F Lang, MJ LeBohec, S Maier, G McCann, A McCutcheon, M Milovanovic, A Moriarty, P Nagai, T Ong, RA Otte, AN Pandel, D Perkins, JS Pichel, A Pohl, M Ragan, K Reyes, LC Reynolds, PT Roache, E Rose, HJ Schroedter, M Sembroski, GH Smith, AW Steele, D Swordy, SP Theiling, M Toner, JA Valcarcel, L Varlotta, A Wakely, SP Ward, JE Weekes, TC Weinstein, A Williams, DA Wissel, S Wood, M Zitzer, B AF Donnarumma, I. Vittorini, V. Vercellone, S. Del Monte, E. Feroci, M. D'Ammando, F. Pacciani, L. Chen, A. W. Tavani, M. Bulgarelli, A. Giuliani, A. Longo, F. Pucella, G. Argan, A. Barbiellini, G. Boffelli, F. Caraveo, P. Cattaneo, P. W. Cocco, V. Costa, E. De Paris, G. Di Cocco, G. Evangelista, Y. Fiorini, M. Froysland, T. Frutti, M. Fuschino, F. Galli, M. Gianotti, F. Labanti, C. Lapshov, I. Lazzarotto, F. Lipari, P. Marisaldi, M. Mastropietro, M. Mereghetti, S. Morelli, E. Morselli, A. Pellizzoni, A. Perotti, F. Picozza, P. Porrovecchio, G. Prest, M. Rapisarda, M. Rappoldi, A. Rubini, A. Soffitta, P. Trifoglio, M. Trois, A. Vallazza, E. Zambra, A. Zanello, D. Pittori, C. Santolamazza, P. Verrecchia, F. Giommi, P. Colafrancesco, S. Salotti, L. Villata, M. Raiteri, C. M. Chen, W. P. Efimova, N. V. Jordan, B. Konstantinova, T. S. Koptelova, E. Kurtanidze, O. M. Larionov, V. M. Ros, J. A. Sadun, A. C. Anderhub, H. Antonelli, L. A. Antoranz, P. Backes, M. Baixeras, C. Balestra, S. Barrio, J. A. Bartko, H. Bastieri, D. Becerra Gonzalez, J. Becker, J. K. Bednarek, W. Berger, K. Bernardini, E. Biland, A. Bock, R. K. Bonnoli, G. Bordas, P. Tridon, D. Borla Bosch-Ramon, V. Bretz, T. Britvitch, I. Camara, M. Carmona, E. Chilingarian, A. Commichau, S. Contreras, J. L. Cortina, J. Costado, M. T. Covino, S. Curtef, V. Dazzi, F. De Angelis, A. De Cea Del Pozo, E. Reyes, R. De Los De Lotto, B. De Maria, M. De Sabata, F. Delgado Mendez, C. Dominguez, A. Dorner, D. Doro, M. Elsaesser, D. Errando, M. Ferenc, D. Fernandez, E. Firpo, R. Fonseca, M. V. Font, L. Galante, N. Garcia Lopez, R. J. Garczarczyk, M. Gaug, M. Goebel, F. Hadasch, D. Hayashida, M. Herrero, A. Hoehne-Moench, D. Hose, J. Hsu, C. C. Huber, S. Jogler, T. Kranich, D. La Barbera, A. Laille, A. Leonardo, E. Lindfors, E. Lombardi, S. Lopez, M. Lorenz, E. Majumdar, P. Maneva, G. Mankuzhiyil, N. Mannheim, K. Maraschi, L. Mariotti, M. Martinez, M. Mazin, D. Meucci, M. Meyer, M. Miranda, J. M. Mirzoyan, R. Moldon, J. Moles, M. Moralejo, A. Nieto, D. Nilsson, K. Ninkovic, J. Oya, I. Paoletti, R. Paredes, J. M. Pasanen, M. Pascoli, D. Pauss, F. Pegna, R. G. Perez-Torres, M. A. Persic, M. Peruzzo, L. Prada, F. Prandini, E. Puchades, N. Raymers, A. Rhode, W. Ribo, M. Rico, J. Rissi, M. Robert, A. Ruegamer, S. Saggion, A. Saito, T. Y. Salvati, M. Sanchez-Conde, M. Sartori, P. Satalecka, K. Scalzotto, V. Scapin, V. Schweizer, T. Shayduk, M. Shinozaki, K. Shore, S. N. Sidro, N. Sierpowska-Bartosik, A. Sillanpaa, A. Sitarek, J. Sobczynska, D. Spanier, F. Stamerra, A. Stark, L. S. Takalo, L. Tavecchio, F. Temnikov, P. Tescaro, D. Teshima, M. Tluczykont, M. Torres, D. F. Turini, N. Vankov, H. Venturini, A. Vitale, V. Wagner, R. M. Wittek, W. Zabalza, V. Zandanel, F. Zanin, R. Zapatero, J. Acciari, V. Aliu, E. Arlen, T. Beilicke, M. Benbow, W. Bradbury, S. M. Buckley, J. H. Bugaev, V. Butt, Y. Byrum, K. Cannon, A. Cesarini, A. Chow, Y. C. Ciupik, L. Cogan, P. Colin, P. Cui, W. Daniel, M. K. Dickherber, R. Duke, C. Ergin, T. Fegan, S. J. Finley, J. P. Finnegan, G. Fortin, P. Furniss, A. Gall, D. Gillanders, G. H. Guenette, R. Gyuk, G. Grube, J. Hanna, D. Holder, J. Horan, D. Hui, C. M. Humensky, T. Brian Imran, A. Kaaret, P. Karlsson, N. Kertzman, M. Kieda, D. Kildea, J. Konopelko, A. Krawczynski, H. Krennrich, F. Lang, M. J. LeBohec, S. Maier, G. McCann, A. McCutcheon, M. Milovanovic, A. Moriarty, P. Nagai, T. Ong, R. A. Otte, A. N. Pandel, D. Perkins, J. S. Pichel, A. Pohl, M. Ragan, K. Reyes, L. C. Reynolds, P. T. Roache, E. Rose, H. J. Schroedter, M. Sembroski, G. H. Smith, A. W. Steele, D. Swordy, S. P. Theiling, M. Toner, J. A. Valcarcel, L. Varlotta, A. Wakely, S. P. Ward, J. E. Weekes, T. C. Weinstein, A. Williams, D. A. Wissel, S. Wood, M. Zitzer, B. CA AGILE Team GASP-WEBT Team MAGIC Collaboration VERITAS Collaboration TI THE JUNE 2008 FLARE OF MARKARIAN 421 FROM OPTICAL TO TeV ENERGIES SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE BL Lacertae objects: individual (Mrk 421); gamma rays: observations; galaxies: jets; radiation mechanisms: non-thermal; X-rays: galaxies ID BL-LACERTAE OBJECTS; X-RAY-SPECTRA; MAGIC TELESCOPE; LAC OBJECTS; GAMMA-RAYS; XMM-NEWTON; BLAZARS; WEBT; OUTBURST; CAMPAIGN AB We present optical, X-ray, high-energy ((sic) 30 GeV) and very high energy ((sic) 100 GeV; VHE) observations of the high-frequency peaked blazar Mrk 421 taken between 2008 May 24 and June 23. A high-energy gamma-ray signal was detected by AGILE with root TS = 4.5 between June 9 and 15, with F(E > 100 MeV) = 42(-12)(+14) x 10(-8) photons cm(-2) s(-1). This flaring state is brighter than the average flux observed by EGRET by a factor of similar to 3, but still consistent with the highest EGRET flux. In hard X-rays (20-60 keV) SuperAGILE resolved a five-day flare (June 9-15) peaking at similar to 55 mCrab. SuperAGILE, RXTE/ASM and Swift/BAT data show a correlated flaring structure between soft and hard X-rays. Hints of the same flaring behavior are also detected in the simultaneous optical data provided by the GASP-WEBT. A Swift/XRT observation near the flaring maximum revealed the highest 2-10 keV flux ever observed from this source, of 2.6 x 10(-9) erg cm(-2) s(-1) (i.e. > 100 mCrab). A peak synchrotron energy of similar to 3 keV was derived, higher than typical values of similar to 0.5-1 keV. VHE observations with MAGIC and VERITAS between June 6 and 8 showed the flux peaking in a bright state, well correlated with the X-rays. This extraordinary set of simultaneous data, covering a 12-decade spectral range, allowed for a deep analysis of the spectral energy distribution as well as of correlated light curves. 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[Cogan, P.; Guenette, R.; Hanna, D.; Maier, G.; McCann, A.; McCutcheon, M.; Valcarcel, L.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Colin, P.; Finnegan, G.; Hui, C. M.; Kieda, D.; LeBohec, S.] Univ Utah, Dept Phys, Salt Lake City, UT 84112 USA. [Cui, W.; Finley, J. P.; Gall, D.; Ragan, K.; Sembroski, G. H.; Varlotta, A.; Zitzer, B.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Duke, C.] Grinnell Coll, Dept Phys, Grinnell, IA 50112 USA. [Fortin, P.] Columbia Univ Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA. [Furniss, A.; Otte, A. N.; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Furniss, A.; Otte, A. N.; Williams, D. A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA. [Humensky, T. Brian; Swordy, S. P.; Wakely, S. P.; Wissel, S.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Imran, A.; Krennrich, F.; Nagai, T.; Pohl, M.; Schroedter, M.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Kaaret, P.; Pandel, D.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Kertzman, M.] Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA. [Konopelko, A.] Pittsburg State Univ, Dept Phys, Pittsburg, KS 66762 USA. [Reyes, L. C.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Reynolds, P. T.] Cork Inst Technol, Dept Appl Phys & Instumentat, Cork, Ireland. [Horan, D.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France. RP Donnarumma, I (reprint author), INAF IASF Roma, I-00133 Rome, Italy. EM immacolata.donnarumma@iasf-roma.inaf.it; villata@oato.inaf.it; raiteri@oato.inaf.it; cchsu@mpp.mpg.de; satalk@ifh.de; robert.wagner@mpp.mpg.de; jeffrey.grube@ucd.ie RI GAug, Markus/L-2340-2014; De Angelis, Alessandro/B-5372-2009; Mannheim, Karl/F-6705-2012; Morselli, Aldo/G-6769-2011; Doro, Michele/F-9458-2012; Lazzarotto, Francesco/J-4670-2012; Larionov, Valeri/H-1349-2013; Efimova, Natalia/I-2196-2013; Tjus, Julia/G-8145-2012; chilingarian, ashot/B-1901-2014; Kurtanidze, Omar/J-6237-2014; Rico, Javier/K-8004-2014; Fernandez, Ester/K-9734-2014; Lopez Moya, Marcos/L-2304-2014; Font, Lluis/L-4197-2014; Fernandez, Enrique/L-5387-2014; Moralejo Olaizola, Abelardo/M-2916-2014; Ribo, Marc/B-3579-2015; Trifoglio, Massimo/F-5302-2015; Antoranz, Pedro/H-5095-2015; Delgado, Carlos/K-7587-2014; Nieto, Daniel/J-7250-2015; Grishina, Tatiana/H-6873-2013; Miranda, Jose Miguel/F-2913-2013; Pittori, Carlotta/C-7710-2016; Contreras Gonzalez, Jose Luis/K-7255-2014; Maneva, Galina/L-7120-2016; Backes, Michael/N-5126-2016; Torres, Diego/O-9422-2016; Temnikov, Petar/L-6999-2016; Barrio, Juan/L-3227-2014; Cortina, Juan/C-2783-2017; Daniel, Michael/A-2903-2010; Fonseca Gonzalez, Maria Victoria/I-2004-2015; OI GAug, Markus/0000-0001-8442-7877; Morselli, Aldo/0000-0002-7704-9553; Doro, Michele/0000-0001-9104-3214; Larionov, Valeri/0000-0002-4640-4356; Efimova, Natalia/0000-0002-8071-4753; chilingarian, ashot/0000-0002-2018-9715; Rico, Javier/0000-0003-4137-1134; Lopez Moya, Marcos/0000-0002-8791-7908; Font, Lluis/0000-0003-2109-5961; Fernandez, Enrique/0000-0002-6405-9488; Moralejo Olaizola, Abelardo/0000-0002-1344-9080; Trifoglio, Massimo/0000-0002-2505-3630; Antoranz, Pedro/0000-0002-3015-3601; Delgado, Carlos/0000-0002-7014-4101; Nieto, Daniel/0000-0003-3343-0755; Grishina, Tatiana/0000-0002-3953-6676; Miranda, Jose Miguel/0000-0002-1472-9690; Pittori, Carlotta/0000-0001-6661-9779; Contreras Gonzalez, Jose Luis/0000-0001-7282-2394; Backes, Michael/0000-0002-9326-6400; Torres, Diego/0000-0002-1522-9065; Temnikov, Petar/0000-0002-9559-3384; Barrio, Juan/0000-0002-0965-0259; Cortina, Juan/0000-0003-4576-0452; Cattaneo, Paolo Walter/0000-0001-6877-6882; galli, marcello/0000-0002-9135-3228; Pacciani, Luigi/0000-0001-6897-5996; Costado, M. Teresa/0000-0002-2672-4061; Labanti, Claudio/0000-0002-5086-3619; LA BARBERA, ANTONINO/0000-0002-5880-8913; Cui, Wei/0000-0002-6324-5772; Feroci, Marco/0000-0002-7617-3421; Soffitta, Paolo/0000-0002-7781-4104; Picozza, Piergiorgio/0000-0002-7986-3321; Daniel, Michael/0000-0002-8053-7910; Cesarini, Andrea/0000-0002-8611-8610; leonardo, elvira/0000-0003-0271-7673; de los Reyes Lopez, Raquel/0000-0003-0485-9552; Villata, Massimo/0000-0003-1743-6946; Fuschino, Fabio/0000-0003-2139-3299; Fonseca Gonzalez, Maria Victoria/0000-0003-2235-0725; De Lotto, Barbara/0000-0003-3624-4480; Gianotti, Fulvio/0000-0003-4666-119X; Lazzarotto, Francesco/0000-0003-4871-4072; Costa, Enrico/0000-0003-4925-8523; Fiorini, Mauro/0000-0001-8297-1983; Bulgarelli, Andrea/0000-0001-6347-0649; Hsu, Ching-Cheng/0000-0001-9406-2023; giommi, paolo/0000-0002-2265-5003; trois, alessio/0000-0002-3180-6002; De Angelis, Alessandro/0000-0002-3288-2517; Donnarumma, Immacolata/0000-0002-4700-4549; Pellizzoni, Alberto Paolo/0000-0002-4590-0040; Persic, Massimo/0000-0003-1853-4900; Ward, John E/0000-0003-1973-0794; Caraveo, Patrizia/0000-0003-2478-8018; PREST, MICHELA/0000-0003-3161-4454; Verrecchia, Francesco/0000-0003-3455-5082; Marisaldi, Martino/0000-0002-4000-3789; Vercellone, Stefano/0000-0003-1163-1396; Spanier, Felix/0000-0001-6802-4744; Raiteri, Claudia Maria/0000-0003-1784-2784; Dominguez, Alberto/0000-0002-3433-4610; Otte, Adam Nepomuk/0000-0002-5955-6383; Bastieri, Denis/0000-0002-6954-8862; Ribo, Marc/0000-0002-9931-4557; MEREGHETTI, SANDRO/0000-0003-3259-7801; Pandel, Dirk/0000-0003-2085-5586; Lang, Mark/0000-0003-4641-4201; Tavani, Marco/0000-0003-2893-1459; Covino, Stefano/0000-0001-9078-5507; Bordas, Pol/0000-0002-0266-8536; Paredes, Josep M./0000-0002-1566-9044; Oya, Igor/0000-0002-3881-9324; Turini, Nicola/0000-0002-9395-5230; Bonnoli, Giacomo/0000-0003-2464-9077; Stamerra, Antonio/0000-0002-9430-5264; Prandini, Elisa/0000-0003-4502-9053 FU ASI [I/R/045/04, I/089/06/0, I/011/07/0]; Italian Ministry of University and Research [2005025417]; (ASDC) [I/024/05/1]; ETH Research [34/043]; Polish MNiSzW [N N203 390834]; Helmholtz Gemeinschaft; Georgian National Science Foundation [GNSF/ST07/4180]; NCS [96-2811-M-008-058]; U.S. Department of Energy; National Science Foundation; Smithsonian Institution; NSERC in Canada; Science Foundation Ireland; PPARC in the UK FX AGILE is a mission of ASI, with co-participation of INAF and INFN. This work was partially supported by ASI grants I/R/045/04, I/089/06/0, I/011/07/0 and by the Italian Ministry of University and Research (PRIN 2005025417), (ASDC) I/024/05/1. The MAGIC collaboration thanks the Instituto de Astrofisica de Canarias for the excellent working conditions at the Observatorio del Roque de Los Muchachos in La Palma and support by the German BMBF and MPG, the Italian INFN and Spanish MCINN is acknowledged. This work was supported by ETH Research Grant TH 34/043, by the Polish MNiSzW Grant N N203 390834, the YIP of the Helmholtz Gemeinschaft, the grant of Georgian National Science Foundation GNSF/ST07/4180. E. K. acknowledges financial support from the NCS grant No. 96-2811-M-008-058. The VERITAS collaboration is supported by grants from the U.S. Department of Energy, the National Science Foundation, and the Smithsonian Institution, by NSERC in Canada, Science Foundation Ireland, and PPARC in the UK. We acknowledge the technical support staff at the FLWO. We also acknowledge the Swift Team for carrying out the ToO observation. NR 49 TC 53 Z9 56 U1 1 U2 9 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JAN 20 PY 2009 VL 691 IS 1 BP L13 EP L19 DI 10.1088/0004-637X/691/1/L13 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 404JU UT WOS:000263148600004 ER PT J AU Patel, NA Young, KH Brunken, S Menten, KM Thaddeus, P Wilson, RW AF Patel, Nimesh A. Young, Ken H. Bruenken, Sandra Menten, Karl M. Thaddeus, Patrick Wilson, Robert W. TI DETECTION OF VIBRATIONALLY EXCITED CO IN IRC+10216 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE circumstellar matter; radio lines: stars; stars: individual (IRC+10216); stars: late-type; submillimeter ID LATE-TYPE STARS; MASER EMISSION; SIO MASERS; IRC &10216; EXCITATION; ENVELOPE; GHZ; C4H AB Using the Submillimeter Array we have detected the J = 3-2 and 2-1 rotational transitions from within the first vibrationally excited state of CO toward the extreme carbon star IRC+10216 (CW Leo). The emission remains spatially unresolved with an angular resolution of similar to 2 '' and, given that the lines originate from energy levels that are similar to 3100 K above the ground state, almost certainly originates from a much smaller (similar to 10(14) cm) sized region close to the stellar photosphere. Thermal excitation of the lines requires a gas density of similar to 10(9) cm(-3), about an order of magnitude higher than the expected gas density based on previous infrared observations and models of the inner dust shell of IRC+10216. C1 [Patel, Nimesh A.; Young, Ken H.; Bruenken, Sandra; Thaddeus, Patrick; Wilson, Robert W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bruenken, Sandra] Ecole Polytech Fed Lausanne, LCPM, SB ISIC, CH-1015 Lausanne, Switzerland. [Menten, Karl M.] Max Planck Inst Radio Astron, D-53121 Bonn, Germany. RP Patel, NA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM npatel@cfa.harvard.edu RI Brunken, Sandra/B-1880-2010; OI Brunken, Sandra/0000-0001-7175-4828; Wilson, Robert/0000-0001-5694-6725 NR 28 TC 11 Z9 11 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JAN 20 PY 2009 VL 691 IS 1 BP L55 EP L58 DI 10.1088/0004-637X/691/1/L55 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 404JU UT WOS:000263148600013 ER PT J AU Espino, CI Gomez, T Gonzalez, G do Santos, MFB Solano, J Sousa, O Moreno, N Windsor, D Ying, A Vilchez, S Osuna, A AF Espino, C. I. Gomez, T. Gonzalez, G. Brazil do Santos, M. F. Solano, J. Sousa, O. Moreno, N. Windsor, D. Ying, A. Vilchez, S. Osuna, A. TI Detection of Wolbachia Bacteria in Multiple Organs and Feces of the Triatomine Insect Rhodnius pallescens (Hemiptera, Reduviidae) SO APPLIED AND ENVIRONMENTAL MICROBIOLOGY LA English DT Article ID TRYPANOSOMA-CRUZI; ENDOSYMBIONT WOLBACHIA; LYMPHATIC FILARIASIS; SURFACE PROTEIN; TSETSE-FLY; WSP GENE; INFECTION; PCR; SEQUENCES; PIPIENTIS AB At least two types of Wolbachia bacteria were detected in wild and insectarium-raised Rhodnius pallescens, a natural vector of Trypanosoma cruzi and Trypanosoma rangeli. Wolbachia was detected in all the organs and tissues studied and in the feces, and this provided a methodological advantage for determining the presence of this endosymbiont in this host, obviating the need to kill the specimens. The occurrence of trypanosomatids in wild individuals was also studied. C1 [Gonzalez, G.; Brazil do Santos, M. F.; Solano, J.; Vilchez, S.; Osuna, A.] Univ Granada, Inst Biotechnol, Grp Bioquim & Parasitol Mol, E-18071 Granada, Spain. [Espino, C. I.; Gomez, T.; Gonzalez, G.; Sousa, O.; Moreno, N.; Ying, A.] Univ Panama, Fac Med, Dept Microbiol & Parasitol, Panama City, Panama. [Windsor, D.] Smithsonian Trop Res Inst, Panama City, Panama. RP Osuna, A (reprint author), Univ Granada, Inst Biotechnol, Grp Bioquim & Parasitol Mol, Campus Univ Fuentenueva, E-18071 Granada, Spain. EM aosuna@ugr.es RI Vilchez, Susana/L-9022-2014; Osuna, Antonio/H-1896-2015 OI Vilchez, Susana/0000-0003-3729-4113; FU Programa Ramon y Cajal (MEC, Spain, and EDRF, European Union); Spanish Agency for International Co-operation [A/5115/06, A/8187/07] FX Susana Vilchez received a grant from the Programa Ramon y Cajal (MEC, Spain, and EDRF, European Union). We thank the Spanish Agency for International Co-operation for covering the travel expenses of the research team (grants A/5115/06 and A/8187/07). NR 46 TC 12 Z9 13 U1 0 U2 12 PU AMER SOC MICROBIOLOGY PI WASHINGTON PA 1752 N ST NW, WASHINGTON, DC 20036-2904 USA SN 0099-2240 J9 APPL ENVIRON MICROB JI Appl. Environ. Microbiol. PD JAN 15 PY 2009 VL 75 IS 2 BP 547 EP 550 DI 10.1128/AEM.01665-08 PG 4 WC Biotechnology & Applied Microbiology; Microbiology SC Biotechnology & Applied Microbiology; Microbiology GA 390XT UT WOS:000262197700034 PM 19028913 ER PT J AU Latychev, K Mitrovica, JX Ishii, M Chan, NH Davis, JL AF Latychev, Konstantin Mitrovica, Jerry X. Ishii, Miaki Chan, Ngai-Ham Davis, James L. TI Body tides on a 3-D elastic earth: Toward a tidal tomography SO EARTH AND PLANETARY SCIENCE LETTERS LA English DT Article DE body tides; 3-D Earth models; seismic tomography ID MANTLE LATERAL VARIATIONS; ELASTOGRAVITATIONAL DEFORMATIONS; FREE OSCILLATIONS; PARAMETERS; MODEL AB The deformational and gravitational response of the Earth to the tide generating potential has generally involved I-D (i.e., depth varying) Earth models. Progressive improvement in observational constraints on body tides, generated from both ground and space-based surveys, suggests that an examination of the potential impact of lateral variations in Earth structure is warranted. We present a suite of predictions of the body tide response within the semi-diurnal. diurnal and long-period tidal bands computed using a finite-volume numerical code. The calculations adopt 3-D density and elastic structure taken from seismic inferences and, in a subset of the Calculations, dynamic topography on the surface and internal interfaces. We find that perturbations in the radial displacement and surface gravity within the semi-diurnal band reach similar to 1 mm and 0.15 mu gal, respectively. The perturbations in the diurnal band are comparable to these values, and within the long-period band they are a factor of 3-5 smaller. We also demonstrate that lateral variations in the elastic moduli, which have been ignored in recent work, contribute greater than 50% of the total perturbation. The level of perturbation associated with 3-D Structure exceeds the current observational uncertainty obtainable using space-geodetic methods, and this suggests the possibility of performing tidal tomographic inversions Of Such data. (c) 2008 Elsevier B.V. All rights reserved. C1 [Latychev, Konstantin; Mitrovica, Jerry X.; Chan, Ngai-Ham] Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada. [Ishii, Miaki] Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA. [Davis, James L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Mitrovica, JX (reprint author), Univ Toronto, Dept Phys, 60 St George St, Toronto, ON M5S 1A7, Canada. EM jxm@physics.utoronto.ca RI Davis, James/D-8766-2013 OI Davis, James/0000-0003-3057-477X FU CIFAR; NSERC; NSF [EAR-0809658]; NASA [NNX07AM77G] FX The MPI library used in this study was provided courtesy of the Argonne National Laboratory. Furthermore, we adopt the GMRES software package written by V. Fraysse, L. Giraud G S. Gratton, available from http://www.cerfacs.fr/algor/. We thank two anonymous reviewers for their constructive comments. We acknowledge support from CIFAR and NSERC (to KL and JXM), NSF Grant EAR-0809658 and NASA Grant NNX07AM77G OLD). NR 27 TC 19 Z9 20 U1 1 U2 8 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0012-821X EI 1385-013X J9 EARTH PLANET SC LETT JI Earth Planet. Sci. Lett. PD JAN 15 PY 2009 VL 277 IS 1-2 BP 86 EP 90 DI 10.1016/j.epsl.2008.10.008 PG 5 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 399PP UT WOS:000262812100010 ER PT J AU Beadell, JS Covas, R Gebhard, C Ishtiaq, F Melo, M Schmidt, BK Perkins, SL Graves, GR Fleischer, RC AF Beadell, Jon S. Covas, Rita Gebhard, Christina Ishtiaq, Farah Melo, Martim Schmidt, Brian K. Perkins, Susan L. Graves, Gaty R. Fleischer, Robert C. TI Host associations and evolutionary relationships of avian blood parasites from West Africa SO INTERNATIONAL JOURNAL FOR PARASITOLOGY LA English DT Article DE DHFR-TS; Haemoproteus; Host-specificity; Mitochondrial lineage; Plasmodium; Transferase ID B GENE-SEQUENCES; MALARIA PARASITES; MITOCHONDRIAL-DNA; REPRODUCTIVE EFFORT; BLUE TITS; PLASMODIUM; BIRDS; SPECIFICITY; PREVALENCE; PHYLOGENY AB The host specificity of blood parasites recovered from a survey of 527 birds in Cameroon and Gabon was examined at several levels within an evolutionary framework. Unique mitochondrial lineages of Haemoproteus were recovered from an average of 1.3 host species (maximum = 3) and 1.2 host families (maximum-3) while lineages of Plasmodium were recovered from an average of 2.5 species (maximum = 27) and 1.6 families (maximum = 9). Averaged within genera, lineages of both Plasmodium and Haemoproteus were constrained in their host distribution relative to random expectations. However, while several individual lineages within both genera exhibited significant host constraint. host breadth varied widely among related lineages, particularly within the genus Plasmodium. Several lineages of Plasmodium exhibited extreme generalist host-parasitism strategies while other lineages appeared to have been constrained to certain host families over recent evolutionary history. Sequence data from two nuclear genes recovered from a limited sample of Plasmodium parasites indicated that, at the resolution of this study, inferences regarding host breadth were unlikely to be grossly affected by the use of parasite mitochondrial lineages as a proxy for biological species. The use of divergent host-parasitism strategies among closely related parasite lineages suggests that host range is a relatively labile character. Since host specificity may also influence parasite virulence, these results argue for considering the impact of haematozoa on avian hosts on a lineage-specific basis. (c) 2008 Australian Society for Parasitology Inc. Published by Elsevier Ltd. All rights reserved. C1 [Beadell, Jon S.; Ishtiaq, Farah; Fleischer, Robert C.] Smithsonian Inst, Natl Zool Pk, Ctr Conservat & Evolutionary Genet, Washington, DC 20008 USA. [Covas, Rita; Melo, Martim] CNRS, CEFE, F-34293 Montpellier, France. [Gebhard, Christina; Schmidt, Brian K.; Graves, Gaty R.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20013 USA. [Perkins, Susan L.] Sackler Inst Comparat Genom, New York, NY 10024 USA. [Perkins, Susan L.] Amer Museum Nat Hist, Div Invertebrate Zool, New York, NY 10024 USA. RP Beadell, JS (reprint author), Yale Univ, Dept Ecol & Evolutionary Biol, ESC158b,21 Sachem St, New Haven, CT 06520 USA. EM jon.beadell@yale.edu RI Melo, Martim/L-7704-2013; OI Melo, Martim/0000-0003-1394-4361; Covas, Rita/0000-0001-7130-144X; Perkins, Susan/0000-0002-5400-5662 FU Shell Foundation; NIH [GM063258]; French Research Ministry; Alexander Wetmore Fund; Division of Birds, National Museum of Natural History,; Smithsonian Institution's Monitoring and Assessment of Biodiversity (SIMAB) FX We thank the governments of Cameroon and Gabon for allowing us to conduct our surveys and providing the necessary permits. Fieldwork in Cameroon and Gabon was only possible thanks to the support of Roger Fotso, Joe Mbelle, Okah Monya, Nohou Ndam, Francis Njie, Martin A.E. Ombenotori, Landry Tchignoumba, Patrice Christy and the staff of the Ipassa Research Station. We also thank Liliana Davalos, Eben Gering and jell Reed for help in the lab. MM was supported by a post-doctoral grant from the French Research Ministry. Fieldwork by CG and BS was supported by the Alexander Wetmore Fund of the Division of Birds, National Museum of Natural History, the Smithsonian Institution's Monitoring and Assessment of Biodiversity (SIMAB) program, Shell Gabon, and the Shell Foundation. Laboratory work was supported by NIH grant GM063258 to RCF. NR 43 TC 62 Z9 64 U1 2 U2 22 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0020-7519 J9 INT J PARASITOL JI Int. J. Parasit. PD JAN 15 PY 2009 VL 39 IS 2 BP 257 EP 266 DI 10.1016/j.ijpara.2008.06.005 PG 10 WC Parasitology SC Parasitology GA 398ZM UT WOS:000262770200014 PM 18713636 ER PT J AU Campbell, BA Hawke, BR Campbell, DB AF Campbell, Bruce A. Hawke, B. R. Campbell, Donald B. TI Surface morphology of domes in the Marius Hills and Mons Rumker regions of the Moon from Earth-based radar data SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID LAVA FLOW; WAVELENGTH RADAR; LUNAR; SCATTERING; ROUGHNESS; DEPOSITS; PLATEAU; TERRAIN; VENUS; TIO2 AB Clusters and coalesced complexes of domes represent a relatively rare landform within the extensive, low-relief, lunar maria. While they are typically spectroscopically similar to mare basalts emplaced by high-volume, low-viscosity eruptions, the large-scale morphology of the domes is more consistent with slower emplacement and/or more viscous magma. We use new Earth-based radar data to study the decimeter-to meter-scale rock abundance, at the surface and buried within the probing range of the radar signal, of domes in the Marius Hills and Mons Rumker regions. Domes of the Marius Hills are characterized by high circular polarization ratio (CPR) values at 12.6-cm and 70-cm wavelength, similar to the near-rim ejecta deposits of young lunar craters like Tycho, areas of large ejecta fragments near the rim of Meteor Crater, and blocky lavas such as SP flow in Arizona. We infer that a very rugged flow surface morphology, associated with the original dome-forming eruption rather than postemplacement modification, exists beneath at most a few meters of regolith. Magmas with greater silica content than sampled lunar basalts are unlikely, so the blocky structure of the dome-forming lava must arise from some combination of compositional change, effusion rate, and/or cooling effects not typically observed in basaltic landforms on the Earth. Much of the 80-km diameter Mons Rumker has low backscatter and CPR at 12.6-cm wavelength relative to nearby mare terrain. At 70-cm wavelength, the northern and most of the southern parts of the complex are radar dark, but there is a radar bright feature that extends from the central region eastward into Oceanus Procellarum. We conclude that much of Mons Rumker is mantled by rock-poor, fine-grained pyroclastic material; the radar bright feature in the 70-cm map is detectable owing to some combination of greater roughness ( like the Marius domes) and thinner mantling cover. C1 [Campbell, Bruce A.] Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. [Hawke, B. R.] Univ Hawaii, Sch Ocean & Earth Sci & Technol, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA. [Campbell, Donald B.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. RP Campbell, BA (reprint author), Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. FU NASA FX We thank two anonymous reviewers who provided helpful comments on the manuscript. This work was supported in part by a grant from NASA's Planetary Geology and Geophysics Program. The authors thank the staff at Arecibo Observatory and the Green Bank Telescope for invaluable assistance in collecting the lunar radar data. In particular, we thank F. Ghigo at the GBT and M. Nolan at Arecibo. J. Chandler of SAO provided ephemeris data for the observations. 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. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. NR 33 TC 20 Z9 20 U1 1 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD JAN 15 PY 2009 VL 114 AR E01001 DI 10.1029/2008JE003253 PG 10 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 396YP UT WOS:000262629000001 ER PT J AU Zimmermann, B Elsenbeer, H AF Zimmermann, Beate Elsenbeer, Helmut TI The near-surface hydrological consequences of disturbance and recovery: A simulation study SO JOURNAL OF HYDROLOGY LA English DT Article DE Hydrological flowpaths; Tropical montane rainforest; Saturated hydraulic conductivity; Disturbance and recovery; Landslides; Land use ID MONTANE RAIN-FOREST; SATURATED HYDRAULIC CONDUCTIVITY; OVERLAND-FLOW; SMALL CATCHMENTS; LAND MANAGEMENT; WATER BUDGETS; NEW-ZEALAND; SOIL; GENERATION; HILLSLOPE AB Changes in soil hydraulic properties following ecosystem disturbances can become relevant for regional water cycles depending on the prevailing rainfall regime. In a tropical montane rainforest ecosystem in southern Ecuador, plot-scale investigations revealed that man-made disturbances were accompanied by a decrease in mean saturated hydraulic conductivity (Ks), whereas mean Ks of two different aged landslides was undistinguishable from the reference forest. Ks spatial structure weakened after disturbances in the topsoil. We used this spatial-temporal information combined with local rain intensities to assess the probability of impermeable soil layers under undisturbed, disturbed, and regenerating land-cover types. We furthermore compared the Ecuadorian man-made disturbance cycle with a similar land-use sequence in a tropical lowland rainforest region in Brazil. The studied montane rainforest is characterized by prevailing vertical flowpaths in the topsoil, whereas larger rainstorms in the study area potentially result in impermeable layers below 20 cm depth. In spite of the low frequency of such higher-intensity events, they transport a high portion of the annual runoff and may therefore significant for the regional water cycle. Hydrological flowpaths under two studied landslides are similar to the natural forest except for a somewhat higher probability of impermeable layer formation in the topsoil of the 2-year-old landslide. In contrast, human disturbances likely affect near-surface hydrology. Under a pasture and a young fallow, impermeable layers potentially develop already in the topsoil for larger rain events. A 10-year-old fallow indicates regeneration towards the original vertical flowpaths, though the land-use signal was still detectable. The consequences of land-cover change on near-surface hydrological behaviour are of similar magnitude in the tropical montane and the lowland rainforest region. This similarity can be explained by a more pronounced drop of soil permeability after pasture establishment in the montane rainforest region in spite of the prevailing much lower rain intensities. (C) 2008 Elsevier B.V. All rights reserved. C1 [Zimmermann, Beate] Smithsonian Trop Res Inst, Balboa, Panama. [Zimmermann, Beate; Elsenbeer, Helmut] Univ Potsdam, Inst Geoecol, D-14476 Potsdam, Germany. RP Zimmermann, B (reprint author), Smithsonian Trop Res Inst, Balboa, Panama. EM ZimmermannB@si.edu RI Zimmermann, Beate/B-5164-2012 FU German Research Foundation (DFG) [FOR 402, TP B3, El 255/4-1]; Fundacion Cientifica San Francisco (Nature and Culture International (NCI) FX We thank the German Research Foundation (DFG) for funding the project (FOR 402, TP B3, El 255/4-1), the Fundacion Cientifica San Francisco (Nature and Culture International (NCI)) for providing the study area and the research station, our field assistants, T. Peters for providing climatic data, and P. Vorpahl for the information on average slopes. We greatly acknowledge the contributions of two anonymous reviewers. NR 45 TC 12 Z9 12 U1 2 U2 13 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0022-1694 J9 J HYDROL JI J. Hydrol. PD JAN 15 PY 2009 VL 364 IS 1-2 BP 115 EP 127 DI 10.1016/j.jhydrol.2008.10.016 PG 13 WC Engineering, Civil; Geosciences, Multidisciplinary; Water Resources SC Engineering; Geology; Water Resources GA 399HB UT WOS:000262789900011 ER PT J AU Reinert, JF AF Reinert, John F. TI Descriptions of Danielsia Theobald, a genus recently resurrected from synonymy (Diptera: Culicidae: Aedini), and its type species Dn. albotaeniata Leicester SO ZOOTAXA LA English DT Article DE Culicidae; Aedini; Danielsia; Dn. albotaeniata; Dn. harperi; Dn. lepchana; mosquitoes ID ALLIED TAXA DIPTERA; LIFE STAGES; MORPHOLOGICAL DATA; CLASSIFICATION; PHYLOGENY; OCHLEROTATUS; FINLAYA AB A detailed morphological description of the recently reestablished genus Danielsia and its type species, Dn. albotaeniata, are provided. An extensive list of previous literature pertaining to the genus is included. Genus Danielsia includes three species, Dn. albotaeniata, Dn. harperi and Dn. lepchana. Distribution, bionomics, distinguishing features of each life stage and background information for the genus are provided. C1 [Reinert, John F.] ARS, CMAVE, USDA, Gainesville, FL 32608 USA. [Reinert, John F.] Natl Museum Nat Hist, WRBU, Smithsonian Inst, Washington, DC 20560 USA. RP Reinert, JF (reprint author), ARS, CMAVE, USDA, 1600-1700 SW 23rd Dr, Gainesville, FL 32608 USA. EM John.Reinert@usda.ars.gov NR 70 TC 0 Z9 0 U1 0 U2 0 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD JAN 12 PY 2009 IS 1976 BP 25 EP 38 PG 14 WC Zoology SC Zoology GA 396ZP UT WOS:000262631800002 ER PT J AU Sale, SE Drew, JE Unruh, YC Irwin, MJ Knigge, C Phillipps, S Zijlstra, AA GAnsicke, BT Greimel, R Groot, PJ Mampaso, A Morris, RAH Napiwotzki, R Steeghs, D Walton, NA AF Sale, Stuart E. Drew, J. E. Unruh, Y. C. Irwin, M. J. Knigge, C. Phillipps, S. Zijlstra, A. A. GAnsicke, B. T. Greimel, R. Groot, P. J. Mampaso, A. Morris, R. A. H. Napiwotzki, R. Steeghs, D. Walton, N. A. TI High spatial resolution Galactic 3D extinction mapping with IPHAS SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: miscellaneous; surveys; stars: general; dust, extinction; ISM: structure; Galaxy: disc ID OLD OPEN CLUSTERS; FORNAX SPECTROSCOPIC SURVEY; INITIAL MASS FUNCTION; MILKY-WAY TOMOGRAPHY; H-ALPHA SURVEY; INTERSTELLAR EXTINCTION; SOLAR NEIGHBORHOOD; MODEL ATMOSPHERES; CHEMICAL EVOLUTION; REDDENING MATERIAL AB We present an algorithm ( MEAD, for 'Mapping Extinction Against Distance') which will determine intrinsic (r' - i') colour, extinction, and distance for early-A to K4 stars extracted from the IPHAS r'/ i'/H alpha photometric data base. These data can be binned up to map extinction in three dimensions across the northern Galactic plane. The large size of the IPHAS data base (similar to 200 million unique objects), the accuracy of the digital photometry it contains and its faint limiting magnitude (r' similar to 20) allow extinction to be mapped with fine angular (similar to 10 arcmin) and distance (similar to 0.1 kpc) resolution to distances of up to 10 kpc, outside the solar circle. High reddening within the solar circle on occasion brings this range down to similar to 2 kpc. The resolution achieved, both in angle and depth, greatly exceeds that of previous empirical 3D extinction maps, enabling the structure of the Galactic Plane to be studied in increased detail. MEAD accounts for the effect of the survey magnitude limits, photometric errors, unresolved interstellar medium (ISM) substructure and binarity. The impact of metallicity variations, within the range typical of the Galactic disc is small. The accuracy and reliability of MEAD are tested through the use of simulated photometry created with Monte Carlo sampling techniques. The success of this algorithm is demonstrated on a selection of fields and the results are compared to the literature. C1 [Sale, Stuart E.; Drew, J. E.; Unruh, Y. C.] Univ London Imperial Coll Sci Technol & Med, Astrophys Grp, Blackett Lab, London SW7 2AZ, England. [Drew, J. E.; Napiwotzki, R.] Univ Hertfordshire, STRI, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. [Irwin, M. J.; Walton, N. A.] Inst Astron, Cambridge CB3 0HA, England. [Knigge, C.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Phillipps, S.; Morris, R. A. H.] Univ Bristol, Dept Phys, Astrophys Grp, Bristol BS8 1TL, Avon, England. [Zijlstra, A. A.] Univ Manchester, Jodrell Bank, Ctr Astrophys, Manchester M13 9PL, Lancs, England. [GAnsicke, B. T.; Steeghs, D.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Greimel, R.] Karl Franzens Univ Graz, Inst Phys, A-8010 Graz, Austria. [Groot, P. J.] Radboud Univ Nijmegen, IMAPP, Dept Astrophys, NL-6500 GL Nijmegen, Netherlands. [Mampaso, A.] Inst Astrofis Canarias, E-38200 San Cristobal la Laguna, Santa Cruz Tene, Spain. [Steeghs, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Sale, SE (reprint author), Univ London Imperial Coll Sci Technol & Med, Astrophys Grp, Blackett Lab, Prince Consort Rd, London SW7 2AZ, England. EM s.sale06@imperial.ac.uk RI Sale, Stuart/E-1815-2010; Gaensicke, Boris/A-9421-2012; Steeghs, Danny/C-5468-2009; Groot, Paul/K-4391-2016; OI Phillipps, Steven/0000-0001-5991-3486; Gaensicke, Boris/0000-0002-2761-3005; Steeghs, Danny/0000-0003-0771-4746; Groot, Paul/0000-0002-4488-726X; Unruh, Yvonne/0000-0001-8217-6998; Sale, Stuart/0000-0003-2155-0995; Morris, Rhys/0000-0002-9210-1567; Drew, Janet/0000-0003-1192-7082 FU Science & Technology Facilities Council of the United Kingdom FX This research has made use of the VizieR catalogue access tool and the SIMBAD data base, both operated at CDS, Strasbourg, France. This research has made use of NASA's Astrophysics Data System Bibliographic Services NR 88 TC 50 Z9 51 U1 0 U2 1 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JAN 11 PY 2009 VL 392 IS 2 BP 497 EP 513 DI 10.1111/j.1365-2966.2008.14083.x PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 387WK UT WOS:000261982100001 ER PT J AU Bastian, N Gieles, M Ercolano, B Gutermuth, R AF Bastian, Nate Gieles, Mark Ercolano, Barbara Gutermuth, Rob TI The spatial evolution of stellar structures in the Large Magellanic Cloud SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE Magellanic Clouds; galaxies: star clusters; galaxies: structure ID HIERARCHICAL STAR-FORMATION; HUBBLE-SPACE-TELESCOPE; FRACTAL ANALYSIS; GAS EXPULSION; SCALE HEIGHT; CLUSTERS; GALAXY; ASSOCIATIONS; COMPLEXES; OBJECTS AB We present an analysis of the spatial distribution of various stellar populations within the Large Magellanic Cloud (LMC). We combine mid-infrared selected young stellar objects, optically selected samples with mean ages between similar to 9 and similar to 1000 Myr and existing stellar cluster catalogues to investigate how stellar structures form and evolve within the LMC. For the analysis we use Fractured Minimum Spanning Trees, the statistical Q parameter and the two-point correlation function. Restricting our analysis to young massive (OB) stars, we confirm our results obtained for M33, namely that the luminosity function of the groups is well described by a power law with index -2, and that there is no characteristic length-scale of star-forming regions. We find that stars in the LMC are born with a large amount of substructure, consistent with a two-dimensional fractal distribution with dimension similar to 1.8 and evolve towards a uniform distribution on a time-scale of similar to 175 Myr. This is comparable to the crossing time of the galaxy, and we suggest that stellar structure, regardless of spatial scale, will be eliminated in a crossing time. This may explain the smooth distribution of stars in massive/dense young clusters in the Galaxy, while other, less massive, clusters still display large amounts of structure at similar ages. By comparing the stellar and star cluster distributions and evolving time-scales, we show that infant mortality of clusters (or 'popping clusters') has a negligible influence on the galactic structure. Finally, we quantify the influence of the elongation, differential extinction and contamination of a population on the measured Q value. C1 [Bastian, Nate; Ercolano, Barbara] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Bastian, Nate] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Gieles, Mark] European So Observ, Santiago 19, Chile. [Ercolano, Barbara; Gutermuth, Rob] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Bastian, N (reprint author), Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. EM bastian@ast.cam.ac.uk OI Gieles, Mark/0000-0002-9716-1868 FU Harvard-Smithsonian Center for Astrophysics; [GO6-7008X]; [GO6-7009X] FX We gratefully thank Simon Goodwin for discussions and help with generating fractal distributions. We also thank Barbara Whitney for providing her list of YSO candidates before publication and Anil Seth for interesting discussions. The referee, Jason Harris, is thanked for helpful comments and suggestions on the text, techniques and results presented in this paper. NB gratefully acknowledges the support of the Harvard-Smithsonian Center for Astrophysics, where a large part of this work was carried out. BE was partially supported by Chandra grants GO6-7008X and GO6-7009X. NR 52 TC 64 Z9 64 U1 1 U2 2 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JAN 11 PY 2009 VL 392 IS 2 BP 868 EP 878 DI 10.1111/j.1365-2966.2008.14107.x PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 387WK UT WOS:000261982100027 ER PT J AU Miller-Ricci, E Seager, S Sasselov, D AF Miller-Ricci, Eliza Seager, Sara Sasselov, Dimitar TI THE ATMOSPHERIC SIGNATURES OF SUPER-EARTHS: HOW TO DISTINGUISH BETWEEN HYDROGEN-RICH AND HYDROGEN-POOR ATMOSPHERES SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; stars: individual (Gl 581) ID PLANET HD 189733B; EXTRASOLAR PLANET; GIANT PLANETS; TERRESTRIAL PLANETS; KEPLER MISSION; MASS; EMISSION; 209458B; TRANSIT; STAR AB Extrasolar super-Earths (1-10 M(circle plus)) are likely to exist with a wide range of atmospheres. Some super-Earths may be able to retain massive hydrogen-rich atmospheres. Others might never accumulate hydrogen or experience significant escape of lightweight elements, resulting in atmospheres more like those of the terrestrial planets in our solar system. We examine how an observer could differentiate between hydrogen-rich and hydrogen-poor atmospheres by modeling super-Earth emission and transmission spectra, and we find that discrimination is possible by observing the transmission spectrum alone. An Earth-like atmosphere, composed of mostly heavy elements and molecules, will have a very weak transmission signal due to its small atmospheric scale height (since the scale height is inversely proportional to molecular weight). However, a large hydrogen-rich atmosphere reveals a relatively large transmission signal. The super-Earth emission spectrum can additionally constrain the atmospheric composition and temperature structure. Super-Earths with massive hydrogen atmospheres will reveal strong spectral features due to water, whereas those that have lost most of their hydrogen (and have no liquid ocean) will be marked by CO(2) features and a lack of H(2)O. We apply our study specifically to the low-mass planet orbiting an M star, Gl 581c (M sin i = 5M(circle plus)), although our conclusions are relevant for super-Earths in general. The ability to distinguish hydrogen-rich atmospheres might be essential for interpreting mass and radius observations of planets in the transition between rocky super-Earths and Neptune-like planets. C1 [Miller-Ricci, Eliza; Sasselov, Dimitar] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Seager, Sara] MIT, Dept Phys, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. RP Miller-Ricci, E (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM emillerricci@cfa.harvard.edu NR 67 TC 97 Z9 97 U1 2 U2 9 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 2009 VL 690 IS 2 BP 1056 EP 1067 DI 10.1088/0004-637X/690/2/1056 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 398IX UT WOS:000262726900002 ER PT J AU Avalos, M Lizano, S Franco-Hernandez, R Rodriguez, LF Moran, JM AF Avalos, Martin Lizano, Susana Franco-Hernandez, Ramiro Rodriguez, Luis F. Moran, James M. TI HYPERCOMPACT H II REGIONS: RESOLVED IMAGES OF G34.26+0.15 A AND B SO ASTROPHYSICAL JOURNAL LA English DT Article DE H II regions; radiative transfer; radio continuum: ISM; stars: formation ID HII-REGIONS; G24.78+0.08 A1; STARS; PARAMETERS; CLOUDS; WINDS AB We report high angular resolution observations at lambda = 7 mm of the hypercompact (HC) H II regions G34.26+0.15 A and B. The images and the intensity profiles obtained give possible evidence of limb brightening, which may indicate the existence of inner "holes" in the ionized gas. These "holes" were previously inferred from a study of the spectra and angular sizes at different frequencies from lower angular resolution observations. Using a spherical ionized model bounded by an inner and an outer radii with an electron density gradient n(e) alpha r(-alpha), we can reproduce the 7 mm intensity profile, spectral energy distribution, and observed angular sizes of both sources. These models indicate inner radii R(1) similar to 400 AU, outer radii R(2) similar to 1000 AU, and shallow density gradients with slopes alpha similar to 0.3-1.0. These profiles are similar in physical size and shape to those found recently for the HC H II regions G24.78+0.08 A1 and G28.20-0.04N. Therefore, at least four HC H II regions seem to have thick shells of ionized gas with fractional widths, (R(2)-R(1))/R(2) similar to 0.1-0.6, in contrast with the thin ionized shells expected in the case of shells swept up by stellar winds. More observations are needed to determine the origin of these thick ionized shells and their frequency of occurrence in the HC H II region stage. C1 [Avalos, Martin; Lizano, Susana; Franco-Hernandez, Ramiro; Rodriguez, Luis F.] Univ Nacl Autonoma Mexico, Ctr Radioastron & Astrofis, Morelia 58089, Michoacan, Mexico. [Franco-Hernandez, Ramiro; Moran, James M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Avalos, M (reprint author), Univ Nacl Autonoma Mexico, Ctr Radioastron & Astrofis, Apdo Postal 72-3 Xangari, Morelia 58089, Michoacan, Mexico. EM m.avalos@astrosmo.unam.mx OI Moran, James/0000-0002-3882-4414 FU DGAPA/UNAM; CONACyT, Mexico FX M. A., S. L., and L. F. R. are grateful to DGAPA/UNAM and CONACyT, Mexico for their support. NR 18 TC 6 Z9 6 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 2009 VL 690 IS 2 BP 1084 EP 1088 DI 10.1088/0004-637X/690/2/1084 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 398IX UT WOS:000262726900005 ER PT J AU Salvato, M Hasinger, G Ilbert, O Zamorani, G Brusa, M Scoville, NZ Rau, A Capak, P Arnouts, S Aussel, H Bolzonella, M Buongiorno, A Cappelluti, N Caputi, K Civano, F Cook, R Elvis, M Gilli, R Jahnke, K Kartaltepe, JS Impey, CD Lamareille, F Le Floch, E Lilly, S Mainieri, V McCarthy, P McCracken, H Mignoli, M Mobasher, B Murayama, T Sasaki, S Sanders, DB Schiminovich, D Shioya, Y Shopbell, P Silverman, J Smolcic, V Surace, J Taniguchi, Y Thompson, D Trump, JR Urry, M Zamojski, M AF Salvato, M. Hasinger, G. Ilbert, O. Zamorani, G. Brusa, M. Scoville, N. Z. Rau, A. Capak, P. Arnouts, S. Aussel, H. Bolzonella, M. Buongiorno, A. Cappelluti, N. Caputi, K. Civano, F. Cook, R. Elvis, M. Gilli, R. Jahnke, K. Kartaltepe, J. S. Impey, C. D. Lamareille, F. Le Floch, E. Lilly, S. Mainieri, V. McCarthy, P. McCracken, H. Mignoli, M. Mobasher, B. Murayama, T. Sasaki, S. Sanders, D. B. Schiminovich, D. Shioya, Y. Shopbell, P. Silverman, J. Smolcic, V. Surace, J. Taniguchi, Y. Thompson, D. Trump, J. R. Urry, M. Zamojski, M. TI PHOTOMETRIC REDSHIFT AND CLASSIFICATION FOR THE XMM-COSMOS SOURCES SO ASTROPHYSICAL JOURNAL LA English DT Article DE catalogs; galaxies: active; methods: miscellaneous ID WIDE-FIELD SURVEY; SPITZER MIDINFRARED SPECTROSCOPY; INFRARED LUMINOUS GALAXIES; EVOLUTION SURVEY COSMOS; ACTIVE GALACTIC NUCLEI; STAR-FORMING GALAXIES; DIGITAL SKY SURVEY; BLACK-HOLE MASS; X-RAY DATA; DEEP FIELD AB We present photometric redshifts and spectral energy distribution (SED) classifications for a sample of 1542 optically identified sources detected with XMM in the COSMOS field. Our template fitting classifies 46 sources as stars and 464 as nonactive galaxies, while the remaining 1032 require templates with an active galactic nucleus (AGN) contribution. High accuracy in the derived photometric redshifts was accomplished as the result of (1) photometry in up to 30 bands with high-significance detections, (2) a new set of SED templates, including 18 hybrids covering the far-UV to mid-infrared, which have been constructed by the combination of AGNs and nonactive galaxies templates, and (3) multiepoch observations that have been used to correct for variability (most important for type 1 AGNs). The reliability of the photometric redshifts is evaluated using the subsample of 442 sources with measured spectroscopic redshifts. We achieved an accuracy of sigma(Delta z/(1+zspec)) = 0.014 for i(AB)* < 22.5 (sigma(Delta z/(1+zspec)) similar to 0.015 for i(AB)* < 24.5). The high accuracies were accomplished for both type 2 (where the SED is often dominated by the host galaxy) and type 1 AGNs and QSOs out to z = 4.5. The number of outliers is a large improvement over previous photometric redshift estimates for X-ray-selected sources (4.0% and 4.8% outliers for i(AB)* < 22.5 and i(AB)* < 24.5, respectively). We show that the intermediate band photometry is vital to achieving accurate photometric redshifts for AGNs, whereas the broad SED coverage provided by mid-infrared (Spitzer/IRAC) bands is important to reduce the number of outliers for normal galaxies. C1 [Salvato, M.; Scoville, N. Z.; Rau, A.; Capak, P.; Cook, R.; Shopbell, P.; Smolcic, V.] CALTECH, Pasadena, CA 91125 USA. [Hasinger, G.; Brusa, M.; Buongiorno, A.; Cappelluti, N.; Lamareille, F.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Hasinger, G.; Ilbert, O.; Kartaltepe, J. S.; Le Floch, E.; Sanders, D. B.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Zamorani, G.; Bolzonella, M.; Gilli, R.; Mignoli, M.; Schiminovich, D.] Osservatorio Astron Bologna, INAF, I-40127 Bologna, Italy. [Capak, P.; Surace, J.; Zamojski, M.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Arnouts, S.] Canada France Hawaii Telescope Corp, Kamuela, HI 96743 USA. [Aussel, H.] Univ Paris Diderot, CNRS, CEA, DSM,DAPNIA SAp, F-91191 Gif Sur Yvette, France. [Caputi, K.; Lilly, S.; Silverman, J.] ETH, Dept Phys, CH-8093 Zurich, Switzerland. [Civano, F.; Elvis, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Cook, R.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Cook, R.] Brown Univ, Dept Phys, Providence, RI 02912 USA. [Jahnke, K.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Impey, C. D.; Trump, J. R.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Mainieri, V.] European So Observ, D-85748 Garching, Germany. [McCarthy, P.] Carnegie Observ, Pasadena, CA 91101 USA. [McCracken, H.] Univ Paris 06, CNRS, UMR 7095, Inst Astrophys Paris, F-75014 Paris, France. [Mobasher, B.] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA. [Murayama, T.] Tohoku Univ, Grad Sch Sci, Astron Inst, Aoba Ku, Sendai, Miyagi 9808578, Japan. [Sasaki, S.] Ehime Univ, Grad Sch Sci & Engn, Dept Phys, Matsuyama, Ehime 7908577, Japan. [Shioya, Y.; Taniguchi, Y.] Ehime Univ, Res Ctr Space & Cosm Evolut, Matsuyama, Ehime 7908577, Japan. [Thompson, D.] Univ Arizona, LBT Observ, Tucson, AZ 85721 USA. [Urry, M.] Yale Univ, Dept Phys, New Haven, CT 06520 USA. [Zamojski, M.] Columbia Univ, Dept Astron, New York, NY 10027 USA. RP Salvato, M (reprint author), CALTECH, MC 105-24,1200 E Calif Blvd, Pasadena, CA 91125 USA. RI Bolzonella, Micol/O-9495-2015; Mignoli, Marco/O-9426-2015; Gilli, Roberto/P-1110-2015; OI Bolzonella, Micol/0000-0003-3278-4607; Mignoli, Marco/0000-0002-9087-2835; Gilli, Roberto/0000-0001-8121-6177; Cook, Richard/0000-0002-1628-6555; Cappelluti, Nico/0000-0002-1697-186X; Jahnke, Knud/0000-0003-3804-2137; Zamorani, Giovanni/0000-0002-2318-301X; Urry, Meg/0000-0002-0745-9792; Brusa, Marcella/0000-0002-5059-6848 FU German Deutsche Forschungsgemeinschaft, DFG [FKZ HA 1850/28-1]; NASA [GO7-8136A] FX We gratefully acknowledge the contributions of the entire COSMOS collaboration consisting of more than 100 scientists. More information on the COSMOS survey is available at http://www.astro.caltech.edu/cosmos. We acknowledge the anonymous referee for helpful comments that improved the paper. We also acknowledge the hospitality of the Institute for Astronomy, Hawaii, and the support of the Aspen Center for Physics where the work started and the manuscript was completed. G. H. acknowledges support by the German Deutsche Forschungsgemeinschaft, DFG Leibniz Prize (FKZ HA 1850/28-1). This work was supported in part by NASA Grant GO7-8136A. NR 53 TC 183 Z9 183 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 2009 VL 690 IS 2 BP 1250 EP 1263 DI 10.1088/0004-637X/690/2/1250 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 398IX UT WOS:000262726900019 ER PT J AU DeForest, CE Martens, PCH Wills-Davey, MJ AF DeForest, C. E. Martens, P. C. H. Wills-Davey, M. J. TI SOLAR CORONAL STRUCTURE AND STRAY LIGHT IN TRACE SO ASTROPHYSICAL JOURNAL LA English DT Article DE instrumentation: miscellaneous; Sun: corona; Sun: UV radiation ID POINT-SPREAD FUNCTION; TRANSITION-REGION; ACTIVE-REGION; TELESCOPE; EXPLORER; YOHKOH; SUN AB Using the 2004 Venus transit of the Sun to constrain a semiempirical point-spread function (PSF) for the TRACE EUV solar telescope, we have measured the effect of stray light in that telescope. We find that 43% of 171 angstrom EUV light that enters TRACE is scattered, either through diffraction off the entrance filter grid or through other nonspecular effects. We carry this result forward, via known-PSF deconvolution of TRACE images, to identify its effect on analysis of TRACE data. Known-PSF deconvolution by this derived PSF greatly reduces the effect of visible haze in the TRACE 171 angstrom images, enhances bright features, and reveals that the smooth background component of the corona is considerably less bright (and hence more rarefied) than might otherwise be supposed. Deconvolution reveals that some prior conclusions about the Sun appear to have been based on stray light in the images. In particular, the diffuse background "quiet corona" becomes consistent with hydrostatic support of the coronal plasma; feature contrast is greatly increased, possibly affecting derived parameters such as the form of the coronal heating function; and essentially all existing differential emission measure studies of small features appear to be affected by contamination from nearby features. We speculate on further implications of stray light for interpretation of EUV images from TRACE and similar instruments, and advocate deconvolution as a standard tool for image analysis with future instruments. C1 [DeForest, C. E.] SW Res Inst, Boulder, CO 80302 USA. [Martens, P. C. H.; Wills-Davey, M. J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP DeForest, CE (reprint author), SW Res Inst, 1050 Walnut St,Suite 300, Boulder, CO 80302 USA. EM deforest@boulder.swri.edu FU NASA's SHPSRT program FX available to everyone. We also thank L. Golub, J. Cirtain, K. Schrijver, and H. Throop for illuminating discussions, and the anonymous referee for several suggestions that improved the work. SOHO is a project of international cooperation between NASA and ESA. This work was funded under NASA's SHPSR&T program. NR 23 TC 30 Z9 30 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 2009 VL 690 IS 2 BP 1264 EP 1271 DI 10.1088/0004-637X/690/2/1264 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 398IX UT WOS:000262726900020 ER PT J AU Shporer, A Bakos, GA Bouchy, F Pont, F Kovacs, G Latham, DW Sipocz, B Torres, G Mazeh, T Esquerdo, GA Pal, A Noyes, RW Sasselov, DD Lazar, J Papp, I Sari, P Kovacs, G AF Shporer, Avi Bakos, GAspAr A. Bouchy, Francois Pont, Frederic Kovacs, Geza Latham, Dave W. Sipoecz, Brigitta Torres, Guillermo Mazeh, Tsevi Esquerdo, Gilbert A. Pal, Andras Noyes, Robert W. Sasselov, Dimitar D. Lazar, Jozsef Papp, Istvan Sari, Pal Kovacs, Gabor TI HAT-P-9b: A LOW-DENSITY PLANET TRANSITING A MODERATELY FAINT F STAR SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; stars: individual (GSC 02463-00281, HAT-P-9) ID LIGHT-CURVE PROJECT; STELLAR ATMOSPHERE MODELS; EXTRASOLAR GIANT PLANETS; LIMB-DARKENING LAW; SURFACE GRAVITIES; HOT JUPITERS; T-EFF; EXOPLANET; RADIUS; PARAMETERS AB We report the discovery of a planet transiting a moderately faint (V = 12.3 mag) late F star, with an orbital period of 3.92289 +/- 0.00004 days. From the transit light curve and radial velocity measurements, we determine that the radius of the planet is R(p) = 1.40 +/- 0.06 R(Jup) and that the mass is M(p) = 0.78 +/- 0.09 M(Jup). The density of the new planet, rho(p) = 0.35 +/- 0.06 g cm(-3), fits to the low-density tail of the currently known transiting planets. We find that the center of transit is at T(c) = 2454417.9077 +/- 0.0003 (HJD), and the total transit duration is 0.143 +/- 0.004 days. The host star has M(*) = 1.28 +/- 0.13 M(circle dot) and R(*) = 1.32 +/- 0.07 R(circle dot). C1 [Shporer, Avi; Mazeh, Tsevi] Tel Aviv Univ, Wise Observ, IL-69978 Tel Aviv, Israel. [Bakos, GAspAr A.; Latham, Dave W.; Sipoecz, Brigitta; Torres, Guillermo; Esquerdo, Gilbert A.; Pal, Andras; Noyes, Robert W.; Sasselov, Dimitar D.; Kovacs, Gabor] Harvard Smithsonian Ctr Astrophys CfA, Cambridge, MA 02138 USA. [Bouchy, Francois] Inst Astrophys, F-75014 Paris, France. [Pont, Frederic] Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England. [Kovacs, Geza] Konkoly Observ Budapest, H-1125 Budapest, Hungary. [Sipoecz, Brigitta; Pal, Andras] Eotvos Lorand Univ, Dept Astron, H-1518 Budapest, Hungary. [Esquerdo, Gilbert A.] Planetary Sci Inst, Tucson, AZ 85705 USA. [Lazar, Jozsef; Papp, Istvan; Sari, Pal] Hungarian Astron Assoc, H-1461 Budapest, Hungary. RP Shporer, A (reprint author), Tel Aviv Univ, Wise Observ, IL-69978 Tel Aviv, Israel. EM shporer@wise.tau.ac.il NR 55 TC 30 Z9 30 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 2009 VL 690 IS 2 BP 1393 EP 1400 DI 10.1088/0004-637X/690/2/1393 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 398IX UT WOS:000262726900033 ER PT J AU Wagner, AY Lee, JJ Raymond, JC Hartquist, TW Falle, SAEG AF Wagner, A. Y. Lee, J. -J. Raymond, J. C. Hartquist, T. W. Falle, S. A. E. G. TI A COSMIC-RAY PRECURSOR MODEL FOR A BALMER-DOMINATED SHOCK IN TYCHO'S SUPERNOVA REMNANT SO ASTROPHYSICAL JOURNAL LA English DT Review DE acceleration of particles; hydrodynamics; line: profiles; methods: numerical; shock waves; supernova remnants ID HIGH-RESOLUTION SPECTROSCOPY; MODIFIED RADIATIVE SHOCKS; TIME-DEPENDENT EVOLUTION; PARTICLE-ACCELERATION; MAGNETIC-FIELD; CYGNUS LOOP; 2-FLUID MODELS; CASSIOPEIA-A; HYDRODYNAMIC APPROACH; ASTROPHYSICAL SHOCKS AB We present a time-dependent cosmic-ray (CR) modified shock model for which the calculated Ha emissivity profile agrees well with the Ha flux increase ahead of the Balmer-dominated shock at knot g in Tycho's supernova remnant (SNR), observed by Lee et al. The backreaction of the CR component on the thermal component is treated in the two-fluid approximation, and we include thermal particle injection and energy transfer due to the acoustic instability in the precursor. The transient state of our model that describes the current state of the shock at knot g occurs during the evolution from a thermal gas dominated shock to a smooth CR-dominated shock. Assuming a distance of 2.3 kpc to Tycho's remnant, we obtain values for the CR diffusion coefficient,., the injection parameter, epsilon, and the timescale for the energy transfer, tau, of kappa= 2 x 10(24) cm(2) s(-1), epsilon = 4.2 x 10(-3), and tau = 426 yr, respectively. We have also studied the parameter space for fast ( 300 km s(-1) less than or similar to vs less than or similar to 3000 km s- 1), time-asymptotically steady shocks and have identified a branch of solutions, for which the temperature in the CR precursor typically reaches 2 x 10(4) to 6 x 10(4) K and the bulk acceleration of the flow through the precursor is less than 10 km s(-1). These solutions fall into the low CR acceleration efficiency regime and are relatively insensitive to shock parameters. This low CR acceleration efficiency branch of solutions may provide a natural explanation for the line broadening of the Ha narrow component observed in nonradiative shocks in many SNRs. C1 [Lee, J. -J.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Raymond, J. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Wagner, A. Y.; Hartquist, T. W.; Falle, S. A. E. G.] Univ Leeds, Sch Phys & Astron, Leeds LS3 1NS, W Yorkshire, England. RP Wagner, AY (reprint author), Australian Natl Univ, Mt Stromlo & Siding Spring Observ, Cotter Rd, Weston, ACT 2611, Australia. EM ayw@ast.leeds.ac.uk OI Wagner, Alexander/0000-0002-5104-6434 FU HST [GO-10577] FX The authors thank the referee for carefully reviewing the manuscript and providing feedback that has led to a substantial improvement of the paper. A. Y. W is grateful for financial support from the Smithsonian Institution Scholarly Studies Fund, and the hospitality during the course of this work at the CfA. This work was funded by the HST grant number GO-10577 to the Smithsonian Institution. NR 103 TC 20 Z9 20 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 2009 VL 690 IS 2 BP 1412 EP 1423 DI 10.1088/0004-637X/690/2/1412 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 398IX UT WOS:000262726900035 ER PT J AU Chakrabarti, S Whitney, BA AF Chakrabarti, Sukanya Whitney, Barbara A. TI PANCHROMATIC SPECTRAL ENERGY DISTRIBUTIONS OF DUSTY GALAXIES WITH RADISHE. I. PREDICTIONS FOR HERSCHEL: CORRELATING COLORS WITH GALACTIC ENERGY SOURCES SO ASTROPHYSICAL JOURNAL LA English DT Review DE galaxies: active; galaxies: formation; infrared: galaxies; radiative transfer; stars: formation ID ULTRALUMINOUS INFRARED GALAXIES; CARLO RADIATIVE-TRANSFER; YOUNG STELLAR OBJECTS; PARTICLE HYDRODYNAMICS SIMULATIONS; MODEL SCATTERING ENVELOPES; QUASAR LUMINOSITY FUNCTION; SPITZER-SPACE-TELESCOPE; GIANT MOLECULAR CLOUDS; MU-M OBSERVATIONS; X-RAY-EMISSION AB We present three-dimensional, self-consistent radiative transfer solutions with a new Monte Carlo radiative equilibrium code. The code RADISHE can be applied to calculate the emergent spectral energy distributions (SEDs) and broadband images from optical to millimeter wavelengths of arbitrary density geometries with distributed sources of radiation. One of the primary uses of this code has been to interface with hydrodynamical codes to calculate emergent SEDs along a simulation time sequence. We focus the applications of this code in this paper on infrared bright dusty galaxies, but RADISHE is also ideal for calculating emission from star clusters or protostellar environments. The primary methodological focus of this paper is on the radiative equilibrium temperature calculation. We find that an iterative calculation of the temperature, which takes the sum of photon flight paths as the Monte Carlo estimator for the mean free intensity, is significantly faster than relaxation temperature calculation methods, particularly when large numbers of grid cells are required (i.e., in modeling three-dimensional geometries such as the dust envelopes of turbulent massive protostellar cores or infrared-bright galaxies). An accurate long-wavelength SED and corresponding temperature calculation will be essential for analyzing upcoming Herschel Space Observatory observations. We present simulated color-color plots for infrared-bright galaxies at a range of redshifts, and unfold these plots as color versus the fractional active galactic nucleus (AGN) luminosity, to demonstrate that Herschel will be able to effectively discriminate between submillimeter galaxies, where the energy source is dominated by AGN, and those where star formation dominates. We demarcate in particular the "Class II" or energetically active AGN evolutionary phase in Herschel color-color plots. C1 [Chakrabarti, Sukanya] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Whitney, Barbara A.] Space Sci Inst, Boulder, CO 80301 USA. RP Chakrabarti, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM schakrabarti@cfa.harvard.edu; bwhitney@spacescience.org NR 106 TC 20 Z9 20 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 2009 VL 690 IS 2 BP 1432 EP 1451 DI 10.1088/0004-637X/690/2/1432 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 398IX UT WOS:000262726900037 ER PT J AU Hollenbach, D Kaufman, MJ Bergin, EA Melnick, GJ AF Hollenbach, David Kaufman, Michael J. Bergin, Edwin A. Melnick, Gary J. TI WATER, O-2, AND ICE IN MOLECULAR CLOUDS SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; ISM: abundances; ISM: lines and bands; ISM: molecules ID DENSE INTERSTELLAR CLOUDS; WAVE-ASTRONOMY-SATELLITE; RHO-OPHIUCHI CLOUD; LINE-OF-SIGHT; PHOTODISSOCIATION REGIONS; PHOTOIONIZATION RATES; MAPPING OBSERVATIONS; RATE COEFFICIENTS; PRESTELLAR CORES; CHEMICAL-MODELS AB We model the temperature and chemical structure of molecular clouds as a function of depth into the cloud, assuming a cloud of constant density n illuminated by an external far-ultraviolet (FUV; 6 eV < h nu < 13.6 eV) flux G(0) (scaling factor in multiples of the local interstellar field). Extending previous photodissociation region (PDR) models, we include the freezing of species, simple grain surface chemistry, and desorption (including FUV photodesorption) of ices. We also treat the opaque cloud interior with time-dependent chemistry. Here, under certain conditions, gas-phase elemental oxygen freezes out as water ice and the elemental C/O abundance ratio can exceed unity, leading to complex carbon chemistry. Gas-phase H2O and O-2 peak in abundance at intermediate depth into the cloud, roughly A(V) similar to 3 - 8 from the surface, the depth proportional to in(G(0)/n). Closer to the surface, molecules are photodissociated. Deeper into the cloud, molecules freeze to grain surfaces. At intermediate depths, PDRs are attenuated by dust extinction, but photodesorption prevents total freeze-out. For G(0) < 500, abundances of H2O and O-2 peak at values similar to 10(-7), producing columns similar to 10(15) cm(-2), independent of G(0) and n. The peak abundances depend primarily on the product of the photodesorption yield of water ice and the grain surface area per H nucleus. At higher values of G(0), thermal desorption of O atoms from grains slightly enhances the gas-phase H2O peak abundance and column, whereas the gas-phase O-2 peak abundance rises to similar to 10(-5) and the column to similar to 2 x 10(16) cm(-2). We present simple analytical equations for the abundances as a function of depth, which clarify the dependence on parameters. The models are applied to observations of H2O, O-2, andwater ice in a number of sources, including B68, NGC 2024, and rho Oph. C1 [Hollenbach, David; Kaufman, Michael J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Kaufman, Michael J.] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA. [Bergin, Edwin A.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Melnick, Gary J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Hollenbach, D (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM dhollenbach@seti.org NR 86 TC 166 Z9 166 U1 2 U2 16 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 2009 VL 690 IS 2 BP 1497 EP 1521 DI 10.1088/0004-637X/690/2/1497 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 398IX UT WOS:000262726900041 ER PT J AU Backman, D Marengo, M Stapelfeldt, K Su, K Wilner, D Dowell, CD Watson, D Stansberry, J Rieke, G Megeath, T Fazio, G Werner, M AF Backman, D. Marengo, M. Stapelfeldt, K. Su, K. Wilner, D. Dowell, C. D. Watson, D. Stansberry, J. Rieke, G. Megeath, T. Fazio, G. Werner, M. TI EPSILON ERIDANI'S PLANETARY DEBRIS DISK: STRUCTURE AND DYNAMICS BASED ON SPITZER AND CALTECH SUBMILLIMETER OBSERVATORY OBSERVATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; infrared: stars; planetary systems; stars: individual (epsilon Eridani) ID MULTIBAND IMAGING PHOTOMETER; VEGA-LIKE STARS; EDGEWORTH-KUIPER BELT; INFRARED ARRAY CAMERA; SOLAR-TYPE STARS; ABSOLUTE CALIBRATION; SPACE-TELESCOPE; MU-M; SUBSTELLAR COMPANIONS; GIANT PLANETS AB Spitzer and Caltech Submillimeter Observatory images and spectrophotometry of epsilon Eridani at wavelengths from 3.5 to 350 mu m reveal new details of its bright debris disk. The 350 mu m map confirms the presence of a ring at r = 11 '' - 28 ''(35-90 AU), observed previously at longer sub-mm wavelengths. The Spitzer mid-IR and far-IR images do not show the ring, but rather a featureless disk extending from within a few arcsec of the star across the ring to r similar to 34 '' (110 AU). The spectral energy distribution (SED) of the debris system implies a complex structure. A model constrained by the surface brightness profiles and the SED indicates that the sub-mm ring emission is primarily from large (a similar to 135 mu m) grains, with smaller (a similar to 15 mu m) grains also present in and beyond the ring. The Spitzer Infrared Spectrograph and Multiband Imaging Photometer for Spitzer SED-mode spectrophotometry data clearly show the presence of spatially compact excess emission at lambda greater than or similar to 15 mu m that requires the presence of two additional narrow belts of dust within the sub-mm ring's central void. The innermost belt at r similar to 3 AU is composed of silicate dust. A simple dynamical model suggests that dust produced collisionally by a population of about 11 M(circle plus) of planetesimals in the sub-mm ring could be the source of the emission from both in and beyond the sub- mm ring. Maintaining the inner belts and the inner edge to the sub-mm ring may require the presence of three planets in this system including the candidate radial velocity object. C1 [Backman, D.] Stratospher Observ Infrared Astron, Mountain View, CA 94043 USA. [Backman, D.] SETI Inst, Mountain View, CA 94043 USA. [Marengo, M.; Wilner, D.; Megeath, T.; Fazio, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Stapelfeldt, K.; Dowell, C. D.; Werner, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Su, K.; Stansberry, J.; Rieke, G.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Watson, D.] Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. RP Backman, D (reprint author), Stratospher Observ Infrared Astron, 515 N Whisman Rd, Mountain View, CA 94043 USA. RI Stapelfeldt, Karl/D-2721-2012; OI Su, Kate/0000-0002-3532-5580 NR 71 TC 73 Z9 74 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 2009 VL 690 IS 2 BP 1522 EP 1538 DI 10.1088/0004-637/690/2/1522 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 398IX UT WOS:000262726900042 ER PT J AU Brown, WR Geller, MJ Kenyon, SJ AF Brown, Warren R. Geller, Margaret J. Kenyon, Scott J. TI MMT HYPERVELOCITY STAR SURVEY SO ASTROPHYSICAL JOURNAL LA English DT Article DE Galaxy: center; Galaxy: halo; Galaxy: kinematics and dynamics; Galaxy: stellar content; stars: early-type ID HORIZONTAL-BRANCH STARS; MASSIVE BLACK-HOLE; LARGE-MAGELLANIC-CLOUD; DIGITAL SKY SURVEY; A-TYPE STARS; F-DWARF MEMBERS; GALACTIC-CENTER; MILKY-WAY; CHEMICAL ABUNDANCES; STELLAR ENVIRONMENT AB We describe a new survey for unbound hypervelocity stars (HVSs), stars traveling with such extreme velocities that dynamical ejection from a massive black hole is their most likely origin. We investigate the possible contribution of unbound runaway stars, and show that the physical properties of binaries constrain low-mass runaways to bound velocities. We measure radial velocities for HVS candidates with the colors of early A-type and late B-type stars. We report the discovery of six unbound HVSs with velocities and distances exceeding the conservative escape velocity estimate of Kenyon and collaborators. We additionally report four possibly unbound HVSs with velocities and distances exceeding the lower escape velocity estimate of Xue and collaborators. These discoveries increase the number of unbound HVSs by 60%-100%. Other survey objects include 19 newly identified z similar to 2.4 quasars. One of the HVSs may be a horizontal branch star, consistent with the number of evolved HVSs predicted by Galactic center ejection models. Finding more evolved HVSs will one day allow a probe of the low-mass regime of HVSs and will constrain the mass function of stars in the Galactic center. RP Brown, WR (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM wbrown@cfa.harvard.edu; mgeller@cfa.harvard.edu; skenyon@cfa.harvard.edu OI Kenyon, Scott/0000-0003-0214-609X FU Smithsonian Institution FX We thank M. Alegria and A. Milone for their assistance with observations obtained at the MMT Observatory, a joint facility of the Smithsonian Institution and the University of Arizona. This project makes use of data products from the SDSS, which is managed by the Astrophysical Research Consortium for the Participating Institutions. This research makes use of NASA's Astrophysics Data System Bibliographic Services. This work was supported by the Smithsonian Institution. NR 93 TC 63 Z9 64 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 2009 VL 690 IS 2 BP 1639 EP 1647 DI 10.1088/0004-637X/690/2/1639 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 398IX UT WOS:000262726900051 ER PT J AU Rathborne, JM Lada, CJ Walsh, W Saul, M Butner, HM AF Rathborne, J. M. Lada, C. J. Walsh, W. Saul, M. Butner, H. M. TI THE DENSE RING IN THE COALSACK: THE MERGING OF TWO SUBSONIC FLOWS? SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: globules; ISM: kinematics and dynamics; ISM: molecules; stars: formation ID SOUTHERN COALSACK; DARK CLOUD; MOLECULAR CLOUDS; STARLESS CORES; DUST EXTINCTION; DYNAMICAL STATE; BOK GLOBULE; BARNARD-68; CHEMISTRY; EVOLUTION AB A recent high angular resolution extinction map toward the most opaque molecular globule, Globule 2, in the Coalsack Nebula revealed that it contains a strong central ring of dust column density. This ring represents a region of high density and pressure that is likely a transient and possibly turbulent structure. Dynamical models suggest that the ring has formed as a result of a sudden increase in external pressure which is driving a compression wave into the Globule. Here we combine the extinction measurements with a detailed study of the C(18)O (1-0) molecular line profiles toward Globule 2 in order to investigate the overall kinematics and, in doing so, test this dynamical model. We find that the ring corresponds to an enhancement in the C18O nonthermal velocity dispersion and nonthermal pressure. We observe a velocity gradient across the Globule that appears to trace two distinct systematic subsonic velocity flows that happen to converge within the ring. We suggest, therefore, that the ring has formed as two subsonic flows of turbulent gas merge within the Globule. The fact that the outer layers of the Globule appear stable against collapse, and yet there is no centrally condensed core, suggests that the Globule may be evolving from the outside in and has yet to stabilize, confirming its youth. C1 [Rathborne, J. M.; Lada, C. J.; Walsh, W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Butner, H. M.] James Madison Univ, Dept Phys & Astron, Harrisonburg, VA 22807 USA. [Saul, M.] Univ New S Wales, Sch Phys, Sydney, NSW 2052, Australia. RP Rathborne, JM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jrathborne@cfa.harvard.edu; clada@cfa.harvard.edu; wwalsh@cfa.harvard.edu; msaul@phys.unsw.edu.au; butnerhm@jmu.edu OI Butner, Harold/0000-0003-4899-2064 NR 39 TC 5 Z9 5 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 2009 VL 690 IS 2 BP 1659 EP 1671 DI 10.1088/0004-637X/690/2/1659 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 398IX UT WOS:000262726900053 ER PT J AU Cackett, EM Miller, JM Homan, J van der Klis, M Lewin, WHG Mendez, MM Raymond, J Steeghs, D Wijnands, R AF Cackett, E. M. Miller, J. M. Homan, J. van der Klis, M. Lewin, W. H. G. Mendez, M. M. Raymond, J. Steeghs, D. Wijnands, R. TI A SEARCH FOR IRON EMISSION LINES IN THE CHANDRA X-RAY SPECTRA OF NEUTRON STAR LOW-MASS X-RAY BINARIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; stars: neutron; X-rays: binaries ID XMM-NEWTON/EPIC-PN; BLACK-HOLE; BEPPOSAX OBSERVATION; ACCRETION DISKS; SCORPIUS X-1; HARD TAIL; GX 17+2; ENERGY; MCG-6-30-15; STATES AB While iron emission lines are well studied in black hole systems, both in X-ray binaries and active galactic nuclei, there has been less of a focus on these lines in neutron star low-mass X-ray binaries (LMXBs). However, recent observations with Suzaku and XMM-Newton have revealed broad, asymmetric iron line profiles in three neutron star LMXBs, confirming an inner disk origin for these lines in neutron star systems. Here, we present a search for iron lines in six neutron star LMXBs. For each object we have simultaneous Chandra and RXTE observations at two separate epochs, allowing for both a high-resolution spectrum and broadband spectral coverage. Out of the six objects in the survey, we only find significant iron lines in two of the objects, GX 17+2 and GX 349+2. However, we cannot rule out that there are weak, broad lines present in the other sources. The equivalent width of the line in GX 17+2 is consistent between the two epochs, while in GX 349+2 the line equivalent width increases by a factor of similar to 3 between epochs as the source flux decreases by a factor of 1.3. This suggests that the disk is highly ionized, and the line is dominated by recombination emission. We find that there appears to be no specific locations in the long-term hardness-intensity diagrams where iron emission lines are formed, though more sources and further observations are required. C1 [Cackett, E. M.; Miller, J. M.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Homan, J.; Lewin, W. H. G.] MIT, MIT Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [van der Klis, M.; Wijnands, R.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. [Mendez, M. M.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Raymond, J.; Steeghs, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Steeghs, D.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. RP Cackett, EM (reprint author), Univ Michigan, Dept Astron, 500 Church St, Ann Arbor, MI 48109 USA. EM ecackett@umich.edu RI Mendez, Mariano/C-8011-2012; Steeghs, Danny/C-5468-2009; XRAY, SUZAKU/A-1808-2009 OI Mendez, Mariano/0000-0003-2187-2708; Steeghs, Danny/0000-0003-0771-4746; FU Chandra FX J.M.M. gratefully acknowledges support from Chandra. NR 42 TC 24 Z9 24 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 2009 VL 690 IS 2 BP 1847 EP 1855 DI 10.1088/0004-637X/690/2/1847 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 398IX UT WOS:000262726900068 ER PT J AU Acciari, V Aliu, E Arlen, T Bautista, M Beilicke, M Benbow, W Bottcher, M Bradbury, SM Buckley, JH Bugaev, V Butt, Y Byrum, K Cannon, A Celik, O Cesarini, A Chow, YC Ciupik, L Cogan, P Colin, P Cui, W Dickherber, R Duke, C Ergin, T Falcone, A Fegan, SJ Finley, JP Finnegan, G Fortin, P Fortson, L Furniss, A Gall, D Gibbs, K Gillanders, GH Grube, J Guenette, R Gyuk, G Hanna, D Hays, E Holder, J Horan, D Hui, CM Humensky, TB Imran, A Kaaret, P Karlsson, N Kertzman, M Kieda, D Kildea, J Konopelko, A Krawczynski, H Krennrich, F Lang, MJ LeBohec, S Maier, G McCann, A McCutcheon, M Millis, J Moriarty, P Mukherjee, R Nagai, T Ong, RA Otte, AN Pandel, D Perkins, JS Petry, D Pohl, M Quinn, J Ragan, K Reyes, LC Reynolds, PT Roache, E Rose, J Schroedter, M Sembroski, GH Smith, AW Steele, D Swordy, SP Theiling, M Toner, JA Valcarcel, L Varlotta, A Vassiliev, VV Wagner, RG Wakely, SP Ward, JE Weekes, TC Weinstein, A White, RJ Williams, DA Wissel, S Wood, M Zitzer, B AF Acciari, V. Aliu, E. Arlen, T. Bautista, M. Beilicke, M. Benbow, W. Boettcher, M. Bradbury, S. M. Buckley, J. H. Bugaev, V. Butt, Y. Byrum, K. Cannon, A. Celik, O. Cesarini, A. Chow, Y. C. Ciupik, L. Cogan, P. Colin, P. Cui, W. Dickherber, R. Duke, C. Ergin, T. Falcone, A. Fegan, S. J. Finley, J. P. Finnegan, G. Fortin, P. Fortson, L. Furniss, A. Gall, D. Gibbs, K. Gillanders, G. H. Grube, J. Guenette, R. Gyuk, G. Hanna, D. Hays, E. Holder, J. Horan, D. Hui, C. M. Humensky, T. B. Imran, A. Kaaret, P. Karlsson, N. Kertzman, M. Kieda, D. Kildea, J. Konopelko, A. Krawczynski, H. Krennrich, F. Lang, M. J. LeBohec, S. Maier, G. McCann, A. McCutcheon, M. Millis, J. Moriarty, P. Mukherjee, R. Nagai, T. Ong, R. A. Otte, A. N. Pandel, D. Perkins, J. S. Petry, D. Pohl, M. Quinn, J. Ragan, K. Reyes, L. C. Reynolds, P. T. Roache, E. Rose, J. Schroedter, M. Sembroski, G. H. Smith, A. W. Steele, D. Swordy, S. P. Theiling, M. Toner, J. A. Valcarcel, L. Varlotta, A. Vassiliev, V. V. Wagner, R. G. Wakely, S. P. Ward, J. E. Weekes, T. C. Weinstein, A. White, R. J. Williams, D. A. Wissel, S. Wood, M. Zitzer, B. TI DISCOVERY OF VERY HIGH ENERGY GAMMA-RAY RADIATION FROM THE BL LAC 1ES 0806+524 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE BL Lacertae objects: individual (1ES 0806+524); gamma rays: observations; ultraviolet: galaxies; X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; LACERTAE OBJECTS; ASTRONOMY; EMISSION; OPACITY; VERITAS; SYSTEM AB The high-frequency-peaked BL Lacertae object 1ES 0806+524, at redshift z = 0.138, was observed in the very high energy (VHE) gamma-ray regime by VERITAS between 2006 November and 2008 April. These data encompass the two- and three-telescope commissioning phases, as well as observations with the full four-telescope array. 1ES 0806+524 is detected with a statistical significance of 6.3 standard deviations from 245 excess events. Little or no measurable variability on monthly timescales is found. The photon spectrum for the period 2007 November to 2008 April can be characterized by a power law with photon index 3.6 +/- 1.0(stat) +/- 0.3(sys) between similar to 300 GeV and similar to 700 GeV. The integral flux above 300 GeV is ( 2.2 +/- 0.5(stat) +/- 0.4(sys)) x 10(-12)cm(-2)s(-1) which corresponds to 1.8% of the Crab Nebula flux. Non-contemporaneous multiwavelength observations are combined with the VHE data to produce a broadband spectral energy distribution that can be reasonably described using a synchrotron-self-Compton model. C1 [Acciari, V.; Moriarty, P.] Galway Mayo Inst Technol, Dept Life & Phys Sci, Galway, Ireland. [Aliu, E.; Holder, J.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Aliu, E.; Holder, J.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Arlen, T.; Celik, O.; Chow, Y. C.; Fegan, S. J.; Ong, R. A.; Vassiliev, V. V.; Weinstein, A.; Wood, M.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Bautista, M.; Cogan, P.; Guenette, R.; Hanna, D.; Maier, G.; McCann, A.; McCutcheon, M.; Ragan, K.; Valcarcel, L.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Beilicke, M.; Buckley, J. H.; Bugaev, V.; Dickherber, R.; Krawczynski, H.] Washington Univ, Dept Phys, St Louis, MO 63130 USA. [Benbow, W.; Gibbs, K.; Kildea, J.; Perkins, J. S.; Roache, E.; Theiling, M.; Weekes, T. C.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. [Boettcher, M.] Ohio Univ, Dept Phys & Astron, Inst Astrophys, Athens, OH 45701 USA. [Bradbury, S. M.; Rose, J.; White, R. J.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Butt, Y.; Ergin, T.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Byrum, K.; Smith, A. W.; Wagner, R. G.] Argonne Natl Lab, Argonne, IL 60439 USA. [Cannon, A.; Grube, J.; Quinn, J.; Ward, J. E.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland. [Cesarini, A.; Gillanders, G. H.; Lang, M. J.; Toner, J. A.] Natl Univ Ireland, Sch Phys, Galway, Ireland. [Ciupik, L.; Fortson, L.; Gyuk, G.; Karlsson, N.; Steele, D.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA. [Colin, P.; Finnegan, G.; Hui, C. M.; Kieda, D.; LeBohec, S.] Univ Utah, Dept Phys, Salt Lake City, UT 84112 USA. [Cui, W.; Finley, J. P.; Gall, D.; Sembroski, G. H.; Varlotta, A.; Zitzer, B.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Duke, C.] Grinnell Coll, Dept Phys, Grinnell, IA 50112 USA. [Falcone, A.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Fortin, P.; Mukherjee, R.] Columbia Univ, Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA. [Furniss, A.; Otte, A. N.; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Furniss, A.; Otte, A. N.; Williams, D. A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA. [Hays, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Horan, D.] Ecole Polytech, CNRS, Lab Leprince Ringuet, IN2P3, F-91128 Palaiseau, France. [Humensky, T. B.; Swordy, S. P.; Wakely, S. P.; Wissel, S.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Imran, A.; Krennrich, F.; Nagai, T.; Pohl, M.; Schroedter, M.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Kaaret, P.; Pandel, D.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Kertzman, M.] Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA. [Konopelko, A.] Pittsburg State Univ, Dept Phys, Pittsburg, KS 66762 USA. [Millis, J.] Anderson Univ, Dept Phys, Anderson, IN 46012 USA. [Reyes, L. C.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Petry, D.] European So Observ, D-85748 Garching, Germany. [Reynolds, P. T.] Cork Inst Technol, Dept Appl Phys & Instumentat, Cork, Ireland. RP Acciari, V (reprint author), Galway Mayo Inst Technol, Dept Life & Phys Sci, Dublin Rd, Galway, Ireland. EM peter.cogan@mail.mcgill.ca RI Hays, Elizabeth/D-3257-2012; OI Cui, Wei/0000-0002-6324-5772; Cesarini, Andrea/0000-0002-8611-8610; Ward, John E/0000-0003-1973-0794; Pandel, Dirk/0000-0003-2085-5586; Lang, Mark/0000-0003-4641-4201 FU U.S. Department of Energy; U.S. National Science Foundation; Smithsonian Institution; NSERC in Canada; Science Foundation Ireland FX This research is supported by grants from the U.S. Department of Energy, the U.S. National Science Foundation, the Smithsonian Institution, by NSERC in Canada, by Science Foundation Ireland and by PPARC in the UK. We acknowledge the excellent work of the technical support staff at the FLWO and the collaborating institutions in the construction and operation of VERITAS. The authors thank the anonymous referee for helpful comments which helped to improve and clarify the text. NR 29 TC 40 Z9 40 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JAN 10 PY 2009 VL 690 IS 2 BP L126 EP L129 DI 10.1088/0004-637X/690/2/L126 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 398RJ UT WOS:000262748900009 ER PT J AU Bottinelli, S Hughes, AM van Dishoeck, EF Young, KH Chamberlin, R Tilanus, RPJ Gurwell, MA Wilner, DJ van Langevelde, HJ Hogerheijde, MR Christensen, RD Shinnaga, H Yoshida, H AF Bottinelli, Sandrine Hughes, A. Meredith van Dishoeck, Ewine F. Young, Ken H. Chamberlin, Richard Tilanus, Remo P. J. Gurwell, Mark A. Wilner, David J. van Langevelde, Huib Jan Hogerheijde, Michiel R. Christensen, Robert D. Shinnaga, Hiroko Yoshida, Hiroshige TI DETECTION OF C I IN ABSORPTION TOWARD PKS 1830-211 WITH THE eSMA SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: ISM; ISM: abundances; quasars: absorption lines; quasars: individual (PKS 1830) ID REDSHIFTED MOLECULAR ABSORPTION; PHOTON-DOMINATED REGION; GRAVITATIONAL LENS; ATOMIC CARBON; INTERSTELLAR-MEDIUM; SPIRAL GALAXY; DARK CLOUD; PKS-1830-211; SYSTEM; LINE AB We report the first science observations and results obtained with the "extended" SMA (eSMA), which is composed of the SMA (Submillimeter Array), JCMT (James Clerk Maxwell Telescope), and CSO (Caltech Submillimeter Observatory). Redshifted absorptions at z = 0.886 of C I ((P1-P0)-P-3-P-3) were observed with the eSMA with an angular resolution of 0".55 x 0".22 at 1.1 mm toward the southwestern image of the remarkable lensed quasar PKS 1830-211, but not toward the northeastern component at a separation of similar to 1". Additionally, SMA observations of CO, (CO)-C-13, and (CO)-O-18 (all J = 4-3) were obtained toward this object: CO was also detected toward the southwest component, but none of the isotopologues were. This is the first time [C I] has been detected in this object, allowing the first direct determination of relative abundances of neutral atomic carbon to CO in themolecular clouds of a spiral galaxy at z > 0.1. The [C I] and CO profiles can be decomposed into two and three velocity components, respectively. We derive C/CO column density ratios ranging from less than or similar to 0.5 ( representative of dense cores) to similar to 2.5 (close to translucent cloud values). This could indicate that we are seeing environments with different physical conditions or that we are witnessing the chemical evolution of regions where C has not completely been converted into CO. C1 [Bottinelli, Sandrine; van Dishoeck, Ewine F.; van Langevelde, Huib Jan; Hogerheijde, Michiel R.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Hughes, A. Meredith; Young, Ken H.; Gurwell, Mark A.; Wilner, David J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [van Dishoeck, Ewine F.] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. [Chamberlin, Richard; Shinnaga, Hiroko; Yoshida, Hiroshige] CALTECH, Submillimeter Observ Off, Hilo, HI 96720 USA. [Tilanus, Remo P. J.] Joint Astron Ctr, Hilo, HI 96720 USA. [Tilanus, Remo P. J.] Netherlands Org Sci Res, NL-2509 AC The Hague, Netherlands. [van Langevelde, Huib Jan] Joint Inst VLBI Europe, Radiosterrenwacht Dwingeloo, NL-7990 AA Dwingeloo, Netherlands. [Christensen, Robert D.] Harvard Smithsonian Ctr Astrophys, Submillimeter Array, Hilo, HI 96721 USA. RP Bottinelli, S (reprint author), Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. EM sandrine@strw.leidenuniv.nl OI van Langevelde, Huib Jan/0000-0002-0230-5946 FU Netherlands Organisation for Scientific Research, NWO [614.061.416]; National Science FoundationGraduate Research Fellowship FX We are very much indebted to Ray Blundell, Gary Davis, and Tom Phillips, the directors of the SMA, JCMT, and CSO, respectively, for their continued support and without whom the eSMA would not be possible. The development of the eSMA has been facilitated by grant 614.061.416 from the Netherlands Organisation for Scientific Research, NWO. A. M. H. is supported by a National Science FoundationGraduate Research Fellowship. NR 42 TC 3 Z9 3 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 JAN 10 PY 2009 VL 690 IS 2 BP L130 EP L134 DI 10.1088/0004-637X/690/2/L130 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 398RJ UT WOS:000262748900010 ER PT J AU Kenyon, SJ Bromley, BC AF Kenyon, Scott J. Bromley, Benjamin C. TI RAPID FORMATION OF ICY SUPER-EARTHS AND THE CORES OF GAS GIANT PLANETS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE planetary systems; planets and satellites: formation; solar system: formation ID TURBULENT PROTOPLANETARY DISKS; SPECTRAL ENERGY-DISTRIBUTIONS; EARLY KUIPER-BELT; T-TAURI STARS; SOLAR NEBULA; SNOW LINE; DUST COAGULATION; ACCRETION; EVOLUTION; MIGRATION AB We describe a coagulation model that leads to the rapid formation of super-Earths and the cores of gas giant planets. Interaction of collision fragments with the gaseous disk is the crucial element of this model. The gas entrains small collision fragments, which rapidly settle to the disk midplane. Protoplanets accrete the fragments and grow to masses greater than or similar to 1M(circle plus) in similar to 1 Myr. Our model explains the mass distribution of planets in the solar system and predicts that super-Earths form more frequently than gas giants in low-mass disks. C1 [Kenyon, Scott J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Bromley, Benjamin C.] Univ Utah, Dept Phys, Salt Lake City, UT 84112 USA. RP Kenyon, SJ (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM skenyon@cfa.harvard.edu; bromley@physics.utah.edu OI Kenyon, Scott/0000-0003-0214-609X FU NASA TPF Foundation Science Program [NNG06GH25G] FX We acknowledge a generous allotment, similar to 25 cpu years, of computer time on the 1024 cpu Dell Xeon cluster "cosmos" at the Jet Propulsion Laboratory through funding from the NASA Offices of Mission to Planet Earth, Aeronautics, and Space Science. We thank M. Werner for his strong support of this project. We also acknowledge use of similar to 10 cpu years on the CfA cluster "hydra." Advice and comments from T. Currie, M. Geller, G. Kennedy, and an anonymous referee greatly improved our presentation. Portions of this project were supported by the NASA TPF Foundation Science Program, through grant NNG06GH25G. NR 48 TC 54 Z9 54 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JAN 10 PY 2009 VL 690 IS 2 BP L140 EP L143 DI 10.1088/0004-637X/690/2/L140 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 398RJ UT WOS:000262748900012 ER PT J AU Ubelaker, DH AF Ubelaker, Douglas H. TI The forensic evaluation of burned skeletal remains: A synthesis SO FORENSIC SCIENCE INTERNATIONAL LA English DT Review DE Burning; Skeletal; Thermal ID SCANNING ELECTRON-MICROSCOPE; DAVIDIAN COMPOUND VICTIMS; INCINERATED TEETH; CREMATED REMAINS; FIRE VICTIMS; BONE; IDENTIFICATION; ANTHROPOLOGY; DNA; FRAGMENTS AB In recent years, research and case experience have greatly augmented knowledge regarding the effects of extreme heat on skeletal remains. As a result of this effort, enhanced interpretation is now possible on such issues as the extent of recovery, reconstruction, trauma, individual identification, size reduction, thermal effects on histological structures, color variation, the determination if remains were burned with or without soft tissue, DNA recovery and residual weight. The rapidly growing literature in this area of forensic science includes experimental research that elucidates the dynamics of the thermal impact on skeletal structure and morphology. Published by Elsevier Ireland Ltd. C1 Smithsonian Inst, Dept Anthropol, NMNH, Washington, DC 20560 USA. RP Ubelaker, DH (reprint author), Smithsonian Inst, Dept Anthropol, NMNH, MRC 112,10th & Constitut Ave, Washington, DC 20560 USA. EM ubelaked@si.edu NR 81 TC 58 Z9 61 U1 9 U2 56 PU ELSEVIER IRELAND LTD PI CLARE PA ELSEVIER HOUSE, BROOKVALE PLAZA, EAST PARK SHANNON, CO, CLARE, 00000, IRELAND SN 0379-0738 EI 1872-6283 J9 FORENSIC SCI INT JI Forensic Sci.Int. PD JAN 10 PY 2009 VL 183 IS 1-3 BP 1 EP 5 DI 10.1016/j.forsciint.2008.09.019 PG 5 WC Medicine, Legal SC Legal Medicine GA 407VP UT WOS:000263392700001 PM 19010619 ER PT J AU Pohl, T Berman, PR AF Pohl, T. Berman, P. R. TI Breaking the Dipole Blockade: Nearly Resonant Dipole Interactions in Few-Atom Systems SO PHYSICAL REVIEW LETTERS LA English DT Article ID FROZEN RYDBERG GAS AB A dipole blockade, in which Rydberg-atom-Rydberg-atom interactions inhibit all but a single collective Rydberg excitation, has been proposed as a mechanism to store and manipulate quantum information in mesoscopic ensembles. We investigate the excitation dynamics of a collection of a few atoms and show that they undergo an unexpected, qualitative change when the number of atoms increases from two to three. In particular, the combined action of three atoms, each of which pairwise would produce a blockade, can break the dipole blockade. C1 [Pohl, T.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. [Berman, P. R.] Univ Michigan, Dept Phys, FOCUS Ctr, Michigan Ctr Theoret Phys, Ann Arbor, MI 48109 USA. RP Pohl, T (reprint author), Harvard Smithsonian Ctr Astrophys, ITAMP, 60 Garden St, Cambridge, MA 02138 USA. RI Pohl, Thomas/B-5133-2013 FU NSF [PHY-0114336, 0244841] FX We acknowledge fruitful discussions with G. Raithel, A. Reinhard, and K. Younge. This work was supported by the NSF through a grant to ITAMP and Grants No. PHY-0114336 and No. 0244841. NR 21 TC 40 Z9 40 U1 0 U2 5 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 J9 PHYS REV LETT JI Phys. Rev. Lett. PD JAN 9 PY 2009 VL 102 IS 1 AR 013004 DI 10.1103/PhysRevLett.102.013004 PG 4 WC Physics, Multidisciplinary SC Physics GA 393EZ UT WOS:000262355000019 PM 19257188 ER PT J AU Payne, JL Boyer, AG Brown, JH Finnegan, S Kowalewski, M Krause, RA Lyons, SK McClain, CR McShea, DW Novack-Gottshall, PM Smith, FA Stempien, JA Wang, SC AF Payne, Jonathan L. Boyer, Alison G. Brown, James H. Finnegan, Seth Kowalewski, Michal Krause, Richard A., Jr. Lyons, S. Kathleen McClain, Craig R. McShea, Daniel W. Novack-Gottshall, Philip M. Smith, Felisa A. Stempien, Jennifer A. Wang, Steve C. TI Two-phase increase in the maximum size of life over 3.5 billion years reflects biological innovation and environmental opportunity SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE body size; Cambrian; oxygen; Precambrian; trend ID BODY-SIZE; COPES RULE; ATMOSPHERIC OXYGEN; EVOLUTION; EUKARYOTES; OXIDATION; ANIMALS; FOSSILS; TRENDS; OCEANS AB The maximum size of organisms has increased enormously since the initial appearance of life > 3.5 billion years ago (Gya), but the pattern and timing of this size increase is poorly known. Consequently, controls underlying the size spectrum of the global biota have been difficult to evaluate. Our period-level compilation of the largest known fossil organisms demonstrates that maximum size increased by 16 orders of magnitude since life first appeared in the fossil record. The great majority of the increase is accounted for by 2 discrete steps of approximately equal magnitude: the first in the middle of the Paleoproterozoic Era (approximate to 1.9 Gya) and the second during the late Neoproterozoic and early Paleozoic eras (0.6-0.45 Gya). Each size step required a major innovation in organismal complexity-first the eukaryotic cell and later eukaryotic multicellularity. These size steps coincide with, or slightly postdate, increases in the concentration of atmospheric oxygen, suggesting latent evolutionary potential was realized soon after environmental limitations were removed. C1 [Payne, Jonathan L.; Finnegan, Seth] Stanford Univ, Dept Geol & Environm Sci, Stanford, CA 94305 USA. [Boyer, Alison G.; Brown, James H.; Smith, Felisa A.] Univ New Mexico, Dept Biol, Albuquerque, NM 87131 USA. [Kowalewski, Michal] Virginia Polytech Inst & State Univ, Dept Geosci, Blacksburg, VA 24061 USA. [Krause, Richard A., Jr.] Humboldt Univ, Museum Naturkunde, D-10115 Berlin, Germany. [Lyons, S. Kathleen] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. [McClain, Craig R.] Monterey Bay Aquarium Res Inst, Moss Landing, CA 95039 USA. [McShea, Daniel W.] Duke Univ, Dept Biol, Durham, NC 27708 USA. [Novack-Gottshall, Philip M.] Univ W Georgia, Dept Geosci, Carrollton, GA 30118 USA. [Stempien, Jennifer A.] Univ Colorado, Dept Geol Sci, Boulder, CO 80309 USA. [Wang, Steve C.] Swarthmore Coll, Dept Math & Stat, Swarthmore, PA 19081 USA. RP Payne, JL (reprint author), Stanford Univ, Dept Geol & Environm Sci, 450 Serra Mall,Bldg 320, Stanford, CA 94305 USA. EM jlpayne@stanford.edu RI Kowalewski, Michal/B-4263-2008; McClain, Craig/A-4031-2009; Finnegan, Seth/A-5014-2009; Krause, Richard/C-8724-2009; Payne, Jonathan/A-1240-2007; Payne, Jonathan/B-8088-2012; OI Kowalewski, Michal/0000-0002-8575-4711; Krause, Richard/0000-0001-5619-4551; Payne, Jonathan/0000-0002-9601-3310; Wang, Steve/0000-0002-8953-285X; McClain, Craig/0000-0003-0574-428X; Novack-Gottshall, Philip/0000-0002-2583-2968 FU National Evolutionary Synthesis Center (NESCent); National Science Foundation [EF-0423641] FX This study is a product of the working group on body size evolution ( principal investigators: J.L.P., J.A.S., and M. K.) funded by the National Evolutionary Synthesis Center (NESCent), National Science Foundation Grant EF-0423641. We thank N. Butterfield, M, Carrano, W. DiMichele, L. Dong, R. Feldmann, P. Gensel, J. Huntley, P. Janvier, A. Logan, S. Low, S. Lucas, R. Lupia, W. Manger, K. Niklas, W. Ou, S. Porter, C. Schweitzer, H. Steur, R. Taggert, B. Tiffney, S. Truebe, S. Wing, and S. Xiao for advice and assistance in data compilation; J. Denton and especially S. Porter for comments on previous drafts of the manuscript; and G. Hunt and 2 anonymous reviewers for constructive and thoughtful suggestions. NR 60 TC 86 Z9 89 U1 3 U2 36 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD JAN 6 PY 2009 VL 106 IS 1 BP 24 EP 27 DI 10.1073/pnas.0806314106 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 391WC UT WOS:000262263900008 PM 19106296 ER PT S AU Brown, GV Beiersdorfer, P Chen, H Clementson, J Frankel, M Gu, MF Kelley, RL Kilbourne, CA Porter, FS Thorn, DB Wargelin, BJ AF Brown, G. V. Beiersdorfer, P. Chen, H. Clementson, J. Frankel, M. Gu, M. F. Kelley, R. L. Kilbourne, C. A. Porter, F. S. Thorn, D. B. Wargelin, B. J. BE Azuma, T Nakamura, N Yamada, C TI STUDIES OF X-RAY PRODUCTION FOLLOWING CHARGE EXCHANGE RECOMBINATION BETWEEN HIGHLY CHARGED IONS AND NEUTRAL ATOMS AND MOLECULES SO 14TH INTERNATIONAL CONFERENCE ON THE PHYSICS OF HIGHLY CHARGED IONS (HCI 2008) SE Journal of Physics Conference Series LA English DT Proceedings Paper CT 14th International Conference on Physics of Highly Charged Ions CY SEP 01-05, 2008 CL Univ Electro Commun, Chofu, JAPAN SP Japan Soc Promot Sci, Int Union Pure & Appl Phys, Matsuo Fdn, Iwatani Naoji Fdn, CASIO Sci Promot Fdn, Soc Atom Collis Res HO Univ Electro Commun ID EBIT; SPECTROSCOPY; SPECTROMETER; EMISSION; TRAP AB We have used microcalorimeters built by the NASA/Goddard Space Flight Center and the Lawrence Livermore National Laboratory SuperEBIT electron beam ion trap to measure X-ray emission produced by charge exchange reactions between highly charged ions colliding with neutral helium, hydrogen, and nitrogen gas. Our measurements show the spectral dependence on neutral species and also show the distinct differences between spectra produced by charge exchange reactions and those produced by direct electron-impact excitation. These results are part of an ongoing experimental investigation at the LLNL SuperEBIT facility of charge exchange spectral signatures and can be used to interpret X-ray spectra produced by a variety of laboratory and celestial sources including cometary and planetary atmospheres, the Earth's magnetosheath, the heliosphere, and tokamaks. C1 [Brown, G. V.; Beiersdorfer, P.; Chen, H.; Clementson, J.; Frankel, M.; Gu, M. F.; Thorn, D. B.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Kelley, R. L.; Kilbourne, C. A.; Porter, F. S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20770 USA. [Wargelin, B. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Brown, GV (reprint author), Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. EM gregbrown@llnl.gov RI Porter, Frederick/D-3501-2012; Kelley, Richard/K-4474-2012 OI Porter, Frederick/0000-0002-6374-1119; FU US Department of Energy; Lawrence Livermore National Laboratory [DE-AC52-07NA27344]; LLNL; SAO; Stanford University; NASA/GSFC FX Part of this work was performed under the auspices of the U. S. Department of Energy by Lawrence Livermore National Laboratory under Contract DE-AC52-07NA27344 and is also supported by NASA grants to LLNL, SAO, Stanford University, and the NASA/GSFC. NR 14 TC 3 Z9 3 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 2009 VL 163 AR 012052 DI 10.1088/1742-6596/163/1/012052 PG 4 WC Physics, Multidisciplinary; Physics, Particles & Fields SC Physics GA BMT70 UT WOS:000273556200052 ER PT S AU Krawczynski, H Garson, A Li, Q Beilicke, M Dowkontt, P Wulf, E Kurfess, J Novikova, E De Geronimo, G Baring, MG Harding, AK Grindlay, J Hong, JS AF Krawczynski, H. Garson, A., III Li, Q. Beilicke, M. Dowkontt, P. Wulf, E. Kurfess, J. Novikova, E. De Geronimo, G. Baring, M. G. Harding, A. K. Grindlay, J. Hong, J. S. GP IEEE TI HX-POL - A Balloon-Bome Hard X-Ray Polarimeter SO 2008 IEEE NUCLEAR SCIENCE SYMPOSIUM AND MEDICAL IMAGING CONFERENCE (2008 NSS/MIC), VOLS 1-9 SE IEEE Nuclear Science Symposium Conference Record LA English DT Proceedings Paper CT IEEE Nuclear Science Symposium/Medical Imaging Conference CY OCT 19-25, 2008 CL Dresden, GERMANY SP IEEE Nucl & Plasma Sci Soc, Natl Nucl Secur Adm, US Def Threat Reduct Agcy, ICx Radiat GmbH, ORTEC, Hamamatsu, European Phys Journal, Hilger Crystals, SAFC Hitech, ATOMTEX, Canberra, SensL, ASP, Brookhaven Natl Lab, CEA, CERN, DESY, Forschungszentrum Julich GmbH, Int Atom Energy Agcy, Lawrence Livermore Natl Lab ID CMOS; PULSARS; POLARIZATION; AMPLIFIERS; PROSPECTS AB We report on the conceptual design and estimated performance of a balloon-borne hard X-ray polarimeter called HX-POL. The experiment uses a combination of Si and Cadmium Zinc Telluride detectors to measure the polarization of 50 keV-500 keV X-rays from cosmic sources through the dependence of the angular distribution of Compton scattered photons on the polarization direction. On a one-day balloon flight, HX-POL would allow us to measure the polarization of strong Crab-like sources for polarization degrees down to 5%. On a longer (15-30 day) flight from Australia or Antarctica, HX-POL would be be able to measure the polarization of strong sources down to polarization degrees of 1%. Hard X-ray polarization measurements provide unique venues for the study of particle acceleration processes by compact objects. In this contribution, we discuss the overall instrument design and performance. Furthermore, we present results from laboratory tests of the Si and CZT detectors. C1 [Krawczynski, H.; Garson, A., III; Li, Q.; Beilicke, M.; Dowkontt, P.] Washington Univ, St Louis, MO 63130 USA. [Wulf, E.; Novikova, E.] Naval Res Lab, High Energy Space Environm Branch, Washington, DC 20375 USA. [De Geronimo, G.] Brookhaven Natl Lab, Instrumentat Div, Upton, NY 11973 USA. [Baring, M. G.] Rice Univ, Dept Phys & Astron, Houston, TX 77001 USA. [Harding, A. K.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20770 USA. [Grindlay, J.; Hong, J. S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Krawczynski, H (reprint author), Washington Univ, St Louis, MO 63130 USA. EM krawcz@wuphys.wustl.edu RI Wulf, Eric/B-1240-2012; Harding, Alice/D-3160-2012 FU NASA [NNX07AH37G] FX Manuscript received November 15, 2008; revised July 29, 2009. Current version published December 09, 2009. The work of the Washington University group was supported by NASA under Grant NNX07AH37G. NR 38 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 1082-3654 BN 978-1-4244-2714-7 J9 IEEE NUCL SCI CONF R PY 2009 BP 4918 EP + PG 3 WC Radiology, Nuclear Medicine & Medical Imaging SC Radiology, Nuclear Medicine & Medical Imaging GA BKN17 UT WOS:000268656002235 ER PT B AU Li, CH Benedick, AJ Cramer, CE Chang, GQ Chen, LJ Fendel, P Furesz, G Glenday, AG Kaertner, FX Phillips, DF Sasselov, D Szentgyorgyi, A Walsworth, RL AF Li, Chih-Hao Benedick, Andrew J. Cramer, Claire E. Chang, Guoqing Chen, Li-Jin Fendel, Peter Furesz, Gabor Glenday, Alexander G. Kaertner, Franz X. Phillips, David F. Sasselov, Dimitar Szentgyorgyi, Andrew Walsworth, Ronald L. GP IEEE TI Femtosecond Laser Frequency Comb for Precision Astrophysical Spectroscopy SO 2009 CONFERENCE ON LASERS AND ELECTRO-OPTICS AND QUANTUM ELECTRONICS AND LASER SCIENCE CONFERENCE (CLEO/QELS 2009), VOLS 1-5 LA English DT Proceedings Paper CT Conference on Lasers and Electro-Optics/Quantum Electronics and Laser Science Conference (CLEO/QELS 2009) CY JUN 02-04, 2009 CL Baltimore, MD ID PLANETS; SYSTEM AB High-resolution spectroscopy is a crucial tool for cosmology and the search for extrasolar planets. We present a laser comb with up to 40-GHz line spacing for use as a new spectrographic calibration source. (C) 2008 Optical Society of America C1 [Li, Chih-Hao; Cramer, Claire E.; Furesz, Gabor; Glenday, Alexander G.; Phillips, David F.; Sasselov, Dimitar; Szentgyorgyi, Andrew; Walsworth, Ronald L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Li, CH (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM rwalsworth@cfa.harvard.edu NR 9 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA BN 978-1-4244-5184-5 PY 2009 BP 479 EP 480 PG 2 WC Engineering, Electrical & Electronic; Optics; Physics, Applied SC Engineering; Optics; Physics GA BNJ62 UT WOS:000274751300241 ER PT B AU Phillips, JD Huffman, GM Reasenberg, RD AF Phillips, J. D. Huffman, G. M. Reasenberg, R. D. GP IEEE TI Semiconductor Laser Tracking Frequency Distance Gauge SO 2009 CONFERENCE ON LASERS AND ELECTRO-OPTICS AND QUANTUM ELECTRONICS AND LASER SCIENCE CONFERENCE (CLEO/QELS 2009), VOLS 1-5 LA English DT Proceedings Paper CT Conference on Lasers and Electro-Optics/Quantum Electronics and Laser Science Conference (CLEO/QELS 2009) CY JUN 02-04, 2009 CL Baltimore, MD ID INTERFEROMETRY; METROLOGY AB Space-based astronomical instruments and gravitational experiments require dramatically improved distance measurement accuracy. The Tracking Frequency laser distance Gauge measures to picometer accuracy. We discuss the design of the semiconductor laser version and its controller. C1 [Phillips, J. D.; Reasenberg, R. D.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Phillips, JD (reprint author), Smithsonian Astrophys Observ, MS63,60 Garden St, Cambridge, MA 02138 USA. EM jphillips@cfa.harvard.edu 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 BN 978-1-4244-5184-5 PY 2009 BP 1565 EP 1566 PG 2 WC Engineering, Electrical & Electronic; Optics; Physics, Applied SC Engineering; Optics; Physics GA BNJ62 UT WOS:000274751301106 ER PT B AU Cramer, CE Brown, S Caldwell, N Dupree, AK Korzennik, SG Lykke, KR Szentgyorgyi, A AF Cramer, Claire E. Brown, Steven Caldwell, Nelson Dupree, Andrea K. Korzennik, Sylvain G. Lykke, Keith R. Szentgyorgyi, Andrew GP IEEE TI A Tunable Laser System for the Wavelength Calibration of Astronomical Spectrographs SO 2009 CONFERENCE ON LASERS AND ELECTRO-OPTICS AND QUANTUM ELECTRONICS AND LASER SCIENCE CONFERENCE (CLEO/QELS 2009), VOLS 1-5 LA English DT Proceedings Paper CT Conference on Lasers and Electro-Optics/Quantum Electronics and Laser Science Conference (CLEO/QELS 2009) CY JUN 02-04, 2009 CL Baltimore, MD AB Precise wavelength calibration of the multi-object echelle spectrographs used in searches for extrasolar planets is an unsolved problem in astrophysical instrumentation. We present results from a novel tunable laser calibration system that achieves unprecedented precision. (C) 2009 Optical Society of America C1 [Cramer, Claire E.] Harvard Univ, Cambridge, MA 02138 USA. [Brown, Steven; Lykke, Keith R.] NIST, Gaithersburg, MD 20899 USA. [Caldwell, Nelson; Dupree, Andrea K.; Korzennik, Sylvain G.; Szentgyorgyi, Andrew] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Cramer, CE (reprint author), Harvard Univ, Cambridge, MA 02138 USA. EM ccramer@cfa.harvard.edu NR 2 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA BN 978-1-4244-5184-5 PY 2009 BP 2647 EP + PG 2 WC Engineering, Electrical & Electronic; Optics; Physics, Applied SC Engineering; Optics; Physics GA BNJ62 UT WOS:000274751302308 ER PT B AU Chang, SW Tong, CYE Hedden, A Hwang, YJ Blundell, R AF Chang, Su-Wei Tong, Cheuk-yu Edward Hedden, Abigail Hwang, Yuh-Jing Blundell, Raymond GP IEEE TI A 660 GHz Local Oscillator Subsystem: Design, Testing and Alignment SO 2009 EUROPEAN MICROWAVE CONFERENCE, VOLS 1-3 LA English DT Proceedings Paper CT 37th European Microwave Conference CY SEP 29-OCT 01, 2009 CL Rome, ITALY AB A 660 GHz local oscillator (LO) sub-system for the Submillimeter Array is designed, tested and aligned in the laboratory by optical and radio alignment. The LO unit employs a cascade tuneless frequency doubler-tripler based on the planar GaAs Schottky diode technology. It is found that a phase shifter inserted between the first and second multiplier stages can improve the frequency response of the unit, reduce the ripples due to the impedance mismatch between the 2 stages. A new technique for the optical and radio alignment of the beam emerging from the unit is also introduced. A near-field scanner which measures the complex beam pattern facilitates the final alignment and helps to verify proper focusing of the LO output beam. C1 [Chang, Su-Wei; Hwang, Yuh-Jing] Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan. [Tong, Cheuk-yu Edward; Hedden, Abigail; Blundell, Raymond] Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA. RP Chang, SW (reprint author), Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan. EM swchang@asiaa.sinica.edu.tw; etong@cfa.harvard.edu; ahedden@cfa.harvard.edu; yjhwang@asiaa.sinica.edu.tw; rblundell@cfa.harvard.edu OI Tong, Edward/0000-0002-7736-4203 NR 10 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA BN 978-1-4244-4748-0 PY 2009 BP 834 EP + PG 3 WC Engineering, Electrical & Electronic SC Engineering GA BNN89 UT WOS:000275097800210 ER PT J AU Nataf, DM Stanek, KZ Bakos, GA AF Nataf, D. M. Stanek, K. Z. Bakos, G. A. TI Finding the Brightest Galactic Bulge Microlensing Events with a Small Aperture Telescope and Image Subtraction SO ACTA ASTRONOMICA LA English DT Article DE Techniques: photometric; Gravitational lensing; Stars: variables: general ID GRAVITATIONAL LENSING EXPERIMENT; VARIABLE-STARS; ECLIPSING BINARIES; PHOTOMETRY; FIELD; DISCOVERY; CATALOG; SEARCH AB Following the suggestion of Gould and Depoy (1998) we investigate the feasibility of studying the brightest microlensing events towards the Galactic bulge using a small aperture (approximate to 10 cm) telescope. We used one of the HAT telescopes to obtain 151 exposures spanning 88 nights in 2005 of an 8.degrees 4 x 8.degrees 4 FOV centered on (1, b) = (2.85, -5.00). We reduced the data using image subtraction software. We find that such a search method can effectively contribute to monitoring bright microlensing events, as was advocated. Comparing this search method to the existing ones we find a dedicated bulge photometric survey of this nature would fulfill a significant niche at excellent performance and rather low cost. We obtain matches to 7 microlensing events listed in the 2005 OGLE archives. We find several other light Curves whose fits closely resemble microlensing events. Unsurprisingly, many periodic variable stars and miscellaneous variable stars are also detected in our data, and we estimate approximately 50% of these are new discoveries. We conclude by briefly proposing Small Aperture Microlensing Survey, which would monitor the Galactic bulge around the clock to provide dense coverage of the highest magnification microlensing events. C1 [Nataf, D. M.; Stanek, K. Z.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Bakos, G. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Nataf, DM (reprint author), Ohio State Univ, Dept Astron, 140 W 18th Ave, Columbus, OH 43210 USA. EM nataf@astronomy.ohio-state.edu; kstanek@astronomy.ohio-state.edu; gbakos@cfa.harvard.edu FU NASA [NEG04GN74G, NNX08AF23G]; SAO IRD FX HATNet operations have been funded by NASA grants NEG04GN74G, NNX08AF23G and SAO IR&D grants. We thank J.D. Hartman for assistance with use of the VARTOOLS package, G. Pojmafiski for his LC program, W. Pych for his FWHM program, R.J. Siverd for explanations and help with Perl programming, S. Kozlowski for suggestions on microlensing fitting, L. Wyrzykowski for his microlensing curve fitting program, and A. Gould for insights into the observational process. We made use of the Simbad database, operated in Strasbourg, France by the Centre de Donnees astronorniques de Strasbourg. NR 44 TC 4 Z9 6 U1 0 U2 1 PU COPERNICUS FOUNDATION POLISH ASTRONOMY PI WARSAW PA AL UJAZDOWSKIE 4, 00-478 WARSAW, POLAND SN 0001-5237 J9 ACTA ASTRONOM JI Acta Astron. PY 2009 VL 59 IS 3 BP 255 EP 272 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 512BA UT WOS:000271215800002 ER PT J AU Weber, N Kalko, EKV Fahr, J AF Weber, Natalie Kalko, Elisabeth K. V. Fahr, Jakob TI A first assessment of home range and foraging behaviour of the African long-tongued bat Megaloglossus woermanni (Chiroptera: Pteropodidae) in a heterogeneous landscape within the Lama Forest Reserve, Benin SO ACTA CHIROPTEROLOGICA LA English DT Article DE animal-plant interactions; Dahomey Gap; foraging area; nectarivory; radio-tracking; spatial use; West Africa ID PAPUA-NEW-GUINEA; NECTAR-FEEDING BAT; NEW-SOUTH-WALES; BLOSSOM-BAT; SYCONYCTERIS-AUSTRALIS; FRUIT BAT; MACROGLOSSUS-MINIMUS; MEGACHIROPTERA; TERRITORIALITY; ENERGETICS AB We investigated spatial use and foraging behaviour of the nectarivorous African long-tongued bat, Megaloglossus woermanni (Chiroptera Pteropodidae), in the Lama Forest Reserve, southern Benin, West Africa. We monitored movement and activity patterns of two males and two females that were fitted with position-sensitive radio transmitters for five to nine nights within a three-month study period. The study site comprised the central patch of relatively undisturbed forest ('Noyau Central'), and a mosaic of orchards, agroforestry plantations, and degraded forests surrounding the central patch. Spatial use of M. woermanni was characterized by small home ranges and high site-fidelity. Mean home range sizes (minimum convex polygon) were larger in females (139 0 and 146 8 ha) than in males (99 8 and 102 9 ha). Throughout the study period, long-tongued bats were frequently observed visiting flowers of cultivated bananas. The mean foraging areas (95% density kernel) of females (39 0 and 109 4 ha) were much larger than in males (12 3 and 14 1 ha). Difference in core areas (50% density kernel) between the sexes was less marked (both females 6 8 ha, males 2 7 and 2 9 hectares). Core areas constituted only a small part of home ranges (2.6-4.9%). Large segments of the home ranges were only used for commuting flights between discrete resource patches. Our study provides, for the first time, information on home ranges and foraging behaviour of the sole obligate nectar-drinking bat in Africa. C1 [Weber, Natalie; Kalko, Elisabeth K. V.; Fahr, Jakob] Univ Ulm, Inst Expt Ecol Bio 3, D-89069 Ulm, Germany. [Kalko, Elisabeth K. V.] Smithsonian Trop Res Inst, Balboa, Panama. RP Weber, N (reprint author), Univ Ulm, Inst Expt Ecol Bio 3, Albert Einstein Allee 11, D-89069 Ulm, Germany. RI Fahr, Jakob/E-8831-2012 OI Fahr, Jakob/0000-0002-9174-1204 NR 65 TC 11 Z9 11 U1 0 U2 12 PU MUSEUM & INST ZOOLOGY PAS-POLISH ACAD SCIENCES PI WARSAW PA WILCZA STREET 64, 00-679 WARSAW, POLAND SN 1508-1109 J9 ACTA CHIROPTEROL JI Acta Chiropt. PY 2009 VL 11 IS 2 BP 317 EP 329 DI 10.3161/150811009X485558 PG 13 WC Zoology SC Zoology GA 562EE UT WOS:000275031500009 ER PT J AU Marimuthu, K Haniffa, MA Rahman, MA AF Marimuthu, Kasi Haniffa, Mohammed A. Aminur Rahman, Mohammad TI SPAWNING PERFORMANCE OF NATIVE THREATENED SPOTTED SNAKEHEAD FISH, CHANNA PUNCTATUS (ACTINOPTERYGII: CHANNIDAE: PERCIFORMES), INDUCED WITH OVATIDE SO ACTA ICHTHYOLOGICA ET PISCATORIA LA English DT Article DE Snakehead; Channa punctatus; hormones; induced spawning; seed production; conservation ID CARP PITUITARY HOMOGENATE; ARTIFICIAL PROPAGATION; OVULATION; STIMULATION; INDUCTION; HORMONES; ANALOGS; OVOPEL AB Background. The spotted snakehead, Channa punctatus is a highly priced freshwater food fish species in India. The culture of snakeheads is still not common due to the scarcity of quality seed supply and lack of knowledge on their feeding and breeding techniques. Therefore an experiment was conducted to test the efficacy of a new spawning agent, Ovatide in stimulating ovulation of snakehead fish under a controlled captive condition. Materials and Methods. In total, 12 matured females and 24 male fish weighing 50-90 g were randomly selected for three hormonal treatment groups and one control group. Both male and female fish in each treatment group were administered with either saline (0.9% NaCl, control group), or 0.2, 0.4, and 0.6 mL of Ovatide per kg of body weight (BW), respectively. Each breeding set consisted of two males and one female. The hormone-treated fish were then held in concrete tanks for spawning. The breeding performance was evaluated based on spawning fecundity, spawning response, percentage fertilization, and percentage hatching. Results. No spawning behaviour or performance was observed in control group. Partial spawning was observed with the Ovatide dose of 0.2 mL . kg(-1) BW, and complete spawning was noticed in the medium Ovatide dose (0.4 mL . kg(-1) BW), and the higher dose (0.6 mL . kg(-1) BW) administered fish. The highest total spawning fecundity (P < 0.05) was recorded when the females were injected with 0.4 mL of Ovatide . kg(-1) BW than those injected with other doses. The latency period and the number of spawned eggs were ranged from 25 to 31 h and from 1080 to 5814, respectively. The highest fertilization- (90.6%) and hatching (91.33%) rates were also observed at the medium dose (P < 0.05). With regard to hatching rates, no significant difference was noticed between the medium- and higher doses of Ovatide-treated groups. Conclusions. The synthetic gonadotropin-releasing hormone with a dopamine antagonist at the dose of 0.4 mL . kg(-1) BW could be used as an appropriate stimulating agent for successful spawning and induced breeding of C. punctatus under captive conditions. C1 [Marimuthu, Kasi] AIMST Univ, Fac Sci Appl, Dept Biotechnol, Bedong 08100, Kedah Darul Ama, Malaysia. [Haniffa, Mohammed A.] St Xaviers Coll, CARE, Palayankottai 627002, Tamil Nadu, India. [Aminur Rahman, Mohammad] Smithsonian Trop Res Inst, Naos Isl, Panama. RP Marimuthu, K (reprint author), AIMST Univ, Fac Sci Appl, Dept Biotechnol, Baru 3 1-2 Bukit Air Nasi, Bedong 08100, Kedah Darul Ama, Malaysia. EM aquamuthu2k@yahoo.com RI Gebauer, Radek/G-6749-2015 FU Department of Science and Technology, New Delhi FX The authors are thankful to Principal, St. Xavier's College, Palayamkottai, for providing necessary facilities for this research and Department of Science and Technology, New Delhi for providing fellowship to the first author. NR 25 TC 3 Z9 8 U1 0 U2 3 PU WYDAWNICTWO AKAD ROLNICZEJ W SZCZECINIE PI SZCZECIN PA KAZIMIERZA KROLEWICZA 4, SZCZECIN, 71550, POLAND SN 0137-1592 J9 ACTA ICHTHYOL PISCAT JI Acta Ichthyol. Piscat. PY 2009 VL 39 IS 1 BP 1 EP 5 DI 10.3750/AIP2009.39.1.01 PG 5 WC Fisheries; Zoology SC Fisheries; Zoology GA 468IK UT WOS:000267810500001 ER PT S AU Klein, M Xiao, YH Hohensee, M Phillips, DF Walsworth, RL AF Klein, Mason Xiao, Yanhong Hohensee, Michael Phillips, David F. Walsworth, Ronald L. BE Shahriar, SM Hemmer, PR Lowell, JR TI Slow light and EIT under realistic (imperfect) conditions SO ADVANCES IN SLOW AND FAST LIGHT II SE Proceedings of SPIE-The International Society for Optical Engineering LA English DT Proceedings Paper CT Conference on Advances in Slow and Fast Light II CY JAN 25-27, 2009 CL San Jose, CA SP SPIE DE Electromagnetically-induced transparency; slow light; stored light; vapor cell; buffer gas; four-wave mixing; optical depth ID ELECTROMAGNETICALLY INDUCED TRANSPARENCY; ATOMIC ENSEMBLES; PHOTON STATES; QUANTUM; ENTANGLEMENT; MEMORY AB We report a preliminary experimental study of EIT and stored light in the high optical depth regime. In particular, we characterize two ways to mitigate radiation trapping, a decoherence mechanism at high atomic density: nitrogen as buffer gas, and a long, narrow cell geometry. Initial results show the promise of both approaches in minimizing radiation trapping, but also reveal problems such as optical pumping into trapped end-states. We also observe distortion in EIT lineshapes at high optical depth, a result of interference from four-wave mixing. Experimental results are in good qualitative agreement with theoretical predictions. C1 [Klein, Mason; Xiao, Yanhong; Hohensee, Michael; Phillips, David F.; Walsworth, Ronald L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Klein, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 27 TC 0 Z9 0 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 978-0-8194-7472-8 J9 P SOC PHOTO-OPT INS PY 2009 VL 7226 AR 72260H DI 10.1117/12.816326 PG 8 WC Optics SC Optics GA BSQ21 UT WOS:000285377800010 ER PT S AU Meibom, S AF Meibom, Soren BE Mamajek, EE Soderblom, DR Wyse, RFG TI Stellar ages from stellar rotation SO AGES OF STARS SE IAU Symposium Proceedings Series LA English DT Proceedings Paper CT 258th Symposium of the International-Astronomical-Union CY OCT 13-17, 2008 CL Baltimore, MD DE stars: rotation; stars: evolution; Galaxy: open clusters and associations: general ID WIYN OPEN CLUSTER; SOLAR-TYPE; RADIAL-VELOCITIES; STARS; GYROCHRONOLOGY; M35 AB Our ability to determine stellar ages from measurements of stellar rotation, hinges on how well we call measure the dependence of rotation oil age for stars of different masses. Rotation periods for stars in open clusters are essential to determine the relations between stellar age, rotation, and mass. Until recently, ambiguities in nu sin i data and lack of cluster membership information, prevented a clear empirical definition of the dependence of rotation oil color. Direct measurements of stellar rotation periods for members in young clusters have now revealed a, well-defined period-color relation. We show new results for the open clusters M35 and M34. However, rotation periods based oil ground-based observations are limited to young clusters. The Hyades represent the oldest coeval population of stars with measured rotation periods. Measurements of rotation periods for older stars are needed to properly constrain the dependence of stellar rotation on age. We present our plans to use the Kepler space telescope to measure rotation periods in clusters as old as and older than the Sun. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Meibom, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM smeibom@cfa.harvard.edu NR 15 TC 0 Z9 0 U1 1 U2 3 PU CAMBRIDGE UNIV PRESS PI CAMBRIDGE PA THE PITT BUILDING, TRUMPINGTON ST, CAMBRIDGE CB2 1RP, CAMBS, ENGLAND SN 1743-9213 BN 978-0-521-88989-6 J9 IAU SYMP P SERIES JI IAU Symposium Proc. Series PY 2009 VL 4 IS 258 BP 357 EP 362 DI 10.1017/S1743921309032013 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BKQ18 UT WOS:000268929300037 ER PT S AU Irwin, J Bouvier, J AF Irwin, Jonathan Bouvier, Jerome BE Mamajek, EE Soderblom, DR Wyse, RFG TI The rotational evolution of low-mass stars SO AGES OF STARS SE IAU Symposium Proceedings Series LA English DT Proceedings Paper CT 258th Symposium of the International-Astronomical-Union CY OCT 13-17, 2008 CL Baltimore, MD DE stars: late-type; stars: low-mass; stars: pre-main-sequence; stars: rotation ID ALPHA-PERSEI CLUSTER; MAIN-SEQUENCE STARS; PHOTOMETRIC LIGHT CURVES; DISK REGULATION PARADIGM; ORION NEBULA CLUSTER; SOLAR-TYPE STARS; STELLAR ROTATION; MONITOR PROJECT; K-DWARFS; SPITZER OBSERVATIONS AB We summarise recent progress in the understanding of the rotational evolution of low-mass stars (here defined as solar mass down to the hydrogen burning limit) both in terms of observations and modelling. Wide-field imaging surveys on moderate-size telescopes can now efficiently derive rotation periods for hundreds to thousands of open cluster members, providing unprecedented sample sizes which are ripe for exploration. We summarise the available measurements, and provide simple phenomenological and model-based interpretations of the presently-available data, while highlighting regions of parameter space where more observations are required, particularly at the lowest; masses and ages greater than or similar to 500 Myr. C1 [Irwin, Jonathan] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Irwin, J (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St MS-16, Cambridge, MA 02138 USA. EM jirwin@cfa.harvard.edu NR 65 TC 3 Z9 3 U1 0 U2 0 PU CAMBRIDGE UNIV PRESS PI CAMBRIDGE PA THE PITT BUILDING, TRUMPINGTON ST, CAMBRIDGE CB2 1RP, CAMBS, ENGLAND SN 1743-9213 BN 978-0-521-88989-6 J9 IAU SYMP P SERIES JI IAU Symposium Proc. Series PY 2009 VL 4 IS 258 BP 363 EP 374 DI 10.1017/S1743921309032025 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BKQ18 UT WOS:000268929300038 ER PT J AU Touwaide, A AF Touwaide, Alain TI TRANSLATION AND TRANSLITERATION OF PLANT NAMES IN HUNAYN B. ISHAQ'S AND ISTIFAN B. BASIL'S ARABIC VERSION OF DIOSCORIDES, DE MATERIA MEDICA SO AL-QANTARA LA English DT Article DE Arabic translation of Ancient Greek texts; Phytonym; Botany; Andalusian botanist; De materia medica; Dioscorides; Hunayn b. Ishaq; Istifan b. Basil AB This paper deals with the Arabic translation of De materia medica by the Greek author Dioscorides (1(st) century A.D.), particularly the rendering of plant names, which were sometimes properly translated and sometimes transliterated from the Greek. According to a traditional interpretation, the transliteration strategy was used by the translators when they did not know the exact Arabic equivalent of the plant names. I re-examine this interpretation here taking into account the role of plant names in the Greek text and the Andalusian works of botanical lexicography. As a result, I propose to interpret transliterations as a mean used by translators to keep visible the structure of the work, in which plant names played a certain role. C1 Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Touwaide, A (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. NR 73 TC 1 Z9 1 U1 0 U2 4 PU CONSEJO SUPERIOR DE INVESTIGACIONES CIENTIFICAS PI MADRID PA VITRUVIO 8, 28006 MADRID, SPAIN SN 0211-3589 J9 AL-QANTARA JI Al-Qantara PY 2009 VL 30 IS 2 BP 557 EP 580 PG 24 WC History; Religion SC History; Religion GA 539YD UT WOS:000273294300010 ER PT J AU Barreiro, J AF Barreiro, Jose TI Caciques and Cemi Idols: The Web Spun by Taino Riders between Hispaniola and Puerto Rico SO AMERICAN INDIAN CULTURE AND RESEARCH JOURNAL LA English DT Book Review C1 [Barreiro, Jose] Smithsonian Natl Museum Amer Indian, Washington, DC USA. RP Barreiro, J (reprint author), Smithsonian Natl Museum Amer Indian, Washington, DC USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU U C L A, AMER INDIAN STUDIES CENTER PI LOS ANGELES PA 3220 CAMPBELL HALL, BOX 951548, LOS ANGELES, CA 90095-1548 USA SN 0161-6463 J9 AM INDIAN CULT RES J JI Am. Indian Cult. Res. J. PY 2009 VL 33 IS 4 BP 160 EP 163 PG 4 WC History SC History GA 548IQ UT WOS:000273955100011 ER PT J AU Bennett, MR Harris, JWK Richmond, BG Braun, DR Mbua, E Kiura, P Olago, D Kibunjia, M AF Bennett, Matthew R. Harris, John W. K. Richmond, Brian G. Braun, David R. Mbua, Emma Kiura, Purity Olago, Daniel Kibunjia, Mzalendo TI New evidence on the evolution of human foot function based on optical laser scanning of early hominin foot prints. SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 78th Annual Meeting of the American-Association-of-Physical-Anthropologists CY MAR 31-APR 03, 2009 CL Chicago, IL SP Amer Assoc Phys Anthropol C1 [Bennett, Matthew R.] Bournemouth Univ, Sch Conservat Sci, Poole BH12 5BB, Dorset, England. [Harris, John W. K.] Rutgers State Univ, Dept Anthropol, Piscataway, NJ 08855 USA. [Richmond, Brian G.] George Washington Univ, Dept Anthropol, Ctr Adv Study Hominid Paleobiol, Washington, DC 20052 USA. [Richmond, Brian G.] Smithsonian Inst, Natl Museum Nat Hist, Human Origins Program, Washington, DC 20560 USA. [Braun, David R.] Univ Cape Town, Dept Archaeol, ZA-7700 Rondebosch, South Africa. [Olago, Daniel] Univ Nairobi, Dept Geol, Nairobi, Kenya. RI Braun, David/C-9680-2009 NR 0 TC 0 Z9 0 U1 1 U2 5 PU WILEY-LISS PI HOBOKEN PA DIV JOHN WILEY & SONS INC, 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2009 BP 88 EP 89 PG 2 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 408NW UT WOS:000263442700067 ER PT J AU Green, DJ Hamrick, MW Richmond, BG AF Green, D. J. Hamrick, M. W. Richmond, B. G. TI Factors contributing to hominoid shoulder morphology: muscle size, ontogeny, and behavior SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 78th Annual Meeting of the American-Association-of-Physical-Anthropologists CY MAR 31-APR 03, 2009 CL Chicago, IL SP Amer Assoc Phys Anthropol C1 [Green, D. J.] George Washington Univ, Hominid Paleobiol Doctral Program, Washington, DC 20052 USA. [Green, D. J.; Richmond, B. G.] George Washington Univ, Ctr Adv Study Hominid Paleobiol, Dept Anthropol, Washington, DC 20052 USA. [Hamrick, M. W.] Med Coll Georgia, Dept Cellular Biol & Anat, Augusta, GA 30912 USA. [Richmond, B. G.] Smithsonian Inst, Natl Museum Nat Hist, Human Origins Program, Washington, DC 20560 USA. RI Hamrick, Mark/K-1131-2016 NR 0 TC 0 Z9 0 U1 0 U2 1 PU WILEY-LISS PI HOBOKEN PA DIV JOHN WILEY & SONS INC, 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2009 BP 138 EP 138 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 408NW UT WOS:000263442700301 ER PT J AU Griffin, NL Richmond, BG D'Aout, K Gordon, AD Aerts, P AF Griffin, N. L. Richmond, B. G. D'Aout, K. Gordon, A. D. Aerts, P. TI Comparative forefoot form and function in Homo sapiens and Pan: joint orientation and in vivo kinematics SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 78th Annual Meeting of the American-Association-of-Physical-Anthropologists CY MAR 31-APR 03, 2009 CL Chicago, IL SP Amer Assoc Phys Anthropol C1 [Griffin, N. L.] George Washington Univ, Dept Anthropol, Ctr Adv Study Hominid Paleobiol, Hominid Paleobiol Doctoral Program, Washington, DC 20052 USA. [Richmond, B. G.] Smithsonian Inst, Natl Museum Nat Hist, Human Origins Program, Washington, DC 20560 USA. [D'Aout, K.; Aerts, P.] Univ Antwerp, Dept Biol, Antwerp, Belgium. [D'Aout, K.] Royal Zool Soc Antwerp, Ctr Res & Conservat, Antwerp, Belgium. [Gordon, A. D.] SUNY Albany, Dept Anthropol, Albany, NY 12222 USA. [Aerts, P.] Univ Ghent, Dept Movement & Sport Sci, Ghent, Belgium. NR 0 TC 0 Z9 0 U1 1 U2 4 PU WILEY-LISS PI HOBOKEN PA DIV JOHN WILEY & SONS INC, 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2009 BP 139 EP 140 PG 2 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 408NW UT WOS:000263442700306 ER PT J AU Jungers, WL Falk, D Hildebolt, C Smith, K Prior, F Tocheri, MW Orr, CM Burnett, SE Larson, SG Djubiantono, T Morwood, MJ AF Jungers, W. L. Falk, D. Hildebolt, C. Smith, K. Prior, F. Tocheri, M. W. Orr, C. M. Burnett, S. E. Larson, S. G. Djubiantono, T. Morwood, M. J. TI The hobbits (Homo floresiensis) were not cretins. SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 78th Annual Meeting of the American-Association-of-Physical-Anthropologists CY MAR 31-APR 03, 2009 CL Chicago, IL SP Amer Assoc Phys Anthropol C1 [Jungers, W. L.; Larson, S. G.] SUNY Stony Brook, Dept Anat Sci, Med Ctr, Stony Brook, NY USA. [Falk, D.] Florida State Univ, Dept Anthropol, Tallahassee, FL 32306 USA. [Hildebolt, C.; Smith, K.; Prior, F.] Washington Univ, Mallinckrodt Inst Radiol, Sch Med, St Louis, MO 63130 USA. [Tocheri, M. W.] Smithsonian Inst, Dept Anthropol, Human Origins Program, Washington, DC 20560 USA. [Orr, C. M.] Arizona State Univ, Inst Human Origins, Tempe, AZ 85287 USA. [Burnett, S. E.] Eckerd Coll, Comparat Cultures Coll, St Petersburg, FL USA. [Djubiantono, T.] Natl Res & Dev Ctr Archaeol, Jakarta, Indonesia. [Morwood, M. J.] Univ Wollongong, Sch Earth & Environm Sci, Wollongong, NSW 2522, Australia. NR 0 TC 2 Z9 2 U1 3 U2 5 PU WILEY-LISS PI HOBOKEN PA DIV JOHN WILEY & SONS INC, 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2009 BP 161 EP 161 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 408NW UT WOS:000263442700410 ER PT J AU Mulhern, DM Wilczak, CA Jones, EB AF Mulhern, D. M. Wilczak, C. A. Jones, E. B. TI The problem of distinguishing spina bifida occulta from clefting without neural tube defect in the sacrum: what is an anthropologist to do? SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 78th Annual Meeting of the American-Association-of-Physical-Anthropologists CY MAR 31-APR 03, 2009 CL Chicago, IL SP Amer Assoc Phys Anthropol C1 [Mulhern, D. M.] Ft Lewis Coll, Dept Anthropol, Durango, CO USA. [Wilczak, C. A.] San Francisco State Univ, Dept Anthropol, San Francisco, CA USA. [Jones, E. B.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 2 U2 4 PU WILEY-LISS PI HOBOKEN PA DIV JOHN WILEY & SONS INC, 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2009 BP 195 EP 195 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 408NW UT WOS:000263442701089 ER PT J AU Pearlstein, KE Hunt, DR AF Pearlstein, K. E. Hunt, D. R. TI Assessment of pathological conditions in the Huntington Collection, Smithsonian Institution SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 78th Annual Meeting of the American-Association-of-Physical-Anthropologists CY MAR 31-APR 03, 2009 CL Chicago, IL SP Amer Assoc Phys Anthropol C1 [Pearlstein, K. E.] American Univ, Dept Anthropol, Washington, DC 20016 USA. [Hunt, D. R.] Smithsonian Inst, Dept Anthropol, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU WILEY-LISS PI HOBOKEN PA DIV JOHN WILEY & SONS INC, 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2009 BP 208 EP 208 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 408NW UT WOS:000263442701147 ER PT J AU Potts, R AF Potts, R. TI Presenting human evolution at the Smith-sonian: 'What does it mean to be human?' SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 78th Annual Meeting of the American-Association-of-Physical-Anthropologists CY MAR 31-APR 03, 2009 CL Chicago, IL SP Amer Assoc Phys Anthropol C1 [Potts, R.] Smithsonian Inst, Human Origins Program, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU WILEY-LISS PI HOBOKEN PA DIV JOHN WILEY & SONS INC, 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2009 BP 214 EP 214 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 408NW UT WOS:000263442701175 ER PT J AU Richmond, BG Harris, JWK Mbua, E Braun, DR Bamford, M Bobe, R Green, DJ Griffin, NL Mccoy, JT Merritt, S Pante, M Pobiner, B Carter-Menn, H Chirchir, H Kiura, P Kibunjia, M AF Richmond, B. G. Harris, J. W. K. Mbua, E. Braun, D. R. Bamford, M. Bobe, R. Green, D. J. Griffin, N. L. McCoy, J. T. Merritt, S. Pante, M. Pobiner, B. Carter-Menn, H. Chirchir, H. Kiura, P. Kibunjia, M. TI Divergence in hominin upper limb anatomy in the early Pleistocene SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 78th Annual Meeting of the American-Association-of-Physical-Anthropologists CY MAR 31-APR 03, 2009 CL Chicago, IL SP Amer Assoc Phys Anthropol C1 [Richmond, B. G.] George Washington Univ, Dept Anthropol, Ctr Adv Study Hominid Paleobiol, Washington, DC 20052 USA. [Richmond, B. G.; Pobiner, B.] Smithsonian Inst, Human Origins Program, Natl Museum Nat Hist, Washington, DC 20560 USA. [Harris, J. W. K.; McCoy, J. T.; Merritt, S.; Pante, M.] Rutgers State Univ, Dept Anthropol, Piscataway, NJ 08855 USA. [Braun, D. R.] Univ Cape Town, Dept Archaeol, ZA-7700 Rondebosch, South Africa. [Bamford, M.] Univ Witwatersrand, BPI Palaeontol, ZA-2050 Wits, South Africa. [Bobe, R.] Univ Georgia, Dept Anthropol, Athens, GA 30602 USA. [Green, D. J.; Griffin, N. L.; Chirchir, H.] George Washington Univ, Hominid Paleobiol Doctoral Program, Dept Anthropol, Washington, DC 20052 USA. [Carter-Menn, H.] NYU, Dept Anthropol, New York, NY 10003 USA. RI Braun, David/C-9680-2009 NR 0 TC 0 Z9 0 U1 1 U2 4 PU WILEY-LISS PI HOBOKEN PA DIV JOHN WILEY & SONS INC, 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2009 BP 221 EP 221 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 408NW UT WOS:000263442701208 ER PT J AU Williams, EM Gordon, AD Richmond, BG AF Williams, E. M. Gordon, A. D. Richmond, B. G. TI Wrist and upper limb kinematics of amateur knappers during stone tool production SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 78th Annual Meeting of the American-Association-of-Physical-Anthropologists CY MAR 31-APR 03, 2009 CL Chicago, IL SP Amer Assoc Phys Anthropol C1 [Williams, E. M.] George Washington Univ, Ctr Adv Study Hominid Paleobiol, Dept Anthropol, Hominid Paleobiol Doctoral Program, Washington, DC 20052 USA. [Gordon, A. D.] SUNY Albany, Dept Anthropol, Albany, NY 12222 USA. [Richmond, B. G.] Smithsonian Inst, Natl Museum Nat Hist, Human Origins Program, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU WILEY-LISS PI HOBOKEN PA DIV JOHN WILEY & SONS INC, 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2009 BP 272 EP 272 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 408NW UT WOS:000263442701446 ER PT J AU Sun, BL Zhang, CQ Lowry, PP Wen, J AF Sun, Bao-Ling Zhang, Chang-Qin Lowry, Porter P., II Wen, Jun TI CRYPTIC DIOECY IN NYSSA YUNNANENSIS (NYSSACEAE), A CRITICALLY ENDANGERED SPECIES FROM TROPICAL EASTERN ASIA SO ANNALS OF THE MISSOURI BOTANICAL GARDEN LA English DT Article DE Androdioecy; critically endangered; cryptic dioecy; floral phenology; IUCN Red List; Nyssa; Nyssa yunnanensis; Nyssaceae; pollen viability ID PLANT DATISCA-GLOMERATA; FOREST TREES; FLOWERING PLANTS; SEX-RATIOS; EVOLUTION; GENDER; REPRODUCTION; ANDRODIOECY; POPULATIONS; POLLINATION AB Nyssa yunnanensis W. Q. Yin ex H. N. Qin & Phengklai (Nyssaceae) is a critically endangered range-restricted tree species known from only three small populations in a tropical forest area of southern Yunnan Province, southwestern China. Two types, of individuals occur, one bearing staminate flowers and the other with morphologically perfect flowers that produce both pollen and fruit suggesting an androdioecious breeding system. Field an(] laboratory studies conducted between 2004 and 2007 indicate, however, that N yunnanensis is functionally dioecious: pollen front the morphologically perfect flowers is inaperturate and inviable, rendering the trees that bear these flowers functionally female. Field observations showed that the staminate flowers opened 10 to 15 (lays earlier than the protogynous female flowers hot that flowering ceased ill nearly the same time in both sexes. Thirty-six species of insects were observed and collected visting the flowers of N. yunnanensis, four of which served as effective pollinators. Breeding system experiments demonstrated that the predominantly entomophilous pollination system is supplemented by anemophily and further indicated that X yunnanensis is xenogamous and does not appear to exhibit parthenogenesis. The average sex ratio of individuals within the three populations was female-biased (0.5-1:1), but the ratio among flowers was male-biased (2.56:1) because flower production was higher in males. The 37 known trees of N. yunnanensis are likely the remnants of a once more widespread, abundant species that has been heavily impacted by human disturbance, it fine shared with many other threatened Southeast Asian taxa whose continued survival will require dedicated conservation efforts informed by it detailed understanding of population structure an(] reproductive biology. C1 [Sun, Bao-Ling; Zhang, Chang-Qin] Chinese Acad Sci, Kunming Inst Bot, Kunming 650204, Yunnan, Peoples R China. [Sun, Bao-Ling] Chinese Acad Sci, Grad Sch, Beijing 100049, Peoples R China. [Lowry, Porter P., II] Missouri Bot Garden, St Louis, MO 63166 USA. [Lowry, Porter P., II] Museum Natl Hist Nat, Dept Systemat & Evolut, F-75231 Paris 05, France. [Wen, Jun] Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Sun, BL (reprint author), Chinese Acad Sci, Kunming Inst Bot, 132 Lanhei Rd, Kunming 650204, Yunnan, Peoples R China. EM zhangchangqin@mail.kib.ac.cn; wenj@si.edu NR 67 TC 6 Z9 7 U1 0 U2 11 PU MISSOURI BOTANICAL GARDEN PI ST LOUIS PA 2345 TOWER GROVE AVENUE, ST LOUIS, MO 63110 USA SN 0026-6493 J9 ANN MO BOT GARD JI Ann. Mo. Bot. Gard. PY 2009 VL 96 IS 4 BP 672 EP 684 DI 10.3417/2008015 PG 13 WC Plant Sciences SC Plant Sciences GA 541HT UT WOS:000273406600005 ER PT J AU Lewis, SL Lloyd, J Sitch, S Mitchard, ETA Laurance, WF AF Lewis, Simon L. Lloyd, Jon Sitch, Stephen Mitchard, Edward T. A. Laurance, William F. TI Changing Ecology of Tropical Forests: Evidence and Drivers SO ANNUAL REVIEW OF ECOLOGY EVOLUTION AND SYSTEMATICS SE Annual Review of Ecology Evolution and Systematics LA English DT Review; Book Chapter DE carbon balance; carbon dioxide; climate change; Dynamic Global Vegetation Model; Earth observation; ecosystem respiration; eddy-covariance; long-term monitoring plots; global change; tree growth; tree mortality; tree recruitment ID ELEVATED ATMOSPHERIC CO2; AMAZONIAN RAIN-FOREST; CARBON-DIOXIDE UPTAKE; LONG-TERM PLOTS; GLOBAL CHANGE; PERVASIVE ALTERATION; DECADAL VARIABILITY; PLANT RESPIRATION; TREE COMMUNITIES; CLIMATE-CHANGE AB Global environmental changes may be altering the ecology of tropical forests. Long-term monitoring plots have provided much of the evidence for large-scale, directional changes in tropical forests, but the results have been controversial. Here we review evidence from six complementary approaches to understanding possible changes: plant physiology experiments, long-term monitoring plots, ecosystem flux techniques, atmospheric measurements, Earth observations, and global-scale vegetation models. Evidence from four of these approaches suggests that large-scale, directional changes are occurring in the ecology of tropical forests, with the other two approaches providing inconclusive results. Collectively, the evidence indicates that both gross and net primary productivity has likely increased over recent decades, as have tree growth, recruitment, and mortality rates, and forest biomass. These results suggest a profound reorganization of tropical forest ecosystems. We evaluate the most likely drivers of the suite of changes, and suggest increasing resource availability, potentially from rising atmospheric CO2 concentrations, is the most likely cause. C1 [Lewis, Simon L.; Lloyd, Jon; Sitch, Stephen] Univ Leeds, Sch Geog, Earth & Biosphere Inst, Leeds LS2 9JT, W Yorkshire, England. [Sitch, Stephen] Hadley Ctr, Met Off, Exeter EX1 3PB, Devon, England. [Mitchard, Edward T. A.] Univ Edinburgh, Sch Geosci, Edinburgh EH9 3JW, Midlothian, Scotland. [Laurance, William F.] James Cook Univ, Sch Marine & Trop Biol, Cairns, Qld 4870, Australia. [Laurance, William F.] Smithsonian Trop Res Inst, Balboa 340020948, Ancon, Panama. RP Lewis, SL (reprint author), Univ Leeds, Sch Geog, Earth & Biosphere Inst, Leeds LS2 9JT, W Yorkshire, England. EM s.l.lewis@leeds.ac.uk RI Lloyd, Jonathan/F-8893-2010; Laurance, William/B-2709-2012; Sitch, Stephen/F-8034-2015; OI Lloyd, Jonathan/0000-0002-5458-9960; Sitch, Stephen/0000-0003-1821-8561; Mitchard, Edward/0000-0002-5690-4055; Lewis, Simon/0000-0002-8066-6851 FU Royal Society University Research Fellowship FX We thank Luiz Aragao for preparing Figure 1, Manuel Gloor and Oliver Phillips for discussions, and Lars Hedin for valuable comments on the manuscript. S.L.L is supported by a Royal Society University Research Fellowship. NR 111 TC 124 Z9 129 U1 13 U2 117 PU ANNUAL REVIEWS PI PALO ALTO PA 4139 EL CAMINO WAY, PO BOX 10139, PALO ALTO, CA 94303-0139 USA SN 1543-592X EI 1545-2069 J9 ANNU REV ECOL EVOL S JI Annu. Rev. Ecol. Evol. Syst. PY 2009 VL 40 BP 529 EP 549 DI 10.1146/annurev.ecolsys.39.110707.173345 PG 21 WC Ecology; Evolutionary Biology SC Environmental Sciences & Ecology; Evolutionary Biology GA 528OI UT WOS:000272455700025 ER PT J AU Rhainds, M Davis, DR Price, PW AF Rhainds, Marc Davis, Donald R. Price, Peter W. TI Bionomics of Bagworms (Lepidoptera: Psychidae) SO ANNUAL REVIEW OF ENTOMOLOGY SE Annual Review of Entomology LA English DT Review; Book Chapter DE bottom-up effects; flightlessness; mating failure; parthenogeny; phylogenetic constraint hypothesis; protogyny ID THYRIDOPTERYX-EPHEMERAEFORMIS LEPIDOPTERA; OIKETICUS-KIRBYI LEPIDOPTERA; PLANA WALKER LEPIDOPTERA; CLANIA-CRAMERII WESTWOOD; METISA-PLANA; HAWORTH LEPIDOPTERA; SEX-PHEROMONE; FEMALE BAGWORMS; PUPATION SITE; REPRODUCTIVE OUTPUT AB The bagworm family (Lepidoptera: Psychidae) includes approximately 1000 species, all of which complete larval development within a self-enclosing bag. The family is remarkable in that female aptery Occurs in over half of the known species and within 9 of the 10 currently recognized subfamilies. In the more derived subfamilies, several life-history traits ire associated with eruptive population dynamics, e.g., neoteny of females, high fecundity dispersal on silken threads, and high level of polyphagy. Other salient features shared by many species include a short embryonic period, developmental synchrony; sexual segregation of pupation sites, short longevity of adults, male-biased sex ratio, sexual dimorphism, protogyny, parthenogenesis, and oviposition in the pupal case. The unusual mating behavior of bagworms, characterized by an earlier emergence of females than males and a high proportion of females that do not mate as adults, challenges conventional wisdom regarding the evolution of mating systems. C1 [Rhainds, Marc] Purdue Univ, Dept Entomol, W Lafayette, IN 47901 USA. [Davis, Donald R.] Smithsonian Inst, Dept Entomol, Washington, DC 20013 USA. [Price, Peter W.] No Arizona Univ, Dept Biol Sci, Flagstaff, AZ 86011 USA. RP Rhainds, M (reprint author), Purdue Univ, Dept Entomol, W Lafayette, IN 47901 USA. EM mrhainds@purdue.edu; davisd@si.edu; peter.price@nau.edu NR 116 TC 38 Z9 40 U1 1 U2 13 PU ANNUAL REVIEWS PI PALO ALTO PA 4139 EL CAMINO WAY, PO BOX 10139, PALO ALTO, CA 94303-0139 USA SN 0066-4170 EI 1545-4487 J9 ANNU REV ENTOMOL JI Annu. Rev. Entomol. PY 2009 VL 54 BP 209 EP 226 DI 10.1146/annurev.ento.54.110807.090448 PG 18 WC Entomology SC Entomology GA 394VX UT WOS:000262482300012 PM 18767982 ER PT J AU Breitburg, DL Hondorp, DW Davias, LA Diaz, RJ AF Breitburg, Denise L. Hondorp, Darryl W. Davias, Lori A. Diaz, Robert J. TI Hypoxia, Nitrogen, and Fisheries: Integrating Effects Across Local and Global Landscapes SO ANNUAL REVIEW OF MARINE SCIENCE SE Annual Review of Marine Science LA English DT Review; Book Chapter DE low dissolved oxygen; eutrophication; estuaries; fish; macroinvertebrates; scale ID GULF-OF-MEXICO; LOW DISSOLVED-OXYGEN; COD GADUS-MORHUA; COASTAL MARINE ECOSYSTEMS; NEUSE RIVER ESTUARY; ATLANTIC BLUE-CRAB; LONG-ISLAND SOUND; BALTIC COD; CHESAPEAKE BAY; WATER-QUALITY AB Anthropogenic nutrient enrichment and physical characteristics result ill low dissolved oxygen concentrations (hypoxia) in estuaries and semienclosed seas throughout the world. Published research indicates that within and near oxygen-depleted waters, finfish and mobile macroinvertebrates experience negative effects that range from mortality to altered trophic interactions. Chronic exposure to hypoxia and fluctuating oxygen concentrations impair reproduction, immune responses, and growth. We present an analysis of hypoxia, nitrogen loadings, and fisheries landings in 30 estuaries and semien-closed seas worldwide. Our results suggest that hypoxia does not typically reduce systemwide fisheries landings below what would be predicted from nitrogen loadings, except where raw sewage is released or particularly sensitive species lose critical habitat. A number of compensatory mechanisms limit the translation of local-scale effects of hypoxia to the scale of the whole system. Hypoxia is, however, a serious environmental challenge that should be considered in fisheries management strategies and be a direct target of environmental restoration. C1 [Breitburg, Denise L.; Hondorp, Darryl W.; Davias, Lori A.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Diaz, Robert J.] Coll William & Mary, Virginia Inst Marine Sci, Gloucester Point, VA 23062 USA. RP Breitburg, DL (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM breitburgd@si.edu; hondorpd@si.edu; daviasl@si.edu; Diaz@vims.edu FU NOAA-Center for Sponsored Coastal Ocean Research; Smithsonian Marine Science Network FX The cross-system comparison we present could not have been possible without the help of nearly one hundred agencies and colleagues from around the world who generously provided their data and advice, and ran additional analyses to help with this effort. These people are listed in the Supplemental Material. Funding for this project was provided by NOAA-Center for Sponsored Coastal Ocean Research and the Smithsonian Marine Science Network. NR 111 TC 136 Z9 139 U1 11 U2 105 PU ANNUAL REVIEWS PI PALO ALTO PA 4139 EL CAMINO WAY, PO BOX 10139, PALO ALTO, CA 94303-0139 USA SN 1941-1405 EI 1941-0611 J9 ANNU REV MAR SCI JI Annu. Rev. Mar. Sci. PY 2009 VL 1 BP 329 EP 349 DI 10.1146/annurev.marine.010908.163754 PG 21 WC Geochemistry & Geophysics; Marine & Freshwater Biology; Oceanography SC Geochemistry & Geophysics; Marine & Freshwater Biology; Oceanography GA 463HH UT WOS:000267421700014 PM 21141040 ER PT B AU Braatz, JA Reid, MJ Greenhill, LJ Kuo, CY Condon, JJ Lo, KY Henkel, C AF Braatz, J. A. Reid, M. J. Greenhill, L. J. Kuo, C. -Y. Condon, J. J. Lo, K. -Y. Henkel, C. BE Hagiwara, Y Fomalont, E Tsuboi, M Murata, Y TI Water Masers in AGN Accretion Disks SO APPROACHING MICRO-ARCSECOND RESOLUTION WITH VSOP-2: ASTROPHYSICS AND TECHNOLOGY SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT Workshop on Approaching Micro-Arcsecond Resolution with VSOP-2 CY DEC 03-07, 2007 CL Inst Space & Astronaut Sci, Kanagawa, JAPAN SP Natl Astron Observ Japan, Soc Promot Space Sci, Inoue Fdn Sci, Fdn Promot Astron HO Inst Space & Astronaut Sci ID ACTIVE GALAXY NGC-4258; GEOMETRIC DISTANCE; EMISSION AB Water vapor masers at 22 GHz have been detected in over 100 galaxies, most of them AGNs. High resolution VLBI observations of these masers provide the only opportunity for direct imaging of sub-paxsec structure in AGN accretion disks. The key science goals associated with such observations are concentrated in two areas. First, observations of nearby, bright sources, exemplified by NGC 4258, enable unique investigations of accretion disk geometry, substructure, thickness, and rotation properties. Second, when combined with spectral line monitoring, VLBI imaging and subsequent disk modeling enables the estimation of a distance to the host galaxy independent of standard candle arguments. In this contribution we present VLBI observations of two maser disk systems in galaxies well into the Hubble flow, UGC 3789 and NGC 6323. A long term goal in these studies is to measure the Hubble constant with high precision and, as a complement to CMB observations, constrain several key cosmological parameters, including the equation of state for dark energy. Observations with VSOP-2 at 22 GHz will have the resolution critical for mapping substructure in these accretion disks and will contribute to reducing systematic errors in the measurement of distances to galaxies. C1 [Braatz, J. A.; Kuo, C. -Y.; Condon, J. J.; Lo, K. -Y.] Natl Radio Astron Observ, 520 Edgemont Rd, Charlottesville, VA 22903 USA. [Reid, M. J.; Greenhill, L. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kuo, C. -Y.] Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA. [Henkel, C.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. RP Braatz, JA (reprint author), Natl Radio Astron Observ, 520 Edgemont Rd, Charlottesville, VA 22903 USA. NR 12 TC 1 Z9 2 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-679-0 J9 ASTR SOC P PY 2009 VL 402 BP 274 EP + PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BLE30 UT WOS:000270005100058 ER PT J AU O'Dea, A AF O'Dea, Aaron TI Relation of form to life habit in free-living cupuladriid bryozoans SO AQUATIC BIOLOGY LA English DT Article DE Cupuladria spp.; Discoporella spp.; Lunulitiform; Realised niche; Life mode; Soft sediments; Disturbance; Form and function ID TROPICAL AMERICA; NEOGENE CUPULADRIIDAE; SELENARIA BRYOZOA; OPPOSITE SIDES; PANAMA; ISTHMUS; DISPERSAL; CHEILOSTOMATA; DISCOPORELLA; COMPETITION AB Since the late Mesozoic, several bryozoan groups have occupied unstable soft-sediment habitats by adopting a free-living and motile mode of life. Today, the free-living bryozoans often dominate epibenthic faunal communities in these expansive habitats, yet their biology and ecology remain poorly understood. This study examines their unique mode of life by exploring the relationship between form and function in the free-living Cupuladriidae of tropical America. Cupuladriid species occupy distinct niches in water depth and sediment type, and these variables correlate with a variety of morphological traits amongst species, thereby helping formulate hypotheses on functional morphology. These hypotheses were tested with disturbance, burial and mobility experiments. Species deal both passively and actively with disturbance and burial. Colony size and shape passively influences colony stability on the sea floor, susceptibility to burial and the ability to emerge once buried. Movable mandibles (setae) assist in emergence following burial, actively increase colony stability, and deter the settlement and disruption of encrusting growth of other organisms. Mandibles also enable colonies to move over the sea floor, but such behaviour appears to be of minimal benefit to avoid predation or to influence dispersal. Disturbance on the sea floor is the most important factor in driving the convergent evolution of the mobile free-living form. Colony shape and size and the employment of mandibles to improve stability, return to the surface after burial, and remove epibiota are central to the post-Mesozoic success of free-living bryozoans. C1 Smithsonian Trop Res Inst, Panama City, Panama. RP O'Dea, A (reprint author), Smithsonian Trop Res Inst, MRC 0580-01,Apartado 0843-03092, Panama City, Panama. EM odeaa@si.edu RI O'Dea, Aaron/D-4114-2011 FU Smithsonian Tropical Research Institute; National Science Foundation [EAR03-45471]; SENACYT; National Geographic Exploration Grant FX J. B. C. Jackson was instrumental in the conception of this study and F. Rodriguez helped in myriad ways with its implementation. B. DeGracia and Y. DelValle sorted thousands of bryozoan colonies. Collections were made by many, including M. Dick, H. Fortunato, A. Herrera, J. Jara, M. Pacheco, L. Ramalho, T. Smith and the crew of RV 'Urraca'. W. Green and S. Punyasena helped with statistical analyses. J. Ceballos helped produce the scanning electron micrographs. The manuscript benefited greatly from discussion and comments from A. N. Ostrovsky, S. Jagadeeshan, B. Okamura, P. D. Taylor and 3 anonymous reviewers. I would like to thank the Republic of Panama and the Kuna Nation for permission to collect. Financial support was provided by the Tupper fellowship program at the Smithsonian Tropical Research Institute, National Science Foundation grant (EAR03-45471), SENACYT and a National Geographic Exploration Grant. NR 66 TC 11 Z9 11 U1 0 U2 3 PU INTER-RESEARCH PI OLDENDORF LUHE PA NORDBUNTE 23, D-21385 OLDENDORF LUHE, GERMANY SN 1864-7790 J9 AQUAT BIOL JI Aquat. Biol. PY 2009 VL 7 IS 1-2 BP 1 EP 18 DI 10.3354/ab00175 PG 18 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 529BK UT WOS:000272490500001 ER PT J AU Willis, KJ Woods, CMC Ashton, GV AF Willis, Kate J. Woods, Chris M. C. Ashton, Gail V. TI Caprella mutica in the Southern Hemisphere: Atlantic origins, distribution, and reproduction of an alien marine amphipod in New Zealand SO AQUATIC BIOLOGY LA English DT Article DE Caprellid amphipod; Bioinvasion; COI gene; Population genetics; Population biology; Dispersal; Hull fouling ID DNA; EVOLUTION AB The caprellid amphipod Caprella mutica, a native of northeast Asia, was first detected in the Southern Hemisphere in the Port of Timaru, New Zealand, in 2002. It has since become established in the Port of Lyttelton and at 2 aquaculture sites in the Marlborough Sounds in New Zealand. Direct sequencing of C. mutica mitochondrial DNA (cytochrome c oxidase subunit I gene) identified 3 haplotypes: 1 unique to New Zealand and 2 previously found in non-native Atlantic populations. Higher haplotype diversity and lower F(ST) distances between the Port of Lyttelton and global populations suggest Lyttelton may be the introduction site in New Zealand. C. mutica populations were sampled on 7 occasions, primarily in winter, and densities generally exceeded 10 000 ind. m(-2), contrasting with the winter declines seen in native and European populations. Sex ratios were generally close to 0.5 and the proportion of brooding females ranged from 0 to 98%. In the Marlborough Sounds, juveniles comprised 32 to 38% of the population regardless of season, brooding females were present throughout the year and males were dominant in winter. Population structure and adult size in the Port of Lyttelton differed with habitat type in August 2008; densities were higher, adults significantly larger on floating than on fixed structures and juveniles and brooding females dominated on vessel hulls, Given the high level of anthropogenic activity and connectivity between coastal locations, it is likely that C. mutica will continue to spread in New Zealand. C1 [Willis, Kate J.; Woods, Chris M. C.] Natl Inst Water & Atmospher Res, Christchurch, New Zealand. [Ashton, Gail V.] Smithsonian Environm Res Ctr, Tiburon, CA 94920 USA. RP Willis, KJ (reprint author), Natl Inst Water & Atmospher Res, POB 8602, Christchurch, New Zealand. EM k.willis@niwa.co.nz FU Lyttelton Port Company FX Thank you to Dr. G. Ruiz, J. Hunt, A. Ormos, Dr. R. Pratt and the Smithsonian's Laboratories of Analytical Biology (LAB), Suitland, Maryland, USA, for assistance with the genetic analyses, and L. Peacock for Figs. 1 & 2. The assistance of the following NIWA (National Institute for Water and Atmospheric Research) personnel during field collections of Caprella mutica is gratefully acknowledged: D. Cairney, N. Davey, M. Kospartov, S. Miller, K. Neill, L. Peacock and K. Schimanski. Access to structures within the Port of Lyttelton was granted by the Lyttelton Port Company, and to fish and mussel farm sites in the Marlborough Sounds from The New Zealand King Salmon Company and Marlborough Mussel Company, respectively. Thank you to G. Fenwick for his comments on an earlier draft of this manuscript and the journal reviewers for their comments by which the manuscript was improved. NR 32 TC 4 Z9 6 U1 0 U2 7 PU INTER-RESEARCH PI OLDENDORF LUHE PA NORDBUNTE 23, D-21385 OLDENDORF LUHE, GERMANY SN 1864-7790 J9 AQUAT BIOL JI Aquat. Biol. PY 2009 VL 7 IS 3 BP 249 EP 259 DI 10.3354/ab00197 PG 11 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 544TE UT WOS:000273681400007 ER PT J AU Fitzhugh, WW AF Fitzhugh, William W. TI Stone Shamans and Flying Deer of Northern Mongolia: Deer Goddess of Siberia or Chimera of the Steppe? SO ARCTIC ANTHROPOLOGY LA English DT Article AB Mongolia's Bronze Age deer stones are one of the most striking expressions of early monumental art in Central Asia, yet their age, origins, relationships, and meaning remain obscure. Speculation about Scythian connections has stimulated recent research in Mongolia that has begun to peel away their mysteries and reveals connections to Scytho-Siberian and northern art. Radiocarbon-dated horse skulls indicate pre-Scythian ages of "classic Mongolian" deer stones as well as firm association with the Late Bronze Age khirigsuur [kurgan] burial mound complex. C1 Natl Museum Nat Hist, Smithsonian Inst, Arctic Studies Ctr, Dept Anthropol, Washington, DC 20560 USA. RP Fitzhugh, WW (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Arctic Studies Ctr, Dept Anthropol, Nat Hist Bldg,10th & Constitut NW,MRC112, Washington, DC 20560 USA. NR 33 TC 8 Z9 8 U1 0 U2 2 PU UNIV WISCONSIN PRESS PI MADISON PA JOURNAL DIVISION, 1930 MONROE ST, 3RD FL, MADISON, WI 53711 USA SN 0066-6939 J9 ARCTIC ANTHROPOL JI Arct. Anthropol. PY 2009 VL 46 IS 1-2 BP 72 EP 88 PG 17 WC Anthropology SC Anthropology GA 550GN UT WOS:000274116400007 ER PT J AU Cockell, CS Leger, A Fridlund, M Herbst, TM Kaltenegger, L Absil, O Beichman, C Benz, W Blanc, M Brack, A Chelli, A Colangeli, L Cottin, H du Foresto, FC Danchi, WC Defrere, D den Herder, JW Eiroa, C Greaves, J Henning, T Johnston, KJ Jones, H Labadie, L Lammer, H Launhardt, R Lawson, P Lay, OP LeDuigou, JM Liseau, R Malbet, F Martin, SR Mawet, D Mourard, D Moutou, C Mugnier, LM Ollivier, M Paresce, F Quirrenbach, A Rabbia, YD Raven, JA Rottgering, HJA Rouan, D Santos, NC Selsis, F Serabyn, E Shibai, H Tamura, M Thiebaut, E Westall, F White, GJ AF Cockell, C. S. Leger, A. Fridlund, M. Herbst, T. M. Kaltenegger, L. Absil, O. Beichman, C. Benz, W. Blanc, M. Brack, A. Chelli, A. Colangeli, L. Cottin, H. du Foresto, F. Coude Danchi, W. C. Defrere, D. den Herder, J. -W. Eiroa, C. Greaves, J. Henning, T. Johnston, K. J. Jones, H. Labadie, L. Lammer, H. Launhardt, R. Lawson, P. Lay, O. P. LeDuigou, J. -M. Liseau, R. Malbet, F. Martin, S. R. Mawet, D. Mourard, D. Moutou, C. Mugnier, L. M. Ollivier, M. Paresce, F. Quirrenbach, A. Rabbia, Y. D. Raven, J. A. Rottgering, H. J. A. Rouan, D. Santos, N. C. Selsis, F. Serabyn, E. Shibai, H. Tamura, M. Thiebaut, E. Westall, F. White, G. J. TI Darwin-A Mission to Detect and Search for Life on Extrasolar Planets SO ASTROBIOLOGY LA English DT Review DE Darwin; Extrasolar planets; Orbital telescopes; M stars; Earth-like planets; Interferometry ID EARTH-LIKE PLANETS; IN HABITABLE ZONES; HIGH-RESOLUTION SIMULATIONS; EJECTION CME ACTIVITY; MAIN-SEQUENCE STARS; MASS M-STARS; NULLING INTERFEROMETERS; SPECTRAL SIGNATURES; SYNTHETIC SPECTRA; TERRESTRIAL ATMOSPHERES AB The discovery of extrasolar planets is one of the greatest achievements of modern astronomy. The detection of planets that vary widely in mass demonstrates that extrasolar planets of low mass exist. In this paper, we describe a mission, called Darwin, whose primary goal is the search for, and characterization of, terrestrial extrasolar planets and the search for life. Accomplishing the mission objectives will require collaborative science across disciplines, including astrophysics, planetary sciences, chemistry, and microbiology. Darwin is designed to detect rocky planets similar to Earth and perform spectroscopic analysis at mid-infrared wavelengths (6-20 mu m), where an advantageous contrast ratio between star and planet occurs. The baseline mission is projected to last 5 years and consists of approximately 200 individual target stars. Among these, 25-50 planetary systems can be studied spectroscopically, which will include the search for gases such as CO2, H2O, CH4, and O-3. Many of the key technologies required for the construction of Darwin have already been demonstrated, and the remainder are estimated to be mature in the near future. Darwin is a mission that will ignite intense interest in both the research community and the wider public. C1 [Cockell, C. S.] Open Univ, CEPSAR, Milton Keynes MK7 6AA, Bucks, England. [Leger, A.; Ollivier, M.] Univ Paris 11, Inst Astrophys Spatiale, Orsay, France. [Fridlund, M.] European Space Agcy, Estec, Astrophys Miss Div, NL-2200 AG Noordwijk, Netherlands. [Herbst, T. M.; Henning, T.; Labadie, L.; Launhardt, R.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Kaltenegger, L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Absil, O.; Chelli, A.; Malbet, F.] Univ Grenoble 1, CNRS, Astrophys Lab, Grenoble, France. [Beichman, C.] CALTECH, Michelson Sci Ctr, Pasadena, CA 91125 USA. [Benz, W.] Univ Bern, Inst Phys, Bern, Switzerland. [Blanc, M.] Observ Midi Pyrenees, F-31400 Toulouse, France. [Brack, A.] CNPS, Ctr Biophys Mol, Orleans, France. [Colangeli, L.] Osserv Astron Capodimonte, INAF, I-80131 Naples, Italy. [Cottin, H.] Univ Paris 12, Lab Interuniv Syst Atmospher, Creteil, France. [Cottin, H.] Univ Paris 07, CNRS, Creteil, France. [du Foresto, F. Coude] Observ Paris, LESIA, Meudon, France. [Danchi, W. C.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Defrere, D.] Inst Astrophys & Geophys Liege, Liege, Belgium. [den Herder, J. -W.] SRON, Netherlands Inst Space Res, Utrecht, Netherlands. [Eiroa, C.] Univ Autonoma Madrid, Dept Fis Teor C11, Fac Ciencas, Madrid, Spain. [Greaves, J.] Univ St Andrews Phys & Astron, St Andrews, Fife, Scotland. [Johnston, K. J.] USN Observ, Washington, DC 20392 USA. [Jones, H.] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. [Lammer, H.] Austrian Acad Sci, Space Res Inst, A-8010 Graz, Austria. [Lawson, P.; Lay, O. P.; Martin, S. R.; Mawet, D.; Serabyn, E.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [LeDuigou, J. -M.] Ctr Natl Etud Spatiales, Dept Opt, F-31055 Toulouse, France. [Liseau, R.] Chalmers, Onsala Space Observ, S-43900 Onsala, Sweden. [Mourard, D.; Rabbia, Y. D.] Observ Cote Azur, Grasse, France. [Moutou, C.] CNRS, LAM, Marseille, France. [Mugnier, L. M.] ONERA DOTA, Chatillon, France. [Paresce, F.] INAF, IASF Bologna, Bologna, Italy. [Quirrenbach, A.] Univ Heidelberg, ZAH, Heidelberg, Germany. [Raven, J. A.] Univ Dundee, SCRI, Div Plant Sci, Dundee, Scotland. [Rottgering, H. J. A.] Leiden Univ, Leiden Observ, Leiden, Netherlands. [Rouan, D.] Observ Paris, PHASE, LESIA, Meudon, France. [Santos, N. C.] Univ Porto, Ctr Astrofis, P-4100 Oporto, Portugal. [Selsis, F.] Univ Lyon, Ecole Super Lyon, CNRS, UMR 5574,CRAL, Lyon, France. [Shibai, H.] Nagoya Univ, Grad Sch Sci, Nagoya, Aichi 4648601, Japan. [Tamura, M.] Natl Astron Observ, Tokyo 181, Japan. [Thiebaut, E.] Univ Lyon 1, F-69622 Villeurbanne, France. [Thiebaut, E.] Ecole Normale Super Lyon, Observ Lyon, Ctr Rech Astron Lyon, F-69364 Lyon, France. [Westall, F.] CNRS, Ctr Biophys Mol, Orleans, France. [White, G. J.] Open Univ, Dept Phys & Astron, Milton Keynes MK7 6AA, Bucks, England. [White, G. J.] Rutherford Appleton Lab, CCLRC, Space Sci & Technol Dept, Didcot OX11 0QX, Oxon, England. RP Cockell, CS (reprint author), Open Univ, CEPSAR, Milton Keynes MK7 6AA, Bucks, England. EM c.s.cockell@open.ac.uk RI Appourchaux, Thierry/F-4692-2010; Santos, Nuno/E-9957-2011; Mugnier, Laurent/A-7630-2012; Cottin, Herve/H-5654-2013; OI Santos, Nuno/0000-0003-4422-2919; Cottin, Herve/0000-0001-9170-5265; Mugnier, Laurent/0000-0002-8364-4957; Absil, Olivier/0000-0002-4006-6237 NR 126 TC 56 Z9 57 U1 2 U2 23 PU MARY ANN LIEBERT INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1531-1074 J9 ASTROBIOLOGY JI Astrobiology PD JAN-FEB PY 2009 VL 9 IS 1 BP 1 EP 22 DI 10.1089/ast.2007.0227 PG 22 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA 430GR UT WOS:000264977400001 PM 19203238 ER PT B AU Ord, S Greenhill, L Wayth, R Mitchell, D Dale, K Pfister, H Edgar, RG AF Ord, S. Greenhill, L. Wayth, R. Mitchell, D. Dale, K. Pfister, H. Edgar, R. G. BE Bohlender, DA Durand, D Dowler, P TI Graphics Processing Units for Data Processing in the Murchison Wide-field Array SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS XVIII SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 18th Annual Conference on Astronomical Data Analysis Software and Systems CY NOV 02-05, 2008 CL Quebec City, CANADA SP Natl Res Council Canada, Univ Montreal, Univ Laval ID HEALPIX AB The Murchison Wide-field Array (MWA) is a next-generation radio interferometer under construction in remote Western Australia. The data rate from the correlator makes storing the raw data infeasible, so the data must be processed in real-time. The processing task is of order 10 TFLOPs(-1). The remote location of the MWA limits the power that can be allocated to computing. We describe the design and implementation of elements of the MWA real-time data processing system which leverage the computing abilities of modern graphics processing units (GPUs). The matrix algebra and texture mapping capabilities of GPUs are well suited to the majority of tasks involved in real-time calibration and imaging. Considerable performance advantages over a conventional CPU-based reference implementation are obtained. C1 [Ord, S.; Greenhill, L.; Wayth, R.; Mitchell, D.] Harvard Smithsonian Ctr Astrophys, 60 Garden St,Mail Stop 42, Cambridge, MA 02138 USA. [Dale, K.; Pfister, H.; Edgar, R. G.] Harvard Univ, Cambridge, MA USA. RP Ord, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,Mail Stop 42, Cambridge, MA 02138 USA. EM sord@cfa.harvard.edu; greenhill@cfa.harvard.edu RI Wayth, Randall/B-2444-2013; Ord, Stephen/C-6138-2013 OI Wayth, Randall/0000-0002-6995-4131; NR 4 TC 3 Z9 3 U1 0 U2 1 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-702-5 J9 ASTR SOC P PY 2009 VL 411 BP 127 EP + PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BQJ95 UT WOS:000281196100020 ER PT B AU Kim, DW Protopapas, P Alcock, C Bianco, FB Byun, YI AF Kim, Dae-Won Protopapas, Pavlos Alcock, Charles Bianco, Federica B. Byun, Yong-Ik BE Bohlender, DA Durand, D Dowler, P TI De-trending Time Series for Astronomical Variability Surveys SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS XVIII SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 18th Annual Conference on Astronomical Data Analysis Software and Systems CY NOV 02-05, 2008 CL Quebec City, CANADA SP Natl Res Council Canada, Univ Montreal, Univ Laval ID LIGHT CURVES; PHOTOMETRY; PLANET; CATALOG; STARS AB We present a de-trending algorithm for the removal of trends in time series. Trends in time series could be caused by various systematic and random noise sources such as cloud passages, changes of airmass, telescope vibration or CCD noise. We determine the trends from subsets of stars that are highly correlated among themselves. These subsets are selected based on a hierarchical tree clustering algorithm. A bottom-up merging algorithm based on the departure from normal distribution in the correlation is developed to identify subsets, which we call clusters. After identification of clusters, we determine a trend per cluster by weighted sum of normalized light curves. We then use quadratic programming to de-trend all individual light curves based on these determined trends. Experimental results with synthetic light curves containing artificial trends and events are presented. C1 [Kim, Dae-Won; Protopapas, Pavlos; Alcock, Charles; Bianco, Federica B.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Kim, Dae-Won; Protopapas, Pavlos] Harvard Univ, Initiat Innovat Comp, Cambridge, MA 02138 USA. [Kim, Dae-Won; Byun, Yong-Ik] Yonsei Univ, Dept Astron, Seoul 120749, South Korea. [Bianco, Federica B.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. RP Kim, DW (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM dakim@cfa.harvard.edu; pprotopapas@cfa.harvard.edu FU Korea Research Foundation; FAS Research Computing Group at the Harvard; [KRF-2007-C00020] FX This work is supported by the Korea Research Foundation. Y.-I. Byun also acknowledges the grant of KRF-2007-C00020. We thank R. Reid, R. Dave, G. Wachman and D. Preston at the Harvard, Initiative in Innovative Computing (IIC), and A. W. Blocker at the Harvard University Department of Statistics for comments and suggestions on this paper. We also thank the Harvard-Smithsonian Center for Astrophysics and IIC for providing computing facilities and research space. The simulations and the de-trending of datasets in this paper were run on the Odyssey cluster supported by the FAS Research Computing Group at the Harvard. NR 19 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 978-1-58381-702-5 J9 ASTR SOC P PY 2009 VL 411 BP 247 EP + PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BQJ95 UT WOS:000281196100044 ER PT B AU Rebbapragada, U Protopapas, P Brodley, CE Alcock, C AF Rebbapragada, Umaa Protopapas, Pavlos Brodley, Carla E. Alcock, Charles BE Bohlender, DA Durand, D Dowler, P TI Anomaly Detection in Catalogs of Periodic Variable Stars SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS XVIII SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 18th Annual Conference on Astronomical Data Analysis Software and Systems CY NOV 02-05, 2008 CL Quebec City, CANADA SP Natl Res Council Canada, Univ Montreal, Univ Laval ID LIGHT AB We present an anomaly detection method for identifying potentially novel astronomical phenomena from catalogs of periodic variable stars. The challenge of working with large catalogs of light-curve data is that the data are unsynchronized, a fact which precludes the use of out-of-the-box anomaly detection methods. We present PCAD, a novel method whose primary innovation is the efficient integration of phase shift calculations with model calculation. Because our model calculation is robust on samplings of the data, PCAD scales to large data sets. An analysis of our results shows that PCAD is useful for identifying misclassifications in the catalogs, as well as truly unusual phenomena worthy of further investigation. C1 [Rebbapragada, Umaa; Brodley, Carla E.] Tufts Univ, Dept Comp Sci, 161 Coll Ave, Medford, MA 02155 USA. [Protopapas, Pavlos; Alcock, Charles] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Protopapas, Pavlos] Harvard Univ, Initiat Innovat Comp, Cambridge, MA 02138 USA. RP Rebbapragada, U (reprint author), Tufts Univ, Dept Comp Sci, 161 Coll Ave, Medford, MA 02155 USA. EM urebbapr@cs.tufts.edu; pprotopapas@cfa.harvard.edu FU NASA [NNX07AV75G]; NSF [IIS0713259] FX This material is based upon work supported by NASA under Grant No. NNX07AV75G, and the NSF under Grant No. IIS0713259. NR 7 TC 3 Z9 3 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-702-5 J9 ASTR SOC P PY 2009 VL 411 BP 264 EP + PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BQJ95 UT WOS:000281196100048 ER PT B AU Henneken, EA Accomazzi, A Kurtz, MJ Grant, CS Thompson, D Bohlen, E Murray, SS Rosvall, M Bergstrom, C AF Henneken, Edwin A. Accomazzi, Alberto Kurtz, Michael J. Grant, Carolyn S. Thompson, Donna Bohlen, Elizabeth Murray, Stephen S. Rosvall, Martin Bergstrom, Carl BE Bohlender, DA Durand, D Dowler, P TI Exploring the Astronomy Literature Landscape SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS XVIII SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 18th Annual Conference on Astronomical Data Analysis Software and Systems CY NOV 02-05, 2008 CL Quebec City, CANADA SP Natl Res Council Canada, Univ Montreal, Univ Laval ID ASTROPHYSICS DATA SYSTEM AB Although powerful, list searches have their limitations. Using second order bibliometric operators (Kurtz et al. 2002) in the SAO/NASA Astrophysics Data System (ADS), one is able to easily find review papers or the most popular papers on a given subject. Because of their one-dimensionality, lists cannot display a rich context for a given paper. The best analogy is probably that of a map. A point on a map has a certain contextual meaning, depending on the information being displayed on that map. We can form a landscape based on the astronomy literature in various ways. A set of astronomy papers can be regarded as an ensemble of points that interact with each other in a certain way. This interaction can, for example, represent the citations between papers, the number of keywords papers have in common, a similarity between abstracts of papers or a combination of these. As a result, papers get clustered into modules. In other words, we compress the complex network of hundreds of thousands of papers and, for example, millions of citations into a set of modules with an information flow between these modules. A variety of methods are available to perform this clustering. Often, the actual network is compared to a null model, which is used to calculate an expected number of edges. Our approach (Rosvall & Bergstrom 2007) is different in the sense that we use information theory and require that the optimal clustering for a given network minimizes the description length of the original network. C1 [Henneken, Edwin A.; Accomazzi, Alberto; Kurtz, Michael J.; Grant, Carolyn S.; Thompson, Donna; Bohlen, Elizabeth; Murray, Stephen S.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Rosvall, Martin; Bergstrom, Carl] Univ Washington, Dept Biol, Seattle, WA USA. RP Henneken, EA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM ehenneken@cfa.harvard.edu FU NASA [NNX09AB39G] FX The ADS is Funded by NASA Grant NNX09AB39G. NR 7 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 978-1-58381-702-5 J9 ASTR SOC P PY 2009 VL 411 BP 384 EP + PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BQJ95 UT WOS:000281196100076 ER PT J AU Caldwell, N Harding, P Morrison, H Rose, JA Schiavon, R Kriessler, J AF Caldwell, Nelson Harding, Paul Morrison, Heather Rose, James A. Schiavon, Ricardo Kriessler, Jeff TI STAR CLUSTERS IN M31. I. A CATALOG AND A STUDY OF THE YOUNG CLUSTERS SO ASTRONOMICAL JOURNAL LA English DT Article DE catalogs; galaxies: individual (M31); galaxies: star clusters; globular clusters: general ID CURRENTLY FORMING STARS; GALACTIC OPEN CLUSTERS; WIDE-FIELD SURVEY; GLOBULAR-CLUSTERS; MAGELLANIC-CLOUD; MILKY-WAY; STELLAR POPULATIONS; FUNDAMENTAL PLANE; UBVRI PHOTOMETRY; MASS FUNCTION AB We present an updated catalog of 1300 objects in the field of M31, including 670 likely star clusters of various types, the rest being stars or background galaxies once thought to be clusters. The coordinates in the catalog are accurate to 0 ''.2, and are based on images from the Local Group Survey (LGS) or from the Digitized Sky Survey (DSS). Archival Hubble Space Telescope (HST) images and the LGS were inspected to confirm cluster classifications where possible, but most of the classifications are based on spectra taken of similar to 1000 objects with the Hectospec fiber positioner and spectrograph on the 6.5 m MMT. The spectra and images of young clusters are analyzed in detail in this paper; analysis of older clusters will appear in a later paper. Ages and reddenings of 140 young clusters are derived by comparing the observed spectra with model spectra. Seven of these clusters also have ages derived from HST color-magnitude diagrams (two of which we present here); these agree well with the spectroscopically determined ages. Combining new V-band photometry with the M/L values that correspond to the derived cluster ages, we derive masses for the young clusters, finding them to have masses as great as 105 with a median of 10(4) M(circle dot), and a median age of 0.25 Gyr. In comparison, therefore, Milky Way (MW) open clusters have the lowest median mass, the MW and M31 globulars the highest, and the LMC young massive clusters and the M31 young clusters are in between. The young clusters in M31 show a range of structures. Most have the low concentration typical of MW open clusters, but there are a few which have high concentrations. We expect that most of these young clusters will be disrupted in the next Gyr or so; however, some of the more massive and concentrated of the young clusters will likely survive for longer. The spatial distribution of the young clusters is well correlated with the star-forming regions as mapped out by mid-IR emission. A kinematic analysis likewise confirms the spatial association of the young clusters with the star-forming young disk in M31. C1 [Caldwell, Nelson] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Harding, Paul; Morrison, Heather; Kriessler, Jeff] Case Western Reserve Univ, Dept Astron, Cleveland, OH 44106 USA. [Rose, James A.] Univ N Carolina, Dept Phys & Astron, Chapel Hill, NC 27599 USA. [Schiavon, Ricardo] Gemini Observ, Hilo, HI 96720 USA. RP Caldwell, N (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM caldwell@cfa.harvard.edu; paul.harding@case.edu; heather@vegemite.case.edu; jim@physics.unc.edu; rschiavo@gemini.edu; jeffrey.kriessler@case.edu FU NSF [AST-0607518]; HST [GO10407] FX We thank Dan Fabricant for leading the effort to design & build the Hectospec fiber positioner and spectrograph, Perry Berlind and Mike Calkins for help with the observations, John Roll, Maureen Conroy, and Bill Joye for their many contributions to the Hectospec software development project, and PhilMassey, Pauline Barmby, and Jay Strader for comments and data tables on M31. H. L. M. was supported by NSF grant AST-0607518, and thanks Dean McLaughlin for helpful conversations. Work on this project has also been supported by HST grant GO10407. NR 85 TC 87 Z9 88 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD JAN PY 2009 VL 137 IS 1 BP 94 EP 110 DI 10.1088/0004-6256/137/1/94 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 393AJ UT WOS:000262343000009 ER PT J AU Barmby, P Boyer, ML Woodward, CE Gehrz, RD van Loon, JT Fazio, GG Marengo, M Polomski, E AF Barmby, Pauline Boyer, Martha L. Woodward, Charles E. Gehrz, Robert D. van Loon, Jacco Th. Fazio, Giovanni G. Marengo, Massimo Polomski, Elisha TI A SPITZER SEARCH FOR COLD DUST WITHIN GLOBULAR CLUSTERS SO ASTRONOMICAL JOURNAL LA English DT Article DE globular clusters: general; globular clusters: individual (NGC 104, NGC 362, NGC 1851, NGC 5272, NGC 5904, NGC 6205, NGC 6341, NGC 6752); infrared: stars; stars: mass loss ID RED-GIANT-BRANCH; MULTIBAND IMAGING PHOTOMETER; INFRARED ARRAY CAMERA; STELLAR MASS-LOSS; X-RAY EMISSION; SPACE-TELESCOPE; ABSOLUTE CALIBRATION; INTRACLUSTER MEDIUM; BRIGHTNESS PROFILES; MAGELLANIC CLOUDS AB Globular cluster (GC) stars evolving off the main sequence are known to lose mass, and it is expected that some of the lost material should remain within the cluster as an intracluster medium (ICM). Most attempts to detect such an ICM have been unsuccessful. The Multiband Imaging Photometer for Spitzer on the Spitzer Space Telescope was used to observe eight Galactic GCs in an attempt to detect the thermal emission from ICM dust. Most clusters do not have significant detections at 70 mu m; one cluster, NGC 6341, has tentative evidence for the presence of dust, but 90 mu m observations do not confirm the detection. Individual 70 mu m point sources which appear in several of the cluster images are likely to be background galaxies. The inferred dust mass and upper limits are less than 4 x 10(-4) M-circle dot, well below expectations for cluster dust production from mass loss in red and asymptotic giant branch stars. This implies that either GC dust production is less efficient, or that ICM removal or dust destruction is more efficient, than previously believed. We explore several possibilities for ICM removal and conclude that present data do not yet permit us to distinguish between them. C1 [Barmby, Pauline] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada. [Barmby, Pauline; Fazio, Giovanni G.; Marengo, Massimo] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Boyer, Martha L.; Woodward, Charles E.; Gehrz, Robert D.] Univ Minnesota, Dept Astron, Sch Phys & Astron, Minneapolis, MN 55455 USA. [van Loon, Jacco Th.] Keele Univ, Lennard Jones Labs, Astrophys Grp, Keele, Staffs, England. [Polomski, Elisha] Univ Wisconsin Stevens Point, Dept Phys & Astron, Stevens Point, WI 54481 USA. RP Barmby, P (reprint author), Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada. EM pbarmby@uwo.ca RI Barmby, Pauline/I-7194-2016 OI Barmby, Pauline/0000-0003-2767-0090 FU NASA [1407, 1276760, 1256406, 1215746]; Natural Sciences and Engineering Research Council of Canada; University of Minnesota FX We thank the anonymous referee for a careful reading of the manuscript and helpful comments and R. T. Rood for early access to the IRAC data on NGC 6205 and NGC 6341. This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under NASA contract 1407. P. B. was partially supported by a Discovery Grant from the Natural Sciences and Engineering Research Council of Canada. M. L. B., C. E. W., E. P., and R. D. G. are supported in part by NASA through Spitzer contracts 1276760, 1256406, and 1215746 issued by JPL/Caltech to the University of Minnesota. NR 66 TC 18 Z9 18 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD JAN PY 2009 VL 137 IS 1 BP 207 EP 217 DI 10.1088/0004-6256/137/1/207 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 393AJ UT WOS:000262343000018 ER PT J AU Kaplan, DL Chatterjee, S Hales, CA Gaensler, BM Slane, PO AF Kaplan, D. L. Chatterjee, S. Hales, C. A. Gaensler, B. M. Slane, P. O. TI CONSTRAINING THE PROPER MOTIONS OF TWO MAGNETARS SO ASTRONOMICAL JOURNAL LA English DT Article DE astrometry; pulsars: general; stars: individual (SGR 1900+14, 1E2259+58.6); stars: neutron; X-rays: stars ID X-RAY PULSAR; MAGNETIZED NEUTRON-STARS; SOFT-GAMMA-REPEATERS; HIGH-RESOLUTION CAMERA; SGR 1900+14; INFRARED OBSERVATIONS; RADIO PULSARS; 1E 2259+586; PUPPIS-A; CHANDRA AB We attempt to measure the proper motions of two magnetars-the soft gamma-ray repeater SGR 1900+14 and the anomalous X-ray pulsar 1E 2259+586-using two epochs of Chandra observations separated by similar to 5 yr. We perform extensive tests using these data, archival data, and simulations to verify the accuracy of our measurements and understand their limitations. We find 90% upper limits on the proper motions of 54 mas yr(-1) (SGR 1900+14) and 65 mas yr(-1) (1E 2259+586), with the limits largely determined by the accuracy with which we could register the two epochs of data and by the inherent uncertainties on two-point proper motions. We translate the proper motions limits into limits on the transverse velocity using distances, and find nu(perpendicular to) < 1300 km s(-1) (SGR 1900+14, for a distance of 5 kpc) and nu(perpendicular to) < 930 km s(-1) (1E 2259+586, for a distance of 3 kpc) at 90% confidence; the range of possible distances for these objects makes a wide range of velocities possible, but it seems that the magnetars do not have uniformly high space velocities greater than 3000 km s(-1). Unfortunately, our proper motions also cannot significantly constrain the previously proposed origins of these objects in nearby supernova remnants or star clusters, limited as much by our ignorance of ages as by our proper motions. C1 [Kaplan, D. L.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Kaplan, D. L.] MIT, Dept Phys, Cambridge, MA 02139 USA. [Chatterjee, S.; Hales, C. A.; Gaensler, B. M.] Univ Sydney, Sch Phys, Inst Astron, Sydney, NSW 2006, Australia. [Slane, P. O.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kaplan, DL (reprint author), MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA. EM dlk@space.mit.edu; schatterjee@usyd.edu.au; chales@physics.usyd.edu.au; bgaensler@usyd.edu.au; slane@cfa.harvard.edu RI Gaensler, Bryan/F-8655-2010; Hales, Christopher/J-6048-2014; OI Hales, Christopher/0000-0002-3733-2565; Gaensler, Bryan/0000-0002-3382-9558 FU National Aeronautics and Space Administration through Chandra [GO6-7066X]; NASA through Hubble Fellowship [01207.01-A]; Association of Universities for Research in Astronomy, Inc., for NASA [NAS 5-26555]; Australian Research Council [FF0561298]; University of Sydney Postdoctoral Fellowship; NASA [NAS8-201039073]; Natural Sciences and Engineering Research Council FX Support for this work was provided by the National Aeronautics and Space Administration through Chandra award GO6-7066X. Partial support for D. L. K. was also provided by NASA through Hubble Fellowship grant #01207.01-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. B. M. G. acknowledges the support of a Federation Fellowship from the Australian Research Council through grant FF0561298. Support for S.C. was provided by the University of Sydney Postdoctoral Fellowship program. P.O.S. also acknowledges support from NASA contract NAS8-201039073. The research presented in this paper has used data from the Canadian Galactic Plane Survey, a Canadian project with international partners, supported by the Natural Sciences and Engineering Research Council. NR 61 TC 12 Z9 12 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD JAN PY 2009 VL 137 IS 1 BP 354 EP 366 DI 10.1088/0004-6256/137/1/354 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 393AJ UT WOS:000262343000032 ER PT J AU Beuther, H Zhang, Q Bergin, EA Sridharan, TK AF Beuther, H. Zhang, Q. Bergin, E. A. Sridharan, T. K. TI CHEMICAL DIVERSITY IN HIGH-MASS STAR FORMATION SO ASTRONOMICAL JOURNAL LA English DT Article DE stars: formation; stars: early type; stars: individual (Orion-KL, G29.96, IRAS 23151+5912, IRAS 05358+3543); ISM: molecules; ISM: lines and bands; ISM: evolution ID (PROTO)STAR IRAS 20126+4104; ULTRACOMPACT HII-REGIONS; GHZ SPECTRAL SURVEY; HOT-CORE; ORION-KL; SUBMILLIMETER ARRAY; FORMING REGIONS; YOUNG STARS; PROTOSTELLAR CANDIDATES; PHYSICAL CONDITIONS AB Massive star formation exhibits an extremely rich chemistry. However, few evolutionary details are known yet, especially at high spatial resolution. Therefore, we synthesize previously published Submillimeter Array high spatial resolution spectral line observations toward four regions of high-mass star formation that are in various evolutionary stages with a range of luminosities. Estimating column densities and comparing the spatially resolved molecular emission allow us to characterize the chemical evolution in more detail. Furthermore, we model the chemical evolution of massive warm molecular cores to be directly compared with the data. The four regions reveal many different characteristics. While some of them, e. g., the detection rate of CH(3)OH, can be explained by variations of the average gas temperatures, other features are attributed to chemical effects. For example, C(34)S is observed mainly at the core edges and not toward their centers because of temperature-selective desorption and successive gas-phase chemistry reactions. Most nitrogen-bearing molecules are only found toward the hot molecular cores and not the earlier evolutionary stages, indicating that the formation and excitation of such complex nitrogen-bearing molecules needs significant heating and time to be fully developed. Furthermore, we discuss the observational difficulties to study massive accretion disks in the young deeply embedded phase of massive star formation. The general potential and limitations of such kinds of data sets are discussed, and future directions are outlined. The analysis and modeling of this source sample reveal many interesting features toward a chemical evolutionary sequence. However, it is only an early step, and many observational and theoretical challenges in that field lie ahead. C1 [Beuther, H.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Zhang, Q.; Sridharan, T. K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bergin, E. A.] Univ Michigan, Ann Arbor, MI 48109 USA. RP Beuther, H (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. OI Zhang, Qizhou/0000-0003-2384-6589 FU Deutsche Forschungsgemeinschaft [BE2578] FX H. B. acknowledges financial support by the Emmy-Noether-Program of the Deutsche Forschungsgemeinschaft (DFG, grant BE2578). NR 65 TC 23 Z9 23 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD JAN PY 2009 VL 137 IS 1 BP 406 EP 418 DI 10.1088/0004-6256/137/1/406 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 393AJ UT WOS:000262343000036 ER PT J AU Williams, BF Dalcanton, JJ Seth, AC Weisz, D Dolphin, A Skillman, E Harris, J Holtzman, J Girardi, L De Jong, RS Olsen, K Cole, A Gallart, C Gogarten, SM Hidalgo, SL Mateo, M Rosema, K Stetson, PB Quinn, T AF Williams, Benjamin F. Dalcanton, Julianne J. Seth, Anil C. Weisz, Daniel Dolphin, Andrew Skillman, Evan Harris, Jason Holtzman, Jon Girardi, Leo De Jong, Roelof S. Olsen, Knut Cole, Andrew Gallart, Carme Gogarten, Stephanie M. Hidalgo, Sebastian L. Mateo, Mario Rosema, Keith Stetson, Peter B. Quinn, Thomas TI THE ACS NEARBY GALAXY SURVEY TREASURY. I. THE STAR FORMATION HISTORY OF THE M81 OUTER DISK SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies: individual (M81); galaxies: stellar content; galaxies: spiral; galaxies: evolution ID HUBBLE-SPACE-TELESCOPE; DIGITAL SKY SURVEY; EXTRAGALACTIC DISTANCE SCALE; COLOR-MAGNITUDE DIAGRAMS; TULLY-FISHER RELATIONS; SPIRAL DENSITY WAVES; GIANT BRANCH BUMP; STELLAR POPULATIONS; HORIZONTAL-BRANCH; STRUCTURAL PARAMETERS AB The Advanced Camera for Surveys (ACS) Nearby Galaxy Survey Treasury is a large Hubble Space Telescope (HST)/ACS treasury program to obtain resolved stellar photometry for a volume-limited sample of galaxies out to 4 Mpc. As part of this program, we have obtained deep ACS imaging of a field in the outer disk of the large spiral galaxy M81. The field contains the outskirts of a spiral arm as well as an area containing no current star formation. Our imaging results in a color-magnitude diagram (CMD) reaching to m(F814W) = 28.8 and m(F606W) = 29.5, one magnitude fainter than the red clump. Through detailed modeling of the full CMD, we quantify the age and metallicity distribution of the stellar populations contained in the field. The mean metallicity in the field is -1 < [M/H] < 0 and only a small fraction of stars have ages less than or similar to 1 Gyr. The results show that most of the stars in this outer disk field were formed by z similar to 1 and that the arm structure at this radius has a lifetime of greater than or similar to 100 Myr. We discuss the measured evolution of the M81 disk in the context of surveys of high redshift disk galaxies and deep stellar photometry of other nearby galaxies. All of these indicate that massive spiral disks are mostly formed by z similar to 1 and that they have experienced rapid metal enrichment. C1 [Williams, Benjamin F.; Dalcanton, Julianne J.; Gogarten, Stephanie M.; Rosema, Keith; Quinn, Thomas] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Seth, Anil C.] Harvard Smithsonian Ctr Astrophys, Ctr Astrophys Fellow, Cambridge, MA 02138 USA. [Weisz, Daniel; Skillman, Evan; Hidalgo, Sebastian L.] Univ Minnesota, Dept Astron, Minneapolis, MN 55455 USA. [Dolphin, Andrew] Raytheon Co, Tucson, AZ 85706 USA. [Harris, Jason] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Holtzman, Jon] New Mexico State Univ, Dept Astron, Las Cruces, NM 88003 USA. [Girardi, Leo] Inst Nazl Astrofis, Osservatorio Astron Padova, I-35122 Padua, Italy. [De Jong, Roelof S.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Olsen, Knut] Natl Opt Astron Observ, Cerro Tololo Inter Amer Observ, La Serena, Chile. [Cole, Andrew] Univ Tasmania, Sch Math & Phys, Hobart, Tas, Australia. [Gallart, Carme] Inst Astrofis Canarias, Tenerife 38200, Spain. [Mateo, Mario] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Stetson, Peter B.] Natl Res Council Canada, Herzberg Inst Astrophys, Dominion Astrophys Observ, Victoria, BC V9E 2E7, Canada. RP Williams, BF (reprint author), Univ Washington, Dept Astron, Box 351580, Seattle, WA 98195 USA. EM ben@astro.washington.edu; jd@astro.washington.edu; aseth@cfa.harvard.edu; dweisz@astro.umn.edu; dolphin@raytheon.com; skillman@astro.umn.edu; jharris@as.arizona.edu; holtz@nmsu.edu; leo.girardi@oapd.inaf.it; dejong@stsci.edu; kolsen@ctio.noao.edu; andrew.cole@utas.edu.au; carme@iac.es; stephanie@astro.washington.edu; slhidalgo@astro.umn.edu; mmateo@umich.edu; krosema@astro.washington.edu; Peter.Stetson@nrc-cnrc.gc.ca; trq@astro.washington.edu OI Cole, Andrew/0000-0003-0303-3855; Gogarten, Stephanie/0000-0002-7231-9745; Hidalgo, Sebastian/0000-0002-0002-9298 FU NASA [GO-10915, NAS5-26555] FX Support for this work was provided by NASA through grant GO-10915 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 82 TC 43 Z9 43 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD JAN PY 2009 VL 137 IS 1 BP 419 EP 430 DI 10.1088/0004-6256/137/1/419 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 393AJ UT WOS:000262343000037 ER PT J AU Torres, G Lacy, CHS AF Torres, Guillermo Lacy, Claud H. Sandberg TI ABSOLUTE DIMENSIONS OF THE F-TYPE ECLIPSING BINARY STAR VZ CEPHEI SO ASTRONOMICAL JOURNAL LA English DT Article DE binaries: eclipsing; stars: evolution; stars: fundamental parameters; stars: individual (VZ Cep) ID LIMB-DARKENING COEFFICIENTS; MODEL STELLAR ATMOSPHERES; LOW-MASS STARS; MAIN-SEQUENCE; LIGHT CURVES; SPECTROSCOPIC BINARIES; EVOLUTIONARY MODELS; VELOCITY CURVES; Y-2 ISOCHRONES; ORBITS AB We present new V-band differential photometry and radial velocity measurements of the unevolved, 1.18 day period, F+G-type, double-lined eclipsing binary VZ Cep. We determine accurate values for the absolute masses, radii, and effective temperatures as follows: M(A) = 1.402 +/- 0.015M(circle dot), R(A) = 1.534 +/- 0.012 R(circle dot), and T(eff) = 6690 +/- 160 K for the primary, and M(B) = 1.1077 +/- 0.0083M(circle dot), R(B) = 1.042 +/- 0.039 R(circle dot), and T(eff) = 5720 +/- 120 K for the secondary. A comparison with current stellar evolution models suggests an age of 1.4 Gyr for a metallicity that is near solar. The temperature difference between the stars, which is much better determined than the absolute values, is found to be similar to 250 K larger than predicted by theory. If all of this discrepancy is attributed to the secondary (which would then be too cool compared to models), the effect would be consistent with similar differences found for other low-mass stars, generally believed to be associated with chromospheric activity. However, the radius of VZ Cep B (which unlike the primary, still has a thin convective envelope) appears normal, whereas in other stars affected by activity the radius is systematically larger than predicted. Thus, VZ Cep poses a challenge not only to standard theory but also to our understanding of the discrepancies in other low-mass systems. C1 [Torres, Guillermo] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lacy, Claud H. Sandberg] Univ Arkansas, Dept Phys, Fayetteville, AR 72701 USA. RP Torres, G (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM gtorres@cfa.harvard.edu; clacy@uark.edu NR 70 TC 5 Z9 5 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD JAN PY 2009 VL 137 IS 1 BP 507 EP 516 DI 10.1088/0004-6256/137/1/507 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 393AJ UT WOS:000262343000042 ER PT J AU Gilli, R Zamorani, G Miyaji, T Silverman, J Brusa, M Mainieri, V Cappelluti, N Daddi, E Porciani, C Pozzetti, L Civano, F Comastri, A Finoguenov, A Fiore, F Salvato, M Vignali, C Hasinger, G Lilly, S Impey, C Trump, J Capak, P McCracken, H Scoville, N Taniguchi, Y Carollo, CM Contini, T Kneib, JP Le Fevre, O Renzini, A Scodeggio, M Bardelli, S Bolzonella, M Bongiorno, A Caputi, K Cimatti, A Coppa, G Cucciati, O de la Torre, S de Ravel, L Franzetti, P Garilli, B Iovino, A Kampczyk, P Knobel, C Kovac, K Lamareille, F Le Borgne, JF Le Brun, V Maier, C Mignoli, M Pello, R Peng, Y Montero, EP Ricciardelli, E Tanaka, M Tasca, L Tresse, L Vergani, D Zucca, E Abbas, U Bottini, D Cappi, A Cassata, P Fumana, M Guzzo, L Leauthaud, A Maccagni, D Marinoni, C Memeo, P Meneux, B Oesch, P Scaramella, R Walcher, J AF Gilli, R. Zamorani, G. Miyaji, T. Silverman, J. Brusa, M. Mainieri, V. Cappelluti, N. Daddi, E. Porciani, C. Pozzetti, L. Civano, F. Comastri, A. Finoguenov, A. Fiore, F. Salvato, M. Vignali, C. Hasinger, G. Lilly, S. Impey, C. Trump, J. Capak, P. McCracken, H. Scoville, N. Taniguchi, Y. Carollo, C. M. Contini, T. Kneib, J. -P. Le Fevre, O. Renzini, A. Scodeggio, M. Bardelli, S. Bolzonella, M. Bongiorno, A. Caputi, K. Cimatti, A. Coppa, G. Cucciati, O. de la Torre, S. de Ravel, L. Franzetti, P. Garilli, B. Iovino, A. Kampczyk, P. Knobel, C. Kovac, K. Lamareille, F. Le Borgne, J. -F. Le Brun, V. Maier, C. Mignoli, M. Pello, R. Peng, Y. Montero, E. Perez Ricciardelli, E. Tanaka, M. Tasca, L. Tresse, L. Vergani, D. Zucca, E. Abbas, U. Bottini, D. Cappi, A. Cassata, P. Fumana, M. Guzzo, L. Leauthaud, A. Maccagni, D. Marinoni, C. Memeo, P. Meneux, B. Oesch, P. Scaramella, R. Walcher, J. TI The spatial clustering of X-ray selected AGN in the XMM-COSMOS field SO ASTRONOMY & ASTROPHYSICS LA English DT Review DE galaxies: active; cosmology: large-scale structure of Universe; cosmology: observations; X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; SUPERMASSIVE BLACK-HOLES; GALAXY REDSHIFT SURVEY; STAR-FORMING GALAXIES; DIGITAL SKY SURVEY; 2-POINT CORRELATION-FUNCTION; EVOLUTION SURVEY COSMOS; POINT-SOURCE CATALOGS; LUMINOSITY FUNCTION; ANGULAR-CORRELATION AB We study the spatial clustering of 538 X-ray selected AGN in the 2 deg(2) XMM-COSMOS field that are spectroscopically identified with I(AB) < 23 and span the redshift range z = 0.2-3.0. The median redshift and X-ray luminosity of the sample are z = 0.98 and L(0.5-10) = 6.3 x 10(43) erg s(-1), respectively. A strong clustering signal is detected at similar to 18 sigma level, which is the most significant measurement obtained to date for clustering of X-ray selected AGN. By fitting the projected correlation function w(r(p)) with a power law on scales of r(p) = 0.3-40 h(-1) Mpc, we derive a best-fit comoving correlation length of r(0) = 8.6 +/- 0.5 h(-1) Mpc and slope of. = 1.88 +/- 0.07 (Poissonian errors; bootstrap errors are about a factor of 2 larger). An excess signal is observed in the range r(p) similar to 5-15 h(-1) Mpc, which is due to a large-scale structure at z similar to 0.36 containing about 40 AGN, a feature which is evident over many wavelengths in the COSMOS field. When removing the z similar to 0.36 structure or computing w(r(p)) in a narrower range around the peak of the redshift distribution (e. g. z = 0.4-1.6), the correlation length decreases to r(0) similar to 5-6 h(-1) Mpc, which is consistent with what is observed for bright optical QSOs at the same redshift. We investigate the clustering properties of obscured and unobscured AGN separately, adopting different definitions for the source obscuration. For the first time, we are able to provide a significant measurement for the spatial clustering of obscured AGN at z similar to 1. Within the statistical uncertainties, we do not find evidence that AGN with broad optical lines (BLAGN) cluster differently from AGN without broad optical lines (non-BLAGN). Based on these results, which are limited by object statistics, however, obscured and unobscured AGN are consistent with inhabiting similar environments. The evolution of AGN clustering with redshift is also investigated. No significant difference is found between the clustering properties of XMM-COSMOS AGN at redshifts below or above z = 1. The correlation length measured for XMM-COSMOS AGN at z similar to 1 is similar to that of massive galaxies (stellar mass M(*) greater than or similar to 3 x 10(10) M(circle dot)) at the same redshift. This suggests that AGN at z similar to 1 are preferentially hosted by massive galaxies, as observed both in the local and in the distant (z similar to 2) Universe. According to a simple clustering evolution scenario, we find that the relics of AGN are expected to have a correlation length as large as r(0) similar to 8 h(-1) Mpc by z = 0, and hence to be hosted by local bright (L similar to L(*)) ellipticals. We make use of dark matter halo catalogs from the Millennium simulation to determine the typical halo hosting moderately luminous z similar to 1 AGN. We find that XMM-COSMOS AGN live in halos with masses M greater than or similar to 2.5 x 10(12) M(circle dot) h(-1). By combining the number density of XMM-COSMOS AGN to that of the hosting dark matter halos we estimate the AGN duty cycle and lifetimes. We find lifetimes approximately of 1 Gyr for AGN at z similar to 1, which are longer than those estimated for optically bright QSOs at the same redshift. These longer lifetimes mainly reflect the higher number density of AGN selected by X-ray samples. C1 [Gilli, R.; Zamorani, G.; Pozzetti, L.; Comastri, A.; Bardelli, S.; Bolzonella, M.; Mignoli, M.; Vergani, D.; Zucca, E.; Cappi, A.] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy. [Miyaji, T.] Univ Nacl Autonoma Mexico, Inst Astron, Ensenada, Baja California, Mexico. [Silverman, J.; Porciani, C.; Lilly, S.; Carollo, C. M.; Kampczyk, P.; Knobel, C.; Kovac, K.; Peng, Y.; Oesch, P.] Swiss Fed Inst Technol ETH Honggerberg, Inst Astron, CH-8093 Zurich, Switzerland. [Brusa, M.; Cappelluti, N.; Finoguenov, A.; Hasinger, G.; Bongiorno, A.; Meneux, B.] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. [Mainieri, V.; Tanaka, M.] European So Observ, D-85748 Garching, Germany. [Daddi, E.] Univ Paris Diderot, CNRS, CEA DSM, Lab AIM,DAPNIA SAp, F-91191 Gif Sur Yvette, France. [Civano, F.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Fiore, F.; Scaramella, R.] INAF Osservatorio Astron Roma, I-00040 Rome, Italy. [Salvato, M.; Capak, P.; Scoville, N.] CALTECH, Pasadena, CA 91125 USA. [Vignali, C.; Cimatti, A.; Coppa, G.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. [Impey, C.; Trump, J.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [McCracken, H.; Walcher, J.] Inst Astrophys, F-75014 Paris, France. [Taniguchi, Y.] Ehime Univ, Res Ctr Space & Cosm Evolut, Matsuyama, Ehime 7908577, Japan. [Contini, T.; Lamareille, F.; Le Borgne, J. -F.; Pello, R.; Montero, E. Perez] Univ Toulouse, CNRS, Lab Astrophys Toulouse Tarbes, F-31400 Toulouse, France. [Kneib, J. -P.; Le Fevre, O.; de la Torre, S.; Le Brun, V.; Tasca, L.; Tresse, L.; Abbas, U.; Cassata, P.] Univ Aix Marseille 1, CNRS, Astrophys Lab, F-13012 Marseille, France. [Renzini, A.; Ricciardelli, E.] Univ Padua, Dipartimento Astron, I-35122 Padua, Italy. [Scodeggio, M.; Franzetti, P.; Garilli, B.; Bottini, D.; Fumana, M.; Maccagni, D.; Memeo, P.] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy. [Cucciati, O.; Iovino, A.; Guzzo, L.] INAF Osservatorio Astron Brera, I-23807 Merate, LC, Italy. [Leauthaud, A.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Marinoni, C.] Univ Aix Marseille 1, CNRS, UMR 6207, Ctr Phys Theor, F-13288 Marseille, France. RP Gilli, R (reprint author), INAF Osservatorio Astron Bologna, Via Ranzani 1, I-40127 Bologna, Italy. EM roberto.gilli@oabo.inaf.it RI Pello, Roser/G-4754-2010; Le Fevre, Olivier/G-7389-2011; Daddi, Emanuele/D-1649-2012; Vignali, Cristian/J-4974-2012; Kneib, Jean-Paul/A-7919-2015; Cappi, Alberto/O-9391-2015; Bardelli, Sandro/O-9369-2015; Zucca, Elena/O-9396-2015; Bolzonella, Micol/O-9495-2015; Mignoli, Marco/O-9426-2015; Comastri, Andrea/O-9543-2015; Gilli, Roberto/P-1110-2015; OI Fumana, Marco/0000-0001-6787-5950; Scaramella, Roberto/0000-0003-2229-193X; Bongiorno, Angela/0000-0002-0101-6624; Iovino, Angela/0000-0001-6958-0304; bottini, dario/0000-0001-6917-041X; Pozzetti, Lucia/0000-0001-7085-0412; Scodeggio, Marco/0000-0002-2282-5850; Daddi, Emanuele/0000-0002-3331-9590; Vignali, Cristian/0000-0002-8853-9611; Kneib, Jean-Paul/0000-0002-4616-4989; Cappi, Alberto/0000-0002-9200-7167; Bardelli, Sandro/0000-0002-8900-0298; Zucca, Elena/0000-0002-5845-8132; Bolzonella, Micol/0000-0003-3278-4607; Mignoli, Marco/0000-0002-9087-2835; Comastri, Andrea/0000-0003-3451-9970; Gilli, Roberto/0000-0001-8121-6177; Perez Montero, E/0000-0003-3985-4882; Brusa, Marcella/0000-0002-5059-6848; Fiore, Fabrizio/0000-0002-4031-4157; Franzetti, Paolo/0000-0002-6986-0127; Vergani, Daniela/0000-0003-0898-2216; Cappelluti, Nico/0000-0002-1697-186X; Oesch, Pascal/0000-0001-5851-6649; Maier, Christian/0000-0001-6405-2182; Garilli, Bianca/0000-0001-7455-8750; Zamorani, Giovanni/0000-0002-2318-301X FU ESA Member States; USA (NASA); ASI-INAF; PRIN/MIUR [I/023/05/00, 200602-5203]; zCOSMOS ESO [175] FX This work is based on observations obtained with XMM-Newton, an ESA Science Mission with instruments and contributions directly funded by ESA Member States and the USA (NASA). We gratefully acknowledge the contribution of the entire COSMOS collaboration (http://www.astro.caltech.edu/similar to cosmos). In Italy, the XMM-COSMOS projects is supported by ASI-INAF and PRIN/MIUR under grants I/023/05/00 and 200602-5203. The zCOSMOS ESO Large Program Number 175. A-0839 is acknowledged. R. G. thanks Carlo Nipoti, Federico Marulli, Enzo Branchini, and Lauro Moscardini for stimulating discussions. The referee is acknowledged for providing useful comments. The Millennium Simulation databases used in this paper and the web application providing online access to them were constructed as part of the activities of the German Astrophysical Virtual Observatory. NR 115 TC 63 Z9 63 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JAN PY 2009 VL 494 IS 1 BP 33 EP 48 DI 10.1051/0004-6361:200810821 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 402VC UT WOS:000263040200004 ER PT J AU Rabus, M Alonso, R Belmonte, JA Deeg, HJ Gilliland, RL Almenara, JM Brown, TM Charbonneau, D Mandushev, G AF Rabus, M. Alonso, R. Belmonte, J. A. Deeg, H. J. Gilliland, R. L. Almenara, J. M. Brown, T. M. Charbonneau, D. Mandushev, G. TI A cool starspot or a second transiting planet in the TrES-1 system? SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE starspots; planetary systems ID TIME-SERIES PHOTOMETRY; HD-209458 AB Aims. We investigate the origin of a flux increase found during a transit of TrES-1, observed with the HST (Hubble Space Telescope). This feature in the HST light curve cannot be attributed to noise and is supposedly a dark area on the stellar surface of the host star eclipsed by TrES-1 during its transit. We investigate the likelihood of two possible hypotheses for its origin. A starspot or a second transiting planet. Methods. We made use of several transit observations of TrES-1 from space with the HST and from ground with the IAC 80-cm telescope ( IAC-80). On the basis of these observations we did a statistical study of flux variations in each of the observed events to investigate whether similar flux increases are present in other parts of the data set. Results. The HST observation presents a single clear flux rise during a transit, whereas the ground observations lead to detecting two such events but with low significance. In the case of having observed a starspot in the HST data, assuming a central impact between the spot and TrES-1, we would obtain a lower limit for the spot radius of 42 000 km. For this radius the spot temperature would be 4690 K, 560 K lower then the stellar surface of 5250 K. For a putative second transiting planet, we can set a lower limit for its radius at 0.37 R(J) and for periods of less than 10.5 days, we can set an upper limit at 0.72 R(J). Conclusions. Assuming a conventional interpretation, this HST observation then constitutes the detection of a starspot. Alternatively, this flux rise might also be caused by an additional transiting planet. The true nature of the origin can be revealed if a wavelength dependency of the flux rise can be shown or discarded with higher certainty. Additionally, the presence of a second planet can be detected by radial velocity measurements. C1 [Rabus, M.; Belmonte, J. A.; Deeg, H. J.; Almenara, J. M.] Inst Astrofis Canarias, San Cristobal la Laguna 38205, Spain. [Alonso, R.] Astrophys Lab, UMR 6110, F-13388 Marseille, France. [Gilliland, R. L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Brown, T. M.] Las Cumbres Observ, Santa Barbara, CA 93117 USA. [Charbonneau, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Mandushev, G.] Lowell Observ, Flagstaff, AZ 86001 USA. RP Rabus, M (reprint author), Inst Astrofis Canarias, Via Lactea S-N, San Cristobal la Laguna 38205, Spain. EM mrabus@iac.es RI Rabus, Markus/B-8029-2009; Alonso, Roi/D-8799-2014 OI Alonso, Roi/0000-0001-8462-8126 FU European Association for Research in Astronomy (EARA); EARA - Marie Curie Early Stage Training FX This article publishes observations made with the IAC-80 telescope operated by the Instituto de Astrofisica de Canarias in the Observatorio del Teide. M. R. likes to thank the European Association for Research in Astronomy (EARA) for their support with an EARA - Marie Curie Early Stage Training fellowship. Some of the analysis described here is also based on data from the STARE and PSST telescopes. We also thank the anonymous referee for valuable comments. NR 16 TC 56 Z9 56 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JAN PY 2009 VL 494 IS 1 BP 391 EP 397 DI 10.1051/0004-6361:200811110 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 402VC UT WOS:000263040200034 ER PT J AU Simionescu, A Werner, N Bohringer, H Kaastra, JS Finoguenov, A Bruggen, M Nulsen, PEJ AF Simionescu, A. Werner, N. Boehringer, H. Kaastra, J. S. Finoguenov, A. Brueggen, M. Nulsen, P. E. J. TI Chemical enrichment in the cluster of galaxies Hydra A SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE X-rays: galaxies: clusters; galaxies: clusters: individual: Hydra A; galaxies: abundances; galaxies: cooling flows; galaxies: intergalactic medium ID RAY-EMITTING GAS; XMM-NEWTON; X-RAY; INTRACLUSTER MEDIUM; ELLIPTIC GALAXIES; A CLUSTER; VORONOI TESSELLATIONS; ELEMENTAL ABUNDANCES; CENTAURUS CLUSTER; BUOYANT BUBBLES AB We analyzed global properties, radial profiles, and 2D maps of the metal abundances and temperature in the cool core cluster of galaxies Hydra A using a deep similar to 120 ks XMM-Newton exposure. The best fit among the available spectral models is provided by a Gaussian distribution of the emission measure (gdem). We can accurately determine abundances for 7 elements in the cluster core with EPIC (O, Si, S, Ar, Ca, Fe, Ni) and 3 elements (O, Ne, Fe) with RGS. The gdem model gives lower Fe abundances than a single-temperature model. Based on this, we explain why simulations show that the best-fit Fe abundance in clusters with intermediate temperatures is overestimated. The abundance profiles for Fe, Si, S, but also O are centrally peaked. Combining the Hydra A results with 5 other clusters for which detailed chemical abundance studies are available, we find a significant decrease in O with radius, while the increase in the O/Fe ratio with radius is small within 0.1 r(200), where the O abundances can be accurately determined, with d(O/Fe)/d(log(10)r/r(200)) = 0.25 +/- 0.09. We compare the observed abundance ratios with the mixing of various supernova type Ia and core-collapse yield models in different relative amounts. Producing the estimated O, Si, and S peaks in Hydra A requires either the amount of metals ejected by stellar winds to be 3-8 times higher than predicted by available models or the initial enrichment by core-collapse supernovae in the protocluster phase not to be as well mixed on large scales as previously thought. The temperature map shows cooler gas extending in arm-like structures towards the north and south. These structures, and especially the northern one, appear to be richer in metals than the ambient medium and spatially correlated with the large-scale radio lobes. With different sets of assumptions, we estimate the mass of cool gas, which was probably uplifted by buoyant bubbles of relativistic plasma produced by the AGN, to 1.6-6.1 x 10(9) M-circle dot, and the energy associated with this uplift to 3.3-12.5 x 10(58) erg. The best estimate of the mass of Fe uplifted together with the cool gas is 1.7 x 10(7) M-circle dot, 15% of the total mass of Fe in the central 0.5' region. C1 [Simionescu, A.; Boehringer, H.; Finoguenov, A.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Werner, N.; Kaastra, J. S.] SRON, Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands. [Finoguenov, A.] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA. [Brueggen, M.] Jacobs Univ Bremen, D-28759 Bremen, Germany. [Nulsen, P. E. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Simionescu, A (reprint author), Max Planck Inst Extraterr Phys, Giessenbachstr, D-85748 Garching, Germany. EM aurora@mpe.mpg.de OI Nulsen, Paul/0000-0003-0297-4493 FU DFG [BR 2026/3]; BMBF/DLR [50 OR 0207]; MPG; ESA; USA (NASA) [NNX07AQ18G 16610022]; NWO; Netherlands Organization for Scientific Research FX We would like to thank W. R. Forman and J. Vink for helpful discussions. We acknowledge the support by the DFG grant BR 2026/3 within the Priority Programme "Witnesses of Cosmic History" and NASA grant NNX07AQ18G 16610022. AS would like to thank the Harvard-Smithsonian CfA, SRON, and Jacobs University Bremen for their hospitality. A. F. acknowledges support from BMBF/DLR under grant 50 OR 0207 and MPG. This work is based on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA member states and the USA (NASA). The Netherlands Institute for Space Research (SRON) is supported financially by NWO, the Netherlands Organization for Scientific Research. NR 67 TC 67 Z9 67 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 JAN PY 2009 VL 493 IS 2 BP 409 EP 424 DI 10.1051/0004-6361:200810225 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 396OP UT WOS:000262601300010 ER PT J AU Aalto, S Wilner, D Spaans, M Wiedner, MC Sakamoto, K Black, JH Caldas, M AF Aalto, S. Wilner, D. Spaans, M. Wiedner, M. C. Sakamoto, K. Black, J. H. Caldas, M. TI High-resolution HNC 3-2 SMA observations of Arp 220 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: evolution; galaxies: individual: Arp 220; galaxies: starburst; galaxies: active; radio lines: ISM; ISM: molecules ID GALAXY NUCLEI; ARP-220; LINE; GAS; DIAGNOSTICS; ABUNDANCES; MEGAMASER; CONTINUUM; CHEMISTRY; EMISSION AB Aims. We study the properties of the nuclear molecular gas of the ultra luminous merger Arp 220 and effects of the nuclear source on gas excitation and chemistry. Specifically, our aim is to investigate the spatial location of the luminous HNC 3-2 line emission and address the underlying cause of its unusual brightness. Methods. We present high resolution observations of HNC J = 3-2 with the submillimeter array (SMA). Results. We find luminous HNC 3-2 line emission in the western part of Arp 220, centred on the western nucleus, while the eastern side of the merger shows relatively faint emission. A bright (36 K at 0 ''.4 resolution), narrow (60 km s(-1)) emission feature emerges from the western nucleus, superposed on a broader spectral component. A possible explanation is weak maser emission through line-of-sight amplification of the background continuum source. There is also a more extended HNC 3-2 emission feature north and south of the nucleus. This feature resembles the bipolar OH maser morphology around the western nucleus. Substantial HNC abundances are required to explain the bright line emission from this warm environment - even when the high gas column density towards the western nucleus is taken into account. We discuss this briefly in the context of an X-ray affected chemistry and radiative excitation. Conclusions. The luminous and possibly amplified HNC emission of the western nucleus of the Arp 220 merger reflects the unusual, and perhaps transient environment of the starburst/AGN activity there. The faint HNC line emission towards Arp 220-east reveals a real difference in physical conditions between the two merger nuclei. C1 [Aalto, S.; Black, J. H.; Caldas, M.] Chalmers, Onsala Observ, Dept Radio & Space Sci, S-43994 Onsala, Sweden. [Wilner, D.; Sakamoto, K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Wiedner, M. C.] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. [Spaans, M.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Sakamoto, K.] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Sakamoto, K.] Natl Inst Nat Sci, Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. RP Aalto, S (reprint author), Chalmers, Onsala Observ, Dept Radio & Space Sci, S-43994 Onsala, Sweden. EM saalto@chalmers.se FU Smithsonian Institution; Academia Sinica FX We thank an anonymous referee for useful comments and suggestions that helped improve the paper. The Submillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. NR 21 TC 21 Z9 21 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JAN PY 2009 VL 493 IS 2 BP 481 EP 487 DI 10.1051/0004-6361:200810394 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 396OP UT WOS:000262601300016 ER PT J AU Forbrich, J Stanke, T Klein, R Henning, T Menten, KM Schreyer, K Posselt, B AF Forbrich, J. Stanke, Th. Klein, R. Henning, Th. Menten, K. M. Schreyer, K. Posselt, B. TI A multi-wavelength study of a double intermediate-mass protostar - from large-scale structure to collimated jets SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: formation; ISM: jets and outflows ID YOUNG STELLAR OBJECTS; MOLECULAR OUTFLOWS; STAR-FORMATION; MULTIPLE OUTFLOWS; REGIONS; ORION; N2H+; CLOUDS; CORES; GAS AB Aims. The earliest stages of intermediate- and high-mass star formation remain poorly understood. To gain deeper insights, we study a previously discovered protostellar source that is deeply embedded and drives an energetic molecular outflow. Methods. The source, UYSO 1, located close to IRAS 07029-1215 at a distance of about 1 kpc, was observed in the (sub) millimeter and centimeter wavelength ranges, as well as at near-, mid-, and far-infrared wavelengths. Results. The multi-wavelength observations resulted in the detection of a double intermediate- mass protostar at the location of UYSO1. In addition to the associated molecular outflow, with a projected size of 0.25 pc, two intersecting near- infrared jets with projected sizes of 0.4 pc and 0.2 pc were found. However, no infrared counterparts to the driving sources could be detected in sensitive near- to far-infrared observations (including Spitzer). In interferometric millimeter observations, UYSO 1 was resolved into two continuum sources with high column densities (>10(24) cm(-2)) and gas masses of 3.5 M(circle dot) and 1.2 M(circle dot), with a linear separation of 4200 AU. We report the discovery of a H(2)O maser towards one of the two sources. Within an appropriate multi-wavelength coverage, the total luminosity is roughly estimated to be less than or similar to 50 L(circle dot), shared by the two components, one of which is driving the molecular outflow that has a dynamical timescale of less than a few thousand years. The jets of the two individual components are not aligned. Submillimeter observations show that the region lacks the typical hot-core chemistry. Conclusions. We find two protostellar objects, whose associated circumstellar and parent core masses are high enough to suggest that they may evolve into intermediate- mass stars. This is corroborated by their association with a very massive and energetic CO outflow, suggesting high protostellar accretion rates. The short dynamical timescale of the outflow, the pristine chemical composition of the cloud core and absence of hot core tracers, the absence of detectable radio continuum emission, and the very low protostellar luminosity argue for an extremely early evolutionary stage. C1 [Forbrich, J.; Menten, K. M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Forbrich, J.; Schreyer, K.; Posselt, B.] Inst Astrophys, D-07745 Jena, Germany. [Forbrich, J.; Schreyer, K.; Posselt, B.] Univ Sternwarte, D-07745 Jena, Germany. [Forbrich, J.; Posselt, B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Stanke, Th.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Stanke, Th.] European So Observ, D-85748 Garching, Germany. [Klein, R.; Posselt, B.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Klein, R.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Henning, Th.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. RP Forbrich, J (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. EM jforbrich@cfa.harvard.edu OI Klein, Randolf/0000-0002-7187-9126; Posselt, Bettina/0000-0003-2317-9747 FU A. V. Humboldt Foundation; Spitzer [JPL 1276999]; National Science Foundation; INSU/CNRS (France); MPG (Germany); IGN (Spain); ESO Telescopes at the Paranal Observatory [074.C-0648(A), 076.C-0773(B)]; NASA FX We wish to thank Sandra Bruenken for additional observations at Effelsberg, Jens Kauffmann for help with the 30 m observations, Marian Szymczak for trying to detect CH3OH emission towards UYSO 1 at Torun, Philippe Salome and Robert Zylka, both at IRAM Grenoble, for support in analyzing the PdBI data, as well as Henrik Beuther for helpful discussions. We would like to thank the referee, John Bally, for his helpful comments. T. S. is grateful for support through the A. V. Humboldt Foundation during his stay at the University of Hawaii. R. K. acknowledges support through Spitzer grant JPL no. 1276999. Partly based on Director's Discretionary Time observations collected at the Centro Astronomico Hispano Aleman (CAHA) at Calar Alto, operated jointly by the Max-Planck Institut fur Astronomie and the Instituto de Astrofisica de Andalucia (CSIC). The National Radio Astronomy Observatory (NRAO) is operated by Associated Universities, Inc., under a cooperative agreement with the National Science Foundation. Partly based on observations carried out with the IRAM Plateau de Bure Interferometer and the IRAM 30 m telescope. IRAM is supported by INSU/CNRS (France), MPG (Germany) and IGN (Spain). Partly based on observations made with ESO Telescopes at the Paranal Observatory under programme IDs 074.C-0648(A) and 076.C-0773(B). The James Clerk Maxwell Telescope is operated by The Joint Astronomy Centre on behalf of the Science and Technology Facilities Council of the United Kingdom, the Netherlands Organisation for Scientific Research, and the National Research Council of Canada. 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. Partly based on observations with the 100-m telescope of the MPIfR (Max-Planck-Institut fur Radioastronomie) at Effelsberg. NR 34 TC 9 Z9 9 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JAN PY 2009 VL 493 IS 2 BP 547 EP 556 DI 10.1051/0004-6361:200810598 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 396OP UT WOS:000262601300022 ER PT J AU Orlando, S Drake, JJ Laming, JM AF Orlando, S. Drake, J. J. Laming, J. M. TI Three-dimensional modeling of the asymmetric blast wave from the 2006 outburst of RS Ophiuchi: Early X-ray emission SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE shock waves; stars: binaries: symbiotic; stars: individual: RS Oph; stars: novae, cataclysmic variables; X-rays: binaries ID INTERSTELLAR GAS CLOUDS; ELECTRON THERMAL CONDUCTION; SUPERNOVA-REMNANTS; RECURRENT NOVAE; SYMBIOTIC STARS; LIGHT-CURVE; SHOCK-WAVE; SYSTEMS; HYDRODYNAMICS; SPECTROSCOPY AB Context. Chandra/HETG observations of the recurrent nova RS Ophiuchi at day 13.9 of its 2006 outburst reveal a spectrum covering a large range in plasma temperature and characterized by asymmetric and blue-shifted emission lines (Nelson et al. 2008; Drake et al. 2008). Aims. We investigate the origin of asymmetries and broadening of the emission lines observed with Chandra/HETG. We explore possible diagnostics of the early blast wave and of the circumstellar medium (CSM) in which the explosion occurred. Methods. We perform 3D hydrodynamic simulations of the blast wave from the 2006 outburst, propagating through the inhomogeneous CSM. The model takes into account the thermal conduction (including the effects of heat flux saturation) and the radiative cooling. From the simulations, we synthesize the X-ray emission and derive the spectra as they would be observed with Chandra/HETG. Results. The simulated nova remnant is highly aspherical and the blast wave is efficiently collimated by the inhomogeneous CSM. Our model reproduces the observed X-ray emission in a natural way if the CSM in which the outburst occurred is characterized by an equatorial density enhancement. Our "best-fit" model predicts that most of the early X-ray emission originates from a small region propagating in the direction perpendicular to the line-of-sight and localized just behind the interaction front between the blast wave and the equatorial density enhancement. The model predicts asymmetric and blue-shifted line profiles remarkably similar to those observed. These asymmetries are due to substantial X-ray absorption of red-shifted emission by ejecta material. Conclusions. The comparison of high quality data of Chandra/HETG with detailed hydrodynamic modeling has allowed us to unveil, for the first time, the details of the structure emitting in the X-ray band in early phases of the outburst evolution, contributing to a better understanding of the physics of interactions between nova blasts and CSM in recurrent novae. This may have implications for whether or not RS Ophiuchi is a type Ia SN progenitor system. C1 [Orlando, S.] INAF Osservatorio Astron Palermo GS Vaiana, I-90134 Palermo, Italy. [Orlando, S.] Consorzio COMETA, I-95123 Catania, Italy. [Drake, J. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Laming, J. M.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA. RP Orlando, S (reprint author), INAF Osservatorio Astron Palermo GS Vaiana, Piazza Parlamento 1, I-90134 Palermo, Italy. EM orlando@astropa.inaf.it OI Orlando, Salvatore/0000-0003-2836-540X FU Ministry of University and Research (MIUR); Istituto Nazionale di Astrofisica (INAF); Piano Operativo Nazionale "Ricerca Scientifica, Sviluppo Tecnologico [20002006] FX This work was supported in part by the Italian Ministry of University and Research (MIUR) and by Istituto Nazionale di Astrofisica (INAF). The software used in this work was in part developed by the DOEsupported ASC/Alliance Center for Astrophysical Thermonuclear Flashes at the University of Chicago, using modules for thermal conduction and optically thin radiation built at the Osservatorio Astronomico di Palermo. The simulations were executed on the Grid infrastructure of the Consorzio COMETA. This work makes use of results produced by the PI2S2 Project managed by the Consorzio COMETA, a project co-funded by the Italian Ministry of University and Research (MIUR) within the Piano Operativo Nazionale "Ricerca Scientifica, Sviluppo Tecnologico, Alta Formazione" (PON 20002006). More information is available at http://www. pi2s2. it and http://www. consorzio-cometa. it. NR 53 TC 24 Z9 24 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JAN PY 2009 VL 493 IS 3 BP 1049 EP 1059 DI 10.1051/0004-6361:200810109 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 397DA UT WOS:000262641100024 ER PT J AU Dijkstra, M AF Dijkstra, Mark TI CONTINUUM EMISSION BY COOLING CLOUDS SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: theory; galaxies: formation; galaxies: high-redshift; radiation mechanisms: general ID LY-ALPHA EMITTERS; HIGH-REDSHIFT GALAXIES; EQUATION-OF-STATE; SUBARU DEEP FIELD; COLD ACCRETION; POPULATION III; RADIATION; REIONIZATION; LUMINOSITY; UNIVERSE AB The collapse of baryons into the center of a host dark matter halo is accompanied by radiation that may be detectable as compact (less than or similar to 10 kpc) UV-continuum and Ly alpha emission with Ly alpha luminosities as high as similar to 10(42)-10(43) erg s(-1) in halos of mass M = 10(11)-10(12) M(circle dot). We show that the observed equivalent width (EW) of the Ly alpha line emitted by these cooling clouds is EW less than or similar to 400 angstrom ( rest frame). These luminosities and EWs are comparable to those detected in narrowband surveys for redshifted Ly alpha emission. The rest-frame ultraviolet of Ly alpha-emitting cooling clouds radiation may be dominated by two-photon transitions from 2s -> 1s. The resulting spectrum can distinguish cooling clouds from a broad class of young star-forming galaxies. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Dijkstra, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 51 TC 19 Z9 19 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 1 PY 2009 VL 690 IS 1 BP 82 EP 88 DI 10.1088/0004-637X/690/1/82 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 398IU UT WOS:000262726600006 ER PT J AU Grimm, HJ McDowell, J Fabbiano, G Elvis, M AF Grimm, H. -J. McDowell, J. Fabbiano, G. Elvis, M. TI AN X-RAY PHOTOMETRY SYSTEM I: CHANDRA ACIS SO ASTROPHYSICAL JOURNAL LA English DT Article DE techniques: photometric; X-rays: general ID CONFIDENCE-LIMITS; EFFECTIVE AREA; SKY SURVEY; CCD; NUMBERS AB We present a system of X-ray photometry for the Chandra satellite. X-ray photometry can be a powerful tool to obtain flux estimates, hardness ratios, and colors unbiased by assumptions about spectral shape and independent of temporal and spatial changes in instrument characteristics. The system we have developed relies on our knowledge of effective area and the energy-to-channel conversion to construct filters similar to photometric filters in the optical bandpass. We show that the filters are well-behaved functions of energy and that this X-ray photometric system is able to reconstruct fluxes to within about 20%, without color corrections, for non-pathological spectra. Even in the worst cases it is better than 50%. Our method also treats errors in a consistent manner, both statistical and systematic. C1 [Grimm, H. -J.; McDowell, J.; Fabbiano, G.; Elvis, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Grimm, HJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. FU NASA [GO2-3135X]; CXC [NAS8-03060] FX H. J. G. thanks Ralph Kraft for providing the source code for computing confidence limits, and Paul Plucinsky for discussions about the RMF. This work has been supported by NASA grant GO2-3135X and CXC grant NAS8-03060. NR 23 TC 6 Z9 6 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 1 PY 2009 VL 690 IS 1 BP 128 EP 142 DI 10.1088/0004-637X/690/1/128 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 398IU UT WOS:000262726600011 ER PT J AU Ling, ZX Zhang, SN Xiang, JG Tang, SC AF Ling, Zhixing Zhang, Shuang Nan Xiang, Jingen Tang, Shichao TI A STUDY OF THE X-RAY DUST SCATTERING HALO OF CYG X-1 WITH A CROSS-CORRELATION METHOD SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; scattering; X-rays: binaries; X-rays: ISM ID INTERSTELLAR GRAINS; BLACK-HOLE; DISTANCE; DISTRIBUTIONS; EXTINCTION; AFTERGLOWS; BURSTS; DARK AB X-ray photons scattered by the interstellar medium carry information about dust distribution, dust grain model, scattering cross section, and the distance of the source; they also take a longer time than unscattered photons to reach the observer. Using a cross-correlation method, we study the light curves of the X-ray dust scattering halo of Cyg X-1, observed with the Chandra X-ray Observatory. Significant time lags are found between the light curves of the point source and its halo. This time lag increases with the angular distance from Cyg X-1, implying a dust concentration at a distance along the line of sight (LOS) of 2.0 kpc x (0.876 +/- 0.002) from the Earth. By fitting the observed light curves of the halo at different radii with simulated light curves, we obtain a width of Delta L = 33(-13)(+18) pc of this dust concentration. The origin of this dust concentration is still not clearly known. The advantage of our method is that we need no assumption of scattering cross section, dust grain model, or dust distribution along the LOS. Combining the derived dust distribution from the cross-correlation study with the surface brightness distribution of the halo, we conclude that the two commonly accepted models of dust grain size distribution need to be modified significantly. C1 [Ling, Zhixing; Zhang, Shuang Nan; Tang, Shichao] Tsinghua Univ, Dept Phys, Beijing 100084, Peoples R China. [Ling, Zhixing; Zhang, Shuang Nan; Tang, Shichao] Tsinghua Univ, Tsinghua Ctr Astrophys, Beijing 100084, Peoples R China. [Zhang, Shuang Nan] Chinese Acad Sci, Key Lab Particle Astrophys, Inst High Energy Phys, Beijing 100049, Peoples R China. [Zhang, Shuang Nan] Univ Alabama, Dept Phys, Huntsville, AL 35899 USA. [Xiang, Jingen] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Ling, ZX (reprint author), Tsinghua Univ, Dept Phys, Beijing 100084, Peoples R China. EM lingzhixing@tsinghua.org.cn; zhangsn@tsinghua.edu.cn; jxiang@cfa.harvard.edu; tsc02@mails.tsinghua.edu.cn FU Ministry of Education of China, Directional Research Project of the Chinese Academy of Sciences [KJCX2-YW-T03]; Chinese Academy of Sciences [10521001, 10733010, 10725313]; 973 Program of China [2009CB824800] FX We thank Jian Hu, Yuan Liu, Yue Wu, and Li Shao for useful discussions and RandallK. Smith for providing the model codes. The anonymous referee is thanked for kind suggestions which helped to clarify several points. This study is supported in part by the Ministry of Education of China, Directional Research Project of the Chinese Academy of Sciences under project No. KJCX2-YW-T03 and by the National Natural Science Foundation of China under project No. 10521001, 10733010, 10725313, and by 973 Program of China under grant 2009CB824800. NR 25 TC 7 Z9 8 U1 1 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 1 PY 2009 VL 690 IS 1 BP 224 EP 230 DI 10.1088/0004-637X/690/1/224 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 398IU UT WOS:000262726600019 ER PT J AU Lidz, A Zahn, O Furlanetto, SR McQuinn, M Hernquist, L Zaldarriaga, M AF Lidz, Adam Zahn, Oliver Furlanetto, Steven R. McQuinn, Matthew Hernquist, Lars Zaldarriaga, Matias TI PROBING REIONIZATION WITH THE 21 CM GALAXY CROSS-POWER SPECTRUM SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: theory; intergalactic medium; large-scale structure of universe ID LY-ALPHA EMITTERS; LOW-MASS GALAXIES; HIGH-REDSHIFT; HII-REGIONS; HYDROGEN REIONIZATION; INTERGALACTIC MEDIUM; COSMIC REIONIZATION; STAR-FORMATION; BUBBLE-GROWTH; EPOCH AB The cross-correlation between high-redshift galaxies and 21 cm emission from the high-redshift intergalactic medium promises to be an excellent probe of the Epoch of Reionization. On large scales, the 21 cm and galaxy fields are anticorrelated during most of the reionization epoch. However, on scales smaller than the size of the H II regions around detectable galaxies, the two fields become roughly uncorrelated. Consequently, the 21 cm galaxy cross-power spectrum provides a tracer of bubble growth during reionization, with the signal turning over on progressively larger scales as reionization proceeds. The precise turnover scale depends on the minimum host mass of the detectable galaxies, and the galaxy selection technique. Measuring the turnover scale as a function of galaxy luminosity constrains the characteristic bubble size around galaxies of different luminosities. The cross-spectrum becomes positive on small scales if ionizing photons fail to escape from low-mass galaxies, and these galaxies are detectable longward of the hydrogen ionization edge, because in this case some identifiable galaxies lie outside the ionized regions. The Murchison Widefield Array (MWA) and Low Frequency Array can potentially measure the 21 cm galaxy cross-spectrum in conjunction with mild extensions to the existing Subaru survey for z = 6.6 Ly alpha emitters. A futuristic galaxy survey covering a sizable fraction of the MWA field of view (similar to 800 deg(2)) can probe the scale dependence of the cross-spectrum, constraining the filling factor of H II regions at different redshifts during reionization, and providing other valuable constraints on reionization models. C1 [Lidz, Adam; McQuinn, Matthew; Hernquist, Lars; Zaldarriaga, Matias] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Zahn, Oliver] Univ Calif Berkeley, Dept Phys, Berkeley Ctr Cosmol Phys, Berkeley, CA 94720 USA. [Zahn, Oliver] Lawrence Berkeley Natl Labs, Berkeley, CA 94720 USA. [Furlanetto, Steven R.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Zaldarriaga, Matias] Harvard Univ, Jefferson Lab Phys, Cambridge, MA 02138 USA. RP Lidz, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM alidz@cfa.harvard.edu FU David and Lucile Packard Foundation; Alfred P. Sloan Foundation; Berkeley Center for Cosmological Physics (BCCP) Fellowship [AST-0506556, NNG05GJ40G] FX We thank Mark Dijkstra and Miguel Morales for helpful discussions. We thank Suvendra Dutta for useful conversations and for his collaboration in related work. We are grateful to Saleem Zaroubi and the anonymous referee for pointing us to the new LOFAR specifications in Jelic et al. (2008), and to Saleem Zaroubi for helpful conversations regarding LOFAR. Support was provided, in part, by the David and Lucile Packard Foundation, the Alfred P. Sloan Foundation, and grants AST-0506556 and NNG05GJ40G. O.Z. acknowledges additional support by a Berkeley Center for Cosmological Physics (BCCP) Fellowship. NR 57 TC 34 Z9 34 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 1 PY 2009 VL 690 IS 1 BP 252 EP 266 DI 10.1088/0004-637X/690/1/252 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 398IU UT WOS:000262726600023 ER PT J AU Hanke, M Wilms, J Nowak, MA Pottschmidt, K Schulz, NS Lee, JC AF Hanke, Manfred Wilms, Joern Nowak, Michael A. Pottschmidt, Katja Schulz, Norbert S. Lee, Julia C. TI CHANDRA X-RAY SPECTROSCOPY OF THE FOCUSED WIND IN THE CYGNUS X-1 SYSTEM. I. THE NONDIP SPECTRUM IN THE LOW/HARD STATE SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; stars: individual (HDE 226868, Cyg X-1); stars: winds, outflows; techniques: spectroscopic; X-rays: binaries ID LONG-TERM VARIABILITY; REFLECTION GRATING SPECTROMETER; PHOTOIONIZATION CROSS-SECTIONS; RADIATION-DRIVEN WINDS; BLACK-HOLE CANDIDATES; ION LINE-INTENSITIES; HELIUM-LIKE IONS; MASS-LOSS RATES; TIMING-EXPLORER; INTERSTELLAR-MEDIUM AB We present analyses of a 50 ks observation of the supergiant X-ray binary system Cygnus X-1 (Cyg X-1)/HDE226868 taken with the Chandra High Energy Transmission Grating Spectrometer (HETGS). Cyg X-1 was in its spectrally hard state and the observation was performed during superior conjunction of the black hole, allowing for the spectroscopic analysis of the accreted stellar wind along the line of sight. A significant part of the observation covers X-ray dips as commonly observed for Cyg X-1 at this orbital phase, however, here we analyze only the high count rate nondip spectrum. The full 0.5-10 keV continuum can be described by a single model consisting of a disk, a narrow and a relativistically broadened Fe K alpha line, and a power-law component, which is consistent with simultaneous Rossi X-Ray Timing Explorer broadband data. We detect absorption edges from overabundant neutral O, Ne, and Fe, and absorption line series from highly ionized ions and infer column densities and Doppler shifts. With emission lines of He-like Mg XI, we detect two plasma components with velocities and densities consistent with the base of the spherical wind and a focused wind. A simple simulation of the photoionization zone suggests that large parts of the spherical wind outside of the focused stream are completely ionized, which is consistent with the low velocities (<200 km s(-1)) observed in the absorption lines, as the position of absorbers in a spherical wind at low projected velocity is well constrained. Our observations provide input for models that couple the wind activity of HDE 226868 to the properties of the accretion flow onto the black hole. C1 [Hanke, Manfred; Wilms, Joern] Univ Erlangen Nurnberg, Astron Inst, Dr Karl Remeis Sternwarte, D-96049 Bamberg, Germany. [Hanke, Manfred; Wilms, Joern] Univ Erlangen Nurnberg, Erlangen Ctr Astroparticle Phys, D-91058 Erlangen, Germany. [Nowak, Michael A.; Schulz, Norbert S.] MIT, CXC, Cambridge, MA 02139 USA. [Pottschmidt, Katja] Univ Maryland Baltimore Cty, Ctr Res & Explorat Space Sci & Technol, Baltimore, MD 21250 USA. [Pottschmidt, Katja] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Pottschmidt, Katja] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA. [Lee, Julia C.] Harvard Univ, Dept Astron, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Hanke, M (reprint author), Univ Erlangen Nurnberg, Astron Inst, Dr Karl Remeis Sternwarte, Sternwartstr 7, D-96049 Bamberg, Germany. EM Manfred.Hanke@sternwarte.uni-erlangen.de RI Wilms, Joern/C-8116-2013; Lee, Julia/G-2381-2015 OI Wilms, Joern/0000-0003-2065-5410; Lee, Julia/0000-0002-7336-3588 NR 97 TC 41 Z9 41 U1 1 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 1 PY 2009 VL 690 IS 1 BP 330 EP 346 DI 10.1088/0004-637X/690/1/330 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 398IU UT WOS:000262726600029 ER PT J AU Raghavan, D McAlister, HA Torres, G Latham, DW Mason, BD Boyajian, TS Baines, EK Williams, SJ ten Brummelaar, TA Farrington, CD Ridgway, ST Sturmann, L Sturmann, J Turner, NH AF Raghavan, Deepak McAlister, Harold A. Torres, Guillermo Latham, David W. Mason, Brian D. Boyajian, Tabetha S. Baines, Ellyn K. Williams, Stephen J. ten Brummelaar, Theo A. Farrington, Chris D. Ridgway, Stephen T. Sturmann, Laszlo Sturmann, Judit Turner, Nils H. TI THE VISUAL ORBIT OF THE 1.1 DAY SPECTROSCOPIC BINARY sigma(2) CORONAE BOREALIS FROM INTERFEROMETRY AT THE CHARA ARRAY SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: spectroscopic; stars: fundamental parameters; stars: individual (sigma(2) Coronae Borealis); techniques: interferometric ID PROPER-MOTION STARS; SOLAR NEIGHBORHOOD; RADIAL-VELOCITIES; MULTIPLE STARS; NEARBY STARS; F-DWARF; MASS; CALIBRATION; ASTROMETRY; ISOCHRONES AB We present an updated spectroscopic orbit and a new visual orbit for the double-lined spectroscopic binary sigma(2) Coronae Borealis (CrB) based on radial velocity measurements at the Oak Ridge Observatory in Harvard, MA and interferometric visibility measurements at the Center for High Angular Resolution Astronomy (CHARA) Array on Mount Wilson in California. sigma(2) CrB is composed of two Sun-like stars of roughly equal mass in a circularized orbit with a period of 1.14 days. The long baselines of the CHARA Array have allowed us to resolve the visual orbit for this pair, the shortest-period binary yet resolved interferometrically, enabling us to determine component masses of 1.137 +/- 0.037 M-circle dot and 1.090 +/- 0.036 M-circle dot. We have also estimated absolute V-band magnitudes of M-V(primary) = 4.35 +/- 0.02 and M-V(secondary) = 4.74 +/- 0.02. A comparison with stellar evolution models indicates a relatively young age of 0.1-3 Gyr, consistent with the high-Li abundance measured previously. This pair is the central component of a quintuple system, along with another similar-mass star, sigma(1) CrB, in a similar to 730-year visual orbit, and a distant M-dwarf binary, sigma CrB C, at a projected separation of similar to 10'. We also present differential proper motion evidence to show that components C & D ( ADS 9979C & D) listed for this system in the Washington Double Star Catalog are optical alignments that are not gravitationally bound to the sigma CrB system. C1 [Raghavan, Deepak; McAlister, Harold A.; Boyajian, Tabetha S.; Baines, Ellyn K.; Williams, Stephen J.] Georgia State Univ, Ctr High Angular Resolut Astron, Atlanta, GA 30302 USA. [Torres, Guillermo; Latham, David W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Mason, Brian D.] USN Observ, Washington, DC 20392 USA. [ten Brummelaar, Theo A.; Farrington, Chris D.; Sturmann, Laszlo; Sturmann, Judit; Turner, Nils H.] Mt Wilson Observ, CHARA Array, Mt Wilson, CA 91023 USA. [Ridgway, Stephen T.] Natl Opt Astron Observ, Tucson, AZ 85726 USA. RP Raghavan, D (reprint author), Georgia State Univ, Ctr High Angular Resolut Astron, POB 3969, Atlanta, GA 30302 USA. EM raghvan@chara.gsu.edu FU College of Arts and Sciences at Georgia State University; National Science Foundation (NSF) [AST-0606958, AST-0708229]; NASA [BLF5704] FX We thank Andy Boden and Doug Gies for their many useful suggestions that improved the quality of this work, and Richard Gray for making new observations at our request to confirm the spectral typing of the components. The CfA spectroscopic observations of sigma1 CrB and sigma2 CrB used in this paper were obtained with the help of J. Caruso, R.P. Stefanik, and J. Zajac. We also thank the CHARA Array operator P.J. Goldfinger for obtaining some of the data used here and for her able assistance of remote operations of the Array from AROC. Research at the CHARA Array is supported by the College of Arts and Sciences at Georgia State University and by the National Science Foundation (NSF) through NSF grant AST-0606958. G.T. acknowledges partial support for this work from NSF grant AST-0708229 and NASA's MASSIF SIM Key Project (BLF5704). This research has made use of the SIMBAD literature database, operated at Centre de Donnees Astronomiques de Strasbourg, France, and of NASA's Astrophysics Data System. This effort used multi-epoch images from the Digitized Sky Survey, which was produced at the Space Telescope Science Institute under U.S. Government grant NAG W-2166. This publication also made use of data products from the 2MASS, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by NASA and the NSF. NR 48 TC 27 Z9 27 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 1 PY 2009 VL 690 IS 1 BP 394 EP 406 DI 10.1088/0004-637X/690/1/394 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 398IU UT WOS:000262726600034 ER PT J AU Green, PJ Aldcroft, TL Richards, GT Barkhouse, WA Constantin, A Haggard, D Karovska, M Kim, DW Kim, M Vikhlinin, A Anderson, SF Mossman, A Kashyap, V Myers, AC Silverman, JD Wilkes, BJ Tananbaum, H AF Green, Paul J. Aldcroft, T. L. Richards, G. T. Barkhouse, W. A. Constantin, A. Haggard, D. Karovska, M. Kim, D. -W. Kim, M. Vikhlinin, A. Anderson, S. F. Mossman, A. Kashyap, V. Myers, A. C. Silverman, J. D. Wilkes, B. J. Tananbaum, H. TI A FULL YEAR'S CHANDRA EXPOSURE ON SLOAN DIGITAL SKY SURVEY QUASARS FROM THE CHANDRA MULTIWAVELENGTH PROJECT SO ASTROPHYSICAL JOURNAL LA English DT Review DE galaxies: active; quasars: absorption lines; quasars: general; surveys; X-rays: general ID ACTIVE GALACTIC NUCLEI; BROAD-ABSORPTION-LINE; RADIO-QUIET QUASARS; X-RAY-PROPERTIES; SUPERMASSIVE BLACK-HOLES; PHOTOMETRICALLY CLASSIFIED QUASARS; DEEP FIELD-SOUTH; LUMINOSITY FUNCTION; STELLAR OBJECTS; HIGH-REDSHIFT AB We study the spectral energy distributions and evolution of a large sample of optically selected quasars from the Sloan Digital Sky Survey that were observed in 323 Chandra images analyzed by the Chandra Multiwavelength Project. Our highest-confidence matched sample includes 1135 X-ray detected quasars in the redshift range 0.2 < z < 5.4, representing some 36 Msec of effective exposure. We provide catalogs of QSO properties, and describe our novel method of calculating X-ray flux upper limits and effective sky coverage. Spectroscopic redshifts are available for about 1/3 of the detected sample; elsewhere, redshifts are estimated photometrically. We detect 56 QSOs with redshift z > 3, substantially expanding the known sample. We find no evidence for evolution out to z similar to 5 for either the X-ray photon index Gamma or for the ratio of optical/UV to X-ray flux alpha(ox). About 10% of detected QSOs show best-fit intrinsic absorbing columns greater than 10(22) cm(-2), but the fraction might reach similar to 1/3 if most nondetections are absorbed. We confirm a significant correlation between alpha(ox) and optical luminosity, but it flattens or disappears for fainter (M-B greater than or similar to -23) active galactic nucleus (AGN) alone. We report significant hardening of Gamma both toward higher X-ray luminosity, and for relatively X-ray loud quasars. These trends may represent a relative increase in nonthermal X-ray emission, and our findings thereby strengthen analogies between Galactic black hole binaries and AGN. For uniformly selected subsamples of narrow-line Seyfert 1s and narrow absorption line QSOs, we find no evidence for unusual distributions of either alpha(ox) or Gamma. C1 [Green, Paul J.; Aldcroft, T. L.; Constantin, A.; Karovska, M.; Kim, D. -W.; Vikhlinin, A.; Mossman, A.; Kashyap, V.; Wilkes, B. J.; Tananbaum, H.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Richards, G. T.] Drexel Univ, Dept Phys, Philadelphia, PA 15260 USA. [Barkhouse, W. A.] Univ N Dakota, Dept Phys, Grand Forks, ND 58202 USA. [Haggard, D.; Anderson, S. F.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Kim, M.] Korea Astron & Space Sci Inst, Int Ctr Astrophys, Taejon 305348, South Korea. [Myers, A. C.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA. [Silverman, J. D.] ETH, Inst Astron, CH-8093 Zurich, Switzerland. RP Green, PJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM pgreen@cfa.harvard.edu OI Constantin, Anca/0000-0002-2441-1619; Wilkes, Belinda/0000-0003-1809-2364 NR 137 TC 45 Z9 45 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 1 PY 2009 VL 690 IS 1 BP 644 EP 669 DI 10.1088/0004-637X/690/1/644 PG 26 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 398IU UT WOS:000262726600052 ER PT J AU Reach, WT Faied, D Rho, J Boogert, A Tappe, A Jarrett, TH Morris, P Cambresy, L Palla, F Valdettaro, R AF Reach, William T. Faied, Dohy Rho, Jeonghee Boogert, Adwin Tappe, Achim Jarrett, Thomas H. Morris, Patrick Cambresy, Laurent Palla, Francesco Valdettaro, Riccardo TI PROPERTIES OF PROTOSTARS IN THE ELEPHANT TRUNK IN THE GLOBULE IC 1396A SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared: stars; ISM: globules; ISM: individual (IC 1396A); planetary systems: protoplanetary discs ID YOUNG STELLAR OBJECTS; SPITZER-SPACE-TELESCOPE; BRIGHT-RIMMED CLOUDS; INTERSTELLAR SILICATE MINERALOGY; INFRARED SPECTROGRAPH IRS; MAIN-SEQUENCE EVOLUTION; HERBIG AE/BE STARS; ORION-NEBULA; MASS STARS; PROTOPLANETARY DISKS AB Extremely red objects, identified in the early Spitzer Space Telescope observations of the bright-rimmed globule IC 1396A and photometrically classified as Class I protostars and Class II T Tauri stars based on their mid-infrared (mid-IR) colors, were spectroscopically observed at 5.5-38 mu m (Spitzer Infrared Spectrograph), at the 22 GHz water maser frequency (National Radio Astronomy Observatory Green Bank Telescope), and in the optical (Palomar Hale 5 m) to confirm their nature and further elucidate their properties. The sources photometrically identified as Class I, including IC 1396A:alpha, gamma, delta, epsilon, and zeta, are confirmed as objects dominated by accretion luminosity from dense envelopes, with accretion rates 1-10 x 10(-6) M(circle dot) yr(-1) and present stellar masses 0.1-2 M(circle dot). The Class I sources have extremely red continua, still rising at 38 mu m, with a deep silicate absorption at 9-11 mu m, weaker silicate absorption around 18 mu m, and weak ice features including CO(2) at 15.2 mu m and H(2)O at 6 mu m. The ice/silicate absorption ratio in the envelope is exceptionally low for the IC 1396A protostars, compared to those in nearby star-forming regions, suggesting that the envelope chemistry is altered by the radiation field or globule pressure. Only one 22 GHz water maser was detected in IC 1396A; it is coincident with a faint mid-IR source, offset from near the luminous Class I protostar IC 1396A:gamma. The maser source, IC 1396A:gamma(b), has luminosity less than 0.1 L(circle dot), the first H(2)O maser from such a low-luminosity object. Two near-infrared (NIR) H(2) knots on opposite sides of IC 1396A:gamma reveal a jet, with an axis clearly distinct from the H(2)O maser of IC 1396A:gamma(b). The objects photometrically classified as Class II, including IC 1396A:beta, theta, Two Micron All Sky Survey (2MASS)J 21364964+5722270, 2MASSJ 21362507+5727502, LkH alpha 349c, Tr 37 11-2146, and Tr 37 11-2037, are confirmed as stars with warm, luminous disks, with a silicate emission feature at 9-11 mu m, and bright H alpha emission; therefore, they are young, disk-bearing, classical T Tauri stars. The disk properties change significantly with source luminosity: low-mass (G-K) stars have prominent 9-11 emission features due to amorphous silicates while higher-mass (A-F) stars have weaker features requiring abundant crystalline silicates. A mineralogical model that fits the wide- and low-amplitude silicate feature of IC 1396A:theta requires small grains of crystalline olivine (11.3 mu m peak) and another material to to explain its 9.1 mu m peak; reasonable fits are obtained with a phyllosilicate, quartz, or relatively large (greater than 10 mu m) amorphous olivine grains. The distribution of Class I sources is concentrated within the molecular globule, while the Class II sources are more widely scattered. Combined with the spectral results, this suggests two phases of star formation, the first (4 Myr ago) leading to the widespread Class II sources and the central O star of IC 1396 and the second (less than 1 Myr ago) occurring within the globule. The recent phase was likely triggered by the wind and radiation of the central O star of the IC1396 H II region. C1 [Reach, William T.; Boogert, Adwin; Jarrett, Thomas H.; Morris, Patrick] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Reach, William T.; Faied, Dohy; Rho, Jeonghee; Tappe, Achim; Jarrett, Thomas H.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Tappe, Achim] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Cambresy, Laurent] Observat Strasbourg, Strasbourg, France. [Palla, Francesco; Valdettaro, Riccardo] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. RP Reach, WT (reprint author), CALTECH, Ctr Infrared Proc & Anal, MS 100-22, Pasadena, CA 91125 USA. EM reach@ipac.caltech.edu OI palla, francesco/0000-0002-3321-0456; Reach, William/0000-0001-8362-4094 FU W. M. Keck Foundation; University of Massachusetts; National Aeronautics and Space Administration; National Science Foundation FX Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. This publication makes use of data products from the 2MASS, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. NR 76 TC 23 Z9 24 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 1 PY 2009 VL 690 IS 1 BP 683 EP 705 DI 10.1088/0004-637X/690/1/683 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 398IU UT WOS:000262726600054 ER PT J AU Krongold, Y Jimenez-Bailon, E Santos-Lleo, M Nicastro, F Elvis, M Brickhouse, N Andrade-Velazquez, M Binette, L Mathur, S AF Krongold, Yair Jimenez-Bailon, Elena Santos-Lleo, Maria Nicastro, Fabrizio Elvis, Martin Brickhouse, Nancy Andrade-Velazquez, Mercedes Binette, Luc Mathur, Smita TI XMM-NEWTON VIEW OF THE MULTIPHASE WARM ABSORBER IN SEYFERT 1 GALAXY NGC 985 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: Seyfert; X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; REFLECTION GRATING SPECTROMETER; SUPERSOLAR METAL ABUNDANCES; X-RAY; ACCRETION-DISK; PG QUASARS; ABSORPTION; EMISSION; NGC-5548; LINE AB We present an analysis of a new XMM-Newton observation of the Seyfert 1 galaxy NGC 985. The European Photon Imaging Camera (EPIC) spectra present strong residuals to a single power-law model, indicating the presence of ionized absorbing gas and a soft excess. A broadband fit to the EPIC and RGS spectra shows that the continuum can be well fitted with a power law (Gamma approximate to 1.57) and a blackbody component (kT approximate to 0.09 keV). The RGS can be modeled either with two or three absorption components. In the two absorber model the low-ionization one, with log U approximate to .05 and log N-H approximate to 21.08, accounts for the presence of the Fe M-shell unresolved transition array (Fe VII-XIII), and the high-ionization component (log U approximate to 1.31 and log N-H approximate to 21.99) is required by the presence of several Fe L-shell transitions. The data suggest the presence of a third ionized component with higher ionization, so that the Fe L-shell absorption features are produced by two different components (one producing absorption by Fe XVII-XX, and the other absorption by Fe XX-XXII). However, the presence of the third absorbing component cannot be detected by means of an isolated absorption line in a significant way, so we consider this detection only as tentative. Interestingly, all ionization components have similar kinematics (with outflow velocities similar to 280 km s(-1)). In addition, whether two or three absorbers are considered, the components appear to be in pressure balance within 1 sigma. These results give further support to the idea that warm absorbers in active galactic nuclei consist of a two- or three-phase medium. We note that, while in the model with only two absorbers one of them (the high-ionization component) lies on an unstable branch of the thermal equilibrium curve, in the model with three absorbers all of the components lie on stable branches of the curve. This gives further plausibility to a multiphase absorber. C1 [Krongold, Yair; Jimenez-Bailon, Elena; Andrade-Velazquez, Mercedes; Binette, Luc] Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico. [Santos-Lleo, Maria] ESA XMM Newton Sci Operat Ctr, ESAC, E-28691 Madrid, Spain. [Nicastro, Fabrizio] Osserv Astron Roma, INAF, Rome, Italy. [Nicastro, Fabrizio; Elvis, Martin; Brickhouse, Nancy] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Binette, Luc] Univ Laval, Dept Phys Genie Phys & Opt, Quebec City, PQ G1K 7P4, Canada. [Mathur, Smita] Ohio State Univ, Columbus, OH 43210 USA. RP Krongold, Y (reprint author), Univ Nacl Autonoma Mexico, Inst Astron, Apartado Postal 70-264, Mexico City 04510, DF, Mexico. OI Nicastro, Fabrizio/0000-0002-6896-1364; Brickhouse, Nancy/0000-0002-8704-4473 FU UNAM PAPIIT [IN118905]; CONACyT [J-49594]; Spanish MEC [AYA2001-3939-C03-02]; ESA FX We thank the referee for constructive comments that helped to improve the paper. This research is based on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. This work was supported by the UNAM PAPIIT grant IN118905 and the CONACyT grant J-49594. E.J.B. and M.S.Ll. have been supported by Spanish MEC under grant AYA2001-3939-C03-02. Y.K. and E.J.B. acknowledge support by the ESA faculty program. NR 47 TC 17 Z9 17 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JAN 1 PY 2009 VL 690 IS 1 BP 773 EP 782 DI 10.1088/0004-637X/690/1/773 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 398IU UT WOS:000262726600061 ER PT J AU Knutson, HA Charbonneau, D Cowan, NB Fortney, JJ Showman, AP Agol, E Henry, GW Everett, ME Allen, LE AF Knutson, Heather A. Charbonneau, David Cowan, Nicolas B. Fortney, Jonathan J. Showman, Adam P. Agol, Eric Henry, Gregory W. Everett, Mark E. Allen, Lori E. TI MULTIWAVELENGTH CONSTRAINTS ON THE DAY-NIGHT CIRCULATION PATTERNS OF HD 189733b SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: eclipsing; infrared: stars; planetary systems; stars: individual (HD 189733); techniques: photometric ID EXTRASOLAR GIANT PLANETS; SPITZER-SPACE-TELESCOPE; LIGHT-CURVE PROJECT; HOT JUPITERS; ATMOSPHERIC CIRCULATION; TRANSMISSION SPECTRUM; TRANSITING PLANETS; THERMAL EMISSION; HD-189733 SYSTEM; ROTATION PERIOD AB We present new Spitzer observations of the phase variation of the hot Jupiter HD 189733b in the MIPS 24 mu m bandpass, spanning the same part of the planet's orbit as our previous observations in the IRAC 8 mu m bandpass (Knutson et al. 2007). We find that the minimum hemisphere-averaged flux from the planet in this bandpass is 76% +/- 3% of the maximum flux; this corresponds to minimum and maximum hemisphere-averaged brightness temperatures of 984 +/- 48 K and 1220 +/- 47 K, respectively. The planet reaches its maximum flux at an orbital phase of 0.396 +/- 0.022, corresponding to a hot region shifted 20 degrees-30 degrees east of the substellar point. Because tidally locked hot Jupiters would have enormous day-night temperature differences in the absence of winds, the small amplitude of the observed phase variation indicates that the planet's atmosphere efficiently transports thermal energy from the day side to the night side at the 24 mu m photosphere, leading to modest day-night temperature differences. The similarities between the 8 and 24 mu m phase curves for HD 189733b lead us to conclude that the circulation on this planet behaves in a fundamentally similar fashion across the range of pressures sensed by these two wavelengths. One-dimensional radiative transfer models indicate that the 8 mu m band should probe pressures 2-3 times greater than at 24 mu m, although the uncertain methane abundance complicates the interpretation. If these two bandpasses do probe different pressures, it would indicate that the temperature varies only weakly between the two sensed depths, and hence that the atmosphere is not convective at these altitudes. We also present an analysis of the possible contribution of star spots to the time series at both 8 and 24 mu m based on near-simultaneous ground-based observations and additional Spitzer observations. Accounting for the effects of these spots results in a slightly warmer night-side temperature for the planet in both bandpasses, but does not otherwise affect our conclusions. C1 [Knutson, Heather A.; Charbonneau, David; Allen, Lori E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Cowan, Nicolas B.; Agol, Eric] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Fortney, Jonathan J.] Univ Calif Santa Cruz, UCO Lick Observ, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Showman, Adam P.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Showman, Adam P.] Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA. [Henry, Gregory W.] Tennessee State Univ, Ctr Excellence Informat Syst, Nashville, TN 37209 USA. [Everett, Mark E.] Inst Plant Sci, Tucson, AZ 85719 USA. RP Knutson, HA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM hknutson@cfa.harvard.edu RI Agol, Eric/B-8775-2013; OI Agol, Eric/0000-0002-0802-9145; Fortney, Jonathan/0000-0002-9843-4354; Charbonneau, David/0000-0002-9003-484X FU Kepler mission under Cooperative Agreement [NCC2-1390]; Jet Propulsion Laboratory/California Institute of Technology; National Science Foundation FX We thank David Latham, Matthew Holman, Joshua Winn, Gilbert Esquerdo, Jose Fernandez, Gaspar Bakos, and Cesar Fuentes for their assistance in obtaining observations of HD 189733 with the FLWO 1.2 m telescope, and for sharing time on their previously scheduled nights to obtain these observations. We thank Mark Marley for helpful discussions, and the referee for a thoughtful and detailed review. This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract to NASA. We also utilize observations made with KeplerCam, which was developed with partial support from the Kepler mission under Cooperative Agreement NCC2-1390. Support for this work was provided by NASA through an award issued by Jet Propulsion Laboratory/California Institute of Technology. H.A.K. was supported by a National Science Foundation Graduate Research Fellowship. NR 74 TC 139 Z9 140 U1 1 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 1 PY 2009 VL 690 IS 1 BP 822 EP 836 DI 10.1088/0004-637X/690/1/822 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 398IU UT WOS:000262726600065 ER PT J AU Brown, WR Geller, MJ Kenyon, SJ Bromley, BC AF Brown, Warren R. Geller, Margaret J. Kenyon, Scott J. Bromley, Benjamin C. TI THE ANISOTROPIC SPATIAL DISTRIBUTION OF HYPERVELOCITY STARS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE Galaxy: center; Galaxy: halo; Galaxy: kinematics and dynamics; Galaxy: stellar content ID SUPERMASSIVE BLACK-HOLE; GALACTIC-CENTER; RUNAWAY STARS; SDSS J090745.0+024507; INITIAL BINARIES; O-STAR; B-STAR; VELOCITY; MASS; EJECTION AB We study the distribution of angular positions and angular separations of unbound hypervelocity stars (HVSs). HVSs are spatially anisotropic at the 3 sigma level. The spatial anisotropy is significant in Galactic longitude, not in latitude, and the inclusion of lower velocity, possibly bound HVSs reduces the significance of the anisotropy. We discuss how the observed distribution of HVSs may be linked to their origin. In the future, measuring the distribution of HVSs in the southern sky will provide additional constraints on the spatial anisotropy and the origin of HVSs. C1 [Brown, Warren R.; Geller, Margaret J.; Kenyon, Scott J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Bromley, Benjamin C.] Univ Utah, Dept Phys, Salt Lake City, UT 84112 USA. RP Brown, WR (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM wbrown@cfa.harvard.edu; mgeller@cfa.harvard.edu; skenyon@cfa.harvard.edu; bromley@physics.utah.edu OI Kenyon, Scott/0000-0003-0214-609X FU Smithsonian Institution FX This work is based on observations obtained at the MMT Observatory, a joint facility of the Smithsonian Institution and the University of Arizona. This research makes use of NASA's Astrophysics Data System Bibliographic Services. We thank the anonymous referee and Oleg Gnedin for helpful comments. This work was supported by the Smithsonian Institution. NR 45 TC 31 Z9 31 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JAN 1 PY 2009 VL 690 IS 1 BP L69 EP L71 DI 10.1088/0004-637X/690/1/L69 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 398RB UT WOS:000262748100017 ER PT J AU Gordon, KD Bot, C Muller, E Misselt, KA Bolatto, A Bernard, JP Reach, W Engelbracht, CW Babler, B Bracker, S Block, M Clayton, GC Hora, J Indebetouw, R Israel, FP Li, A Madden, S Meade, M Meixner, M Sewilo, M Shiao, B Smith, LJ van Loon, JT Whitney, BA AF Gordon, K. D. Bot, C. Muller, E. Misselt, K. A. Bolatto, A. Bernard, J. -P. Reach, W. Engelbracht, C. W. Babler, B. Bracker, S. Block, M. Clayton, G. C. Hora, J. Indebetouw, R. Israel, F. P. Li, A. Madden, S. Meade, M. Meixner, M. Sewilo, M. Shiao, B. Smith, L. J. van Loon, J. Th. Whitney, B. A. TI THE DUST-TO-GAS RATIO IN THE SMALL MAGELLANIC CLOUD TAIL SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE dust, extinction; galaxies: individual (SMC); galaxies: ISM ID MULTIBAND IMAGING PHOTOMETER; SPITZER-SPACE-TELESCOPE; GALAXY EVOLUTION SAGE; CHEMICAL-COMPOSITION; MOLECULAR CLOUDS; STAR-FORMATION; MILKY-WAY; BRIDGE; EMISSION; METALLICITY AB The Tail region of the Small Magellanic Cloud (SMC) was imaged using the MIPS instrument on the Spitzer Space Telescope as part of the SAGE-SMC Spitzer Legacy. Diffuse infrared emission from dust was detected in all the MIPS bands. The Tail gas-to-dust ratio was measured to be 1200 +/- 350 using the MIPS observations combined with existing IRAS and H I observations. This gas-to-dust ratio is higher than the expected 500-800 from the known Tail metallicity indicating possible destruction of dust grains. Two cluster regions in the Tail were resolved into multiple sources in the MIPS observations and local gas-to-dust ratios were measured to be similar to 440 and similar to 250 suggest dust formation and/or significant amounts of ionized gas in these regions. These results support the interpretation that the SMC Tail is a tidal Tail recently stripped from the SMC that includes gas, dust, and young stars. C1 [Gordon, K. D.; Meixner, M.; Sewilo, M.; Shiao, B.; Smith, L. J.] STScI, Baltimore, MD 21218 USA. [Whitney, B. A.] Space Sci Inst, Boulder, CO 80301 USA. [van Loon, J. Th.] Keele Univ, Lennard Jones Lab, Astrophys Grp, Keele ST5 5BG, Staffs, England. [Smith, L. J.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Madden, S.] CEA Saclay, Serv Astrophys, F-91191 Gif Sur Yvette, France. [Li, A.] Univ Missouri, Dept Phys & Astron, Columbia, MO 65211 USA. [Israel, F. P.] Leiden Univ, Sterrewacht Leiden, NL-2300 RA Leiden, Netherlands. [Indebetouw, R.] Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA. [Hora, J.] Harvard Smithsonian, CfA, Cambridge, MA 02138 USA. [Clayton, G. C.] Louisiana State Univ, Dept Phys & Astron, Baton Rouge, LA 70803 USA. [Babler, B.; Bracker, S.; Meade, M.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Reach, W.] CALTECH, IPAC, Pasadena, CA 91125 USA. [Bernard, J. -P.] CESR, F-31028 Toulouse, France. [Bolatto, A.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Misselt, K. A.; Engelbracht, C. W.; Block, M.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Muller, E.] Nagoya Univ, Dept Astrophys, Chikusa Ku, Nagoya, Aichi 4648602, Japan. [Bot, C.] Univ Strasbourg, Ctr Donnees Astron Strasbourg CDS, UMR 7550, F-67000 Strasbourg, France. RP Gordon, KD (reprint author), STScI, 3700 San Martin Dr, Baltimore, MD 21218 USA. EM kgordon@stsci.edu; bot@astro.u-strasbg.fr; erik.muller@csiro.au; misselt@as.arizona.edu; bolatto@astro.umd.edu; jean-philippe.bernard@cesr.fr; reach@ipac.caltech.edu; cengelbracht@as.arizona.edu; brian@sal.wisc.edu; s_bracker@hotmail.com; mblock@as.arizona.edu; gclayton@fenway.phys.lsu.edu; jhora@cfa.harvard.edu; remy@virginia.edu; israel@strw.leidenuniv.nl; lia@missouri.edu; suzanne.madden@cea.fr; meade@astro.wisc.edu; meixner@stsci.edu; mmsewilo@stsci.edu; shiao@stsci.edu; lsmith@stsci.edu; jacco@astro.keele.ac.uk; bwhitney@spacescience.org OI Bot, Caroline/0000-0001-6118-2985; Reach, William/0000-0001-8362-4094 FU NASA FX This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under NASA contract 1407. Support for this work was provided by NASA NR 41 TC 27 Z9 27 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JAN 1 PY 2009 VL 690 IS 1 BP L76 EP L80 DI 10.1088/0004-637X/690/1/L76 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 398RB UT WOS:000262748100019 ER PT J AU Liu, JF Bregman, JN McClintock, JE AF Liu, Jifeng Bregman, Joel N. McClintock, Jeffrey E. TI HUBBLE SPACE TELESCOPE MONITORING REVEALS A 6.1 DAY PERIOD FOR AN ULTRALUMINOUS X-RAY SOURCE IN NGC 1313 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: individual (NGC 1313); X-rays: binaries ID SOURCE NGC-1313 X-2; BLACK-HOLE; COUNTERPARTS; STELLAR; BINARY AB Ultraluminous X-ray sources (ULXs) in nearby galaxies have X-ray luminosities of 10(39)-10(41) erg s(-1), and are possibly intermediate mass black holes of 10(2)-10(5) M(circle dot). NGC 1313 X-2 is an extreme ULX with a maximum luminosity of 3 x 10(40) erg s(-1), and a frequent target of X-ray and optical observations. Here we report our Hubble Space Telescope Guest Observer (GO) program to monitor its optical counterpart in a search of its period. The 20 monitoring observations over three weeks exhibited periodic modulations at the 6 sigma level with a period of P = 6.12 +/- 0.16 days and an amplitude of A = 0.102 +/- 0.016 mag. The periodicity is understood as from the orbital motion of the gravitationally distorted secondary that is unevenly irradiated by the X-ray radiation from the primary accretion disk. This is the first photometric period ever discovered for a ULX counterpart. The periodicity rules out a radiation mechanism through relativistic beaming effects. Combined with the photometry, the periodicity suggests that the secondary is most likely a giant branch star with a mass of 11.3-21.0 M(circle dot) and a radius of 14.4-18.3R(circle dot). C1 [Liu, Jifeng; McClintock, Jeffrey E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bregman, Joel N.] Univ Michigan, Ann Arbor, MI 48109 USA. RP Liu, JF (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. FU NASA [HST-GO-11227]; Chandra Fellowship Program [PF6-70043] FX We thank Rosanne Di Stefano, Ramesh Narayan, Ryan Hichox, and Alison Farmer for helpful discussions. J.F.L. acknowledges the support for this work provided by NASA through grant HST-GO-11227 and the Chandra Fellowship Program, grant PF6-70043. NR 23 TC 19 Z9 19 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JAN 1 PY 2009 VL 690 IS 1 BP L39 EP L42 DI 10.1088/0004-637X/690/1/L39 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 398RB UT WOS:000262748100010 ER PT J AU Stutz, AM Bourke, TL Rieke, GH Bieging, JH Misselt, KA Myers, PC Shirley, YL AF Stutz, Amelia M. Bourke, Tyler L. Rieke, George H. Bieging, John H. Misselt, Karl A. Myers, Philip C. Shirley, Yancy L. TI SPITZER OBSERVATIONS OF L429: A NEAR-COLLAPSE OR COLLAPSING STARLESS CORE SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE dust, extinction; infrared: ISM; ISM: globules; ISM: individual (LDN 429) ID INTERSTELLAR DUST GRAINS; PRE-STELLAR CORES; IRAS 16293-2422; INITIAL CONDITIONS; MOLECULAR CLOUDS; INFALL MOTIONS; DARK CLOUDS; PIPE NEBULA; IRAS-16293-2422; EXTINCTION AB We present Spitzer infrared (IR) observations of the starless core L429. The IR images of this core show an absorption feature, caused by the dense core material, at wavelengths <= 70 mu m. The core has a steep density profile, and reaches A(V) > 35 mag near the center. We show that L429 is either collapsing or in a near-collapse state. C1 [Stutz, Amelia M.; Rieke, George H.; Bieging, John H.; Misselt, Karl A.; Shirley, Yancy L.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Bourke, Tyler L.; Myers, Philip C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Stutz, AM (reprint author), Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA. EM astutz@as.arizona.edu OI Stutz, Amelia/0000-0003-2300-8200 FU NASA; University of Arizona [1255094]; SAO [1279198, 1288806]; National Science Foundation [AST-0708131]; The University of Arizona FX We thank the referee for his/her helpful comments. Support for this work was provided through NASA contracts issued by Caltech/JPL to the University of Arizona (1255094) and to SAO (1279198 and 1288806). This work was also supported by the National Science Foundation grant AST-0708131 to The University of Arizona. NR 40 TC 4 Z9 4 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JAN 1 PY 2009 VL 690 IS 1 BP L35 EP L38 DI 10.1088/0004-637X/690/1/L35 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 398RB UT WOS:000262748100009 ER PT J AU Jordan, A Peng, EW Blakeslee, JP Cote, P Eyheramendy, S Ferrarese, L Mei, S Tonry, JL West, MJ AF Jordan, Andres Peng, Eric W. Blakeslee, John P. Cote, Patrick Eyheramendy, Susana Ferrarese, Laura Mei, Simona Tonry, John L. West, Michael J. TI THE ACS VIRGO CLUSTER SURVEY XVI. SELECTION PROCEDURE AND CATALOGS OF GLOBULAR CLUSTER CANDIDATES SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE catalogs; galaxies: elliptical and lenticular, cD; galaxies: star clusters; globular clusters: general; methods: statistical ID EARLY-TYPE GALAXIES; DATA REDUCTION PROCEDURES; HUBBLE-SPACE-TELESCOPE; X-RAY BINARIES; ADVANCED CAMERA; LUMINOSITY FUNCTION; STAR-CLUSTERS; DWARF GALAXIES; MASS; STELLAR AB We present catalogs of globular cluster candidates for the 100 galaxies of the Advanced Camera for Surveys Virgo Cluster Survey, a large program to carry out imaging of early-type members of the Virgo Cluster using the Advanced Camera for Surveys (ACS) on the Hubble Space Telescope. We describe the procedure used to select bona fide globular cluster candidates out of the full list of detections based on model-based clustering methods with the use of expected contamination catalogs constructed using blank field observations and which are customized for each galaxy. We also present the catalogs of expected contaminants for each of our target galaxies. For each detected source we measure its position, magnitudes in the F475W (approximate to Sloan g) and F850LP (approximate to Sloan z) bandpasses, and half-light radii by fitting point-spread function convolved King models to the observed light distribution. These measurements are presented for 20,375 sources, of which 12,763 are likely to be globular clusters. Finally, we detail the calculation of the aperture corrections adopted for the globular cluster photometry. C1 [Jordan, Andres] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Jordan, Andres] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 22, Chile. [Peng, Eric W.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Peng, Eric W.] Peking Univ, Dept Astron, Beijing 100871, Peoples R China. [Peng, Eric W.; Blakeslee, John P.; Cote, Patrick; Ferrarese, Laura] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Blakeslee, John P.] Washington State Univ, Dept Phys & Astron, Pullman, WA 99163 USA. [Eyheramendy, Susana] Pontificia Univ Catolica Chile, Dept Estadist, Santiago 22, Chile. [Mei, Simona] Observ Paris, GEPI, Sect Meudon, F-92195 Meudon, France. [Tonry, John L.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [West, Michael J.] ESO, Santiago, Chile. RP Jordan, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM ajordan@cfa.harvard.edu OI Jordan, Andres/0000-0002-5389-3944; Blakeslee, John/0000-0002-5213-3548 FU Space Telescope Science Institute [GO-9401]; Association of Universities for Research in Astronomy, Inc.; NASA [NAS5-26555, NAG5-11714]; National Research Council of Canada FX Support for program GO-9401 was provided through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. E. W. P. acknowledges the support of the National Research Council of Canada's Plaskett Research Fellowship at the Herzberg Institute of Astrophysics. P. C. acknowledges additional support provided by NASA LTSA grant NAG5-11714. NR 38 TC 81 Z9 82 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD JAN PY 2009 VL 180 IS 1 BP 54 EP 66 DI 10.1088/0067-0049/180/1/54 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 400IX UT WOS:000262862400004 ER PT J AU Laird, ES Nandra, K Georgakakis, A Aird, JA Barmby, P Conselice, CJ Coil, AL Davis, M Faber, SM Fazio, GG Guhathakurta, P Koo, DC Sarajedini, V Willmer, CNA AF Laird, E. S. Nandra, K. Georgakakis, A. Aird, J. A. Barmby, P. Conselice, C. J. Coil, A. L. Davis, M. Faber, S. M. Fazio, G. G. Guhathakurta, P. Koo, D. C. Sarajedini, V. Willmer, C. N. A. TI AEGIS-X: THE CHANDRA DEEP SURVEY OF THE EXTENDED GROTH STRIP SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE galaxies: active; galaxies: nuclei; surveys; X-rays: galaxies ID FIELD-NORTH SURVEY; RAY SOURCES; OPTICAL-IDENTIFICATION; MIDINFRARED PROPERTIES; CONFIDENCE-LIMITS; SOURCE CATALOG; LOCKMAN-HOLE; GALAXIES; EMISSION; XBOOTES AB We present the AEGIS-X survey, a series of deep Chandra ACIS-I observations of the Extended Groth Strip. The survey comprises pointings at eight separate positions, each with nominal exposure of 200 ks, covering a total area of approximately 0.67 deg(2) in a strip of length 2 degrees. We describe in detail an updated version of our data reduction and point-source-detection algorithms used to analyze these data. A total of 1325 band-merged sources have been found to a Poisson probability limit of 4 x 10(-6), with limiting fluxes of 5.3 x 10(-17) erg cm(2) s(-1) in the soft (0.5-2 keV) band and 3.8 x 10(-16) erg cm(-2) s(-1) in the hard (2-10 keV) band. We present simulations verifying the validity of our source-detection procedure and showing a very small, < 1.5%, contamination rate from spurious sources. Optical/NIR counterparts have been identified from the DEEP2, CFHTLS, and Spitzer/Infrared Array Camera (IRAC) surveys of the same region. Using a likelihood ratio method, we find optical counterparts for 76% of our sources, complete to R(AB) = 24.1, and, of the 66% of the sources that have IRAC coverage, 94% have a counterpart to a limit of 0.9 mu Jy at 3.6 mu m (m(AB) = 23.8). After accounting for (small) positional offsets in the eight Chandra fields, the astrometric accuracy of Chandra positions is found to be 0".8 rms; however, this number depends both on the off-axis angle and the number of detected counts for a given source. All data products described in this paper are made available via a public Web site. C1 [Laird, E. S.; Nandra, K.; Georgakakis, A.; Aird, J. A.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England. [Barmby, P.] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada. [Conselice, C. J.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. [Coil, A. L.; Willmer, C. N. A.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Davis, M.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Faber, S. M.; Guhathakurta, P.; Koo, D. C.] Univ Calif Santa Cruz, Lick Observ, UCO, Santa Cruz, CA 95064 USA. [Fazio, G. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Sarajedini, V.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. RP Laird, ES (reprint author), Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, Prince Consort Rd, London SW7 2AZ, England. EM e.laird@imperial.ac.uk RI Conselice, Christopher/B-4348-2013; Georgakakis, Antonis/K-4457-2013; Barmby, Pauline/I-7194-2016; OI Georgakakis, Antonis/0000-0002-3514-2442; Barmby, Pauline/0000-0003-2767-0090; Conselice, Christopher/0000-0003-1949-7638 FU Leverhulme trust; PPARC/STFC; Chandra grant [GO56141A]; [MEIF-CT-2005-025108] FX We thank the referee for helpful comments that improved the clarity of the paper. We thank those who have built and operate the Chandra X-ray observatory so successfully. We acknowledge financial support from the Leverhulme trust (K.N.), PPARC/STFC (E.S.L., J.A.A.), Marie-Curie fellowship grant MEIF-CT-2005-025108 (A. G.), and Chandra grant GO56141A (D. C. K.). NR 46 TC 125 Z9 125 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD JAN PY 2009 VL 180 IS 1 BP 102 EP 116 DI 10.1088/0067-0049/180/1/102 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 400IX UT WOS:000262862400007 ER PT S AU Lada, CJ AF Lada, Charles J. BE Thronson, HA Stiavelli, M Tielens, AGGM TI The Unsolved Problem of Star Formation: Dusty Dense Cores and the Origin of Stellar Masses SO ASTROPHYSICS IN THE NEXT DECADE SE Astrophysics and Space Science Proceedings LA English DT Proceedings Paper CT Conference on Astrophysics in the Next Decade CY SEP 24-27, 2007 CL Tucson, AZ SP Space Telescope Sci Inst, JWST Project, Johns Hopkins Univ, NASA Goddard Space Flight Ctr Flight Programs ID MOLECULAR CLOUDS; PIPE NEBULA; POPULATION; EXTINCTION; LUMINOSITY; BARNARD-68; PRESSURE; CLUSTERS; EMISSION; PERSEUS AB The development of a predictive theory of star formation is one of the prime goals of modern astrophysics. The problem of star formation is a very complex one and its solution depends critically on empirical data. In this contribution, I review some of the progress that has been achieved in identifying and measuring the fundamental boundary and initial conditions that constrain the solution and must be met by any complete theory of star formation. In particular, I discuss what is known about the stellar IMF and the nature of dense cores on the verge of star formation. I then discuss how these two topics contribute to our general understanding of the origin of stellar mass, the key mystery in the star formation process. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Lada, CJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM clada@cfa.harvard.edu NR 27 TC 2 Z9 2 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 1570-6591 BN 978-1-4020-9456-9 J9 ASTROPHYSICS SPACE PY 2009 BP 147 EP 166 DI 10.1007/978-1-4020-9457-6_6 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BJC00 UT WOS:000264638300006 ER PT J AU Dupuy, E Walker, KA Kar, J Boone, CD McElroy, CT Bernath, PF Drummond, JR Skelton, R McLeod, SD Hughes, RC Nowlan, CR Dufour, DG Zou, J Nichitiu, F Strong, K Baron, P Bevilacqua, RM Blumenstock, T Bodeker, GE Borsdorff, T Bourassa, AE Bovensmann, H Boyd, IS Bracher, A Brogniez, C Burrows, JP Catoire, V Ceccherini, S Chabrillat, S Christensen, T Coffey, MT Cortesi, U Davies, J De Clercq, C Degenstein, DA De Maziere, M Demoulin, P Dodion, J Firanski, B Fischer, H Forbes, G Froidevaux, L Fussen, D Gerard, P Godin-Beekmann, S Goutail, F Granville, J Griffith, D Haley, CS Hannigan, JW Hopfner, M Jin, JJ Jones, A Jones, NB Jucks, K Kagawa, A Kasai, Y Kerzenmacher, TE Kleinbohl, A Klekociuk, AR Kramer, I Kullmann, H Kuttippurath, J Kyrola, E Lambert, JC Livesey, NJ Llewellyn, EJ Lloyd, ND Mahieu, E Manney, GL Marshall, BT McConnell, JC McCormick, MP McDermid, IS McHugh, M McLinden, CA Mellqvist, J Mizutani, K Murayama, Y Murtagh, DP Oelhaf, H Parrish, A Petelina, SV Piccolo, C Pommereau, JP Randall, CE Robert, C Roth, C Schneider, M Senten, C Steck, T Strandberg, A Strawbridge, KB Sussmann, R Swart, DPJ Tarasick, DW Taylor, JR Tetard, C Thomason, LW Thompson, AM Tully, MB Urban, J Vanhellemont, F Vigouroux, C von Clarmann, T von der Gathen, P von Savigny, C Waters, JW Witte, JC Wolff, M Zawodny, JM AF Dupuy, E. Walker, K. A. Kar, J. Boone, C. D. McElroy, C. T. Bernath, P. F. Drummond, J. R. Skelton, R. McLeod, S. D. Hughes, R. C. Nowlan, C. R. Dufour, D. G. Zou, J. Nichitiu, F. Strong, K. Baron, P. Bevilacqua, R. M. Blumenstock, T. Bodeker, G. E. Borsdorff, T. Bourassa, A. E. Bovensmann, H. Boyd, I. S. Bracher, A. Brogniez, C. Burrows, J. P. Catoire, V. Ceccherini, S. Chabrillat, S. Christensen, T. Coffey, M. T. Cortesi, U. Davies, J. De Clercq, C. Degenstein, D. A. Maziere, M. De Demoulin, P. Dodion, J. Firanski, B. Fischer, H. Forbes, G. Froidevaux, L. Fussen, D. Gerard, P. Godin-Beekmann, S. Goutail, F. Granville, J. Griffith, D. Haley, C. S. Hannigan, J. W. Hoepfner, M. Jin, J. J. Jones, A. Jones, N. B. Jucks, K. Kagawa, A. Kasai, Y. Kerzenmacher, T. E. Kleinboehl, A. Klekociuk, A. R. Kramer, I. Kuellmann, H. Kuttippurath, J. Kyroelae, E. Lambert, J. -C. Livesey, N. J. Llewellyn, E. J. Lloyd, N. D. Mahieu, E. Manney, G. L. Marshall, B. T. McConnell, J. C. McCormick, M. P. McDermid, I. S. McHugh, M. McLinden, C. A. Mellqvist, J. Mizutani, K. Murayama, Y. Murtagh, D. P. Oelhaf, H. Parrish, A. Petelina, S. V. Piccolo, C. Pommereau, J. -P. Randall, C. E. Robert, C. Roth, C. Schneider, M. Senten, C. Steck, T. Strandberg, A. Strawbridge, K. B. Sussmann, R. Swart, D. P. J. Tarasick, D. W. Taylor, J. R. Tetard, C. Thomason, L. W. Thompson, A. M. Tully, M. B. Urban, J. Vanhellemont, F. Vigouroux, C. von Clarmann, T. von der Gathen, P. von Savigny, C. Waters, J. W. Witte, J. C. Wolff, M. Zawodny, J. M. TI Validation of ozone measurements from the Atmospheric Chemistry Experiment (ACE) SO ATMOSPHERIC CHEMISTRY AND PHYSICS LA English DT Review ID MICROWAVE LIMB SOUNDER; GROUND-BASED FTIR; HALOGEN OCCULTATION EXPERIMENT; STRATOSPHERIC OZONE; TECHNICAL NOTE; ERROR ANALYSIS; POAM-III; SAGE-II; VERTICAL-DISTRIBUTION; OBSERVING SYSTEM AB This paper presents extensive bias determination analyses of ozone observations from the Atmospheric Chemistry Experiment (ACE) satellite instruments: the ACE Fourier Transform Spectrometer (ACE-FTS) and the Measurement of Aerosol Extinction in the Stratosphere and Troposphere Retrieved by Occultation (ACE-MAESTRO) instrument. Here we compare the latest ozone data products from ACE-FTS and ACE-MAESTRO with coincident observations from nearly 20 satellite-borne, airborne, balloon-borne and ground-based instruments, by analysing volume mixing ratio profiles and partial column densities. The ACE-FTS version 2.2 Ozone Update product reports more ozone than most correlative measurements from the upper troposphere to the lower mesosphere. At altitude levels from 16 to 44 km, the average values of the mean relative differences are nearly all within +1 to +8%. At higher altitudes (45 60 km), the ACE-FTS ozone amounts are significantly larger than those of the comparison instruments, with mean relative differences of up to +40% (about + 20% on average). For the ACE-MAESTRO version 1.2 ozone data product, mean relative differences are within +/- 10% (average values within +/- 6%) between 18 and 40 km for both the sunrise and sunset measurements. At higher altitudes (similar to 35-55 km), systematic biases of opposite sign are found between the ACE-MAESTRO sunrise and sunset observations. While ozone amounts derived from the ACE-MAESTRO sunrise occultation data are often smaller than the coincident observations (with mean relative differences down to -10%), the sunset occultation profiles for ACE-MAESTRO show results that are qualitatively similar to ACE-FTS, indicating a large positive bias (mean relative differences within +10 to +30%) in the 45-55 km altitude range. In contrast, there is no significant systematic difference in bias found for the ACE-FTS sunrise and sunset measurements. C1 [Dupuy, E.; Walker, K. A.; Boone, C. D.; Bernath, P. F.; Skelton, R.; McLeod, S. D.; Hughes, R. C.] Univ Waterloo, Dept Chem, Waterloo, ON N2L 3G1, Canada. [Walker, K. A.; Kar, J.; McElroy, C. T.; Drummond, J. R.; Nowlan, C. R.; Zou, J.; Nichitiu, F.; Strong, K.; Kerzenmacher, T. E.; Taylor, J. R.; Wolff, M.] Univ Toronto, Dept Phys, Toronto, ON, Canada. [McElroy, C. T.; Davies, J.; McLinden, C. A.; Tarasick, D. W.] Environm Canada, Downsview, ON, Canada. [Bernath, P. F.] Univ York, Dept Chem, York YO10 5DD, N Yorkshire, England. [Drummond, J. R.] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS, Canada. [Dufour, D. G.] Picomole Instruments Inc, Edmonton, AB, Canada. [Baron, P.; Kagawa, A.; Kasai, Y.; Mizutani, K.; Murayama, Y.] Natl Inst Informat & Commun Technol NICT, Koganei, Tokyo, Japan. [Bevilacqua, R. M.] USN, Res Lab, Washington, DC 20375 USA. [Blumenstock, T.; Fischer, H.; Hoepfner, M.; Kramer, I.; Oelhaf, H.; Schneider, M.; Steck, T.; von Clarmann, T.] Forschungszentrum Karlsruhe, Inst Meteorol & Klimaforsch, D-76021 Karlsruhe, Germany. [Blumenstock, T.; Fischer, H.; Hoepfner, M.; Kramer, I.; Oelhaf, H.; Schneider, M.; Steck, T.; von Clarmann, T.] Univ Karlsruhe, Karlsruhe, Germany. [Bodeker, G. E.] Natl Inst Water & Atmospher Res, Lauder, New Zealand. [Borsdorff, T.; Sussmann, R.] Forschungszentrum Karlsruhe, Inst Meteorol & Klimaforsch Atmosphar Umweltforsc, Garmisch Partenkirchen, Germany. [Bourassa, A. E.; Degenstein, D. A.; Llewellyn, E. J.; Lloyd, N. D.; Petelina, S. V.; Roth, C.] Univ Saskatchewan, Inst Space & Atmospher Studies, Saskatoon, SK S7N 0W0, Canada. [Bovensmann, H.; Bracher, A.; Burrows, J. P.; Kleinboehl, A.; Kuellmann, H.; Kuttippurath, J.; von Savigny, C.] Univ Bremen, IUP, Bremen, Germany. [Boyd, I. S.] Univ Massachusetts, NIWA Environm Res Inst, Amherst, MA 01003 USA. [Brogniez, C.; Tetard, C.] Univ Lille 1, Opt Atmospher Lab, CNRS, F-59655 Villeneuve Dascq, France. [Catoire, V.; Robert, C.] Univ Orleans, CNRS, Lab Phys & Chim Environm, Orleans, France. [Ceccherini, S.; Cortesi, U.] CNR, Inst Fis Applicata N Carrara IFAC, Sesto Fiorentino, Italy. [Chabrillat, S.; De Clercq, C.; Maziere, M. De; Dodion, J.; Fussen, D.; Gerard, P.; Granville, J.; Lambert, J. -C.; Senten, C.; Vanhellemont, F.; Vigouroux, C.] Inst Aeron Spatiale Belgique BIRA IASB, Brussels, Belgium. [Christensen, T.] Danish Meteorol Inst, Danish Climate Ctr, Copenhagen, Denmark. [Coffey, M. T.; Hannigan, J. W.] Natl Ctr Atmospher Res, Earth & Sun Syst Lab, Boulder, CO 80307 USA. [Demoulin, P.; Mahieu, E.] Univ Liege, Inst Astrophys & Geophys, Liege, Belgium. [Firanski, B.; Strawbridge, K. B.] Environm Canada, Ctr Atmospher Res Expt, Sci & Technol Branch, Egbert, ON, Canada. [Forbes, G.] Environm Canada Sable Isl, Dartmouth, NS, Canada. [Froidevaux, L.; Kleinboehl, A.; Livesey, N. J.; Manney, G. L.; Waters, J. W.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Godin-Beekmann, S.; Kuttippurath, J.] Univ Paris 06, CNRS, Serv Aeron, Paris, France. [Goutail, F.; Pommereau, J. -P.] CNRS, Serv Aeron, F-91371 Verrieres Le Buisson, France. [Griffith, D.; Jones, N. B.] Univ Wollongong, Sch Chem, Wollongong, NSW, Australia. [Haley, C. S.] York Univ, Ctr Res Earth & Space Sci, Toronto, ON M3J 2R7, Canada. [Jin, J. J.] York Univ, Dept Earth & Space Sci & Engn, Toronto, ON M3J 2R7, Canada. [Jones, A.; Mellqvist, J.; Murtagh, D. P.; Strandberg, A.; Urban, J.] Chalmers, Dept Radio & Space Sci, S-41296 Gothenburg, Sweden. [Jucks, K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kagawa, A.] Fujitsu FIP Corp, Tokyo, Japan. [Klekociuk, A. R.] Australian Antarctic Div, Ice Ocean Atmosphere & Climate IOAC Program, Kingston, Australia. [Kyroelae, E.] Finnish Meteorol Inst, Earth Observat, FIN-00101 Helsinki, Finland. [Manney, G. L.] New Mexico Inst Min & Technol, Socorro, NM 87801 USA. [Marshall, B. T.; McHugh, M.] GATS Inc, Newport News, VA USA. [McCormick, M. P.; Thomason, L. W.; Zawodny, J. M.] NASA, Langley Res Ctr, Div Atmospher Sci, Hampton, VA 23665 USA. [McDermid, I. S.] Table Mt Facil, Jet Prop Lab, Wrightwood, CA USA. [Parrish, A.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Petelina, S. V.] La Trobe Univ, Dept Phys, Bundoora, Vic 3086, Australia. [Piccolo, C.] Univ Oxford, Oxford OX1 2JD, England. [Randall, C. E.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA. [Swart, D. P. J.] Natl Inst Publ Hlth & Environm RIVM, Bilthoven, Netherlands. [Thompson, A. M.] Penn State Univ, Dept Meteorol, University Pk, PA 16802 USA. [Tully, M. B.] Bur Meteorol, Atmosphere Watch Sect, Melbourne, Vic, Australia. [von der Gathen, P.] Alfred Wegener Inst Polar & Marine Res, Res Unit Potsdam, Potsdam, Germany. [Witte, J. C.] Sci Syst & Applicat Inc, Lanham, MD USA. [Witte, J. C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Dupuy, E (reprint author), Univ Waterloo, Dept Chem, Waterloo, ON N2L 3G1, Canada. RI Urban, Jo/F-9172-2010; McLinden, Chris/A-7710-2010; von der Gathen, Peter/B-8515-2009; Bernath, Peter/B-6567-2012; Bodeker, Greg/A-8870-2008; Blumenstock, Thomas/K-2263-2012; Sussmann, Ralf/K-3999-2012; Hopfner, Michael/A-7255-2013; Oelhaf, Hermann/A-7895-2013; von Clarmann, Thomas/A-7287-2013; Strong, Kimberly/D-2563-2012; Jin, Jianjun/G-8357-2012; Burrows, John/B-6199-2014; Thompson, Anne /C-3649-2014; Bracher, Astrid/B-7805-2013; Schneider, Matthias/B-1441-2013; von Savigny, Christian/B-3910-2014; Kyrola, Erkki/E-1835-2014; Garmisch-Pa, Ifu/H-9902-2014; Drummond, James/O-7467-2014; Catoire, Valery/E-9662-2015; Jones, Nicholas/G-5575-2011; Murtagh, Donal/F-8694-2011; Randall, Cora/L-8760-2014; Bovensmann, Heinrich/P-4135-2016; Klekociuk, Andrew/A-4498-2015; Cortesi, Ugo/D-2704-2012 OI Urban, Jo/0000-0001-7026-793X; McLinden, Chris/0000-0001-5054-1380; von der Gathen, Peter/0000-0001-7409-1556; Bernath, Peter/0000-0002-1255-396X; Bodeker, Greg/0000-0003-1094-5852; Hopfner, Michael/0000-0002-4174-9531; von Clarmann, Thomas/0000-0003-2219-3379; Burrows, John/0000-0002-6821-5580; Thompson, Anne /0000-0002-7829-0920; Thomason, Larry/0000-0002-1902-0840; Murayama, Yasuhiro/0000-0003-1129-334X; Mahieu, Emmanuel/0000-0002-5251-0286; Tarasick, David/0000-0001-9869-0692; Mellqvist, Johan/0000-0002-6578-9220; Bracher, Astrid/0000-0003-3025-5517; Catoire, Valery/0000-0001-8126-3096; Jones, Nicholas/0000-0002-0111-2368; Murtagh, Donal/0000-0003-1539-3559; Randall, Cora/0000-0002-4313-4397; Bovensmann, Heinrich/0000-0001-8882-4108; Klekociuk, Andrew/0000-0003-3335-0034; Cortesi, Ugo/0000-0002-2827-5239 FU NSERC; CSA; CFCAS; ABB Bomem; Ontario Research and Development Challenge Fund; Premier's Excellence Research Award; University of Toronto; NASA [NNG05GN46G] FX Work at the Toronto Atmospheric Observatory was supported by NSERC, CSA, CFCAS, ABB Bomem, the Ontario Research and Development Challenge Fund, the Premier's Excellence Research Award and the University of Toronto.; Thanks to B. Bojkov of the Aura Validation Data Center (AVDC) and the Aura-MLS Data Distribution Team for access to the Aura-MLS dataset (see http://avdc.gsfc.nasa.gov). Work at the Jet Propulsion Laboratory (JPL), California Institute of Technology (CalTech), is carried out under a contract with NASA. Work at the University of Massachusetts is supported by NASA under award No. NNG05GN46G. NR 152 TC 63 Z9 63 U1 3 U2 27 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 2009 VL 9 IS 2 BP 287 EP 343 PG 57 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 406WN UT WOS:000263325700001 ER PT J AU Croft, B Lohmann, U Martin, RV Stier, P Wurzler, S Feichter, J Posselt, R Ferrachat, S AF Croft, B. Lohmann, U. Martin, R. V. Stier, P. Wurzler, S. Feichter, J. Posselt, R. Ferrachat, S. TI Aerosol size-dependent below-cloud scavenging by rain and snow in the ECHAM5-HAM SO ATMOSPHERIC CHEMISTRY AND PHYSICS LA English DT Article ID CLIMATE MODEL ECHAM5-HAM; MICROWAVE IMAGER SSM/I; COLLISION EFFICIENCY; TERMINAL VELOCITY; ELECTRIC CHARGES; LIQUID WATER; PARTICLES; DROPS; PARAMETERIZATION; ATMOSPHERE AB Wet deposition processes are highly efficient in the removal of aerosols from the atmosphere, and thus strongly influence global aerosol concentrations, and clouds, and their respective radiative forcings. In this study, physically detailed size-dependent below-cloud scavenging parameterizations for rain and snow are implemented in the ECHAM5-HAM global aerosol-climate model. Previously, below-cloud scavenging by rain in the ECHAM5-HAM was simply a function of the aerosol mode, and then scaled by the rainfall rate. The below-cloud scavenging by snow was a function of the snowfall rate alone. The global mean aerosol optical depth, and sea salt burden are sensitive to the below-cloud scavenging coefficients, with reductions near to 15% when the more vigorous size-dependent below-cloud scavenging by rain and snow is implemented. The inclusion of a prognostic rain scheme significantly reduces the fractional importance of below-cloud scavenging since there is higher evaporation in the lower troposphere, increasing the global mean sea salt burden by almost 15%. Thermophoretic effects are shown to produce increases in the global and annual mean number removal of Aitken size particles of near to 10%, but very small increases (near 1%) in the global mean below-cloud mass scavenging of carbonaceous and sulfate aerosols. Changes in the assumptions about the below-cloud scavenging by rain of particles with radius smaller than 10 nm do not cause any significant changes to the global and annual mean aerosol mass or number burdens, despite a change in the below-cloud number removal rate for nucleation mode particles by near to five-fold. Annual and zonal mean nucleation mode number concentrations are enhanced by up to 30% in the lower troposphere with the more vigourous size-dependent below-cloud scavenging. Closer agreement with different observations is found when the more physically detailed below-cloud scavenging parameterization is employed in the ECHAM5-HAM model. C1 [Croft, B.; Martin, R. V.] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS, Canada. [Lohmann, U.; Ferrachat, S.] ETH, Inst Atmospher & Climate Sci, Zurich, Switzerland. [Martin, R. V.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA. [Stier, P.] Univ Oxford, Oxford, England. [Wurzler, S.] Landesamt Nat Umwelt & Verbraucherschutz NRW, Recklinghausen, Germany. [Feichter, J.] Max Planck Inst Meteorol, Hamburg, Germany. [Posselt, R.] Fed Off Meteorol & Climatol MeteoSwiss, Zurich, Switzerland. RP Croft, B (reprint author), Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS, Canada. EM croft@mathstat.dal.ca RI Lohmann, Ulrike/B-6153-2009; Stier, Philip/B-2258-2008; Martin, Randall/C-1205-2014 OI Lohmann, Ulrike/0000-0001-8885-3785; Stier, Philip/0000-0002-1191-0128; Martin, Randall/0000-0003-2632-8402 FU National Science and Engineering Research Council of Canada; Killam Trusts Foundation of Canada; ETH Zurich FX The authors thank Jan Kazil, Corinna Hoose, and two anonymous reviewers for their helpful comments and discussions. We are also grateful to the National Science and Engineering Research Council of Canada and Killam Trusts Foundation of Canada for financial support, and to ETH Zurich for computing time. NR 49 TC 53 Z9 53 U1 0 U2 16 PU COPERNICUS PUBLICATIONS PI KATHLENBURG-LINDAU PA MAX-PLANCK-STR 13, KATHLENBURG-LINDAU, 37191, GERMANY SN 1680-7316 J9 ATMOS CHEM PHYS JI Atmos. Chem. Phys. PY 2009 VL 9 IS 14 BP 4653 EP 4675 PG 23 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 477RF UT WOS:000268535500010 ER PT J AU Dunlea, EJ DeCarlo, PF Aiken, AC Kimmel, JR Peltier, RE Weber, RJ Tomlinson, J Collins, DR Shinozuka, Y McNaughton, CS Howell, SG Clarke, AD Emmons, LK Apel, EC Pfister, GG van Donkelaar, A Martin, RV Millet, DB Heald, CL Jimenez, JL AF Dunlea, E. J. DeCarlo, P. F. Aiken, A. C. Kimmel, J. R. Peltier, R. E. Weber, R. J. Tomlinson, J. Collins, D. R. Shinozuka, Y. McNaughton, C. S. Howell, S. G. Clarke, A. D. Emmons, L. K. Apel, E. C. Pfister, G. G. van Donkelaar, A. Martin, R. V. Millet, D. B. Heald, C. L. Jimenez, J. L. TI Evolution of Asian aerosols during transpacific transport in INTEX-B SO ATMOSPHERIC CHEMISTRY AND PHYSICS LA English DT Review ID MARINE BOUNDARY-LAYER; LONG-RANGE TRANSPORT; TRANSBOUNDARY POLLUTION INFLUENCES; OXYGENATED ORGANIC AEROSOLS; PARTICULATE AIR-POLLUTION; WESTERN UNITED-STATES; MASS-SPECTROMETER; ACE-ASIA; NORTH-AMERICA; CHEMICAL-COMPOSITION AB Measurements of aerosol composition were made with an Aerodyne High Resolution Time-of-Flight Aerosol Mass Spectrometer (HR-ToF-AMS) on board the NSF/NCAR C-130 aircraft as part of the Intercontinental Chemical Transport Experiment Phase B (INTEX-B) field campaign over the Eastern Pacific Ocean. The HR-ToF-AMS measurements of non-refractory submicron aerosol mass are shown to compare well with other aerosol instrumentation in the INTEX-B field study. Two case studies are described for pollution layers transported across the Pacific from the Asian continent, intercepted 3-4 days and 7-10 days downwind of Asia, respectively. Aerosol chemistry is shown to be a robust tracer for air masses originating in Asia, specifically the presence of sulfate dominated aerosol is a distinguishing feature of Asian pollution layers that have been transported to the Eastern Pacific. We examine the time scales of processing for sulfate and organic aerosol in the atmosphere and show that our observations confirm a conceptual model for transpacific transport from Asia proposed by Brock et al. (2004). Our observations of both sulfate and organic aerosol in aged Asian pollution layers are consistent with fast formation near the Asian continent, followed by washout during lofting and subsequent transformation during transport across the Pacific. Our observations are the first atmospheric measurements to indicate that although secondary organic aerosol (SOA) formation from pollution happens on the timescale of one day, the oxidation of organic aerosol continues at longer timescales in the atmosphere. Comparisons with chemical transport models of data from the entire campaign reveal an under-prediction of organic aerosol mass in the MOZART model, but much smaller discrepancies with the GEOS-Chem model than found in previous studies over the Western Pacific. No evidence is found to support a previous hypothesis for significant secondary organic aerosol formation in the free troposphere. C1 [Dunlea, E. J.; DeCarlo, P. F.; Aiken, A. C.; Kimmel, J. R.; Jimenez, J. L.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. [DeCarlo, P. F.] Univ Colorado, Dept Atmospher & Ocean Sci, Boulder, CO 80309 USA. [Aiken, A. C.; Jimenez, J. L.] Univ Colorado, Dept Chem & Biochem, Boulder, CO 80309 USA. [Peltier, R. E.; Weber, R. J.] Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA. [Tomlinson, J.; Collins, D. R.] Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA. [Shinozuka, Y.; McNaughton, C. S.; Howell, S. G.; Clarke, A. D.] Univ Hawaii, Dept Oceanog, Honolulu, HI 96822 USA. [Emmons, L. K.; Apel, E. C.; Pfister, G. G.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [van Donkelaar, A.; Martin, R. V.] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 3J5, Canada. [Martin, R. V.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Millet, D. B.] Univ Minnesota, Dept Soil Water & Climate, St Paul, MN 55108 USA. [Heald, C. L.] Univ Calif Berkeley, Dept Chem, Berkeley, CA 94720 USA. RP Dunlea, EJ (reprint author), Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. EM edward.dunlea@colorado.edu RI Tomlinson, Jason/C-6566-2009; Aiken, Allison/B-9659-2009; Heald, Colette/A-6813-2011; Collins, Don/F-9617-2012; Millet, Dylan/G-5832-2012; Pfister, Gabriele/A-9349-2008; Martin, Randall/C-1205-2014; Chem, GEOS/C-5595-2014; Emmons, Louisa/R-8922-2016; Jimenez, Jose/A-5294-2008; DeCarlo, Peter/B-2118-2008 OI Aiken, Allison/0000-0001-5749-7626; Martin, Randall/0000-0003-2632-8402; Emmons, Louisa/0000-0003-2325-6212; Jimenez, Jose/0000-0001-6203-1847; DeCarlo, Peter/0000-0001-6385-7149 FU NASA [NNG06GB03G, NNG06GB27G, NNG04GA67G]; NSF [ATM 0513116]; NSF/UCAR [S05-39607]; NASA; EPA [NNG04GR06H, FP-91650801]; National Science Foundation FX We thank the following people for helpful discussions and/or providing data or model products: Roya Bahreini, Darrel Baumgardner, Teresa Campos, John Crounse, Frank Flocke, Henry Fuelberg, David Knapp, Ann Middlebrook, Denise Montzka, Michael Porter, Gregory Roberts, R. Subramanian, Ingrid Ulbrich, Andrew Weinheimer, Paul Wennberg, Qi Zhang. We would also like to thank the crew of the NSF/NCAR C-130 aircraft, especially William Irwin, Mark Lord, Pavel Romashkin, and Allen Schanot. This study was supported by NASA grants NNG06GB03G, NNG06GB27G and NNG04GA67G, and by NSF grant ATM 0513116, and NSF/UCAR grant S05-39607. ACA and PDF are grateful for graduate fellowships from NASA and EPA respectively (NNG04GR06H and FP-91650801). The National Center for Atmospheric Research is sponsored by the National Science Foundation. NR 175 TC 88 Z9 88 U1 5 U2 29 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1680-7316 EI 1680-7324 J9 ATMOS CHEM PHYS JI Atmos. Chem. Phys. PY 2009 VL 9 IS 19 BP 7257 EP 7287 PG 31 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 506MT UT WOS:000270779700001 ER PT J AU Wang, H Jacob, DJ Kopacz, M Jones, DBA Suntharalingam, P Fisher, JA Nassar, R Pawson, S Nielsen, JE AF Wang, H. Jacob, D. J. Kopacz, M. Jones, D. B. A. Suntharalingam, P. Fisher, J. A. Nassar, R. Pawson, S. Nielsen, J. E. TI Error correlation between CO2 and CO as constraint for CO2 flux inversions using satellite data SO ATMOSPHERIC CHEMISTRY AND PHYSICS LA English DT Article ID ATMOSPHERIC CO2; CARBON-DIOXIDE; TRANSPORT MODELS; SCIAMACHY; EMISSIONS; SENSITIVITY; VALIDATION; MONOXIDE; COLUMNS; PACIFIC AB Inverse modeling of CO2 satellite observations to better quantify carbon surface fluxes requires a chemical transport model (CTM) to relate the fluxes to the observed column concentrations. CTM transport error is a major source of uncertainty. We show that its effect can be reduced by using CO satellite observations as additional constraint in a joint CO2-CO inversion. CO is measured from space with high precision, is strongly correlated with CO2, and is more sensitive than CO2 to CTM transport errors on synoptic and smaller scales. Exploiting this constraint requires statistics for the CTM transport error correlation between CO2 and CO, which is significantly different from the correlation between the concentrations themselves. We estimate the error correlation globally and for different seasons by a paired-model method (comparing GEOS-Chem CTM simulations of CO2 and CO columns using different assimilated meteorological data sets for the same meteorological year) and a paired-forecast method (comparing 48-vs. 24-h GEOS-5 CTM forecasts of CO2 and CO columns for the same forecast time). We find strong error correlations (r(2)>0.5) between CO2 and CO columns over much of the extra-tropical Northern Hemisphere throughout the year, and strong consistency between different methods to estimate the error correlation. Application of the averaging kernels used in the retrieval for thermal IR CO measurements weakens the correlation coefficients by 15% on average (mostly due to variability in the averaging kernels) but preserves the large-scale correlation structure. We present a simple inverse modeling application to demonstrate that CO2-CO error correlations can indeed significantly reduce uncertainty on surface carbon fluxes in a joint CO2-CO inversion vs. a CO2-only inversion. C1 [Wang, H.; Jacob, D. J.; Kopacz, M.; Fisher, J. A.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA. [Wang, H.] Smithsonian Astrophys Observ, Cambridge, MA USA. [Jones, D. B. A.; Nassar, R.] Univ Toronto, Dept Phys, Toronto, ON, Canada. [Suntharalingam, P.] Univ E Anglia, Sch Environm Sci, Norwich NR4 7TJ, Norfolk, England. [Nassar, R.] Univ Toronto, Dept Geog, Toronto, ON M5S 1A1, Canada. [Pawson, S.; Nielsen, J. E.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA. RP Wang, H (reprint author), Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA. EM hwang@cfa.harvard.edu RI Fisher, Jenny/J-3979-2012; Jones, Dylan/O-2475-2014; Chem, GEOS/C-5595-2014; Pawson, Steven/I-1865-2014; OI Fisher, Jenny/0000-0002-2921-1691; Jones, Dylan/0000-0002-1935-3725; Pawson, Steven/0000-0003-0200-717X; Nassar, Ray/0000-0001-6282-1611 FU NASA Atmospheric Composition Modeling and Analysis Program; Natural Sciences and Engineering Research Council of Canada FX Work at Harvard was funded by the NASA Atmospheric Composition Modeling and Analysis Program. Work at University of Toronto was funded by the Natural Sciences and Engineering Research Council of Canada. We thank Hartmut Bosch at University of Leicester for providing OCO averaging kernels. We thank Jean-Daniel Paris at and two anonymous reviewers for providing thoughtful comments of our paper. NR 66 TC 19 Z9 19 U1 0 U2 8 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1680-7316 J9 ATMOS CHEM PHYS JI Atmos. Chem. Phys. PY 2009 VL 9 IS 19 BP 7313 EP 7323 PG 11 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 506MT UT WOS:000270779700004 ER PT J AU Wespes, C Hurtmans, D Clerbaux, C Santee, ML Martin, RV Coheur, PF AF Wespes, C. Hurtmans, D. Clerbaux, C. Santee, M. L. Martin, R. V. Coheur, P. F. TI Global distributions of nitric acid from IASI/MetOP measurements SO ATMOSPHERIC CHEMISTRY AND PHYSICS LA English DT Article ID ARCTIC LOWER STRATOSPHERE; TROPOSPHERIC OZONE; HNO3 PROFILES; IASI; MIPAS; SPECTROMETER; ASSIMILATION; RETRIEVALS; VALIDATION; SATELLITE AB This paper presents the first global distributions of HNO3 total columns acquired by the Infrared Atmospheric Sounding Interferometer (IASI) instrument, launched on-board the MetOp platform in October 2006. IASI is an infrared nadir-looking Fourier transform spectrometer providing atmospheric radiance spectra at 0.5 cm(-1) spectral resolution, from which temperature and infrared absorbing gas concentration profiles are retrieved with global Earth coverage twice a day. A first analysis of the IASI measurements in terms of information content demonstrates the possibility of retrieving a total column for HNO3 at all latitudes with a maximal sensitivity in the middle stratosphere. The retrievals are performed from IASI spectra in the atmospheric window using a fast radiative transfer model and inversion software (FORLI) relying on the Optimal Estimation Method. The operational processing of HNO3 total columns is achieved since March 2008. We show that FORLI-HNO3 performs well at all latitudes (RMS of the spectral residuals around 2.3x10(-6) W/m(2) sr m(-1)) and provides HNO3 total columns with on average statistical errors of about 12%, reaching the threshold value of 32% at the equatorial belt. The global distributions of the retrieved total columns for one year (from March 2008 to February 2009) are presented and discussed with emphasis given to seasonal and interhemispheric variations. Local seasonal variations at 6 specific locations are also described and discussed in comparison with MLS volume mixing ratios at 46.5 hPa. The seasonal cycle observed in Polar regions is highlighted, with maxima observed in fall-winter and minima during spring-summer. The denitrification inside the Antarctic polar vortex during winter is clearly revealed with unprecedented horizontal resolution: HNO3 columns decreasing down to about 1x10(16) molecules cm(-2) are observed, which is consistent with the lower values of temperature observed between 50 and 15 hPa (similar to 20-25 km) and the resulting formation and sedimentation of polar stratospheric clouds. During the same period, the collar region of high quantities of HNO3 at the vortex edge is also observed around 65-60 degrees S latitude. Preliminary correlations between IASI derived HNO3 and O-3 columns inside the polar vortex are presented and discussed. C1 [Wespes, C.; Hurtmans, D.; Clerbaux, C.; Coheur, P. F.] Univ Libre Bruxelles, Brussels, Belgium. [Clerbaux, C.] Univ Paris 06, Paris, France. [Clerbaux, C.] Univ Versailles St Quentin, CNRS, INSU, LATMOS,IPSL, Paris, France. [Santee, M. L.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Martin, R. V.] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 3J5, Canada. [Martin, R. V.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. EM cwespes@ulb.ac.be RI Martin, Randall/C-1205-2014; clerbaux, cathy/I-5478-2013 OI Martin, Randall/0000-0003-2632-8402; FU Fonds National de la Recherche Scientifique [4511.08]; Belgian State Federal Office for Scientific, Technical and Cultural Affairs; European Space Agency [C90-327]; FRIA; Communaute Franc, aise de Belgique-Actions de Recherche Concertees FX IASI has been developed and built under the responsibility of the Centre National d'Etudes Spatiales (CNES, France). It is flown onboard the Metop satellites as part of the EUMETSAT Polar System. The IASI L1 data are received through the EUMETCast near real time data distribution service. The research was funded by the Fonds National de la Recherche Scientifique (FNRS, Belgium M. I. S. F. 4511.08), the Belgian State Federal Office for Scientific, Technical and Cultural Affairs and the European Space Agency (ESA-Prodex arrangement C90-327). Financial support by FRIA and the "Communaute Franc, aise de Belgique-Actions de Recherche Concertees" and are also acknowledged. Work at the Jet Propulsion Laboratory, California Institute of Technology, was done under contract with the National Aeronautics and Space Administration. NR 56 TC 18 Z9 18 U1 0 U2 5 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 2009 VL 9 IS 20 BP 7949 EP 7962 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 512IL UT WOS:000271240500018 ER PT S AU Kirby, KP AF Kirby, Kate P. BE Fournier, KB TI The Dual Role of Atomic and Molecular Astrophysics: Discovery and Data SO ATOMIC PROCESSES IN PLASMAS SE AIP Conference Proceedings LA English DT Proceedings Paper CT 16th International Conference on Atomic Processes in Plasmas CY MAR 22-26, 2009 CL Monterey, CA SP US DOE Off Fus Engergy Sci, Lawrence Livemore Natl Lab, NIF & Photon Sci Directorate, Lawrence Livemore Natl Lab, Phys & Life Sci Directorate, Los Alamos Natl Lab, Univ Calif, Inst Mat Dynam Extreme Condit DE charge exchange; electron impact excitation; solar wind; diffuse soft X-ray background; cometary X-rays; line ratio diagnostics; stellar coronae ID HELIUM-LIKE IONS; X-RAY; SOLAR-WIND; EXTREME-ULTRAVIOLET; CHARGE-TRANSFER; EMISSION; SPECTRA; CAPELLA; CHANDRA; REGION AB Atomic and molecular astrophysics, including both spectroscopy and collision processes, enables astronomers to translate the information carried by photons, collected and energy-analyzed in both ground- and space-based instruments, into understanding and knowledge of diverse astronomical objects. In this paper I focus on the role of atomic and molecular astrophysics (a part of the general field of Laboratory Astrophysics) in both providing overall understanding of new phenomena and contributing sensitive diagnostic probes to use in characterizing astrophysical X-ray sources. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kirby, KP (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 18 TC 1 Z9 1 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 978-0-7354-0698-8 J9 AIP CONF PROC PY 2009 VL 1161 BP 123 EP 131 PG 9 WC Physics, Fluids & Plasmas SC Physics GA BOC76 UT WOS:000276195200021 ER PT J AU Grus, WE Graves, GR Glenn, TC AF Grus, Wendy E. Graves, Gary R. Glenn, Travis C. TI GEOGRAPHIC VARIATION IN THE MITOCHONDRIAL CONTROL REGION OF BLACK-THROATED BLUE WARBLERS (DENDROICA CAERULESCENS) SO AUK LA English DT Article DE Appalachian Mountains; Black-throated Blue Warbler; Dendroica caerulescens; genetic structure; glaciation; mitochondrial DNA; plumage color; stable isotopes ID MAXIMUM-LIKELIHOOD-ESTIMATION; EASTERN UNITED-STATES; MIGRATORY DIVIDE; GENETIC-BASIS; PHYLLOSCOPUS-TROCHILUS; HISTORICAL DEMOGRAPHY; POPULATION-GROWTH; DNA POLYMORPHISM; STABLE-ISOTOPES; WILLOW WARBLERS AB We investigated the genetic population structure of the Black-throated Blue Warbler (Dendroica caerulescens), a Nearctic-Neotropic migrant passerine that breeds in cool mixed deciduous-coniferous forests in eastern North America. A cline in plumage color in breeding populations in the central Appalachian Mountains suggests either a contact zone between two formerly allopatric populations or the presence of a strong contemporary selection gradient. Analysis of 333 base pairs of the mitochondrial control region from 287 individuals sampled from 14 populations revealed relatively high haplotype diversity, low nucleotide diversity, and limited but significant phylogeographic structure across the breeding range (analysis of molecular variance [AMOVA], variation among populations = 2.7%; P < 0.01) and between northern and southern population groups (AMOVA, variation among groups = 2.9%; P < 0.01). Genetic differentiation among populations did not conform to an isolation-by-distance model. Nucleotide diversity was generally highest in the central Appalachians and lower in geographically peripheral populations. Populations from the northwestern periphery of the breeding range in Michigan had the lowest haplotype diversity and were genetically distinct from populations in the southern Appalachians. The star-shaped haplotype network, extensive sharing of common haplotypes among populations, and the haphazard distribution of rare haplotypes are most likely attributable to the combined effects of postglacial expansion from a single refugium (12,000-84,000 years ago) and long-distance dispersal events. The existence of a cline in plumage color, in the face of inferred recent gene flow, suggests that a strong selection gradient is operating, perhaps related to the migratory divide postulated from stable-isotope data. C1 [Graves, Gary R.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, MRC 116, Washington, DC 20013 USA. [Grus, Wendy E.; Glenn, Travis C.] Univ Georgia, Savannah River Ecol Lab, Aiken, SC 29802 USA. RP Graves, GR (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, MRC 116, POB 37012, Washington, DC 20013 USA. EM gravesg@si.edu RI Glenn, Travis/A-2390-2008 FU Alexander Wetmore Fund; Research Opportunities Fund; Biodiversity Surveys and Inventory Program of the National Museum of Natural History; Scholarly Studies Program; Smithsonian Migratory Bird Center; National Science Foundation [9732138]; U.S. Department of Energy [DE-FC-09-96SR18546, DE-FC09-07SR22506] FX We thank P. Angle, J. Dean, C. Dove, C. Gebhard, C. Milensky, J. Ososky, A. Ross, and B. Schmidt for preparing specimens and several anonymous reviewers for comments on the manuscript. Scientific licenses to sample populations were issued by the Canadian Wildlife Service (Atlantic and Ontario Region), U.S. Fish and Wildlife Service, U.S. Department of Agriculture Forest Service, Georgia Department of Natural Resources, Michigan Department of Natural Resources, New York Department of Environmental Conservation, North Carolina Wildlife Resources Commission, Pennsylvania Game Commission, Tennessee Wildlife Resources Agency, West Virginia Department of Natural Resources, and Wisconsin Department of Natural Resources. M. Schable and C. Outz helped in laboratory analyses. Funding was provided by the Alexander Wetmore Fund, the Research Opportunities Fund, the Biodiversity Surveys and Inventory Program of the National Museum of Natural History, the Scholarly Studies Program, the Smithsonian Migratory Bird Center (all Smithsonian Institution), National Science Foundation Award 9732138 to the Savannah River Ecology Laboratory Research Experience for Undergraduates program, and U.S. Department of Energy (contract numbers DE-FC-09-96SR18546 and DE-FC09-07SR22506) to the University of Georgia's Savannah River Ecology Laboratory. For detailed laboratory protocols, see http://www.uga.edu/srel/DNA_Lab/protocols.htm. ARLEQUIN is available at lgb.unige.ch/arlequin/. NR 61 TC 8 Z9 8 U1 1 U2 10 PU AMER ORNITHOLOGISTS UNION PI LAWRENCE PA ORNITHOLOGICAL SOC NORTH AMER PO BOX 1897, LAWRENCE, KS 66044-8897 USA SN 0004-8038 EI 1938-4254 J9 AUK JI AUK PD JAN PY 2009 VL 126 IS 1 BP 198 EP 210 DI 10.1525/auk.2009.07159 PG 13 WC Ornithology SC Zoology GA 409EJ UT WOS:000263488700021 ER PT J AU Yavitt, JB Harms, KE Garcia, MN Wright, SJ He, F Mirabello, MJ AF Yavitt, J. B. Harms, K. E. Garcia, M. N. Wright, S. J. He, F. Mirabello, M. J. TI Spatial heterogeneity of soil chemical properties in a lowland tropical moist forest, Panama SO AUSTRALIAN JOURNAL OF SOIL RESEARCH LA English DT Article DE base cations; geostatistical analysis; nutrients; spatial variability; trace elements; variogram ID BARRO COLORADO ISLAND; GEOSTATISTICAL ANALYSIS; NUTRIENT AVAILABILITY; PLANT-COMMUNITIES; TRACE-ELEMENTS; RAIN-FOREST; DRY FOREST; VARIABILITY; PATTERNS; RESOURCES AB We evaluated spatial heterogeneity for pH and a comprehensive set of nutrient and trace elements in surface (0-0.1m depth) and subsurface (0.3-0.4m depth) soils across 26.6 ha of old-growth, lowland, tropical moist forest, established on a highly weathered soil in Panama. Little is known about spatial heterogeneity patterns of soil properties in tropical forest soils. Soil was moderately acidic ( pH 5.28) with low concentrations of exchangeable base cations (13.4 cmol(c)/kg), Bray-extractable PO4 (2.2 mg/kg), KCl-extractable NO3 (5.0 mg/kg), and KCl-extractable NH4 (15.5 mg/kg). The coefficient of variation for soil properties ranged from 24% to >200%, with a median value of 84%. Geostatistical analysis revealed spatial dependence at a scale of 10-100m for most of the soil properties; however, pH, NH4, Al, and B had spatial dependence at a scale up to 350 m. Best-fit models to individual variograms included random, exponential, spherical, Gaussian, linear, and power functions, indicating many different spatial patterns among the set of soil properties. Correlation among individual elements was poor, indicating independent patterns. Our results show complex spatial patterns in soil chemical properties and provide a basis for future investigations on soil-plant relationships and soil nutrient niche differentiation. C1 [Yavitt, J. B.; Mirabello, M. J.] Cornell Univ, Dept Nat Resources, Ithaca, NY 14853 USA. [Harms, K. E.] Louisiana State Univ, Dept Biol Sci, Baton Rouge, LA 70803 USA. [Garcia, M. N.; Wright, S. J.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [He, F.] Univ Alberta, Dept Renewable Resources, Edmonton, AB T6G 2H1, Canada. RP Yavitt, JB (reprint author), Cornell Univ, Dept Nat Resources, Fernow Hall, Ithaca, NY 14853 USA. EM jby1@cornell.edu RI Wright, Stuart/M-3311-2013 OI Wright, Stuart/0000-0003-4260-5676 FU Andrew W. Mellon Foundation; Smithsonian Scholarly Studies program; Smithsonian Tropical Research Institute FX Research support provided by grants from the Andrew W. Mellon Foundation and the Smithsonian Scholarly Studies program. The Smithsonian Tropical Research Institute provides much support for the ongoing Gigante Fertilization Project. We thank the many students in Panama and at Cornell for assistance in the field and in the laboratory. NR 68 TC 35 Z9 40 U1 1 U2 22 PU CSIRO PUBLISHING PI COLLINGWOOD PA 150 OXFORD ST, PO BOX 1139, COLLINGWOOD, VICTORIA 3066, AUSTRALIA SN 0004-9573 EI 1446-568X J9 AUST J SOIL RES JI Aust. J. Soil Res. PY 2009 VL 47 IS 7 BP 674 EP 687 DI 10.1071/SR08258 PG 14 WC Soil Science SC Agriculture GA 515XO UT WOS:000271506400003 ER PT B AU Friedberg, AL AF Friedberg, Aaron L. BE Drezner, DW TI Strengthening US Strategic Planning SO AVOIDING TRIVIA: THE ROLE OF STRATEGIC PLANNING IN AMERICAN FOREIGN POLICY LA English DT Article; Book Chapter C1 [Friedberg, Aaron L.] Princeton Univ, Princeton, NJ 08544 USA. [Friedberg, Aaron L.] Smithsonian Inst, Woodrow Wilson Int Ctr Scholars, Washington, DC 20560 USA. [Friedberg, Aaron L.] Harvard Univ, Ctr Int Affairs, Cambridge, MA 02138 USA. RP Friedberg, AL (reprint author), Princeton Univ, Princeton, NJ 08544 USA. NR 5 TC 0 Z9 0 U1 0 U2 0 PU BROOKINGS INST PI WASHINGTON PA 1775 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA BN 978-0-81570-366-2; 978-0-81570-306-8 PY 2009 BP 84 EP 97 PG 14 WC International Relations; Political Science SC International Relations; Government & Law GA BHS03 UT WOS:000326525000006 ER PT J AU Gordon, CE McGill, B Ibarra-Nunez, G Greenberg, R Perfecto, I AF Gordon, Caleb E. McGill, Brian Ibarra-Nunez, Guillermo Greenberg, Russell Perfecto, Ivette TI Simplification of a coffee foliage-dwelling beetle community under low-shade management SO BASIC AND APPLIED ECOLOGY LA English DT Article DE Coleoptera; Biodiversity conservation; Diversity estimators; Morphospecies; Top-down effects; beta diversity; Predator exclusion; Conservation agroecology ID RAREFACTION DIVERSITY MEASUREMENT; BIODIVERSITY CONSERVATION; CLOUD FOREST; AGROECOSYSTEMS; PLANTATIONS; INTENSITY; SYSTEMS; MEXICO; ARTHROPODS; ABUNDANCE AB Coffee agroforests may be structurally and floristically complex and may contain a significant fraction of species from biodiverse and threatened tropical montane forest biotas; hence, understanding the dynamics of tropical forest biodiversity in coffee agroecosystems has emerged as a centrally important area of tropical conservation biology research. We conducted a morphospecies analysis on foliage-dwelling beetles collected from coffee plants on four coffee farms in southern Chiapas, Mexico, to characterize variation in the abundance, species richness, and species composition of this mega-diverse taxon in relation to coffee cultivation system, spatio-temporal variation, and predator removal. We constructed thirty-two cages to exclude birds and bats on four farms, each enclosing 7-10 coffee plants and paired with an adjacent uncaged control plot, and then collected beetles from coffee foliage with D-Vac aspirators in each plot once every 3 months for one year. We classified the 2662 beetles collected into 293 morphospecies, representing 42 families of beetles. Extrapolation and interpolation analyses revealed a very high level of species richness, with no plateau and only a slight leveling trend observed in our species accumulation curves. We found that low-shade systems contain equal or higher beetle abundance, lower species richness, more highly homogenized species composition, and higher abundance of coffee berry borer pests on coffee foliage than do high-shade systems. We observed no effect of flying vertebrate exclusion on the coffee foliage beetle assemblage, but did find significant variation in abundance, species richness, and species composition of coffee foliage beetles across seasons and Study sites. The increased beetle biodiversity of high-shade coffee cultivation systems has important implications both for the preservation of native biodiversity in coffee growing regions and for the control of agricultural pests such as the coffee berry borer. (C) 2008 Gesellschaft fur Okologle. Published by Elsevier GmbH. All rights reserved. C1 [Gordon, Caleb E.] Lake Forest Coll, Dept Biol, Lake Forest, IL 60045 USA. [McGill, Brian] McGill Univ, Dept Biol, Montreal, PQ H3A 1B1, Canada. [Ibarra-Nunez, Guillermo] Colegio Frontera ECOSUR, Dept Entomol Trop, Tapachula, Chiapas, Mexico. [Greenberg, Russell] Smithsonian Inst, Natl Zool Pk, Smithsonian Migratory Bird Ctr, Washington, DC 20008 USA. [Perfecto, Ivette] Univ Michigan, Sch Nat Resources & Environm, Ann Arbor, MI 48109 USA. RP Gordon, CE (reprint author), Lake Forest Coll, Dept Biol, Lake Forest, IL 60045 USA. EM gordon@lfc.edu RI Trejo, Yesenia/D-9257-2012; Ibarra-Nunez, Guillermo/A-6682-2013; McGill, Brian/A-3476-2008 OI Ibarra-Nunez, Guillermo/0000-0003-2042-425X; McGill, Brian/0000-0002-0850-1913 FU NSF [DEB 9981526]; GIN; NSF International Research Fellowship [INT-0076201]; Lake Forest College FX We thank the owners of Finca Irlanda, Belen and Harnburgo for allowing Lis to conduct studies in their farins. Gustavo Lopez Bautista, Alvaro Ballinas, Juan Carlos Lopez de Leon, Aurelio Mendizabal and Peter Bichier helped with insect collection and sorting. Rachel Gratis and Kimberly Lawser helped with the morphospecies analysis. The following beetle taxonomists examined and identified beetle specimens from selected families: Yves Bousquet (Monotornidae), Gene Hall (Corylophidae, Ptiliidae), Michael C. Thomas (Silvanidae), Robert Gordon (Coccinelljdae). The Instituto de Ecologia, A. C. in Xalapa, Veracruz, Mexico, and Lake Forest College, Lake Forest, Illinois provided lab space and equipment for the beetle morphospecies analysis. Financial Support was provided by NSF grant DEB 9981526 awarded to IP, RG, and GIN, NSF International Research Fellowship Award INT-0076201 awarded to CEG, and by Lake Forest College. NR 37 TC 12 Z9 12 U1 3 U2 22 PU ELSEVIER GMBH, URBAN & FISCHER VERLAG PI JENA PA OFFICE JENA, P O BOX 100537, 07705 JENA, GERMANY SN 1439-1791 J9 BASIC APPL ECOL JI Basic Appl. Ecol. PY 2009 VL 10 IS 3 BP 246 EP 254 DI 10.1016/j.baae.2008.04.004 PG 9 WC Ecology SC Environmental Sciences & Ecology GA 444CA UT WOS:000265956500006 ER PT J AU Klose, S Welbergen, J Goldizen, A Kalko, E AF Klose, Stefan M. Welbergen, Justin A. Goldizen, Anne W. Kalko, Elisabeth K. V. TI Spatio-temporal vigilance architecture of an Australian flying-fox colony SO BEHAVIORAL ECOLOGY AND SOCIOBIOLOGY LA English DT Article DE Cooperation; Risk dilution; Antipredatory strategies; Behavioral monitoring; Chiroptera ID GROUP SPATIAL POSITION; GROUP-SIZE; FORAGING BEHAVIOR; EVENING EMERGENCE; SEX-DIFFERENCES; PREDATION RISK; FRUIT BATS; MONKEYS; FEMALES; MALES AB The social structure of animal aggregations may vary considerably in both space and time, yet little is known about how this affects vigilance. Here, we investigate the vigilance architecture of a colony of wild-living grey-headed flying-foxes (Pteropus poliocephalus) in Australia and examine how spatial as well as temporal variation in social organization influences social and environmental vigilance. We sampled color-marked individuals at different stages of the reproductive cycle and the year and at different locations in the colony to examine the effects of temporal and spatial factors on social and environmental vigilance. We found that vigilance architecture reflected the social structure of the colony, with the highest environmental vigilance being displayed by bats at the periphery of the colony, and the highest social vigilance by bats that roosted at intermediate distances from the colony's edge. Furthermore, we found that vigilance levels reflected changes in reproductive state, with social vigilance increasing toward the mating season, particularly in males. Our findings show that spatial and temporal variation in social structure can have differential effects on social and environmental vigilance. This highlights the necessity to differentiate between functions of vigilance to understand fully vigilance architecture in aggregations of social animals. C1 [Klose, Stefan M.; Kalko, Elisabeth K. V.] Univ Ulm, Inst Expt Ecol, D-89069 Ulm, Germany. [Klose, Stefan M.; Goldizen, Anne W.] Univ Queensland, Sch Integrat Biol, Brisbane, Qld 4072, Australia. [Kalko, Elisabeth K. V.] Smithsonian Trop Res Inst, Balboa, Panama. [Welbergen, Justin A.] Univ Cambridge, Dept Zool, Cambridge CB2 3EJ, England. RP Klose, S (reprint author), Univ Ulm, Inst Expt Ecol, Albert Einstein Allee 11, D-89069 Ulm, Germany. EM stefan.klose@uni-ulm.de RI Goldizen, Anne/G-7366-2012 OI Goldizen, Anne/0000-0003-0101-4108 FU Australian Government Endeavour Programme; Donors' Association for the Promotion of Science and Humanities in Germany; Friedrich Ebert Foundation; German Academic Exchange Service and Qantas Airway FX We wish to thank Silke Berger, Joanna Fietz, Les Hall, Kirsten Jung, Christoph Meyer, Nico Janicke, Kevin Murray, Martin Pfeiffer, and an anonymous referee for comments and discussions, and David Drynan, Allan Goodwin, Dave Pinson, Amy Noone, Peter Rohde, and Jodi Thomas as well as the team of Luffley Cafe for their excellent logistic support. The Tweed Shire Council, Diane Mitchell, and Harry Williams allowed us to work on their properties. Financial support at different stages of this project came from the Australian Government Endeavour Programme, Donors' Association for the Promotion of Science and Humanities in Germany ("Stifterverband"), Friedrich Ebert Foundation, German Academic Exchange Service and Qantas Airways (all to S. M. K.). This study was carried out in compliance with the laws of the Commonwealth of Australia under appropriate ethics and research permits issued by the University of Queensland Animal Ethics Committee, NSW Department of Agriculture, NSW Parks and Wildlife Service, and the Australian Nature Conservation Agency (ABBBS). NR 57 TC 12 Z9 12 U1 2 U2 22 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 JAN PY 2009 VL 63 IS 3 BP 371 EP 380 DI 10.1007/s00265-008-0671-8 PG 10 WC Behavioral Sciences; Ecology; Zoology SC Behavioral Sciences; Environmental Sciences & Ecology; Zoology GA 387MA UT WOS:000261955100007 ER PT B AU Martin, S AF Martin, Sergio BE Meech, KJ Keane, JV Mumma, MJ Siefert, JL Werthimer, DJ TI Observing the Molecular Composition of Galaxies SO BIOASTRONOMY 2007: MOLECULES, MICROBES, AND EXTRATERRESTRIAL LIFE SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 9th International Conference on Bioastronomy CY JUL 16-20, 2007 CL San Juan, PR ID NEARBY GALAXIES; DENSE GAS; INTERSTELLAR MEDIUM; NUCLEAR STARBURST; CARBON-MONOXIDE; APM 08279+5255; EMISSION; NGC-253; AMMONIA; IC-342 AB The recent availability of wideband receivers and high sensitivity instruments in the mm and submm wavelengths has opened the possibility of studying in detail the chemistry of the interstellar medium in extragalactic objects. Within the central few hundred parsec of galaxies, we find enormous amounts of molecular material fueling a wide variety of highly energetic events observed in starbursts (galaxies undergoing an intense burst of star formation) and active galactic nuclei (AGN, where activity is driven by the accretion of material onto the nuclear black hole). This paper presents a brief summary of both the history and the latest results in observational chemistry in distant galaxies. It will be shown how the molecular emission is a powerful tool to explore the physics of the dust-enshrouded, buried nuclei of distant ultraluminous galaxies, which are heavily obscured at other wavelengths. Special attention will be given to the possibilities offered by next generation instruments such as ALMA (Atacama Large Millimeter Array), expected to have a vast impact on the field of Extragalactic Chemistry. Molecular studies in the early Universe will become available at unprecedented sensitivity and resolution. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA. RP Martin, S (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA. 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 978-1-58381-720-9 J9 ASTR SOC P PY 2009 VL 420 BP 19 EP 28 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BQL38 UT WOS:000281244800002 ER PT B AU Latham, DW AF Latham, D. W. BE Meech, KJ Keane, JV Mumma, MJ Siefert, JL Werthimer, DJ TI Toward Earth-Like Planets SO BIOASTRONOMY 2007: MOLECULES, MICROBES, AND EXTRATERRESTRIAL LIFE SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 9th International Conference on Bioastronomy CY JUL 16-20, 2007 CL San Juan, PR ID FOLLOW-UP OBSERVATIONS; EXTRASOLAR PLANET AB NASA's Kepler mission has the goal of detecting transiting planets as small as the Earth, even some that might be habitable. Kepler was launched 2009. After transiting planet candidates are detected, the challenge will be to sort out the real planets from the stellar imposters masquerading as planets. The ultimate test is a spectroscopic orbit that confirms the planet's mass. A key facility for this follow-up work will be HARPS-NEE, a collaboration between the Geneva Observatory and Harvard University to build a version of HARPS for a telescope in the North. Kepler stares at a single field of view in Cygnus and Lyra for the entire four-year mission, to allow the detection of planets with orbital periods as long as a year. As a result the systems discovered by Kepler will be relatively far away, faint, and difficult for follow-up observations. To complement Kepler we need an all-sky survey that can identify the nearest and brightest transiting systems. For the photometry to be good enough to push to smaller planets we need to get above the Earth's atmosphere. TESS is a proposal for such a mission. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Latham, DW (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. 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 978-1-58381-720-9 J9 ASTR SOC P PY 2009 VL 420 BP 297 EP 304 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BQL38 UT WOS:000281244800040 ER PT J AU Dobretsov, S Teplitski, M Paul, V AF Dobretsov, Sergey Teplitski, Max Paul, Valerie TI Mini-review: quorum sensing in the marine environment and its relationship to biofouling SO BIOFOULING LA English DT Review DE quorum sensing; inhibitors; biofouling; biofilm formation; marine environment; Gram-negative bacteria ID ACYL-HOMOSERINE-LACTONE; GRAM-NEGATIVE BACTERIA; TO-CELL COMMUNICATION; ALGA DELISEA-PULCHRA; POLYCHAETE HYDROIDES-ELEGANS; PSEUDOMONAS-AERUGINOSA PAO1; N-ACYLHOMOSERINE LACTONES; LARVAL SETTLEMENT; RED ALGA; SECONDARY METABOLITES AB Bacterial quorum sensing (QS) is a cell-cell communication and gene regulatory mechanism that allows bacteria to coordinate swarming, biofilm formation, stress resistance, and production of toxins and secondary metabolites in response to threshold concentrations of QS signals that accumulate within a diffusion-limited environment. This review focuses on the role of QS signaling and QS inhibition in marine bacteria by compounds derived from marine organisms. Since the formation of a biofilm is considered to be an initial step in the development of fouling, direct and indirect effects of QS signals and inhibitors on the process of marine biofouling are discussed. Directions for future investigations and QS-related biotechnological applications are highlighted. C1 [Dobretsov, Sergey] Sultan Qaboos Univ, Coll Agr & Marine Sci, Dept Marine Sci & Fisheries, Muscat, Oman. [Teplitski, Max] Univ Florida, Dept Soil & Water Sci, Gainesville, FL USA. [Paul, Valerie] Smithsonian Marine Stn, Ft Pierce, FL USA. RP Dobretsov, S (reprint author), Sultan Qaboos Univ, Coll Agr & Marine Sci, Dept Marine Sci & Fisheries, Muscat, Oman. EM sergey@squ.edu.om RI Dobretsov, Sergey/C-9733-2012 OI Dobretsov, Sergey/0000-0002-1769-6388 FU Smithsonian Institution (USA); SQU [IG/AGR/FISH/09/03]; Florida Sea [NA060AR4170014 R/LR-MB-27]; CRIS [FLA-SWS-04591]; National Oceanic and Atmospheric Administration [NA05NOS4781194]; NOAA; US Department of Commerce [NA06OAR4170014] FX The work of Sergey Dobretsov was supported by the George E. Burch Fellowship in Theoretical Medicine and Affiliated Sciences at the Smithsonian Institution (USA) and the SQU grant IG/AGR/FISH/09/03. Max Teplitski's contribution was supported by the Florida Sea Grant no. NA060AR4170014 R/LR-MB-27 under CRIS project FLA-SWS-04591. Valerie Paul acknowledges funding by the National Oceanic and Atmospheric Administration's ECOHAB program (the Ecology and Oceanography of Harmful Algal Blooms) Project NA05NOS4781194 and the Florida Sea Grant College Program with support from NOAA, Office of Sea Grant, US Department of Commerce, Grant no. NA06OAR4170014. This is SMSFP contribution no. 773. NR 126 TC 146 Z9 152 U1 12 U2 104 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 0892-7014 J9 BIOFOULING JI Biofouling PY 2009 VL 25 IS 5 BP 413 EP 427 AR PII 909737120 DI 10.1080/08927010902853516 PG 15 WC Biotechnology & Applied Microbiology; Marine & Freshwater Biology SC Biotechnology & Applied Microbiology; Marine & Freshwater Biology GA 436LJ UT WOS:000265415300004 PM 19306145 ER PT J AU Davidson, IC Brown, CW Sytsma, MD Ruiz, GM AF Davidson, Ian C. Brown, Christopher W. Sytsma, Mark D. Ruiz, Gregory M. TI The role of containerships as transfer mechanisms of marine biofouling species SO BIOFOULING LA English DT Article DE containerships; biofouling; fouling; hulls; species introductions; vectors ID BALLAST WATER; SHIPS; INVASION; VESSELS; INTRODUCTIONS; VECTOR; PORT AB Fouling of ships is an important historical and enduring transfer mechanism of marine nonindigenous species (NIS). Although containerships have risen to the forefront of global maritime shipping since the 1950s, few studies have directly sampled fouling communities on their submerged surfaces, and little is known about differences in the fouling characteristics among commercial ship types. Twenty-two in-service containerships at the Port of Oakland (San Francisco Bay, California) were sampled to test the hypothesis that the extent and taxonomic richness of fouling would be low on this type of ship, resulting from relatively fast speeds and short port durations. The data showed that the extent of macroorganisms (invertebrates and algae) was indeed low, especially across the large surface areas of the hull. Less than 1% of the exposed hull was colonized for all apart from one vessel. These ships had submerged surface areas of > 7000 m(2), and fouling coverage on this area was estimated to be <17 m(2) per vessel, with zero biota detected on the hulls of many vessels. The outlying smaller vessel (4465 m(2)) had an estimated coverage of 90% on the hull and also differed substantially from the other ships in terms of its recent voyage history, shorter voyage range and slower speeds. Despite the low extent of fouling, taxonomic richness was high among vessels. Consistent with recent studies, a wide range of organisms were concentrated at more protected and heterogeneous (non-hull) niche areas, including rudders, stern tubes and intake gratings. Green algae and barnacles were most frequently sampled among vessels, but hydroids, bryozoans, bivalves and ascidians were also recorded. One vessel had 20 different species in its fouling assemblage, including non-native species (already established in San Francisco Bay) and mobile species that were not detected in visual surveys. In contrast to other studies, dry dock block areas did not support many organisms, despite little antifouling deterrence in some cases. Comparisons with previous studies suggest that the accumulation of fouling on containerships may be lower than on other ship types (eg bulkers and general cargo vessels), but more data are needed to determine the hierarchy of factors contributing to differences in the extent of macrofouling and non-native species vector risks within the commercial fleet. C1 [Davidson, Ian C.; Sytsma, Mark D.; Ruiz, Gregory M.] Portland State Univ, Aquat Bioinvas Res & Policy Inst, Portland, OR 97207 USA. [Brown, Christopher W.] Smithsonian Environm Res Ctr, Marine Invas Res Lab, Romberg Tiburon Ctr Environm Studies, Tiburon, CA 94920 USA. [Ruiz, Gregory M.] Smithsonian Environm Res Ctr, Marine Invas Res Lab, Edgewater, MD 21037 USA. RP Davidson, IC (reprint author), Portland State Univ, Aquat Bioinvas Res & Policy Inst, POB 751, Portland, OR 97207 USA. EM idavidso@pdx.edu RI Sytsma, Mark/B-2746-2013; OI Ruiz, Gregory/0000-0003-2499-441X; Davidson, Ian/0000-0002-8729-6048 FU California State Lands Commission FX We are grateful to the Port of Oakland, especially Jody Zaitlin and Phil Granger, for access and logistical assistance throughout the project. We very much appreciate all the terminal and shipping line operators, staff and agents for arranging access to vessels as well as participating ship operators for their cooperation and insight. We thank George Smith for planning and advice; Bill Morrison, Don Ockrassa and Kevin Nekinaken for diving expertise; Michael Wright and Underwater Resources Inc for ROV expertise; Christina Simkanin for assistance in the field; Maurya Falkner, Lynn Takata and Suzanne Gilmore for discussions and advice. We also thank three anonymous reviewers for comments and suggestions that improved the manuscript. The Port of Oakland and the California State Lands Commission funded this research. NR 45 TC 50 Z9 52 U1 1 U2 29 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 0892-7014 J9 BIOFOULING JI Biofouling PY 2009 VL 25 IS 7 BP 645 EP 655 DI 10.1080/08927010903046268 PG 11 WC Biotechnology & Applied Microbiology; Marine & Freshwater Biology SC Biotechnology & Applied Microbiology; Marine & Freshwater Biology GA 511SI UT WOS:000271187000006 PM 20183123 ER PT J AU Crow, SE Filley, TR McCormick, M Szlavecz, K Stott, DE Gamblin, D Conyers, G AF Crow, Susan E. Filley, Timothy R. McCormick, Melissa Szlavecz, Katalin Stott, Diane E. Gamblin, David Conyers, Grace TI Earthworms, stand age, and species composition interact to influence particulate organic matter chemistry during forest succession SO BIOGEOCHEMISTRY LA English DT Article; Proceedings Paper CT 3rd International Conference on Mechanisms of Organic Matter Stabilization and Destabilization in Soils and Sediments CY SEP 23-26, 2007 CL Glenelg, AUSTRALIA DE Cutin; Invasive earthworms; Lignin; Litter quality; Forest succession; Particulate organic matter; Suberin; Soil organic matter ID NORTHERN TEMPERATE FORESTS; COASTAL MARINE-ENVIRONMENT; CUO REACTION-PRODUCTS; OXIDATION-PRODUCTS; DECOMPOSITION PATTERN; CONIFER NEEDLES; HARDWOOD FOREST; SOIL CARBON; INVASION; LIGNIN AB The landscapes colonized by invasive earthworms in the eastern U.S. are often patchworks of forest stands in various stages of successional development. We established six field sites in tulip poplar dominated forests in the Smithsonian Environmental Research Center in Edgewater, MD, that span mid (50-70 years-three plots) and late (120-150 years-three plots) successional stages where younger sites had greater earthworm density and biomass than older sites and were dominated by non-native lumbricid species. In particular Lumbricus rubellus, a litter-feeding species, was abundant in mid successional forests. Here, we separated particulate organic matter (POM) from the bulk soil by a combination of size and density fractionation and found that patterns in soil POM chemistry were similar to those found previously during litter decay: in younger forests with high abundance of earthworms, organic carbon normalized cutin- and suberin-derived substituted fatty acid (SFA) concentration was lower and lignin-derived phenols greater than in older forests where earthworms were less abundant. The chemistry of the dominant litter from mid versus late successional tree species did not fully explain the differences in POM chemistry between age classes. Instead, the differences in leaf body versus petiole and leaf versus root chemistry were the dominant drivers of POM chemistry in mid versus late successional stands, although aspects of stand age and tree species also impacted POM chemistry. Our results indicate that preferential ingestion of leaf body tissue by earthworms and the subsequent shifts in sources of plant biopolymers in soil influenced POM chemistry in mid successional forests. These results indicate that invasive earthworm activity in North American forests contributes to a shift in the aromatic and aliphatic composition of POM and thus potentially influences carbon stabilization in soil. C1 [Crow, Susan E.] Queens Univ Belfast, CHRONO Ctr Climate Environm & Chronol, Belfast BT9 6AX, Antrim, North Ireland. [Crow, Susan E.; Filley, Timothy R.; Gamblin, David; Conyers, Grace] Purdue Univ, Dept Earth & Atmospher Sci, W Lafayette, IN 47907 USA. [McCormick, Melissa] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Szlavecz, Katalin] Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21218 USA. [Stott, Diane E.] ARS, USDA, Natl Soil Eros Res Lab, W Lafayette, IN 47907 USA. RP Crow, SE (reprint author), Queens Univ Belfast, CHRONO Ctr Climate Environm & Chronol, 42 Fitzwilliam St, Belfast BT9 6AX, Antrim, North Ireland. EM s.crow@qub.ac.uk RI Filley, Timothy/A-9862-2009; Stott, Diane/A-1270-2010; yang, lixia/D-7815-2011; OI Stott, Diane/0000-0002-6397-3315; Szlavecz, Katalin/0000-0003-2504-0298 NR 59 TC 28 Z9 29 U1 3 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 JAN PY 2009 VL 92 IS 1-2 BP 61 EP 82 DI 10.1007/s10533-008-9260-1 PG 22 WC Environmental Sciences; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Geology GA 403WY UT WOS:000263113900006 ER PT J AU Baker, TR Phillips, OL Laurance, WF Pitman, NCA Almeida, S Arroyo, L DiFiore, A Erwin, T Higuchi, N Killeen, TJ Laurance, SG Nascimento, H Monteagudo, A Neill, DA Silva, JNM Malhi, Y Gonzalez, GL Peacock, J Quesada, CA Lewis, SL Lloyd, J AF Baker, T. R. Phillips, O. L. Laurance, W. F. Pitman, N. C. A. Almeida, S. Arroyo, L. DiFiore, A. Erwin, T. Higuchi, N. Killeen, T. J. Laurance, S. G. Nascimento, H. Monteagudo, A. Neill, D. A. Silva, J. N. M. Malhi, Y. Gonzalez, G. Lopez Peacock, J. Quesada, C. A. Lewis, S. L. Lloyd, J. TI Do species traits determine patterns of wood production in Amazonian forests? SO BIOGEOSCIENCES LA English DT Article ID TROPICAL RAIN-FORESTS; ECOSYSTEM PROPERTIES; NEOTROPICAL FORESTS; SPATIAL-PATTERNS; CARBON STORAGE; BIOMASS; GROWTH; DYNAMICS; DENSITY; ASSOCIATION AB Understanding the relationships between plant traits and ecosystem properties at large spatial scales is important for predicting how compositional change will affect carbon cycling in tropical forests. In this study, we examine the relationships between species wood density, maximum height and above-ground, coarse wood production of trees >= 10 cm diameter (CWP) for 60 Amazonian forest plots. Average species maximum height and wood density are lower in Western than Eastern Amazonia and are negatively correlated with CWP. To test the hypothesis that variation in these traits causes the variation in CWP, we generate plot-level estimates of CWP by resampling the full distribution of tree biomass growth rates whilst maintaining the appropriate tree-diameter and functional-trait distributions for each plot. These estimates are then compared with the observed values. Overall, the estimates do not predict the observed, regional-scale pattern of CWP, suggesting that the variation in communitylevel trait values does not determine variation in coarse wood productivity in Amazonian forests. Instead, the regional gradient in CWP is caused by higher biomass growth rates across all tree types in Western Amazonia. Therefore, the regional gradient in CWP is driven primarily by environmental factors, rather than the particular functional composition of each stand. These results contrast with previous findings for forest biomass, where variation in wood density, associated with variation in species composition, is an important driver of regional-scale patterns in above-ground biomass. Therefore, in tropical forests, above-ground wood productivity may be less sensitive than biomass to compositional change that alters community-level averages of these plant traits. C1 [Baker, T. R.; Phillips, O. L.; Gonzalez, G. Lopez; Peacock, J.; Quesada, C. A.; Lewis, S. L.; Lloyd, J.] Univ Leeds, Sch Geog, Earth & Biosphere Inst, Leeds LS2 9JT, W Yorkshire, England. [Laurance, W. F.; Laurance, S. G.] Smithsonian Trop Res Inst, Balboa, Panama. [Pitman, N. C. A.] Duke Univ, Ctr Trop Conservat, Durham, NC 27706 USA. [Almeida, S.] Museu Paraense Emilio Goeldi, Belem, Para, Brazil. [Arroyo, L.] Museo Noel Kempff Mercado, Santa Cruz, Bolivia. [DiFiore, A.] NYU, Dept Anthropol, New York, NY 10003 USA. [Erwin, T.] Smithsonian Inst, Washington, DC 20560 USA. [Higuchi, N.] Inst Nacl de Pesquisas da Amazonia, Manaus, Amazonas, Brazil. [Killeen, T. J.] Conservat Int, Ctr Appl Biodivers Sci, Washington, DC USA. [Nascimento, H.] Biol Dynam Forest Fragments Project, Manaus, Amazonas, Brazil. [Monteagudo, A.] Jardin Botan Missouri, Proyecto Flora Peru, Oxapampa, Peru. [Neill, D. A.] Nat & Cultura Int, Missouri Bot Gardens, Loja, Ecuador. [Silva, J. N. M.] Ctr Int Forestry Res, Tapajos, Brazil. [Silva, J. N. M.] EMBRAPA Amazonia Oriental, Belem, Para, Brazil. [Malhi, Y.] Univ Oxford, Ctr Environm, Oxford, England. RP Baker, TR (reprint author), Univ Leeds, Sch Geog, Earth & Biosphere Inst, Leeds LS2 9JT, W Yorkshire, England. EM t.r.baker@leeds.ac.uk RI Lloyd, Jonathan/F-8893-2010; Pitman, Nigel/A-7681-2008; Phillips, Oliver/A-1523-2011; Laurance, William/B-2709-2012; Laurance, Susan/G-6021-2011; OI Lloyd, Jonathan/0000-0002-5458-9960; Pitman, Nigel/0000-0002-9211-2880; Phillips, Oliver/0000-0002-8993-6168; Laurance, Susan/0000-0002-2831-2933; Lewis, Simon/0000-0002-8066-6851 NR 51 TC 42 Z9 43 U1 0 U2 26 PU COPERNICUS PUBLICATIONS PI KATHLENBURG-LINDAU PA MAX-PLANCK-STR 13, KATHLENBURG-LINDAU, 37191, GERMANY SN 1726-4170 J9 BIOGEOSCIENCES JI Biogeosciences PY 2009 VL 6 IS 2 BP 297 EP 307 PG 11 WC Ecology; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Geology GA 414BP UT WOS:000263839200014 ER PT J AU Anderson, LO Malhi, Y Ladle, RJ Aragao, LEOC Shimabukuro, Y Phillips, OL Baker, T Costa, ACL Espejo, JS Higuchi, N Laurance, WF Lopez-Gonzalez, G Monteagudo, A Nunez-Vargas, P Peacock, J Quesada, CA Almeida, S AF Anderson, L. O. Malhi, Y. Ladle, R. J. Aragao, L. E. O. C. Shimabukuro, Y. Phillips, O. L. Baker, T. Costa, A. C. L. Espejo, J. S. Higuchi, N. Laurance, W. F. Lopez-Gonzalez, G. Monteagudo, A. Nunez-Vargas, P. Peacock, J. Quesada, C. A. Almeida, S. TI Influence of landscape heterogeneity on spatial patterns of wood productivity, wood specific density and above ground biomass in Amazonia SO BIOGEOSCIENCES LA English DT Article ID NET PRIMARY PRODUCTION; LONG-TERM PLOTS; LANDSAT TM DATA; RAIN-FOREST; TROPICAL FORESTS; IMAGE SEGMENTATION; BRAZILIAN AMAZON; SOIL FERTILITY; TREE; CLASSIFICATION AB Long-term studies using the RAINFOR network of forest plots have generated significant insights into the spatial and temporal dynamics of forest carbon cycling in Amazonia. In this work, we map and explore the landscape context of several major RAINFOR plot clusters using Landsat ETM+ satellite data. In particular, we explore how representative the plots are of their landscape context, and test whether bias in plot location within landscapes may be influencing the regional mean values obtained for important forest biophysical parameters. Specifically, we evaluate whether the regional variations in wood productivity, wood specific density and above ground biomass derived from the RAINFOR network could be driven by systematic and unintentional biases in plot location. Remote sensing data covering 45 field plots were aggregated to generate landscape maps to identify the specific physiognomy of the plots. In the Landsat ETM+ data, it was possible to spectrally differentiate three types of terra firme forest, three types of forests over Paleovarzea geomorphologycal formation, two types of bamboo-dominated forest, palm forest, Heliconia monodominant vegetation, swamp forest, disturbed forests and land use areas. Overall, the plots were generally representative of the forest physiognomies in the landscape in which they are located. Furthermore, the analysis supports the observed regional trends in those important forest parameters. This study demonstrates the utility of landscape scale analysis of forest physiognomies for validating and supporting the finds of plot based studies. Moreover, the more precise geolocation of many key RAINFOR plot clusters achieved during this research provides important contextual information for studies employing the RAINFOR database. C1 [Anderson, L. O.; Malhi, Y.; Ladle, R. J.; Aragao, L. E. O. C.] Univ Oxford, Sch Geog & Environm, Oxford, England. [Shimabukuro, Y.] Natl Inst Space Res, Remote Sensing Div, Sao Jose Dos Campos, Brazil. [Phillips, O. L.; Baker, T.; Lopez-Gonzalez, G.; Peacock, J.; Quesada, C. A.] Univ Leeds, Sch Geog, Earth & Biosphere Inst, Leeds LS2 9JT, W Yorkshire, England. [Costa, A. C. L.] Fed Univ Para, BR-66059 Belem, Para, Brazil. [Monteagudo, A.; Nunez-Vargas, P.] Univ Nacl San Antonia Abad Cusco, Herbario Vargas, Cuzco, Peru. [Higuchi, N.; Quesada, C. A.] Inst Natl Pesquisas Amazonia, Manaus, Amazonas, Brazil. [Laurance, W. F.] Smithsonian Trop Res Inst, Balboa, Panama. [Almeida, S.] Museu Paraense Emilio Goeldi, Belem, Para, Brazil. RP Anderson, LO (reprint author), Univ Oxford, Sch Geog & Environm, Oxford, England. EM liana.anderson@ouce.ox.ac.uk RI Phillips, Oliver/A-1523-2011; Laurance, William/B-2709-2012; aragao, luiz/G-8387-2012; Anderson, Liana/G-8389-2012; Ladle, Richard/E-4228-2014 OI Phillips, Oliver/0000-0002-8993-6168; aragao, luiz/0000-0002-4134-6708; Anderson, Liana/0000-0001-9545-5136; Ladle, Richard/0000-0003-3200-3946 FU Coordenacao de Aperfeic, oamento de Pessoal de Nivel Superior (CAPES) [BEX4018052]; Instituto Internacional de Educacao do Brasil [BECA-B/2006/01/BDE/04] FX We thank the EU-funded PAN-AMAZONIA project for the training and field campaigns funds, the Coordenacao de Aperfeic, oamento de Pessoal de Nivel Superior (CAPES) for the PhD scholarship (BEX4018052) and Instituto Internacional de Educacao do Brasil (BECA-B/2006/01/BDE/04) for the financial support. We also thank the RAINFOR network participants for their helpful comments and effort to better locate the field sites. NR 73 TC 26 Z9 26 U1 1 U2 26 PU COPERNICUS PUBLICATIONS PI KATHLENBURG-LINDAU PA MAX-PLANCK-STR 13, KATHLENBURG-LINDAU, 37191, GERMANY SN 1726-4170 J9 BIOGEOSCIENCES JI Biogeosciences PY 2009 VL 6 IS 9 BP 1883 EP 1902 PG 20 WC Ecology; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Geology GA 500RJ UT WOS:000270321800005 ER PT J AU Coronado, ENH Baker, TR Phillips, OL Pitman, NCA Pennington, RT Martinez, RV Monteagudo, A Mogollon, H Cardozo, ND Rios, M Garcia-Villacorta, R Valderrama, E Ahuite, M Huamantupa, I Neill, DA Laurance, WF Nascimento, HEM de Almeida, SS Killeen, TJ Arroyo, L Nunez, P Alvarado, LF AF Honorio Coronado, E. N. Baker, T. R. Phillips, O. L. Pitman, N. C. A. Pennington, R. T. Vasquez Martinez, R. Monteagudo, A. Mogollon, H. Davila Cardozo, N. Rios, M. Garcia-Villacorta, R. Valderrama, E. Ahuite, M. Huamantupa, I. Neill, D. A. Laurance, W. F. Nascimento, H. E. M. de Almeida, S. Soares Killeen, T. J. Arroyo, L. Nunez, P. Freitas Alvarado, L. TI Multi-scale comparisons of tree composition in Amazonian terra firme forests SO BIOGEOSCIENCES LA English DT Article ID RAIN-FOREST; SPECIES COMPOSITION; BETA-DIVERSITY; FLORISTIC COMPOSITION; SOIL NUTRIENTS; WESTERN AMAZON; PATTERNS; COMMUNITIES; DOMINANCE; ENVIRONMENT AB We explored the floristic composition of terra firme forests across Amazonia using 55 plots. Firstly, we examined the floristic patterns using both genus- and species-level data and found that the species-level analysis more clearly distinguishes among forests. Next, we compared the variation in plot floristic composition at regional- and continental-scales, and found that average among-pair floristic similarity and its decay with distance behave similarly at regional- and continental-scales. Nevertheless, geographical distance had different effects on floristic similarity within regions at distances <100 km, where north-western and southwestern Amazonian regions showed greater floristic variation than plots of central and eastern Amazonia. Finally, we quantified the role of environmental factors and geographical distance for determining variation in floristic composition. A partial Mantel test indicated that while geographical distance appeared to be more important at continental scales, soil fertility was crucial at regional scales within western Amazonia, where areas with similar soil conditions were more likely to share a high number of species. Overall, these results suggest that regional-scale variation in floristic composition can rival continental-scale differences within Amazonian terra firme forests, and that variation in floristic composition at both scales is influenced by geographical distance and environmental factors, such as climate and soil fertility. To fully account for regional-scale variation in continental studies of floristic composition, future floristic studies should focus on forest types poorly represented at regional scales in current datasets, such as terra firme forests with high soil fertility in north-western Amazonia. C1 [Honorio Coronado, E. N.; Freitas Alvarado, L.] Inst Invest Amazonia Peruana, Iquitos, Peru. [Baker, T. R.; Phillips, O. L.; Monteagudo, A.] Univ Leeds, Sch Geog, Earth & Biosphere Inst, Leeds LS2 9JT, W Yorkshire, England. [Pitman, N. C. A.] Duke Univ, Ctr Trop Conservat, Durham, NC 27706 USA. [Honorio Coronado, E. N.; Pennington, R. T.] Royal Bot Garden Edinburgh, Edinburgh EH3 5LR, Midlothian, Scotland. [Vasquez Martinez, R.; Huamantupa, I.] Jardin Bot Missouri, Proyecto Flora Peru, Oxapampa, Peru. [Mogollon, H.] Finding Species, Takoma Pk, MD 20912 USA. [Davila Cardozo, N.; Rios, M.; Garcia-Villacorta, R.; Valderrama, E.; Ahuite, M.] Univ Nacl Amazonia Peruana, Fac Ciencias Biol, Iquitos, Peru. [Neill, D. A.] Naturaleza & Cultura Int, Missouri Bot Garden, Loja, Ecuador. [Laurance, W. F.; Nascimento, H. E. M.] Smithsonian Trop Res Inst, Balboa, Panama. [Nascimento, H. E. M.] Biol Dynam Forest Fragments Project, Manaus, Amazonas, Brazil. [de Almeida, S. Soares] Museu Paraense Emilio Goeldi, BR-66040170 Belem, Para, Brazil. [Killeen, T. J.] Conservat Int, Ctr Appl Biodivers Sci, Washington, DC USA. [Arroyo, L.] Museo Noel Kempff Mercado, Santa Cruz, Bolivia. [Nunez, P.] Univ Nacl San Antonio Abad Cusco, Herbario Vargas, Cuzco, Peru. RP Coronado, ENH (reprint author), Inst Invest Amazonia Peruana, Av A Jose Quinones Km 2-5, Iquitos, Peru. EM eurihc@yahoo.com RI Pitman, Nigel/A-7681-2008; Phillips, Oliver/A-1523-2011; Laurance, William/B-2709-2012; Nascimento, Henrique/F-8612-2012; icmol, icmol/I-5784-2015; Honorio Coronado, Euridice/K-3412-2015 OI Pitman, Nigel/0000-0002-9211-2880; Phillips, Oliver/0000-0002-8993-6168; Honorio Coronado, Euridice/0000-0003-2314-590X NR 52 TC 25 Z9 27 U1 0 U2 8 PU COPERNICUS PUBLICATIONS PI KATHLENBURG-LINDAU PA MAX-PLANCK-STR 13, KATHLENBURG-LINDAU, 37191, GERMANY SN 1726-4170 J9 BIOGEOSCIENCES JI Biogeosciences PY 2009 VL 6 IS 11 BP 2719 EP 2731 PG 13 WC Ecology; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Geology GA 525QU UT WOS:000272232200027 ER PT J AU Bourgeois, S Gilot-Fromont, E Viallefont, A Boussamba, F Deem, SL AF Bourgeois, Stephanie Gilot-Fromont, Emmanuelle Viallefont, Anne Boussamba, Francois Deem, Sharon L. TI Influence of artificial lights, logs and erosion on leatherback sea turtle hatchling orientation at Pongara National Park, Gabon SO BIOLOGICAL CONSERVATION LA English DT Article DE Dermochelys coriacea; Gabon; Hatchlings; Leatherback sea turtle; Orientation; Photopollution ID MARINE TURTLES; CUES; BEACH; BRIGHTNESS AB The coast of Gabon is one of the most important nesting sites for the endangered leatherback sea turtle Dermochelys coriacea. In this study, hatchling orientation was recorded during natural emergences at Pongara National Park, Gabon. This nesting beach is located close to both the capital of Gabon and a developing resort area, Pointe Denis. Under natural conditions most sea turtle hatchlings emerge at night and orient to the ocean by crawling away from dark, high silhouettes landward towards the bright, low seaward horizons. Artificial lights interfere with natural cues and disrupt hatchling orientation. The relative influence of artificial lights, logs and erosion were assessed on the nesting beach in Pongara National Park using a linear mixed model. We found that the attraction to artificial lights was higher than the effect of silhouette cues landward alone, but could be balanced by the simultaneous presence of the moon. Based upon these results, we recommend combining light management in the resort area to reduce the light pollution on the nesting beach and reinforcement of natural cues landward to minimize the effect of the remaining light pollution from the capital. (C) 2008 Elsevier Ltd. All rights reserved C1 [Bourgeois, Stephanie] Natl Vet Sch Alfort, F-94700 Maisons Alfort, France. [Gilot-Fromont, Emmanuelle; Viallefont, Anne] Univ Lyon 1, UMR 5558 Biometrie & Biol Evolut, F-69622 Villeurbanne, France. [Boussamba, Francois] Aventures Sans Frontieres, Libreville, Gabon. [Deem, Sharon L.] Smithsonian Inst, Natl Zool Pk, Dept Anim Hlth, Washington, DC 20008 USA. RP Deem, SL (reprint author), St Louis Zoo, WildCare Inst, 1 Govt Dr, St Louis, MO 63110 USA. EM stephbourgeois_@hotmail.com; fromont@biomserv.univ-lyon1.fr; anne.viallefont@univ-lyon2.fr; deem@stlzoo.org NR 24 TC 19 Z9 21 U1 6 U2 53 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0006-3207 J9 BIOL CONSERV JI Biol. Conserv. PD JAN PY 2009 VL 142 IS 1 BP 85 EP 93 DI 10.1016/j.biocon.2008.09.028 PG 9 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 396MX UT WOS:000262596900008 ER PT J AU Terrell, KA Wildt, DE Anthony, NM Bavister, BD Leibo, SP Penfold, L Marker, LL Crosier, AE AF Terrell, Kimberly A. Wildt, David E. Anthony, Nicola M. Bavister, Barry D. Leibo, Stanley P. Penfold, Linda Marker, Laurie L. Crosier, Adrienne E. TI Sperm Metabolic Function Is Compromised in the Teratospermic Domestic Cat (Felis catus) and Cheetah (Acinonyx jubatus). SO BIOLOGY OF REPRODUCTION LA English DT Meeting Abstract CT 42nd Annual Meeting of the Society-for-the-Study-of-Reproduction CY JUL 18-22, 2009 CL Pittsburgh, PA SP Soc Study Reproduct, David L Lawrence Convent Ctr C1 Smithsonians Natl Zool Pk, Front Royal, VA USA. Univ New Orleans, New Orleans, LA 70148 USA. Univ Puerto Rico, San Juan, PR 00936 USA. White Oak Conservat Ctr, Yulee, FL USA. Cheetah Conservat Fund, Otjiwarongo, Namibia. NR 0 TC 0 Z9 0 U1 1 U2 2 PU SOC STUDY REPRODUCTION PI MADISON PA 1603 MONROE ST, MADISON, WI 53711-2021 USA SN 0006-3363 J9 BIOL REPROD JI Biol. Reprod. PY 2009 SU S MA 170 BP 86 EP 86 PG 1 WC Reproductive Biology SC Reproductive Biology GA 543UY UT WOS:000273605500169 ER PT J AU Hobbs, RJ Howard, J Fleischer, RC Wildt, DE Comizzoli, P AF Hobbs, Rebecca J. Howard, JoGayle Fleischer, Robert C. Wildt, David E. Comizzoli, Pierre TI Increased Gene Expression of Follicle Stimulating Hormone Receptor in Cat Cumulus-Oocyte Complexes During Seasonal Anestrus SO BIOLOGY OF REPRODUCTION LA English DT Meeting Abstract CT 42nd Annual Meeting of the Society-for-the-Study-of-Reproduction CY JUL 18-22, 2009 CL Pittsburgh, PA SP Soc Study Reproduct, David L Lawrence Convent Ctr C1 [Hobbs, Rebecca J.; Howard, JoGayle; Fleischer, Robert C.; Wildt, David E.; Comizzoli, Pierre] Smithsonian Natl Zool Pk, Washington, DC USA. NR 0 TC 0 Z9 0 U1 0 U2 1 PU SOC STUDY REPRODUCTION PI MADISON PA 1603 MONROE ST, MADISON, WI 53711-2021 USA SN 0006-3363 J9 BIOL REPROD JI Biol. Reprod. PY 2009 SU S MA 350 BP 127 EP 128 PG 2 WC Reproductive Biology SC Reproductive Biology GA 543UY UT WOS:000273605500338 ER PT J AU Kersey, DC Wildt, DF Biown, JL Snyder, RJ Huang, Y Monfort, SL AF Kersey, David C. Wildt, David F. Biown, Janine L. Snyder, Rebecca J. Huang, Yan Monfort, Steven L. TI Adrenal Hormone Concentrations in the Female Giant Panda (Ailuropoda melanoleuca), as Measured by Fecal Glucocorticoids, Are Associated with Reproductive Activity SO BIOLOGY OF REPRODUCTION LA English DT Meeting Abstract CT 42nd Annual Meeting of the Society-for-the-Study-of-Reproduction CY JUL 18-22, 2009 CL Pittsburgh, PA SP Soc Study Reproduct, David L Lawrence Convent Ctr C1 Western Univ, Pomona, CA USA. Smithsomans Natl Zool Pk, Front Royal, VA USA. Zoo Atlanta, Atlanta, GA USA. China Conservat & Res Ctr Giant Panda, Wenchuan, Sichuan, Peoples R China. NR 0 TC 0 Z9 0 U1 1 U2 5 PU SOC STUDY REPRODUCTION PI MADISON PA 1603 MONROE ST, MADISON, WI 53711-2021 USA SN 0006-3363 J9 BIOL REPROD JI Biol. Reprod. PY 2009 SU S MA 379 BP 134 EP 134 PG 1 WC Reproductive Biology SC Reproductive Biology GA 543UY UT WOS:000273605500366 ER PT J AU Crosier, AE Brown, J Comizzoli, P Howard, J Putman, S Marker, L Meeks, K Wildt, D AF Crosier, Adrienne E. Brown, Janine Comizzoli, Pierre Howard, JoGayle Putman, Sarah Marker, Laurie Meeks, Katen Wildt, David TI Ovarian Function, Including Steroid Production Patterns and Oocyte Quality, in the Aged Cheetah (Acinonyx jubatus) Is Similar to Younger Counterparts SO BIOLOGY OF REPRODUCTION LA English DT Meeting Abstract CT 42nd Annual Meeting of the Society-for-the-Study-of-Reproduction CY JUL 18-22, 2009 CL Pittsburgh, PA SP Soc Study Reproduct, David L Lawrence Convent Ctr C1 Smithsonians Natl Zool Pk Conservat & Res Ctr, Front Royal, VA USA. Smithsonians Natl Zool Pk, Washington, DC USA. Cheetah Conservat Fund, Otjiwarongo, Namibia. White Oak Conservat Ctr, Yulee, FL USA. NR 0 TC 0 Z9 0 U1 1 U2 10 PU SOC STUDY REPRODUCTION PI MADISON PA 1603 MONROE ST, MADISON, WI 53711-2021 USA SN 0006-3363 J9 BIOL REPROD JI Biol. Reprod. PY 2009 SU S MA 594 BP 184 EP 185 PG 2 WC Reproductive Biology SC Reproductive Biology GA 543UY UT WOS:000273605500571 ER PT J AU Songsasen, N Woodruff, TK Wildt, DE AF Songsasen, Nucharin Woodruff, Teresa K. Wildt, David E. TI Mechanisms Regulating In Vitro Follicle Growth and Differentiation Are Partially Conserved Between the Mouse and Domestic Dog SO BIOLOGY OF REPRODUCTION LA English DT Meeting Abstract CT 42nd Annual Meeting of the Society-for-the-Study-of-Reproduction CY JUL 18-22, 2009 CL Pittsburgh, PA SP Soc Study Reproduct, David L Lawrence Convent Ctr C1 Smithsonians Natl Zool Pk, Front Royal, VA USA. Northwestern Univ, Chicago, IL 60611 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SOC STUDY REPRODUCTION PI MADISON PA 1603 MONROE ST, MADISON, WI 53711-2021 USA SN 0006-3363 J9 BIOL REPROD JI Biol. Reprod. PY 2009 SU S MA 623 BP 190 EP 191 PG 2 WC Reproductive Biology SC Reproductive Biology GA 543UY UT WOS:000273605500597 ER PT J AU Alvarez-Clare, S Kitajima, K AF Alvarez-Clare, Silvia Kitajima, Kaoru TI Susceptibility of Tree Seedlings to Biotic and Abiotic Hazards in the Understory of a Moist Tropical Forest in Panama SO BIOTROPICA LA English DT Article DE artificial seedlings; Barro Colorado Island; herbivory; litterfall; ontogenetic shifts; stem biomechanics; tropical tree seedling survival; vertebrate activity ID SCALE PHYSICAL DISTURBANCE; RAIN-FOREST; NEOTROPICAL FOREST; SEED DISPERSAL; LITTERFALL DAMAGE; SPATIAL-PATTERNS; PALM FRONDS; SURVIVAL; RECRUITMENT; MORTALITY AB We evaluated temporal patterns of seedling survival of eight Neotropical tree species generated under multiple abiotic and biotic hazards (vertebrates, disease, litterfall) in the forest understory on Barro Colorado Island, Panama. Seedlings were transplanted at first leaf expansion in low densities along a 6-km transect and damage and mortality were recorded for 1 yr. We also planted and monitored small and large artificial seedlings to estimate physical disturbance regimes. During 0-2 mo after transplant, vertebrate consumers of reserve cotyledons caused high mortality of real seedlings, but little damage to artificial seedlings. On real seedlings after 2 mo, disease became an important agent of mortality, despite a decrease in overall mortality rates. Damage by litterfall remained relatively low during the 1-yr study period. Survival ranks among species showed ontogenetic shifts over time, as species changed susceptibility to the mortality agents. Survival after 2 mo was positively correlated with stem toughness, not because species with tough stems were less likely to receive mechanical damage, but because they survived better after receiving mechanical damage. Within each transplant station, artificial seedlings were not good predictors of litterfall damage experienced by real seedlings. Forest-wide litterfall damage level, however, was similar for both real and artificial seedlings (ca 10%/yr), a moderate level compared to other tropical forests. In conclusion, species traits including biomechanical traits interact to create complex temporal patterns of first year seedling survival, resulting in ontogenetic shifts that largely reflect changes in the relative importance of vertebrate consumers relative to other hazards. C1 [Alvarez-Clare, Silvia; Kitajima, Kaoru] Univ Florida, Dept Bot, Gainesville, FL 32611 USA. [Kitajima, Kaoru] Smithsonian Trop Res Inst, Balboa, Panama. RP Alvarez-Clare, S (reprint author), Univ Florida, Dept Bot, Gainesville, FL 32611 USA. EM silviacr@ufl.edu RI Kitajima, Kaoru/E-8877-2012 FU NSF [0093303]; STRI FX We would like to thank S. Bernal, L. Coward, J. Hubbard, and M. Vargas for field assistance. F. E. Putz, E. Bruna, J. A. Myers, and two anonymous reviewers provided helpful comments and suggestions. This study was supported by NSF grant 0093303 to K. Kitajima and by a supplemental research grant from STRI to S. Alvarez-Clare. NR 61 TC 18 Z9 19 U1 0 U2 19 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0006-3606 J9 BIOTROPICA JI Biotropica PD JAN PY 2009 VL 41 IS 1 BP 47 EP 56 DI 10.1111/j.1744-7429.2008.00442.x PG 10 WC Ecology SC Environmental Sciences & Ecology GA 387OI UT WOS:000261961100007 ER PT J AU Meyer, CFJ Kalko, EKV Kerth, G AF Meyer, Christoph F. J. Kalko, Elisabeth K. V. Kerth, Gerald TI Small-Scale Fragmentation Effects on Local Genetic Diversity in Two Phyllostomid Bats with Different Dispersal Abilities in Panama SO BIOTROPICA LA English DT Article DE Chiroptera; habitat fragmentation; isolation by distance; land-bridge islands; population genetic structure ID MITOCHONDRIAL-DNA VARIATION; TAILED FRUIT BATS; POPULATION-STRUCTURE; FOREST FRAGMENTATION; HABITAT FRAGMENTATION; MYOTIS-BECHSTEINII; PLECOTUS-AURITUS; EXTINCTION RISK; GLEANING BAT; LANDSCAPE AB Habitat fragmentation is one of the greatest threats to biodiversity. Despite their importance for conservation, the genetic consequences of small-scale habitat fragmentation for bat populations are largely unknown. In this study, we linked genetic with ecological and demographic data to assess the effects of habitat fragmentation on two species of phyllostomid bats (Uroderma bilobatum and Carollia perspicillata) that differ in their dispersal abilities and demographic response to fragmentation. We hypothesized that population differentiation and the effect of habitat fragmentation on levels of genetic diversity will be a function of the species' mobility. We sequenced mtDNA from 232 bats caught on 11 islands in Gatun Lake, Panama, isolated from the mainland for ca 90 yr, and in adjacent, continuous forest on the mainland. Populations of both species showed significant genetic differentiation (F(ST)). Consistent with our prediction, population subdivision was lower in the highly mobile U. bilobatum (F(ST) = 0.01) compared to the less vagile C. perspicillata (F(ST) = 0.06), and only the latter species showed a pattern indicative of isolation by distance and, in addition, an effect of fragmentation. Genetic erosion as a result of fragmentation was also only detectable in the less mobile species, C. perspicillata, where haplotype diversity was lower in island compared to mainland populations. Our results suggest that some Neotropical bat species are prone to loss of genetic variation in response to anthropogenic small-scale habitat fragmentation. In this context, our findings point toward mobility as a good predictor of a species' vulnerability to fragmentation and altered population genetic structure. C1 [Meyer, Christoph F. J.; Kalko, Elisabeth K. V.] Univ Ulm, Inst Expt Ecol, D-89069 Ulm, Germany. [Kalko, Elisabeth K. V.] Smithsonian Trop Res Inst, Balboa, Panama. [Kerth, Gerald] Univ Lausanne, Dept Ecol & Evolut, CH-1015 Lausanne, Switzerland. RP Meyer, CFJ (reprint author), Univ Ulm, Inst Expt Ecol, Albert Einstein Allee 11, D-89069 Ulm, Germany. EM christoph.meyer@uni-ulm.de RI Meyer, Christoph/A-4363-2012 OI Meyer, Christoph/0000-0001-9958-8913 FU German Academic Exchange Service (DAAD); German Science Foundation (DFG) FX We are grateful to L. Berset-Brandli, T. Broquet, J. Jacquiery, N. Perrin, B. Fenton, B. Patterson, and two anonymous reviewers for helpful comments on the manuscript. We cordially thank J. Garbely for the genetic lab work. We thank the Smithsonian Tropical Research Institute for logistical support and the Autoridad del Canal de Panama for permission to work on the islands in Gatun Lake. We would further like to thank the following people for help with fieldwork: A. Bravo, K. Burger, S. Estrada Villegas, J. Frund, I. Geipel, N. Herdina, A. Lang, J. Nagel, A. Reside, R. Rodriguez, A. Sjollema, C. Stubenrauch, and C. Weise. Financial support was provided by a grant from the German Academic Exchange Service (DAAD) to CFJM and two grants from the German Science Foundation (DFG) to EKVK and GK, respectively. NR 66 TC 29 Z9 30 U1 4 U2 35 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0006-3606 J9 BIOTROPICA JI Biotropica PD JAN PY 2009 VL 41 IS 1 BP 95 EP 102 DI 10.1111/j.1744-7429.2008.00443.x PG 8 WC Ecology SC Environmental Sciences & Ecology GA 387OI UT WOS:000261961100013 ER PT J AU Luebert, F Wen, J Dillon, MO AF Luebert, Federico Wen, Jun Dillon, Michael O. TI Systematic placement and biogeographical relationships of the monotypic genera Gypothamnium and Oxyphyllum (Asteraceae: Mutisioideae) from the Atacama Desert SO BOTANICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Review DE arid environments; Chile; Compositae; phylogeny; South America ID SUNFLOWER FAMILY ASTERACEAE; CHLOROPLAST DNA; SUBTRIBE NASSAUVIINAE; PHYLOGENETIC ANALYSIS; BARNADESIOIDEAE ASTERACEAE; CHAETANTHERA ASTERACEAE; MUTISIEAE ASTERACEAE; POLLEN MORPHOLOGY; NORTHERN CHILE; SEQUENCE DATA AB Gypothamnium and Oxyphyllum (Asteraceae) are two monotypic genera endemic to the Atacama Desert of northern Chile. We performed a phylogenetic analysis using published sequences of the plastid rbcL and ndhF genes, the trnL-trnF region and the nuclear ribosomal internal transcribed spacer (ITS) to assess the systematic placement of the two genera within Mutisioideae. On the basis of the phylogenetic results, we constructed area cladograms to explore the biogeographical relationships and origin of the genera. The phylogenetic analysis showed that Gypothamnium is closely related to Aphylloclados, Plazia, Urmenetia, Lycoseris and Onoseris, whereas Oxyphyllum is closely related to Leucheria, Moscharia, Polyachyrus and, with low support, Jungia. These results do not differ substantially from those proposed in previous treatments based on morphological characters. The biogeographical analysis suggests that Gypothamnium in the coastal Atacama Desert is related to taxa that are currently distributed in eastern subtropical South America and in the Puna. Oxyphyllum may have originated from central Chile and other areas in southern South America, but its sister group (Leucheria + Polyachyrus) also reaches the Puna and the coastal Atacama Desert. Both groups show ancestral affinities with elements currently distributed in north-western South America and Mesoamerica. (C) 2009 The Linnean Society of London, Botanical Journal of the Linnean Society, 2009, 159, 32-51. C1 [Luebert, Federico] Univ Chile, Dept Silviculture, Fac Ciencias Forestes, Santiago, Chile. [Luebert, Federico] Free Univ Berlin, Inst Biol Systemat Botan & Pflanzengeog, D-14195 Berlin, Germany. [Wen, Jun] Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, Washington, DC 20013 USA. [Wen, Jun] Chinese Acad Sci, Lab Systemat & Evolutionary Bot, Inst Bot, Beijing 10093, Peoples R China. [Dillon, Michael O.] Field Museum Nat Hist, Dept Bot, Chicago, IL 60605 USA. RP Luebert, F (reprint author), Univ Chile, Dept Silviculture, Fac Ciencias Forestes, Casilla 9206, Santiago, Chile. EM fluebert@zedat.fu-berlin.de RI Luebert, Federico/I-3246-2012 OI Luebert, Federico/0000-0003-2251-4056 FU Smithsonian Institution for a Visiting Scholar Award; Department of Botany and the Laboratory of Analytical Biology of the National Museum of Natural History; German Academic Exchange Service (DAAD); National Science Foundation [DEB 0415573] FX We thank Nicolas Garcia for field assistance, and Ze-Long Nie, Lei Xie and Emilia Danilowicz for help in the laboratory. Patricio Pliscoff kindly elaborated the maps of Fig. 3. Maximilian Weigend and AndrEs Moreira-Munoz provided references and valuable comments. Tod Stuessy provided the chromosome count of Oxyphyllum. Federico Luebert acknowledges the support from the Smithsonian Institution for a Visiting Scholar Award at the Department of Botany and the Laboratory of Analytical Biology of the National Museum of Natural History, and the German Academic Exchange Service (DAAD). Fieldwork was financed by the National Science Foundation (DEB 0415573 to Michael Dillon and Jun Wen). Curators of the herbaria SGO, EIF, F, GH, CONC and ULS permitted the examination of their collections. Laboratory work was supported by the Laboratory of Analytical Biology of the Smithsonian Institution. Professor Dr. Hartmut H. Hilger provided space and resources in his workgroup at the Freie UniversitAt Berlin during the last stage of this study. The suggestions of one anonymous reviewer have helped to improve the manuscript. NR 112 TC 18 Z9 19 U1 1 U2 13 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0024-4074 J9 BOT J LINN SOC JI Bot. J. Linnean Soc. PD JAN PY 2009 VL 159 IS 1 BP 32 EP 51 DI 10.1111/j.1095-8339.2008.00926.x PG 20 WC Plant Sciences SC Plant Sciences GA 395FF UT WOS:000262509300004 ER PT J AU Miller, JS AF Miller, James S. TI GENERIC REVISION OF THE DIOPTINAE (LEPIDOPTERA: NOCTUOIDEA: NOTODONTIDAE) PART 1: DIOPTINI SO BULLETIN OF THE AMERICAN MUSEUM OF NATURAL HISTORY LA English DT Article AB The moth subfamily Dioptinae is almost entirely neotropical. One species-Phryganidia californica-occurs on the west coast of the US, while the remaining taxa are found from Mexico south to northern Argentina and Uruguay. None is known from the Old World. Most dioptines are diurnal as adults, and many exhibit aposematic coloration. A few taxa are nocturnal. Their larval hosts include the families Passifloraceae, Violaceae and Poaceae, plants famous for their use by important butterfly groups. In this paper, a revised generic classification for the Dioptinae is presented. Nearly 17,000 specimens, assembled from 38 private and institutional collections worldwide, form the basis for the First comprehensive analysis of adult morphology in the subfamily. A subset of 115 exemplar species, chosen to represent structural diversity across the Dioptinae, is subjected to detailed morphological Study and cladistic analysis. The resulting matrix includes 305 characters delineated by 938 character states. Cladistic analyses produced a single most parsimonious tree, rooted using three species from the Nystaleinae-the sister-subfamily to the Dioptinae, This phylogenetic hypothesis provides the framework for a revised classification. The 456 species are assigned to 43 genera in two tribes; 10 species are treated as incertae sedis. Twelve genera are synonymized, and seven-Argentala, Chrysoglossa, Nebulosa, Notascea, Pikroprion, Proutieila, and Sagittala-are described as new. The 36 remaining genera are redescribed. Sixteen genera are further Subdivided into species groups. All 574 species-group names of previous authors are addressed; in nearly all cases, primary type material was examined. Forty-seven species are newly synonymized, while 31 names are revived from synonymy. The revised classification includes 118 new combinations. sixty-four Species belonging in 30 different genera are newly described from Brazil, Colombia, Costa Rica, Ecuador, French Guiana, Guyana, Mexico, Panama, Peru, and Venezuela. An illustrated overview of dioptine morphology is presented, demonstrating remarkable variation in a wide range of structures. Dichotomous keys utilizing external adult anatomy are provided to the tribes, genera, species groups and species. The salient features of each genus are figured and described. Heads, labial palpi, antennae, metathoracic tympani, wing scales, wing venation, and male and female terminalia are shown through line drawings, photographs, and scanning electron micrographs. Each species is diagnosed, its habitus is illustrated in color, type material is notated, and a summary of its known geographical distribution is Presented. General themes, as exemplified by the Dioptinae, are discussed. These include: Estimating species diversity in neotropical Lepidoptera; the evolution of aposematic coloration and mimicry; patterns of host-plant use and the potential utility of characters from immature stages and DNA for further refining our understanding of dioptine evolution. C1 [Miller, James S.] Amer Museum Nat Hist, Div Invertebrate Zool, New York, NY 10024 USA. [Miller, James S.] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20560 USA. RP Miller, JS (reprint author), Amer Museum Nat Hist, Div Invertebrate Zool, New York, NY 10024 USA. EM jmiller@amnh.org NR 0 TC 5 Z9 5 U1 1 U2 2 PU AMER MUSEUM NATURAL HISTORY PI NEW YORK PA ATTN: LIBRARY-SCIENTIFIC PUBLICATIONS DISTRIBUTION, CENTRAL PK WEST AT 79TH ST, NEW YORK, NY 10024-5192 USA SN 0003-0090 J9 B AM MUS NAT HIST JI Bull. Amer. Mus. Nat. Hist. PY 2009 IS 321 BP 2 EP 674 PG 677 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 468ED UT WOS:000267796800001 ER PT J AU Carleton, MD AF Carleton, Michael D. TI They Sort Out Like Nuts and Bolts: A Scientific Biography of Guy G. Musser SO BULLETIN OF THE AMERICAN MUSEUM OF NATURAL HISTORY LA English DT Biographical-Item ID MUROID RODENTS; MOLECULAR PHYLOGENY; ENDEMIC RODENTS; GENE-SEQUENCES; MAJOR LINEAGES; NUCLEAR GENES; NEW-GUINEA; MITOCHONDRIAL; SYSTEMATICS; SIGMODONTINAE C1 [Carleton, Michael D.] Amer Museum Nat Hist, Div Vertebrate Zool Mammal, New York, NY 10024 USA. [Carleton, Michael D.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA. RP Carleton, MD (reprint author), Amer Museum Nat Hist, Div Vertebrate Zool Mammal, New York, NY 10024 USA. EM carletonm@si.edu NR 72 TC 0 Z9 0 U1 0 U2 1 PU AMER MUSEUM NATURAL HISTORY PI NEW YORK PA ATTN: LIBRARY-SCIENTIFIC PUBLICATIONS DISTRIBUTION, CENTRAL PK WEST AT 79TH ST, NEW YORK, NY 10024-5192 USA SN 0003-0090 J9 B AM MUS NAT HIST JI Bull. Amer. Mus. Nat. Hist. PY 2009 IS 331 BP 4 EP 32 PG 29 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 535JD UT WOS:000272963500002 ER PT J AU Carleton, MD Arroyo-Cabrales, J AF Carleton, Michael D. Arroyo-Cabrales, Joaquin TI Review of the Oryzomys couesi Complex (Rodentia: Cricetidae: Sigmodontinae) in Western Mexico SO BULLETIN OF THE AMERICAN MUSEUM OF NATURAL HISTORY LA English DT Review ID PEROMYSCUS-BOYLII; RICE RAT; MORPHOLOGICAL EVOLUTION; GENUS ZYGODONTOMYS; MUROID RODENTS; SPECIES GROUP; COTTON RATS; PALUSTRIS; MURIDAE; SYSTEMATICS AB The status and distribution of eight species-group taxa of the Oryzomys couesi group (Rodentia: Cricetidae: Sigmodontinae) described from western Mexico are evaluated based on morphological and morphometric comparisons. Four of these are recognized as valid species within the region: Oryzomys albiventer Merriam, 1901 (including molestus Elliot, 1903), from inland plateau of the Mesa de Anahuac; O. couesi mexicanus J.A. Allen, 1897 (including bulleri J.A. Allen, 1897; lambi Burt, 1934; rufus Merriam, 1901), from Pacific coastal plain, contiguous lower mountain slopes, and interior valleys along the Rios Tepalcatepec-Balsas; O. nelsoni Merriam, 1898, from Isla Maria Madre; and O. peninsulae Thomas, 1897, from the southern tip of the Baja California Peninsula. Three other taxa named from uplands in interior Mexicoa-aztecus Merriam, 1901; crinitus Merriam; 1901; and regillus Goldman, 1915-are provisionally retained within O. couesi, but further study of their specific stature and relationships is required. The recommended taxonomic changes within western Mexico serve to discuss directions for future revisionary research that will refine the definition and distribution of O. couesi sensu stricto in Middle America. C1 [Carleton, Michael D.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA. [Arroyo-Cabrales, Joaquin] INAH, Lab Arqueozool MC Ticul Alvarez Solorzano, Subdirecc Labs & Apoyo Acad, Mexico City 06060, DF, Mexico. RP Carleton, MD (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA. EM carletonm@si.edu; arromatu5@yahoo.com.mx FU Smithsonian Institution's Office FX Foremost, we appreciate the access to specimens, through loans or museum visits, as facilitated by the following museum Staff: Guy G. Musser (AMNH), Paula Jenkins and Daphne Hill (BMNH), Sue McLren (CM), William T. Stanley (FMNH), Thor Holmes and Bob Timm (KU), Fritz Hertel (UCLA), and Steve Hinshaw and Phil Myers (UMMZ). Bill Stanley (FMNH) graciously accommodated our request to provide measurements of the type specimen of Oryzomys molestus. John Steiner (Senior Photographer, NMNH Branch, Smithsonian Photographic Services) photographed the skulls illustrated in figures 8 and 9, and Dan Cole (Office of Information Technology, NMNH) offered assistance and advice on GIS mapping. Data collection for this project was initiated when the junior author was on sabbatical to the USNM Division of Mammals (1998-1999), in a postdoctoral position provided by Don E. Wilson and funded through the Smithsonian Institution's Office of Fellowships and Grants. Duke Rogers and Marcelo Weksler reviewed the manuscript and offered comments that improved it final contents. NR 110 TC 5 Z9 9 U1 0 U2 2 PU AMER MUSEUM NATURAL HISTORY PI NEW YORK PA ATTN: LIBRARY-SCIENTIFIC PUBLICATIONS DISTRIBUTION, CENTRAL PK WEST AT 79TH ST, NEW YORK, NY 10024-5192 USA SN 0003-0090 EI 1937-3546 J9 B AM MUS NAT HIST JI Bull. Amer. Mus. Nat. Hist. PY 2009 IS 331 BP 94 EP 127 PG 34 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 535JD UT WOS:000272963500004 ER PT J AU Gardner, AL Carleton, MD AF Gardner, Alfred L. Carleton, Michael D. TI A New Species of Reithrodontomys, Subgenus Aporodon (Cricetidae: Neotominae), from the Highlands of Costa Rica, with Comments on Costa Rican and Panamanian Reithrodontomys SO BULLETIN OF THE AMERICAN MUSEUM OF NATURAL HISTORY LA English DT Article ID HARVEST MICE REITHRODONTOMYS; MORPHOLOGICAL EVOLUTION; MUROID RODENTS; MURIDAE; SIGMODONTINAE; ZYGODONTOMYS; PATTERNS; MAMMALS; MEXICO AB A new species of the rodent genus Reithrodontomys (Cricetidae: Neotominae) is described from Cerro Asuncion in the western Cordillera de Talamanca, Costa Rica. The long tail, elongate rostrum, bulbous braincase, and complex molars of the new species associate it with members of the subgenus Aporodon, tenuirostris species group. In its diminutive size and aspects of cranial shape, the new species (Reithrodontomys musseri, sp. nov.) most closely resembles R. microdon, a form known from highlands in Guatemala and Chiapas, Mexico. In the course of differentially diagnosing the new species, we necessarily reviewed the Costa Rican and Panamanian subspecies of R. mexicanus based on morphological comparisons, study of paratypes and vouchers used in recent molecular studies, and morphometric analyses. We recognize Reithrodontomys cherrii (Allen, 1891) and R. garichensis finders and Pearson, 1940, as valid species, and allocate R. mexicanus potrerograndei Goodwin, 1945, as a subjective synonym of R. brevirostris Goodwin, 1943. Critical review of museum specimens collected subsequent to Hooper's (1952) revision is needed and would do much to improve understanding of Reithrodontomys taxonomy and distribution in Middle America. C1 [Gardner, Alfred L.] Natl Museum Nat Hist, USGS Patuxent Wildlife Res Ctr, Biol Survey Unit, Washington, DC 20560 USA. [Carleton, Michael D.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA. RP Gardner, AL (reprint author), Natl Museum Nat Hist, USGS Patuxent Wildlife Res Ctr, Biol Survey Unit, Washington, DC 20560 USA. EM gardnera@si.edu; carletonm@si.edu FU NIH [AI-00007] FX The specimen of Reithrodontomys musseri seas collected while Gardner held an appointment as a Fellow in Tropical Medicine with the International Center for Medical Research and Training at Louisiana State University during 1966 and 1967, supported by NIH grant No. AI-00007. We express Our appreciation to the following individuals who made specimens available: Chris Conroy, Museum of Vertebrate Zoology, University of California, Berkeley; Ned Gilmore, Department of Vertebrate Zoology, Academy of Natural Sciences of Philadelphia; Mark Hafner, Museum of Natural Sciences, Louisiana State University; Philip Myers, Museum of Zoology, University of Michigan; and Robert Voss, Division of Vertebrate Zoology (Mammalogy), American Museum of Natural History. This study was greatly facilitated by the fine series of R. microdon recently collected in the Guatemalan highlands by John Matson, San Jose State University, and Walter Bulmer and Ralph Eckerlin, Northern Virginia Community College, Annandale. Finally, we thank David G. Huckaby, Long Beach State University, and Duke S. Rogers, Brigham Young University, for critically reviewing the manuscript and tending helpful suggestions that improved its comprehension. NR 38 TC 0 Z9 1 U1 1 U2 3 PU AMER MUSEUM NATURAL HISTORY PI NEW YORK PA ATTN: LIBRARY-SCIENTIFIC PUBLICATIONS DISTRIBUTION, CENTRAL PK WEST AT 79TH ST, NEW YORK, NY 10024-5192 USA SN 0003-0090 EI 1937-3546 J9 B AM MUS NAT HIST JI Bull. Amer. Mus. Nat. Hist. PY 2009 IS 331 BP 157 EP 182 PG 26 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 535JD UT WOS:000272963500006 ER PT J AU Helgen, KM Helgen, LE AF Helgen, Kristofer M. Helgen, Lauren E. TI Biodiversity and Biogeography of the Moss-Mice of New Guinea: A Taxonomic Revision of Pseudohydromys (Muridae: Murinae) SO BULLETIN OF THE AMERICAN MUSEUM OF NATURAL HISTORY LA English DT Review ID NUCLEAR GENE-SEQUENCES; PAPUA-NEW-GUINEA; TOOTH DEVELOPMENT; MUROID RODENTS; MICROCOMPLEMENT FIXATION; MOLECULAR PHYLOGENY; 3-STRIPED DASYURES; PHALLIC MORPHOLOGY; TERRANE TECTONICS; ENDEMIC RODENTS AB Morphological investigations involving nearly all available museum material representing New Guinea "moss-mice" (rodents traditionally classified in the genera Pseudohydromys, Neohydromys, Mayermys, and Microhrdromys) reveal outstanding undiagnosed taxic diversity (a minimum of 16 species, versus the eight species previously described) and allow for redefinition of generic boundaries among these little-studied rodents. Apart from Microhydromys Tate and Archbold, 1941 (comprising two species, as recently revised by Helgen et al., in press), herein we recognize two genera of New Guinea moss-mice: Pseudohydromys Rummler, 1934 (now incorporating Neohydromys Laurie, 1952, Mayermys Laurie and Hill, 1954, and "Microhydromys" musseri Flannery, 1989) and a newly described genus, Mirzamys. Species of Pseudohydromys are recorded from montane areas throughout New Guinea (elevations spanning 600 to at least 3800 meters), including the mountain ranges of the Central Cordillera, the Huon Peninsula, and the North Coastal ranges. We diagnose and review 12 species of Pseudohydromys, including six species described as new. The ne, v genus Mirzamys is erected to accommodate two newly described species of small terrestrial rodents from middle and upper montane forests and subalpine grassland edges (1900-3450 m) in the mountains of central New Guinea. Together these two new species represent a distinctive hydromyin lineage that resembles the terrestrial New Guinea hydromyin genera Pseudohydromys and Paraleptomys in various traits. Ecological attributes of all recognized moss-mice taxa, both previously and newly described, are reviewed in light of all information currently available about their biology. C1 [Helgen, Kristofer M.] Amer Museum Nat Hist, Div Vertebrate Zool Mammal, New York, NY 10024 USA. [Helgen, Kristofer M.; Helgen, Lauren E.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Div Mammals, Washington, DC 20013 USA. [Helgen, Kristofer M.] Bernice P Bishop Museum, Honolulu, HI USA. [Helgen, Lauren E.] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20013 USA. RP Helgen, KM (reprint author), Amer Museum Nat Hist, Div Vertebrate Zool Mammal, New York, NY 10024 USA. EM helgenk@si.edu; helgenl@si.edu FU National Science Foundation; University of Adelaide; Australian-American Fulbright Commission; American Society of Mammalogists (ASM); Smithsonian Institution; American Museum of Natural History; Bernice P. Bishop Museum; Macquarie University; Fulbright; Bishop Museum FX We dedicate our paper to Guy G. Musser, whose contributions to the study of mammals in the Indo-Australian region, especially rodents, have set the standard in the field. We are grateful to Rob Voss and Michael Carleton, the editors of this Festschrift, for their patience and careful review of our account, and to Ken Aplin, Guy Musser, Titre Flannery, Erik Rickart, and Colin Groves for additional reviews of our manuscript and their kindness in suggesting many improvements. We also thank Mary Knight for further assistance in typesetting our manuscript.; This paper originated as a chapter in the first author's doctoral thesis. Funding for this research was provided primarily by fellowships from the National Science Foundation (Graduate Research Fellowship), the University of Adelaide, the Australian-American Fulbright Commission, the American Society of Mammalogists (ASM), and the Smithsonian Institution. We also gratefully acknowledge fellowship support from an Australian International Postgraduate Research Scholarship and additional funding and assistance from the American Museum of Natural History, the Bernice P. Bishop Museum, and Macquarie University. In particular, we thank Don Wilson (Smithsonian), Mark Darby (Fulbright), Edward Heske (ASM), Anne Witt (University of Adelaide), and Allen Allison (Bishop Museum), for their help in facilitating fellowship and research funding.; We owe an enormous debt of gratitude to the curators, collection managers, and other museum researchers who have enabled our investigations and repeatedly welcomed us into their collections, making relevant specimens and field notes available to us, assisting with specimen preparation and photography, and sending specimen loans both large and small (and patiently awaiting their return). We are especially grateful to Sandy Ingleby, Tish Ennis, Robert Tones, and Ross Sadlier of the Australian Museum; Darrin Lunde, Eileen Westwig, Robert Voss, and Nancy Simmons of the American Museum of Natural History; Paula Jenkins, Daphne Hills, Richard Harbord, and Roberto Portela-Miguez of the Natural History Museum; Carla Kishinami, Pumehana Imada, Allen Allison, Fred Kraus, and Neal Evenhuis of the Bernice P. Bishop Museum; Robert Palmer and Ken Aplin of the Australian National Wildlife Collection; Norah Cooper, Claire Stevenson, and Richard How of the Western Australian Museum; Chris Smeenk of the Naturalis Museum (Leiden); Bulisa Iova and Jim Anamiato of the National Museum and Art Gallery of Papua New Guinea; Rose Singadan of the University of Papua New Guinea; Judith Chupasko, Mark Omura, and Jane Harrison of the Museum of Comparative Zoology; Jim Patton and Christopher Conroy of the Museum of Vertebrate Zoology; and Olavi Gronwall of the Swedish Museum of Natural History.; The Smithsonian Institution's National Museum of Natural History served as our most important base during the completion of this study, and we thank Don Wilson, Linda Gordon, Michael Carleton, Richard Thorington, Louise Emmons, Alfred Gardner, Neal Woodman, James Mead, Craig Ludwig, Charles Potter, Robert Hoffmann, Robert Fisher, Suzanne Peurach, Jeremy Jacobs, Dave Schmidt, Helen Kafka, and John Ososky for their support, assistance, and camaraderie there. For opening their homes to us during travels to other museums, we thank especially Chris and Nellie Smeenk, Allen Allison and Isabela Forster, Nathan Campeau, Conan and Ellie Yuan, Christopher Trapani, Angela Chien, Yance and Evy de Fretes, Ken Aplin and Angela Frost, Juliette Pasveer, Sarah Redmond, Pawel Nowak, Richard and Nora Wells, Jacob and Elizabeth Davis, Neal Evenhuis, Ucok Sinaga, Martin Copley, Emma Teeling, Craig Chosiad, Elizabeth Waterhouse, Michael Brody, Pavel German and Elizabeth Tasker, Tim Flannery and Alex Szalay, Russell, Kaye, and Emma Baudinette, Jonathan and Arlene Andron, Howard, Kari, Katherine, and Michael Helgen, and Geoffrey, Gail, and Brian Johnston. NR 160 TC 17 Z9 17 U1 1 U2 3 PU AMER MUSEUM NATURAL HISTORY PI NEW YORK PA ATTN: LIBRARY-SCIENTIFIC PUBLICATIONS DISTRIBUTION, CENTRAL PK WEST AT 79TH ST, NEW YORK, NY 10024-5192 USA SN 0003-0090 EI 1937-3546 J9 B AM MUS NAT HIST JI Bull. Amer. Mus. Nat. Hist. PY 2009 IS 331 BP 230 EP 313 PG 84 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 535JD UT WOS:000272963500009 ER PT J AU Miller, JS AF Miller, James S. TI GENERIC REVISION OF THE DIOPTINAE (LEPIDOPTERA: NOCTUOIDEA: NOTODONTIDAE) PART 2: JOSIINI SO BULLETIN OF THE AMERICAN MUSEUM OF NATURAL HISTORY LA English DT Review ID HIGHER-LEVEL PHYLOGENY; HOST-PLANT SPECIALIZATION; DNA-SEQUENCE DATA; HELICONIUS BUTTERFLIES; NYMPHALIDAE LEPIDOPTERA; MOTHS LEPIDOPTERA; EXTERNAL MORPHOLOGY; CLADISTIC-ANALYSIS; TRICHOPLUSIA-NI; PHRYGANIDIA-CALIFORNICA C1 [Miller, James S.] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Amer Museum Nat Hist,Div Invertebrate Zool, Washington, DC 20560 USA. RP Miller, JS (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Amer Museum Nat Hist,Div Invertebrate Zool, Washington, DC 20560 USA. EM jmiller@amnh.org NR 537 TC 0 Z9 0 U1 1 U2 2 PU AMER MUSEUM NATURAL HISTORY PI NEW YORK PA ATTN: LIBRARY-SCIENTIFIC PUBLICATIONS DISTRIBUTION, CENTRAL PK WEST AT 79TH ST, NEW YORK, NY 10024-5192 USA SN 0003-0090 EI 1937-3546 J9 B AM MUS NAT HIST JI Bull. Amer. Mus. Nat. Hist. PY 2009 IS 321 BP 675 EP + DI 10.1206/321.1-1 PG 328 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 468EE UT WOS:000267797000001 ER PT J AU Graves, GR AF Graves, Gary R. TI Skeletal correlates of body weight in the Black-billed Streamertail (Trochilus scitulus) of Jamaica SO CARIBBEAN JOURNAL OF SCIENCE LA English DT Article DE Body size index; hummingbirds; museum specimens; Trochilidae; Trochilus scitulus ID FOOD PASSAGE; HUMMINGBIRDS; FLIGHT; MORPHOLOGY; ELEVATION; MODEL AB Analyses of body size evolution in hummingbirds (Trochilidae) are hampered by the lack of standardized weight data for most of the 330 described species. Moreover, little is known of the morphological correlates of body weight upon which a body-size index could be constructed. I investigated the skeletal correlates of body weight in the endemic Black-billed Streamertail (Trochilus scitulus) of Jamaica. Mist-netted males were weighed at initial capture and after the holding period (2.1-6.7 hr). Seven of 10 skeletal characters exhibited marginally higher correlations with the second measure of body weight, which was unbiased by gut contents. Sternum length emerged as the single best skeletal predictor of body weight. A multivariate index (PCA 1) derived from three sternal characters had approximately the same predictive value as a comparable analysis of all ten skeletal characters. This suggests that a simple multivariate measure of sternal morphology may provide a reliable body size index for hummingbirds. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20013 USA. RP Graves, GR (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, MRC 116,POB 37012, Washington, DC 20013 USA. FU Animal Care and Use Committee, National Museum of Natural History; National Museum of Natural History FX Research and export permits were issued by the National Environmental Planning Agency, Kingston (Yvette Strong, Andrea Donaldson, Ricardo Miller) and the Jamaica Conservation and Development Trust (Susan Otuokan). Specimens were collected under the auspices of the Animal Care and Use Committee, National Museum of Natural History. I thank Brian Schmidt and Errol Francis for field assistance and Catherine Levy (Kingston) for logistical assistance. Field work was supported by the James Bond and Alexander Wetmore funds of the National Museum of Natural History. NR 21 TC 1 Z9 1 U1 0 U2 2 PU UNIV PUERTO RICO, PI MAYAGUEZ PA COLLEGE ARTS SCIENCES, MAYAGUEZ, PR 00680 USA SN 0008-6452 J9 CARIBB J SCI JI Caribb. J. Sci. PY 2009 VL 45 IS 1 BP 69 EP 72 PG 4 WC Biodiversity Conservation SC Biodiversity & Conservation GA 695VO UT WOS:000285400900009 ER PT J AU Flachsbarth, B Fritzsche, M Weldon, PJ Schulz, S AF Flachsbarth, Birte Fritzsche, Matthias Weldon, Paul J. Schulz, Stefan TI Composition of the Cloacal Gland Secretion of Tuatara, Sphenodon punctatus SO CHEMISTRY & BIODIVERSITY LA English DT Article ID ACCELERATED CONJUGATE ADDITION; SEX ATTRACTING SECRETION; DOUBLE-BOND POSITION; FATTY-ACID ESTERS; VOLATILE COMPONENTS; DIMETHYL DISULFIDE; LIPID-COMPOSITION; MANGIFERA-INDICA; DUNG BEETLE; CONVENIENT AB The lipophilic content of the cloacal gland secretion of the tuatara (Sphenodon punctatus) was investigated. GC/EI-MS Analysis of CH(2)Cl(2) extracts of the secretions revealed triacylglycerols as major glandular constituents. Twelve major medium-chain fatty acids were found to be conjugated to glycerol in different combinations, resulting in complex mixtures. These acids were identified by transesterification and subsequent derivatization of natural samples, and their structures were verified by synthesis. The natural glycerides contain predominantly three of the following acids: octanoic (A), (E)- and (Z)-oct-4-enoic (B and C, resp.), (4E,6Z)-octa-4,6-dicnoic (tuataric acid; D), (R)-2,6-dimethyltheptanoic (E), (R)2,6-dimethylhept-5-enoic (F), (Z)-dec-4-enoic (G), (4Z,7Z)-deca-4,7 dienoic (H), (R)-3,7-dimethyloct-6-enoic (I), (R)-4,8-dimethylnon-7-enoic (J), (2R,6S)-2,6,10-trimethylundece-9-enoic (K), and (2R,5E)-2,6,10-trimethylundeca-5,9-dienoic acids (L). Several additional acids, occurring in trace amounts only, were tentatively identified by MS. The elucidation of the absolute configuration of the acids was performed by GC on chiral phases. Individual tuatara show specific mixtures of glycerides with up to 100 components, The individual mixtures may permit individual recognition because the bouquets seem to be stable over years. C1 [Flachsbarth, Birte; Fritzsche, Matthias; Schulz, Stefan] Tech Univ Carolo Wilhelmina Braunschweig, Inst Organ Chem, D-38106 Braunschweig, Germany. [Weldon, Paul J.] Smithsonian Inst, Conservat & Res Ctr, Front Royal, VA 22630 USA. RP Schulz, S (reprint author), Tech Univ Carolo Wilhelmina Braunschweig, Inst Organ Chem, Hagenring 30, D-38106 Braunschweig, Germany. EM stefan.schulz@tu-bs.de NR 62 TC 4 Z9 4 U1 0 U2 3 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA PO BOX 10 11 61, D-69451 WEINHEIM, GERMANY SN 1612-1872 J9 CHEM BIODIVERS JI Chem. Biodivers. PY 2009 VL 6 IS 1 BP 1 EP 37 PG 37 WC Biochemistry & Molecular Biology; Chemistry, Multidisciplinary SC Biochemistry & Molecular Biology; Chemistry GA 404GD UT WOS:000263138200001 PM 19180453 ER PT S AU Fraisse, AA Brown, JAC Dobler, G Dotson, JL Draine, BT Frisch, PC Haverkorn, M Hirata, CM Jansson, R Lazarian, A Magalhaes, AM Waelkens, A Wolleben, M AF Fraisse, Aurelien A. Brown, Jo-Anne C. Dobler, Gregory Dotson, Jessie L. Draine, Bruce T. Frisch, Priscilla C. Haverkorn, Marijke Hirata, Christopher M. Jansson, Ronnie Lazarian, Alex Magalhaes, Antonio Mario Waelkens, Andre Wolleben, Maik BE Dodelson, S Baumann, D Cooray, A Dunkley, J Fraisse, A Jackson, MG Kogut, A Krauss, L Smith, K Zaldarriaga, M TI Foreground Science Knowledge and Prospects SO CMB POLARIZATION WORKSHOP: THEORY AND FOREGROUNDS: CMBPOL MISSION CONCEPT STUDY SE AIP Conference Proceedings LA English DT Proceedings Paper CT CMB Polarization Workshop CY JUN 23-26, 2008 CL Batavia, IL SP NASA ID GALACTIC MAGNETIC-FIELD; MICROWAVE-ANISOTROPY-PROBE; INTERSTELLAR DUST GRAINS; PULSAR ROTATION MEASURES; SQUARE KILOMETER ARRAY; WARM IONIZED MEDIUM; SPINNING DUST; PLANE SURVEY; RADIATIVE TORQUES; MOLECULAR CLOUDS AB Detecting "B-mode" (i.e., divergence free) polarization in the Cosmic Microwave Background (CMB) would open a new window on the very early Universe. However, the polarized microwave sky is dominated by polarized Galactic dust and synchrotron emissions, which may hinder our ability to test inflationary predictions. In this paper, we report on our knowledge of these "Galactic foregrounds," as well as on how a CMB satellite mission aiming at detecting a primordial B-mode signal ("CMBPol") will contribute to improving it. We review the observational and analysis techniques used to constrain the structure of the Galactic magnetic field, whose presence is responsible for the polarization of Galactic emissions. Although our current understanding of the magnetized interstellar medium is somewhat limited, dramatic improvements in our knowledge of its properties are expected by the time CMBPol flies. Thanks to high resolution and high sensitivity instruments observing the whole sky at frequencies between 30 GHz and 850 GHz, CMBPol will not only improve this picture by observing the synchrotron emission from our galaxy, but also help constrain dust models. Polarized emission from interstellar dust indeed dominates over any other signal in CMBPol's highest frequency channels. Observations at these wavelengths, combined with ground-based studies of starlight polarization, will therefore enable us to improve our understanding of dust properties and of the mechanism(s) responsible for the alignment of dust grains with the Galactic magnetic field. CMBPol will also shed new light on observations that are presently not well understood. Morphological studies of anomalous dust and synchrotron emissions will indeed constrain their natures and properties, while searching for fluctuations in the emission from heliospheric dust will test our understanding of the circumheliospheric interstellar medium. Finally, acquiring more information on the properties of extra-Galactic sources will be necessary in order to maximize the cosmological constraints extracted from CMBPol's observations of CMB lensing. C1 [Fraisse, Aurelien A.; Draine, Bruce T.] Princeton Univ Observ, Peyton Hall, Princeton, NJ 08544 USA. [Brown, Jo-Anne C.] Univ Calgary, Centre Radio Astron, Calgary, AB T2N 1N4, Canada. [Dobler, Gregory] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Dotson, Jessie L.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Frisch, Priscilla C.] Univ Chicago, Chicago, IL 60637 USA. [Haverkorn, Marijke] Natl Radio Astron Observ, Edgemont Rd, Charlottesville, VA 22903 USA. [Haverkorn, Marijke] Univ Calif Berkeley, Astron Dept, Berkeley, CA 94720 USA. [Haverkorn, Marijke] ASTRON, NL-7990 AA Dwingeloo, Netherlands. [Hirata, Christopher M.] Caltech, Pasadena, CA 91125 USA. [Jansson, Ronnie] NYU, Dept Phys, Cent Cosmol & Particle Phys, 4 Washington Pl, New York, NY 10003 USA. [Lazarian, Alex] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Magalhaes, Antonio Mario] Univ Sao Paulo, IAG, BR-05508900 Sao Paulo, Brazil. [Waelkens, Andre] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Wolleben, Maik] NRC Herzberg Inst Astrophys, Penticton, BC, Canada. RP Fraisse, AA (reprint author), Princeton Univ Observ, Peyton Hall, Princeton, NJ 08544 USA. EM fraisse@astro.princeton.edu; jessie.dotson@nasa.gov; marijke@astro.berkeley.edu; chirata@tapir.caltech.edu; rj486@nyu.edu; mario@astro.iag.usp.br; waelkens@mpa-garching.mpg.de; maik.wolleben@nrc.gc.ca RI Magalhaes, Antonio Mario/K-9532-2013; OI Draine, Bruce/0000-0002-0846-936X FU NASA Mission Concept Study award [NNX08AT71G S01]; NSF [AST-0707932, AST-0507164]; Princeton University; NSF Center for Magnetic Self Organization in Laboratory and Astrophysical Plasmas; FAPESP; CNPq FX This research was partly funded by NASA Mission Concept Study award NNX08AT71G S01. We also acknowledge the organizational work of the Primordial Polarization Program Definition Team (PPPDT). AAF was supported by NSF grant AST-0707932 and Princeton University. PCF acknowledges support from NASA grant NNX08AJ33G, AL from NSF grant AST-0507164 and the NSF Center for Magnetic Self Organization in Laboratory and Astrophysical Plasmas, and AMM from FAPESP and CNPq. AAF would like 303 to thank D. P. Finkbeiner and J. E. Vaillancourt for their contributions to the CMBPol Theory Workshop held at Fermilab in June 2008, L. A. Page for stimulating discussions, D. N. Spergel for comments on a draft version of this paper, and R. H. Lupton for making the SM plotting program available to him. AMM is grateful to all members of the IAG Polarimetry Group for their continued support. Typesetting of this document was made easier by the use of NASAs Astrophysics Data System Bibliographic Services and of the AASTEX package. All the Planck-related numbers and information referred to in this document are from the Planck scientific program (also known as blue book) available online in PDF format at http://www.rssd.esa.int/planck/. NR 188 TC 6 Z9 6 U1 1 U2 5 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 978-0-7354-0678-0 J9 AIP CONF PROC PY 2009 VL 1141 BP 265 EP + PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BLS44 UT WOS:000270939500006 ER PT B AU Roberts, JM Wheeler, AJ Freiwald, A Cairns, SD AF Roberts, J. Murray Wheeler, Andrew J. Freiwald, Andre Cairns, Stephen D. BA Roberts, JM Wheeler, AJ Freiwald, A Cairns, SD BF Roberts, JM Wheeler, AJ Freiwald, A Cairns, SD TI History and research approaches SO COLD-WATER CORALS: THE BIOLOGY AND GEOLOGY OF DEEP-SEA CORAL HABITATS LA English DT Article; Book Chapter ID COLD-WATER CORAL; DEEP-SEA CORAL; GULF-OF-MEXICO; LOPHELIA-PERTUSA SCLERACTINIA; WESTERN NORTH-ATLANTIC; BELGICA MOUND PROVINCE; CRETACEOUS-TERTIARY BOUNDARY; O-18 ISOTOPIC DISEQUILIBRIUM; PREDICTING SUITABLE HABITAT; CARBONATE-ION CONCENTRATION C1 [Roberts, J. Murray] Scottish Assoc Marine Sci, Oban, Argyll 20560, Scotland. [Wheeler, Andrew J.] Univ Coll Cork, Cork, Ireland. [Freiwald, Andre] Univ Erlangen Nurnberg, Erlangen, Germany. [Cairns, Stephen D.] Smithsonian Inst, Washington, DC USA. NR 805 TC 2 Z9 3 U1 0 U2 0 PU CAMBRIDGE UNIV PRESS PI CAMBRIDGE PA THE PITT BUILDING, TRUMPINGTON ST, CAMBRIDGE CB2 1RP, CAMBS, ENGLAND BN 978-0-521-88485-3 PY 2009 BP 1 EP + D2 10.1017/CBO9780511581588 PG 66 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA BKJ97 UT WOS:000268336000001 ER PT B AU Roberts, JM Wheeler, A Freiwald, A Cairns, SD AF Roberts, J. Murray Wheeler, Andrew J. Freiwald, Andre Cairns, Stephen D. BA Roberts, JM Wheeler, AJ Freiwald, A Cairns, SD BF Roberts, JM Wheeler, AJ Freiwald, A Cairns, SD TI Cold-water corals SO COLD-WATER CORALS: THE BIOLOGY AND GEOLOGY OF DEEP-SEA CORAL HABITATS LA English DT Article; Book Chapter C1 [Roberts, J. Murray] Scottish Assoc Marine Sci, Oban, Argyll, Scotland. [Wheeler, Andrew J.] Univ Coll Cork, Cork, Ireland. [Freiwald, Andre] Univ Erlangen Nurnberg, Erlangen, Germany. [Cairns, Stephen D.] Smithsonian Inst, Washington, DC USA. NR 0 TC 0 Z9 0 U1 0 U2 5 PU CAMBRIDGE UNIV PRESS PI CAMBRIDGE PA THE PITT BUILDING, TRUMPINGTON ST, CAMBRIDGE CB2 1RP, CAMBS, ENGLAND BN 978-0-521-88485-3 PY 2009 BP 20 EP 66 DI 10.1017/CBO9780511581588.003 D2 10.1017/CBO9780511581588 PG 47 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA BKJ97 UT WOS:000268336000002 ER PT B AU Roberts, JM Wheeler, AJ Freiwald, A Cairns, SD AF Roberts, J. Murray Wheeler, Andrew J. Freiwald, Andre Cairns, Stephen D. BA Roberts, JM Wheeler, AJ Freiwald, A Cairns, SD BF Roberts, JM Wheeler, AJ Freiwald, A Cairns, SD TI Biology SO COLD-WATER CORALS: THE BIOLOGY AND GEOLOGY OF DEEP-SEA CORAL HABITATS LA English DT Article; Book Chapter C1 [Roberts, J. Murray] Scottish Assoc Marine Sci, Oban, Argyll, Scotland. [Wheeler, Andrew J.] Univ Coll Cork, Cork, Ireland. [Freiwald, Andre] Univ Erlangen Nurnberg, Erlangen, Germany. [Cairns, Stephen D.] Smithsonian Inst, Washington, DC USA. NR 0 TC 0 Z9 0 U1 0 U2 2 PU CAMBRIDGE UNIV PRESS PI CAMBRIDGE PA THE PITT BUILDING, TRUMPINGTON ST, CAMBRIDGE CB2 1RP, CAMBS, ENGLAND BN 978-0-521-88485-3 PY 2009 BP 67 EP 107 DI 10.1017/CBO9780511581588.004 D2 10.1017/CBO9780511581588 PG 41 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA BKJ97 UT WOS:000268336000003 ER PT B AU Roberts, JM Wheeler, AJ Freiwald, A Cairns, SD AF Roberts, J. Murray Wheeler, Andrew J. Freiwald, Andre Cairns, Stephen D. BA Roberts, JM Wheeler, AJ Freiwald, A Cairns, SD BF Roberts, JM Wheeler, AJ Freiwald, A Cairns, SD TI Reefs and mounds SO COLD-WATER CORALS: THE BIOLOGY AND GEOLOGY OF DEEP-SEA CORAL HABITATS LA English DT Article; Book Chapter C1 [Roberts, J. Murray] Scottish Assoc Marine Sci, Oban, Argyll, Scotland. [Wheeler, Andrew J.] Univ Coll Cork, Cork, Ireland. [Freiwald, Andre] Univ Erlangen Nurnberg, Erlangen, Germany. [Cairns, Stephen D.] Smithsonian Inst, Washington, DC USA. NR 0 TC 0 Z9 0 U1 0 U2 2 PU CAMBRIDGE UNIV PRESS PI CAMBRIDGE PA THE PITT BUILDING, TRUMPINGTON ST, CAMBRIDGE CB2 1RP, CAMBS, ENGLAND BN 978-0-521-88485-3 PY 2009 BP 108 EP 141 DI 10.1017/CBO9780511581588.005 D2 10.1017/CBO9780511581588 PG 34 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA BKJ97 UT WOS:000268336000004 ER PT B AU Roberts, JM Wheeler, AJ Freiwald, A Cairns, SD AF Roberts, J. Murray Wheeler, Andrew J. Freiwald, Andre Cairns, Stephen D. BA Roberts, JM Wheeler, AJ Freiwald, A Cairns, SD BF Roberts, JM Wheeler, AJ Freiwald, A Cairns, SD TI Habitats and ecology SO COLD-WATER CORALS: THE BIOLOGY AND GEOLOGY OF DEEP-SEA CORAL HABITATS LA English DT Article; Book Chapter C1 [Roberts, J. Murray] Scottish Assoc Marine Sci, Oban, Argyll, Scotland. [Wheeler, Andrew J.] Univ Coll Cork, Cork, Ireland. [Freiwald, Andre] Univ Erlangen Nurnberg, Erlangen, Germany. [Cairns, Stephen D.] Smithsonian Inst, Washington, DC USA. NR 0 TC 2 Z9 2 U1 0 U2 2 PU CAMBRIDGE UNIV PRESS PI CAMBRIDGE PA THE PITT BUILDING, TRUMPINGTON ST, CAMBRIDGE CB2 1RP, CAMBS, ENGLAND BN 978-0-521-88485-3 PY 2009 BP 142 EP 174 DI 10.1017/CBO9780511581588.006 D2 10.1017/CBO9780511581588 PG 33 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA BKJ97 UT WOS:000268336000005 ER PT B AU Roberts, JM Wheeler, AJ Freiwald, A Cairns, SD AF Roberts, J. Murray Wheeler, Andrew J. Freiwald, Andre Cairns, Stephen D. BA Roberts, JM Wheeler, AJ Freiwald, A Cairns, SD BF Roberts, JM Wheeler, AJ Freiwald, A Cairns, SD TI Palaeontology SO COLD-WATER CORALS: THE BIOLOGY AND GEOLOGY OF DEEP-SEA CORAL HABITATS LA English DT Article; Book Chapter C1 [Roberts, J. Murray] Scottish Assoc Marine Sci, Oban, Argyll, Scotland. [Wheeler, Andrew J.] Univ Coll Cork, Cork, Ireland. [Freiwald, Andre] Univ Erlangen Nurnberg, Erlangen, Germany. [Cairns, Stephen D.] Smithsonian Inst, Washington, DC USA. NR 0 TC 0 Z9 0 U1 0 U2 1 PU CAMBRIDGE UNIV PRESS PI CAMBRIDGE PA THE PITT BUILDING, TRUMPINGTON ST, CAMBRIDGE CB2 1RP, CAMBS, ENGLAND BN 978-0-521-88485-3 PY 2009 BP 175 EP 209 DI 10.1017/CBO9780511581588.007 D2 10.1017/CBO9780511581588 PG 35 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA BKJ97 UT WOS:000268336000006 ER PT B AU Roberts, JM Wheeler, AJ Freiwald, A Cairns, SD AF Roberts, J. Murray Wheeler, Andrew J. Freiwald, Andre Cairns, Stephen D. BA Roberts, JM Wheeler, AJ Freiwald, A Cairns, SD BF Roberts, JM Wheeler, AJ Freiwald, A Cairns, SD TI Corals as archives SO COLD-WATER CORALS: THE BIOLOGY AND GEOLOGY OF DEEP-SEA CORAL HABITATS LA English DT Article; Book Chapter C1 [Roberts, J. Murray] Scottish Assoc Marine Sci, Oban, Argyll, Scotland. [Wheeler, Andrew J.] Univ Coll Cork, Cork, Ireland. [Freiwald, Andre] Univ Erlangen Nurnberg, Erlangen, Germany. [Cairns, Stephen D.] Smithsonian Inst, Washington, DC USA. RI Roberts, Murray/D-8299-2013 OI Roberts, Murray/0000-0003-1688-5133 NR 0 TC 0 Z9 0 U1 0 U2 3 PU CAMBRIDGE UNIV PRESS PI CAMBRIDGE PA THE PITT BUILDING, TRUMPINGTON ST, CAMBRIDGE CB2 1RP, CAMBS, ENGLAND BN 978-0-521-88485-3 PY 2009 BP 210 EP 236 DI 10.1017/CBO9780511581588.008 D2 10.1017/CBO9780511581588 PG 27 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA BKJ97 UT WOS:000268336000007 ER PT B AU Roberts, JM Wheeler, AJ Freiwald, A Cairns, SD AF Roberts, J. Murray Wheeler, Andrew J. Freiwald, Andre Cairns, Stephen D. BA Roberts, JM Wheeler, AJ Freiwald, A Cairns, SD BF Roberts, JM Wheeler, AJ Freiwald, A Cairns, SD TI Impacts and conservation SO COLD-WATER CORALS: THE BIOLOGY AND GEOLOGY OF DEEP-SEA CORAL HABITATS LA English DT Article; Book Chapter C1 [Roberts, J. Murray] Scottish Assoc Marine Sci, Oban, Argyll, Scotland. [Wheeler, Andrew J.] Univ Coll Cork, Cork, Ireland. [Freiwald, Andre] Univ Erlangen Nurnberg, Erlangen, Germany. [Cairns, Stephen D.] Smithsonian Inst, Washington, DC USA. NR 0 TC 1 Z9 1 U1 0 U2 1 PU CAMBRIDGE UNIV PRESS PI CAMBRIDGE PA THE PITT BUILDING, TRUMPINGTON ST, CAMBRIDGE CB2 1RP, CAMBS, ENGLAND BN 978-0-521-88485-3 PY 2009 BP 237 EP 262 DI 10.1017/CBO9780511581588.009 D2 10.1017/CBO9780511581588 PG 26 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA BKJ97 UT WOS:000268336000008 ER PT S AU Meibom, S AF Meibom, Soren BE Stempels, E TI Young Cool Stars Divided on the Issue of Rotation SO COOL STARS, STELLAR SYSTEMS AND THE SUN SE AIP Conference Proceedings LA English DT Proceedings Paper CT 15th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun CY JUL 21-25, 2008 CL St Andrews, SCOTLAND SP Royal Astron Soc, Scottish Univ Phys Alliance, European Space Agcy, NASA Astrobiol Inst DE Stars: late-type; rotation ID LOW-MASS STARS; WIYN OPEN CLUSTER; STELLAR RADIAL-VELOCITIES; SOLAR-TYPE; ANGULAR-MOMENTUM; EVOLUTION; GYROCHRONOLOGY; PLEIADES; M35; AGE AB We present the results of a combination of new stellar rotation periods and extensive information about membership in the young open clusters M 35 and M 34. The observations show that late-type members of both M 35 and M 34 divide into two distinct groups, each with a different dependence of rotation on mass (color). We discuss these new results in the context of existing rotation data for cool stars in older clusters, with a focus on the dependence of rotation on mass and age. We mention briefly tests of rotation as an "astronomical clock" (gyrochronology), and our plans to use the Kepler space mission to push observations of stellar rotation periods beyond the age of the Hyades and the Sun. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Meibom, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 22 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 978-0-7354-0627-8 J9 AIP CONF PROC PY 2009 VL 1094 BP 95 EP 101 PG 7 WC Astronomy & Astrophysics; Physics, Applied SC Astronomy & Astrophysics; Physics GA BJC67 UT WOS:000264752500012 ER PT S AU Saar, SH AF Saar, Steven H. BE Stempels, E TI The Radial Velocity Effects of Stellar Surface Phenomena SO COOL STARS, STELLAR SYSTEMS AND THE SUN SE AIP Conference Proceedings LA English DT Proceedings Paper CT 15th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun CY JUL 21-25, 2008 CL St Andrews, SCOTLAND SP Royal Astron Soc, Scottish Univ Phys Alliance, European Space Agcy, NASA Astrobiol Inst DE stars: planetary systems; stars: activity; stars: spots; convection; techniques: radial velocities ID CHROMOSPHERIC EVAPORATION; MAGNETIC ACTIVITY; ACTIVE REGIONS; PLANET-SEARCH; NO PLANET; VARIABILITY; STARS; FLARE; EXOPLANETS; HYADES AB Radial velocity (RV) studies have been a very successful tool for finding and characterizing extrasolar planets. As RV precision increases, and planet searches press to younger, hotter, and evolved stars, however, this method will snore and more bump against limitations set by the host stars themselves. Cool stellar surfaces present a range of troublesome phenomena such as spots, plage, and convective cells. which can confuse RV measurements. I review how these phenomena affect precision RV, scaling laws and timescales which characterize their properties, and some methods to mitigate, circumvent, or correct for their effects. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Saar, SH (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. NR 35 TC 10 Z9 10 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 978-0-7354-0627-8 J9 AIP CONF PROC PY 2009 VL 1094 BP 152 EP 161 PG 10 WC Astronomy & Astrophysics; Physics, Applied SC Astronomy & Astrophysics; Physics GA BJC67 UT WOS:000264752500020 ER PT S AU Yeates, AR Mackay, DH van Ballegooijen, AA AF Yeates, A. R. Mackay, D. H. van Ballegooijen, A. A. BE Stempels, E TI A Prominence Puzzle Explained? SO COOL STARS, STELLAR SYSTEMS AND THE SUN SE AIP Conference Proceedings LA English DT Proceedings Paper CT 15th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun CY JUL 21-25, 2008 CL St Andrews, SCOTLAND SP Royal Astron Soc, Scottish Univ Phys Alliance, European Space Agcy, NASA Astrobiol Inst DE Sun: magnetic fields; Sun: corona; Sun: prominences ID GLOBAL SOLAR CORONA; MAGNETIC-FIELDS; CHIRALITY; EVOLUTION AB Long-standing observations reveal a global organisation of the magnetic field direction in solar prominences (aka filaments), large clouds of cool dense: plasma suspended in the Sun's hot corona. However, theorists have thus far been unable to explain the origin of this hemispheric pattern. In particular. simple shearing by large-scale surface motions would appear to lead to the wrong magnetic field direction. To explain the observations, we have developed a new model of the global magnetic field evolution in the solar corona over six months. For the first time our model can follow the build-up of magnetic helicity and shear on a global scale, driven by flux emergence and surface motions. The model is successful in predicting the correct magnetic field direction in the vast majority of prominences tested, and has enabled us to determine the key physical mechanisms behind the mysterious hemispheric pattern. C1 [Yeates, A. R.; Mackay, D. H.] Univ St Andrews, Sch Math & Stat, St Andrews KY16 9SS, Fife, Scotland. [van Ballegooijen, A. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Yeates, AR (reprint author), Univ St Andrews, Sch Math & Stat, St Andrews KY16 9SS, Fife, Scotland. RI Yeates, Anthony/D-1338-2014; OI Yeates, Anthony/0000-0002-2728-4053; van Ballegooijen, Adriaan/0000-0002-5622-3540 FU UK STFC; SRIF/STFC FX Financial support for ARY and DHM was provided by the UK STFC. The simulations were performed on the UKMHD parallel computer in St Andrews, funded jointly by SRIF/STFC. Synoptic magnetogram data from NSO/Kitt Peak was produced cooperatively by NSF/NOAO, NASA/GSFC, and NOAA/SEL, and made publicly accessible on the World Wide Web. We thank S.F. Martin for supplying the original filament data set from BBSO/NJIT. NR 13 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 978-0-7354-0627-8 J9 AIP CONF PROC PY 2009 VL 1094 BP 216 EP + PG 2 WC Astronomy & Astrophysics; Physics, Applied SC Astronomy & Astrophysics; Physics GA BJC67 UT WOS:000264752500028 ER PT S AU Dupree, AK AF Dupree, A. K. BE Stempels, E TI Summary Highlights from Cool Stars 15 SO COOL STARS, STELLAR SYSTEMS AND THE SUN SE AIP Conference Proceedings LA English DT Proceedings Paper CT 15th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun CY JUL 21-25, 2008 CL St Andrews, SCOTLAND SP Royal Astron Soc, Scottish Univ Phys Alliance, European Space Agcy, NASA Astrobiol Inst DE Sun; stars; planets; young stars AB A Summary of some scientific highlights of Cool Stars 15 and reflections, as well as awards and a quiz for the participants. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Dupree, AK (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 1 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 978-0-7354-0627-8 J9 AIP CONF PROC PY 2009 VL 1094 BP 299 EP 306 PG 8 WC Astronomy & Astrophysics; Physics, Applied SC Astronomy & Astrophysics; Physics GA BJC67 UT WOS:000264752500038 ER PT S AU Shukla, SJ Weintrau, D Kastner, J Huenemoerder, D Schulz, N Testa, P AF Shukla, Sonali J. Weintrau, David Kastner, Joel Huenemoerder, David Schulz, Norbert Testa, Paola BE Stempels, E TI Characterization of X-ray emission from T Tauri Stars SO COOL STARS, STELLAR SYSTEMS AND THE SUN SE AIP Conference Proceedings LA English DT Proceedings Paper CT 15th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun CY JUL 21-25, 2008 CL St Andrews, SCOTLAND SP Royal Astron Soc, Scottish Univ Phys Alliance, European Space Agcy, NASA Astrobiol Inst DE Stars: pre-main sequence; X-rays: stars ID ACCRETION AB We are analyzing high-resolution Chandra ACIS-S/HETGS long integration spectra for a sample of young stars, including classical, weak-lined, and post-T Tauri stars as well as a young main sequence star. We have identified flaring and quiescent periods, based on overall X-ray luminosity, for several of the stars. We have measured line fluxes in the He-like ions separately in the flaring and quiescent epochs to determine forbidden-to-intercombination line ratios. Results from out analysis of four wTTS and one post-T Tauri star with Chandra/HETGS are included in this presentation. The temperature and density diagnostics for V987 Tau indicate that X-rays are emitted by a cool, high density plasma in the quiescent phase. C1 [Shukla, Sonali J.; Weintrau, David] Vanderbilt Univ, Nashville, TN 37203 USA. [Kastner, Joel] Rochester Inst Technol, Rochester, MI USA. [Huenemoerder, David; Schulz, Norbert] MIT, Cambridge, MA 02139 USA. [Testa, Paola] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RP Shukla, SJ (reprint author), Vanderbilt Univ, Nashville, TN 37203 USA. NR 2 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 978-0-7354-0627-8 J9 AIP CONF PROC PY 2009 VL 1094 BP 333 EP + PG 2 WC Astronomy & Astrophysics; Physics, Applied SC Astronomy & Astrophysics; Physics GA BJC67 UT WOS:000264752500045 ER PT S AU Cranmer, SR AF Cranmer, Steven R. BE Stempels, E TI Accretion-driven winds of T Tauri stars: A new generation of models with self-consistent coronal heating and MHD turbulence SO COOL STARS, STELLAR SYSTEMS AND THE SUN SE AIP Conference Proceedings LA English DT Proceedings Paper CT 15th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun CY JUL 21-25, 2008 CL St Andrews, SCOTLAND SP Royal Astron Soc, Scottish Univ Phys Alliance, European Space Agcy, NASA Astrobiol Inst DE accretion; stars: mass loss; stars: pre-main sequence; turbulence; Alfven waves ID POWERED STELLAR WINDS; DISK ACCRETION; LOW-FREQUENCY; ALFVEN WAVES; SOLAR-WIND; EVOLUTION; EMISSION; LINE AB Classical T Tauri stars are observed to be surrounded by both accretion flows and some kind of wind or jet-like outflow. There are several possible explanations of how and where the outflows arise, including disk winds, X-winds, impulsive (CME-like) ejections, and stellar winds. Recent work by Matt and Pudritz has suggested that if there is a stellar wind with a mass loss rate about 0.1 times the accretion rate, the wind may be able to carry away enough angular momentum to keep the stars from being spun up unrealistically by accretion. In this presentation, I show a preliminary set of theoretical models of accretion-driven winds from the polar regions of T Tauri stars. These models are based on recently published self-consistent simulations of the Sun's coronal heating and wind acceleration. In addition to the convection-driven MHD turbulence (which dominates in the solar case), 1 add a source of wave energy at the photosphere that is driven by the impact of plasma in neighboring flux tubes undergoing magnetospheric accretion. This added energy, which is determined quantitatively from the far-field theory of MHD wave generation, seems to be enough to produce T Tauri-like mass loss rates. It is still uncertain, though, whether it is enough to solve the T Tauri angular momentum problem. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Cranmer, SR (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 33 TC 1 Z9 1 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 978-0-7354-0627-8 J9 AIP CONF PROC PY 2009 VL 1094 BP 357 EP 360 PG 4 WC Astronomy & Astrophysics; Physics, Applied SC Astronomy & Astrophysics; Physics GA BJC67 UT WOS:000264752500051 ER PT S AU Irwin, J Charbonneau, D Nutzman, P Falco, E AF Irwin, Jonathan Charbonneau, David Nutzman, Philip Falco, Emilio BE Stempels, E TI The MEarth project: searching for transiting habitable super-Earth planets around nearby M-dwarfs SO COOL STARS, STELLAR SYSTEMS AND THE SUN SE AIP Conference Proceedings LA English DT Proceedings Paper CT 15th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun CY JUL 21-25, 2008 CL St Andrews, SCOTLAND SP Royal Astron Soc, Scottish Univ Phys Alliance, European Space Agcy, NASA Astrobiol Inst DE telescopes; stars: late-type; stars: low-mass, brown dwarfs; planetary systems ID CATALOG; STARS AB Due to their small radii, M-dwarfs are very promising targets to search for transiting super-Earths, with a planet of 2 Earth radii orbiting an M5 dwarf in the habitable zone giving rise to a 0.5% photometric signal, with a period of two weeks. This can be detected from the ground using modest-aperture telescopes by targeting samples of nearby M-dwarfs. Such planets would be very amenable to follow-up studies due to the brightness of the parent stars, and the favourable planet. star flux ratio. MEarth is such a transit survey of similar to 2000 nearby M-dwarfs. Since the targets are distributed over the entire (Northern) sky, it is necessary to observe them individually, which will be done by using 8 independent 0.4m robotic telescopes, two of which have been in operation since December 2007 at the Fred Lawrence Whipple Observatory (FLWO) located on Mount Hopkins, Arizona. We discuss the survey design and hardware, and report on the current status of the survey, and preliminary results obtained from the commissioning data. C1 [Irwin, Jonathan; Charbonneau, David; Nutzman, Philip] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Falco, Emilio] Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. RP Irwin, J (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. FU David and Lucile Packard Fellowship for Science and Engineering; U.S. National Science Foundation; National Aeronautics and Space Administration; National Science Foundation FX It is a pleasure to acknowledge the assistance of the staff at the Fred Lawrence Whipple Observatory in Arizona, and the Harvard-Smithsonian Center for Astrophysics. We acknowledge funding from the David and Lucile Packard Fellowship for Science and Engineering and the U.S. National Science Foundation. This work 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. NR 4 TC 9 Z9 9 U1 0 U2 3 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 978-0-7354-0627-8 J9 AIP CONF PROC PY 2009 VL 1094 BP 445 EP + PG 2 WC Astronomy & Astrophysics; Physics, Applied SC Astronomy & Astrophysics; Physics GA BJC67 UT WOS:000264752500073 ER PT S AU Caramazza, M Flaccomio, E Prisinzano, L Rebull, L Sciortino, S Stauffer, JR Wolk, S Micela, G AF Caramazza, M. Flaccomio, E. Prisinzano, L. Rebull, L. Sciortino, S. Stauffer, J. R. Wolk, S. Micela, G. BE Stempels, E TI X-ray emission in the Outer Galaxy: the Star Forming Region NGC 1893 SO COOL STARS, STELLAR SYSTEMS AND THE SUN SE AIP Conference Proceedings LA English DT Proceedings Paper CT 15th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun CY JUL 21-25, 2008 CL St Andrews, SCOTLAND SP Royal Astron Soc, Scottish Univ Phys Alliance, European Space Agcy, NASA Astrobiol Inst DE Stars: activity; coronae; flare; pre-main sequence; late-type - X-ray: stars AB A key issue of the star formation process is its independence from the environmental conditions. In particular. it is not clear whether star formation in the outer Galaxy occurs in the same way as in the inner Galaxy. We present preliminary result, of the analysis of a similar to 440Ks ACIS-Chandra observation of NGC 1893, a young cluster(similar to 3-4Myrs), far away from the Galactic Center with the aim to study star formation in the outer region of the Galaxy and investigate the coronal properties of the cluster stars. We detect more than 1000 X-ray sources. most of which arc likely cluster members. We present also a preliminary analysis of X-ray variability of the cluster stars. C1 [Caramazza, M.] Univ Palermo, Dipartimento Sci Fis & Astron, Via Archirafi 36, I-90123 Palermo, Italy. [Caramazza, M.; Flaccomio, E.; Prisinzano, L.; Sciortino, S.; Micela, G.] INAF Osservatorio Astron Palermo, I-90134 Palermo, Italy. [Stauffer, J. R.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Wolk, S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Caramazza, M (reprint author), Univ Palermo, Dipartimento Sci Fis & Astron, Via Archirafi 36, I-90123 Palermo, Italy. OI Flaccomio, Ettore/0000-0002-3638-5788; Prisinzano, Loredana/0000-0002-8893-2210; Micela, Giuseppina/0000-0002-9900-4751; Wolk, Scott/0000-0002-0826-9261; Rebull, Luisa/0000-0001-6381-515X FU ASI-INAF [I/023/05/0]; European Commission [MRTN-CT-2006-035890] FX We acknowledge financial contribution from contract ASI-INAF I/023/05/0 and from European Commission (contract N. MRTN-CT-2006-035890).; This work is based on observations made with the Chandra Telescope. NR 8 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 978-0-7354-0627-8 J9 AIP CONF PROC PY 2009 VL 1094 BP 580 EP + PG 2 WC Astronomy & Astrophysics; Physics, Applied SC Astronomy & Astrophysics; Physics GA BJC67 UT WOS:000264752500107 ER PT S AU Desai, P Beiersdorfer, P Brickhouse, NS Gu, MF Lepson, JK AF Desai, P. Beiersdorfer, P. Brickhouse, N. S. Gu, M. F. Lepson, J. K. BE Stempels, E TI Status of Line identifications in the Chandra LETG Spectrum of Procyon SO COOL STARS, STELLAR SYSTEMS AND THE SUN SE AIP Conference Proceedings LA English DT Proceedings Paper CT 15th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun CY JUL 21-25, 2008 CL St Andrews, SCOTLAND SP Royal Astron Soc, Scottish Univ Phys Alliance, European Space Agcy, NASA Astrobiol Inst DE Stars: coronae; X-rays; techniques: spectroscopic; atomic data; plasmas ID EXTREME-ULTRAVIOLET; EMISSION-LINES; REGION; VII; ANGSTROM AB We report on our ongoing efforts to produce a relatively complete set of Xray emission lines present in the Low Energy Transmission Grating (LETG) spectra of Procyon. In addition to using recently reprocessed HRC-S/LETG spectra of Procyon, we use LETG spectra of Capella, along with recent Electron Bean Ion Trap (EBIT) laboratory data and new Flexible Atomic Code (FAC) calculations to identify the wealth of weaker lines present in the spectrum. Experimental measurements at the EBIT-I and EBIT-II facilities at Livermore of astrophysically abundant elements (Fe VII-Fe X, Lepson et al. 2002, Ar IX- Ar XVI, Lepson et al 2003, S VII- S XIV, Lepson et al 2004) and new FAC calculations of Mg and Ne (Gu, 2008 in press) provide an opportunity to identify many of the previously unassigned lines in Procyon (Raassen et al, 2002). C1 [Desai, P.; Beiersdorfer, P.; Brickhouse, N. S.; Gu, M. F.; Lepson, J. K.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 96620 USA. [Beiersdorfer, P.; Gu, M. F.] Lawrence Livermore Natl Lab, POB 5508, Livermore, CA 94550 USA. [Brickhouse, N. S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02140 USA. RP Desai, P (reprint author), Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 96620 USA. OI Brickhouse, Nancy/0000-0002-8704-4473 FU NASA [AR7-8801X]; DOE [DE-AC53-07NA27344]; Chandra X-ray Center FX Work supported by NASA through Chandra Award AR7-8801X. Work at LLNL was performed under the auspices of DOE under contract DE-AC53-07NA27344. N. S.Brickhouse acknowledges support from the Chandra X-ray Center. NR 13 TC 2 Z9 2 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 978-0-7354-0627-8 J9 AIP CONF PROC PY 2009 VL 1094 BP 588 EP + PG 2 WC Astronomy & Astrophysics; Physics, Applied SC Astronomy & Astrophysics; Physics GA BJC67 UT WOS:000264752500109 ER PT S AU Saar, S Farid, S Deluca, E AF Saar, S. Farid, S. Deluca, E. BE Stempels, E TI Thermal Anal Statistical Properties of X-ray Bright Points SO COOL STARS, STELLAR SYSTEMS AND THE SUN SE AIP Conference Proceedings LA English DT Proceedings Paper CT 15th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun CY JUL 21-25, 2008 CL St Andrews, SCOTLAND SP Royal Astron Soc, Scottish Univ Phys Alliance, European Space Agcy, NASA Astrobiol Inst DE Sun: X-rays; Sun: Corona AB HINODE's X-ray Telescope (XRT) offers a unique combination of high spatial (approximate to 2 '') and thermal resolution, full-Sun observations of the solar corona over a wide range of temperatures (5.8 similar to < log T similar to < 7.6). We use mufti-filter Hinode/XRT data to explore the thermal, satistical and spatial properties of X-ray bright points (XBPs). We have developed an automated XBP finder to study BPs over two periods during November 2007 and May 2008. We detect somewhat fewer XBPs than SOHO EIT in 195 angstrom but find comparable values to the 284 angstrom band. This is likely due in some part to the somewhat stricter requirements on XBP shape and enhancement above local background that we have adopted. We find that most XBPs appear to be relatively cool on average (log T approximate to 6.1), only slightly hotter than the average quiet Sun. There is a trend for larger XBPs to be holler, with a sub-class of XBPs which are hotter still at all sizes. We further investigate the spatial distribution of XBPs, in particular exploring whether the "overhot" XBPs have any tendency to appear in or near coronal holes. We find that there appears to be a notable trend of overhot bright points within the two data sets and a tendency of those to lie within 40 '' of coronal holes. C1 [Saar, S.; Farid, S.; Deluca, E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Saar, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI DeLuca, Edward/L-7534-2013 OI DeLuca, Edward/0000-0001-7416-2895 NR 10 TC 4 Z9 4 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 978-0-7354-0627-8 J9 AIP CONF PROC PY 2009 VL 1094 BP 756 EP 759 PG 4 WC Astronomy & Astrophysics; Physics, Applied SC Astronomy & Astrophysics; Physics GA BJC67 UT WOS:000264752500151 ER PT S AU Bruntt, H Penny, AJ Stello, D Evans, NR Eaton, JA AF Bruntt, H. Penny, A. J. Stello, D. Evans, N. R. Eaton, J. A. BE Stempels, E TI Welcome back, Polaris the Cepheid SO COOL STARS, STELLAR SYSTEMS AND THE SUN SE AIP Conference Proceedings LA English DT Proceedings Paper CT 15th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun CY JUL 21-25, 2008 CL St Andrews, SCOTLAND SP Royal Astron Soc, Scottish Univ Phys Alliance, European Space Agcy, NASA Astrobiol Inst DE Stars: individual: Polaris (alpha UMi); Stars: variable: Cepheids; Stellar evolution ID RADIAL-VELOCITY; PERIOD CHANGE; AMPLITUDE AB For about 100)ears the amplitude of the 4d pulsation in Polaris has decreased. We present new results showing a significant increase in the amplitude based on 4.5 years of continuous monitoring from the ground and with two satellite missions. C1 [Bruntt, H.; Stello, D.] Univ Sydney, Sch Phys A29, Inst Astron, Sydney, NSW 2006, Australia. [Penny, A. J.] Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. [Evans, N. R.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Eaton, J. A.] Tennessee State Univ, Ctr Excellence Informat Syst, Nashville, TN 37209 USA. RP Bruntt, H (reprint author), Univ Sydney, Sch Phys A29, Inst Astron, Sydney, NSW 2006, Australia. NR 18 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 978-0-7354-0627-8 J9 AIP CONF PROC PY 2009 VL 1094 BP 884 EP + PG 2 WC Astronomy & Astrophysics; Physics, Applied SC Astronomy & Astrophysics; Physics GA BJC67 UT WOS:000264752500183 ER PT S AU Wolk, SJ AF Wolk, Scott J. CA SOXS Consortium BE Stempels, E TI A Spitzer, Orion A, XMM-Newton Survey: SOXS SO COOL STARS, STELLAR SYSTEMS AND THE SUN SE AIP Conference Proceedings LA English DT Proceedings Paper CT 15th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun CY JUL 21-25, 2008 CL St Andrews, SCOTLAND SP Royal Astron Soc, Scottish Univ Phys Alliance, European Space Agcy, NASA Astrobiol Inst DE Star Formation; Clusters: Lynds 1641; Facilities: XMM-Newton; Facilities: Spitzer Space Telescope ID CLUSTER AB We report on art XMM-Newton survey of the L 1641 region, covering 3.5x0.5 degrees, just south of the Orion Nebular Cluster. This survey is a companion to a 3.6-24 mu m survey of the same region using Spitzer. We observed 7 XMM-Newton fields specifically for this program and are augmenting the X-ray data with XMM-Newton archival data on the region surrounding the ONC including OMC 2/3, iota Ori, L1641N V833 Ori and V1118 Ori). The full survey plus archival data constitute an essentially complete XMM-Newton survey of the Orion A cloud. The XMM Observations were completed in March 2008. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Wolk, SJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Wolk, Scott/0000-0002-0826-9261 NR 4 TC 2 Z9 2 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 978-0-7354-0627-8 J9 AIP CONF PROC PY 2009 VL 1094 BP 959 EP 962 PG 4 WC Astronomy & Astrophysics; Physics, Applied SC Astronomy & Astrophysics; Physics GA BJC67 UT WOS:000264752500202 ER PT S AU Bochanski, JJ Hawley, SL Reid, IN Covey, KR West, AA Golimowski, DA Ivezic, Z AF Bochanski, John J. Hawley, Suzanne L. Reid, I. Neill Covey, Kevin R. West, Andrew A. Golimowski, David A. Ivezic, Zeljko BE Stempels, E TI Our Nearest 15 Million Neighbors: The Field Low-Mass Stellar Luminosity and Mass Functions SO COOL STARS, STELLAR SYSTEMS AND THE SUN SE AIP Conference Proceedings LA English DT Proceedings Paper CT 15th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun CY JUL 21-25, 2008 CL St Andrews, SCOTLAND SP Royal Astron Soc, Scottish Univ Phys Alliance, European Space Agcy, NASA Astrobiol Inst DE stars: low mass; stars: fundamental parameters; stars: M dwarfs; stars: luminosity function; stars: mass function; Galaxy: structure ID SKY SURVEY; STARS; IV AB We report on a new measurement of the luminosity function (LF) and mass function (MF) of field low-mass dwarfs using Sloan Digital Sky Survey (SDSS) photometry. The final catalog is composed of similar to 15 mullion low-mass stars (0.1 M-circle dot < M < 0.8 M-circle dot), spread over 8,400 square degrees. Distances to the stars are estimated using new photometric parallax relations, constructed from ugriz photometry of nearby low-mass stars with trigonometric parallaxes. The LF is measured with a novel technique, which simultaneously measures Galactic structure and the stellar LF. The resulting LF is compared to previous studies and converted to a MF. The MF is well-described by a log-normal distribution, with M-o = 0.27 M-circle dot. C1 [Bochanski, John J.; West, Andrew A.] MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA. [Bochanski, John J.; Hawley, Suzanne L.; Ivezic, Zeljko] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Reid, I. Neill; Golimowski, David A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Covey, Kevin R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Bochanski, JJ (reprint author), MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA. RI West, Andrew/H-3717-2014; OI Covey, Kevin/0000-0001-6914-7797 FU NSF [AST 06-07644] FX We gratefully acknowledges the support of NSF Grant AST 06-07644. NR 12 TC 6 Z9 6 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 978-0-7354-0627-8 J9 AIP CONF PROC PY 2009 VL 1094 BP 977 EP + PG 2 WC Astronomy & Astrophysics; Physics, Applied SC Astronomy & Astrophysics; Physics GA BJC67 UT WOS:000264752500207 ER PT B AU Gingerich, O AF Gingerich, Owen BE RubinoMartin, JA Belmonte, JA Prada, F Alberdi, A TI How Galileo and Kepler Countered Aristotle's Cosmological Errors SO COSMOLOGY ACROSS CULTURES SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT Workshop on Cosmology Across Cultures CY SEP 08-12, 2008 CL Parque de las Ciencias, Granada, SPAIN SP Spanish Minist Educ & Sci, Govt Andalusia, Superior Invest Cientif, Inst Astrofis Canarias HO Parque de las Ciencias AB Aristotle made two major common sense assumptions that ultimately had to be refuted to open the way to modern science. One was the dichotomy between celestial and terrestrial. The other was the separation of astronomy from physics. Galileo, particularly with his examination of the moon in the Sidereus nuncius, was a pioneer in destroying the first assumption, while Kepler, whose Astronomia nova was subtitled "based on causes, or celestial physics," broke the stranglehold of the second. The importance of these fundamental contributions toward establishing the nature of modern science, which paved the way for Isaac Newton, is often overshadowed by their more specific contributions in optics or mechanics. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Gingerich, O (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 0 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 978-1-58381-698-1 J9 ASTR SOC P PY 2009 VL 409 BP 242 EP 249 PG 8 WC Astronomy & Astrophysics; History & Philosophy Of Science SC Astronomy & Astrophysics; History & Philosophy of Science GA BLZ80 UT WOS:000271616100033 ER PT J AU Zhang, AB Gourley, D AF Zhang, Allison B. Gourley, Don BA Zhang, AB Gourley, D BF Zhang, AB Gourley, D TI Creating Digital Collections A practical guide Introduction SO CREATING DIGITAL COLLECTIONS: A PRACTICAL GUIDE SE Chandos Information Professional Series LA English DT Editorial Material; Book Chapter C1 [Zhang, Allison B.] Washington Res Lib Consortium, Digital Collect Prod Ctr, Washington, MD USA. [Zhang, Allison B.] Univ Rochester Lib, Rochester, NY USA. [Gourley, Don] Digital Humanities Observ, Dublin, Ireland. [Gourley, Don] Hewlett Packard Corp, Mississauga, ON, Canada. [Gourley, Don] Smithsonian Inst, Washington, DC 20560 USA. [Gourley, Don] Univ Maryland, College Pk, MD 20742 USA. RP Zhang, AB (reprint author), Washington Res Lib Consortium, Digital Collect Prod Ctr, Washington, MD USA. EM zhang@wrlc.org; donald.gourley@gmail.com; zhang@wrlc.org; donald.gourley@gmail.com NR 0 TC 0 Z9 0 U1 0 U2 0 PU CHANDOS PUBL PI SAWSTON PA 80 HIGH ST, SAWSTON, CAMBRIDGE CB22 3HJ, ENGLAND BN 978-1-84334-396-7 J9 CHANDOS INF PROF SER PY 2009 BP 1 EP 6 PG 6 WC Information Science & Library Science SC Information Science & Library Science GA BUD84 UT WOS:000288953700002 ER PT J AU Zhang, AB Gourley, D AF Zhang, Allison B. Gourley, Don BA Zhang, AB Gourley, D BF Zhang, AB Gourley, D TI Planning and managing digitisation projects SO CREATING DIGITAL COLLECTIONS: A PRACTICAL GUIDE SE Chandos Information Professional Series LA English DT Article; Book Chapter C1 [Zhang, Allison B.] Washington Res Lib Consortium, Digital Collect Prod Ctr, Washington, MD USA. [Zhang, Allison B.] Univ Rochester Lib, Rochester, NY USA. [Gourley, Don] Digital Humanities Observ, Dublin, Ireland. [Gourley, Don] Hewlett Packard Corp, Mississauga, ON, Canada. [Gourley, Don] Smithsonian Inst, Washington, DC 20560 USA. [Gourley, Don] Univ Maryland, College Pk, MD 20742 USA. RP Zhang, AB (reprint author), Washington Res Lib Consortium, Digital Collect Prod Ctr, Washington, MD USA. EM zhang@wrlc.org; donald.gourley@gmail.com; zhang@wrlc.org; donald.gourley@gmail.com NR 0 TC 0 Z9 0 U1 0 U2 0 PU CHANDOS PUBL PI SAWSTON PA 80 HIGH ST, SAWSTON, CAMBRIDGE CB22 3HJ, ENGLAND BN 978-1-84334-396-7 J9 CHANDOS INF PROF SER PY 2009 BP 7 EP 17 PG 11 WC Information Science & Library Science SC Information Science & Library Science GA BUD84 UT WOS:000288953700003 ER PT J AU Zhang, AB Gourley, D AF Zhang, Allison B. Gourley, Don BA Zhang, AB Gourley, D BF Zhang, AB Gourley, D TI Creating Digital Collections A practical guide Preface SO CREATING DIGITAL COLLECTIONS: A PRACTICAL GUIDE SE Chandos Information Professional Series LA English DT Editorial Material; Book Chapter C1 [Zhang, Allison B.] Washington Res Lib Consortium, Digital Collect Prod Ctr, Washington, MD USA. [Zhang, Allison B.] Univ Rochester Lib, Rochester, NY USA. [Gourley, Don] Digital Humanities Observ, Dublin, Ireland. [Gourley, Don] Hewlett Packard Corp, Mississauga, ON, Canada. [Gourley, Don] Smithsonian Inst, Washington, DC 20560 USA. [Gourley, Don] Univ Maryland, College Pk, MD 20742 USA. RP Zhang, AB (reprint author), Washington Res Lib Consortium, Digital Collect Prod Ctr, Washington, MD USA. EM zhang@wrlc.org; donald.gourley@gmail.com; zhang@wrlc.org; donald.gourley@gmail.com NR 0 TC 0 Z9 0 U1 0 U2 0 PU CHANDOS PUBL PI SAWSTON PA 80 HIGH ST, SAWSTON, CAMBRIDGE CB22 3HJ, ENGLAND BN 978-1-84334-396-7 J9 CHANDOS INF PROF SER PY 2009 BP XIII EP + PG 9 WC Information Science & Library Science SC Information Science & Library Science GA BUD84 UT WOS:000288953700001 ER PT J AU Zhang, AB Gourley, D AF Zhang, Allison B. Gourley, Don BA Zhang, AB Gourley, D BF Zhang, AB Gourley, D TI Selecting material for digitisation SO CREATING DIGITAL COLLECTIONS: A PRACTICAL GUIDE SE Chandos Information Professional Series LA English DT Article; Book Chapter C1 [Zhang, Allison B.] Washington Res Lib Consortium, Digital Collect Prod Ctr, Washington, MD USA. [Zhang, Allison B.] Univ Rochester Lib, Rochester, NY USA. [Gourley, Don] Digital Humanities Observ, Dublin, Ireland. [Gourley, Don] Hewlett Packard Corp, Mississauga, ON, Canada. [Gourley, Don] Smithsonian Inst, Washington, DC 20560 USA. [Gourley, Don] Univ Maryland, College Pk, MD 20742 USA. RP Zhang, AB (reprint author), Washington Res Lib Consortium, Digital Collect Prod Ctr, Washington, MD USA. EM zhang@wrlc.org; donald.gourley@gmail.com; zhang@wrlc.org; donald.gourley@gmail.com NR 0 TC 0 Z9 0 U1 0 U2 0 PU CHANDOS PUBL PI SAWSTON PA 80 HIGH ST, SAWSTON, CAMBRIDGE CB22 3HJ, ENGLAND BN 978-1-84334-396-7 J9 CHANDOS INF PROF SER PY 2009 BP 19 EP 30 PG 12 WC Information Science & Library Science SC Information Science & Library Science GA BUD84 UT WOS:000288953700004 ER PT J AU Zhang, AB Gourley, D AF Zhang, Allison B. Gourley, Don BA Zhang, AB Gourley, D BF Zhang, AB Gourley, D TI Metadata strategy SO CREATING DIGITAL COLLECTIONS: A PRACTICAL GUIDE SE Chandos Information Professional Series LA English DT Article; Book Chapter C1 [Zhang, Allison B.] Washington Res Lib Consortium, Digital Collect Prod Ctr, Washington, MD USA. [Zhang, Allison B.] Univ Rochester Lib, Rochester, NY USA. [Gourley, Don] Digital Humanities Observ, Dublin, Ireland. [Gourley, Don] Hewlett Packard Corp, Mississauga, ON, Canada. [Gourley, Don] Smithsonian Inst, Washington, DC 20560 USA. [Gourley, Don] Univ Maryland, College Pk, MD 20742 USA. RP Zhang, AB (reprint author), Washington Res Lib Consortium, Digital Collect Prod Ctr, Washington, MD USA. EM zhang@wrlc.org; donald.gourley@gmail.com; zhang@wrlc.org; donald.gourley@gmail.com NR 0 TC 0 Z9 0 U1 0 U2 0 PU CHANDOS PUBL PI SAWSTON PA 80 HIGH ST, SAWSTON, CAMBRIDGE CB22 3HJ, ENGLAND BN 978-1-84334-396-7 J9 CHANDOS INF PROF SER PY 2009 BP 31 EP 53 PG 23 WC Information Science & Library Science SC Information Science & Library Science GA BUD84 UT WOS:000288953700005 ER PT J AU Zhang, AB Gourley, D AF Zhang, Allison B. Gourley, Don BA Zhang, AB Gourley, D BF Zhang, AB Gourley, D TI Digitising material SO CREATING DIGITAL COLLECTIONS: A PRACTICAL GUIDE SE Chandos Information Professional Series LA English DT Article; Book Chapter C1 [Zhang, Allison B.] Washington Res Lib Consortium, Digital Collect Prod Ctr, Washington, MD USA. [Zhang, Allison B.] Univ Rochester Lib, Rochester, NY USA. [Gourley, Don] Digital Humanities Observ, Dublin, Ireland. [Gourley, Don] Hewlett Packard Corp, Mississauga, ON, Canada. [Gourley, Don] Smithsonian Inst, Washington, DC 20560 USA. [Gourley, Don] Univ Maryland, College Pk, MD 20742 USA. RP Zhang, AB (reprint author), Washington Res Lib Consortium, Digital Collect Prod Ctr, Washington, MD USA. EM zhang@wrlc.org; donald.gourley@gmail.com; zhang@wrlc.org; donald.gourley@gmail.com NR 0 TC 0 Z9 0 U1 0 U2 0 PU CHANDOS PUBL PI SAWSTON PA 80 HIGH ST, SAWSTON, CAMBRIDGE CB22 3HJ, ENGLAND BN 978-1-84334-396-7 J9 CHANDOS INF PROF SER PY 2009 BP 55 EP 72 PG 18 WC Information Science & Library Science SC Information Science & Library Science GA BUD84 UT WOS:000288953700006 ER PT J AU Zhang, AB Gourley, D AF Zhang, Allison B. Gourley, Don BA Zhang, AB Gourley, D BF Zhang, AB Gourley, D TI Creating metadata SO CREATING DIGITAL COLLECTIONS: A PRACTICAL GUIDE SE Chandos Information Professional Series LA English DT Article; Book Chapter C1 [Zhang, Allison B.] Washington Res Lib Consortium, Digital Collect Prod Ctr, Washington, MD USA. [Zhang, Allison B.] Univ Rochester Lib, Rochester, NY USA. [Gourley, Don] Digital Humanities Observ, Dublin, Ireland. [Gourley, Don] Hewlett Packard Corp, Mississauga, ON, Canada. [Gourley, Don] Smithsonian Inst, Washington, DC 20560 USA. [Gourley, Don] Univ Maryland, College Pk, MD 20742 USA. RP Zhang, AB (reprint author), Washington Res Lib Consortium, Digital Collect Prod Ctr, Washington, MD USA. EM zhang@wrlc.org; donald.gourley@gmail.com; zhang@wrlc.org; donald.gourley@gmail.com NR 0 TC 0 Z9 0 U1 0 U2 0 PU CHANDOS PUBL PI SAWSTON PA 80 HIGH ST, SAWSTON, CAMBRIDGE CB22 3HJ, ENGLAND BN 978-1-84334-396-7 J9 CHANDOS INF PROF SER PY 2009 BP 73 EP 88 PG 16 WC Information Science & Library Science SC Information Science & Library Science GA BUD84 UT WOS:000288953700007 ER PT J AU Zhang, AB Gourley, D AF Zhang, Allison B. Gourley, Don BA Zhang, AB Gourley, D BF Zhang, AB Gourley, D TI Designing a user interface for digital collections SO CREATING DIGITAL COLLECTIONS: A PRACTICAL GUIDE SE Chandos Information Professional Series LA English DT Article; Book Chapter C1 [Zhang, Allison B.] Washington Res Lib Consortium, Digital Collect Prod Ctr, Washington, MD USA. [Zhang, Allison B.] Univ Rochester Lib, Rochester, NY USA. [Gourley, Don] Digital Humanities Observ, Dublin, Ireland. [Gourley, Don] Hewlett Packard Corp, Mississauga, ON, Canada. [Gourley, Don] Smithsonian Inst, Washington, DC 20560 USA. [Gourley, Don] Univ Maryland, College Pk, MD 20742 USA. RP Zhang, AB (reprint author), Washington Res Lib Consortium, Digital Collect Prod Ctr, Washington, MD USA. EM zhang@wrlc.org; donald.gourley@gmail.com; zhang@wrlc.org; donald.gourley@gmail.com NR 0 TC 0 Z9 0 U1 0 U2 0 PU CHANDOS PUBL PI SAWSTON PA 80 HIGH ST, SAWSTON, CAMBRIDGE CB22 3HJ, ENGLAND BN 978-1-84334-396-7 J9 CHANDOS INF PROF SER PY 2009 BP 89 EP 111 PG 23 WC Information Science & Library Science SC Information Science & Library Science GA BUD84 UT WOS:000288953700008 ER PT J AU Zhang, AB Gourley, D AF Zhang, Allison B. Gourley, Don BA Zhang, AB Gourley, D BF Zhang, AB Gourley, D TI The complete digitisation process and workflow management SO CREATING DIGITAL COLLECTIONS: A PRACTICAL GUIDE SE Chandos Information Professional Series LA English DT Article; Book Chapter C1 [Zhang, Allison B.] Washington Res Lib Consortium, Digital Collect Prod Ctr, Washington, MD USA. [Zhang, Allison B.] Univ Rochester Lib, Rochester, NY USA. [Gourley, Don] Digital Humanities Observ, Dublin, Ireland. [Gourley, Don] Hewlett Packard Corp, Mississauga, ON, Canada. [Gourley, Don] Smithsonian Inst, Washington, DC 20560 USA. [Gourley, Don] Univ Maryland, College Pk, MD 20742 USA. RP Zhang, AB (reprint author), Washington Res Lib Consortium, Digital Collect Prod Ctr, Washington, MD USA. EM zhang@wrlc.org; donald.gourley@gmail.com; zhang@wrlc.org; donald.gourley@gmail.com NR 0 TC 0 Z9 0 U1 0 U2 0 PU CHANDOS PUBL PI SAWSTON PA 80 HIGH ST, SAWSTON, CAMBRIDGE CB22 3HJ, ENGLAND BN 978-1-84334-396-7 J9 CHANDOS INF PROF SER PY 2009 BP 113 EP 123 PG 11 WC Information Science & Library Science SC Information Science & Library Science GA BUD84 UT WOS:000288953700009 ER PT J AU Zhang, AB Gourley, D AF Zhang, Allison B. Gourley, Don BA Zhang, AB Gourley, D BF Zhang, AB Gourley, D TI Digital collections management system SO CREATING DIGITAL COLLECTIONS: A PRACTICAL GUIDE SE Chandos Information Professional Series LA English DT Article; Book Chapter C1 [Zhang, Allison B.] Washington Res Lib Consortium, Digital Collect Prod Ctr, Washington, MD USA. [Zhang, Allison B.] Univ Rochester Lib, Rochester, NY USA. [Gourley, Don] Digital Humanities Observ, Dublin, Ireland. [Gourley, Don] Hewlett Packard Corp, Mississauga, ON, Canada. [Gourley, Don] Smithsonian Inst, Washington, DC 20560 USA. [Gourley, Don] Univ Maryland, College Pk, MD 20742 USA. RP Zhang, AB (reprint author), Washington Res Lib Consortium, Digital Collect Prod Ctr, Washington, MD USA. EM zhang@wrlc.org; donald.gourley@gmail.com; zhang@wrlc.org; donald.gourley@gmail.com NR 0 TC 0 Z9 0 U1 0 U2 0 PU CHANDOS PUBL PI SAWSTON PA 80 HIGH ST, SAWSTON, CAMBRIDGE CB22 3HJ, ENGLAND BN 978-1-84334-396-7 J9 CHANDOS INF PROF SER PY 2009 BP 125 EP 148 PG 24 WC Information Science & Library Science SC Information Science & Library Science GA BUD84 UT WOS:000288953700010 ER PT J AU Zhang, AB Gourley, D AF Zhang, Allison B. Gourley, Don BA Zhang, AB Gourley, D BF Zhang, AB Gourley, D TI Selecting software and hardware for digital collections management systems SO CREATING DIGITAL COLLECTIONS: A PRACTICAL GUIDE SE Chandos Information Professional Series LA English DT Article; Book Chapter C1 [Zhang, Allison B.] Washington Res Lib Consortium, Digital Collect Prod Ctr, Washington, MD USA. [Zhang, Allison B.] Univ Rochester Lib, Rochester, NY USA. [Gourley, Don] Digital Humanities Observ, Dublin, Ireland. [Gourley, Don] Hewlett Packard Corp, Mississauga, ON, Canada. [Gourley, Don] Smithsonian Inst, Washington, DC 20560 USA. [Gourley, Don] Univ Maryland, College Pk, MD 20742 USA. RP Zhang, AB (reprint author), Washington Res Lib Consortium, Digital Collect Prod Ctr, Washington, MD USA. EM zhang@wrlc.org; donald.gourley@gmail.com; zhang@wrlc.org; donald.gourley@gmail.com NR 0 TC 0 Z9 0 U1 0 U2 0 PU CHANDOS PUBL PI SAWSTON PA 80 HIGH ST, SAWSTON, CAMBRIDGE CB22 3HJ, ENGLAND BN 978-1-84334-396-7 J9 CHANDOS INF PROF SER PY 2009 BP 149 EP 177 PG 29 WC Information Science & Library Science SC Information Science & Library Science GA BUD84 UT WOS:000288953700011 ER PT J AU Zhang, AB Gourley, D AF Zhang, Allison B. Gourley, Don BA Zhang, AB Gourley, D BF Zhang, AB Gourley, D TI Documentation SO CREATING DIGITAL COLLECTIONS: A PRACTICAL GUIDE SE Chandos Information Professional Series LA English DT Article; Book Chapter C1 [Zhang, Allison B.] Washington Res Lib Consortium, Digital Collect Prod Ctr, Washington, MD USA. [Zhang, Allison B.] Univ Rochester Lib, Rochester, NY USA. [Gourley, Don] Digital Humanities Observ, Dublin, Ireland. [Gourley, Don] Hewlett Packard Corp, Mississauga, ON, Canada. [Gourley, Don] Smithsonian Inst, Washington, DC 20560 USA. [Gourley, Don] Univ Maryland, College Pk, MD 20742 USA. RP Zhang, AB (reprint author), Washington Res Lib Consortium, Digital Collect Prod Ctr, Washington, MD USA. EM zhang@wrlc.org; donald.gourley@gmail.com; zhang@wrlc.org; donald.gourley@gmail.com NR 0 TC 0 Z9 0 U1 0 U2 0 PU CHANDOS PUBL PI SAWSTON PA 80 HIGH ST, SAWSTON, CAMBRIDGE CB22 3HJ, ENGLAND BN 978-1-84334-396-7 J9 CHANDOS INF PROF SER PY 2009 BP 179 EP 187 PG 9 WC Information Science & Library Science SC Information Science & Library Science GA BUD84 UT WOS:000288953700012 ER PT J AU Zhang, AB Gourley, D AF Zhang, Allison B. Gourley, Don BA Zhang, AB Gourley, D BF Zhang, AB Gourley, D TI The knowledge and skills required for creating digital collections SO CREATING DIGITAL COLLECTIONS: A PRACTICAL GUIDE SE Chandos Information Professional Series LA English DT Article; Book Chapter C1 [Zhang, Allison B.] Washington Res Lib Consortium, Digital Collect Prod Ctr, Washington, MD USA. [Zhang, Allison B.] Univ Rochester Lib, Rochester, NY USA. [Gourley, Don] Digital Humanities Observ, Dublin, Ireland. [Gourley, Don] Hewlett Packard Corp, Mississauga, ON, Canada. [Gourley, Don] Smithsonian Inst, Washington, DC 20560 USA. [Gourley, Don] Univ Maryland, College Pk, MD 20742 USA. RP Zhang, AB (reprint author), Washington Res Lib Consortium, Digital Collect Prod Ctr, Washington, MD USA. EM zhang@wrlc.org; donald.gourley@gmail.com; zhang@wrlc.org; donald.gourley@gmail.com NR 0 TC 0 Z9 0 U1 0 U2 0 PU CHANDOS PUBL PI SAWSTON PA 80 HIGH ST, SAWSTON, CAMBRIDGE CB22 3HJ, ENGLAND BN 978-1-84334-396-7 J9 CHANDOS INF PROF SER PY 2009 BP 189 EP 195 PG 7 WC Information Science & Library Science SC Information Science & Library Science GA BUD84 UT WOS:000288953700013 ER PT J AU Zhang, AB Gourley, D AF Zhang, Allison B. Gourley, Don BA Zhang, AB Gourley, D BF Zhang, AB Gourley, D TI Creating Digital Collections A practical guide Conclusion SO CREATING DIGITAL COLLECTIONS: A PRACTICAL GUIDE SE Chandos Information Professional Series LA English DT Editorial Material; Book Chapter C1 [Zhang, Allison B.] Washington Res Lib Consortium, Digital Collect Prod Ctr, Washington, MD USA. [Zhang, Allison B.] Univ Rochester Lib, Rochester, NY USA. [Gourley, Don] Digital Humanities Observ, Dublin, Ireland. [Gourley, Don] Hewlett Packard Corp, Mississauga, ON, Canada. [Gourley, Don] Smithsonian Inst, Washington, DC 20560 USA. [Gourley, Don] Univ Maryland, College Pk, MD 20742 USA. RP Zhang, AB (reprint author), Washington Res Lib Consortium, Digital Collect Prod Ctr, Washington, MD USA. EM zhang@wrlc.org; donald.gourley@gmail.com; zhang@wrlc.org; donald.gourley@gmail.com NR 0 TC 0 Z9 0 U1 0 U2 0 PU CHANDOS PUBL PI SAWSTON PA 80 HIGH ST, SAWSTON, CAMBRIDGE CB22 3HJ, ENGLAND BN 978-1-84334-396-7 J9 CHANDOS INF PROF SER PY 2009 BP 197 EP 199 PG 3 WC Information Science & Library Science SC Information Science & Library Science GA BUD84 UT WOS:000288953700014 ER PT J AU Bilby, KM Neely, DT AF Bilby, Kenneth M. Neely, Daniel T. BE Manuel, P TI The English-Speaking Caribbean Re-embodying the Colonial Ballroom SO CREOLIZING CONTRADANCE IN THE CARIBBEAN SE Studies in Latin American and Caribbean Music LA English DT Article; Book Chapter ID MUSIC; DANCE; TRANSFORMATION; IDENTITY; JAZZ C1 [Bilby, Kenneth M.] Columbia Coll, Ctr Black Mus Res, Chicago, IL 60605 USA. [Bilby, Kenneth M.] Smithsonian Inst, Dept Anthropol, Washington, DC 20560 USA. [Neely, Daniel T.] New Sch Univ, New York, NY USA. [Neely, Daniel T.] SUNY Stony Brook, Stony Brook, NY 11794 USA. RP Bilby, KM (reprint author), Columbia Coll, Ctr Black Mus Res, Chicago, IL 60605 USA. NR 128 TC 1 Z9 1 U1 0 U2 0 PU TEMPLE UNIV PRESS PI PHILADELPHIA PA BROAD & OXFORD ST, PHILADELPHIA, PA 19122 USA BN 978-1-59213-734-3 J9 STUD LAT AMER CARIBB PY 2009 BP 231 EP 270 PG 40 WC Dance SC Dance GA BA8EG UT WOS:000338022800007 ER PT J AU Tan, SW Meiller, JC Mahaffey, KR AF Tan, Shirlee W. Meiller, Jesse C. Mahaffey, Kathryn R. TI The endocrine effects of mercury in humans and wildlife SO CRITICAL REVIEWS IN TOXICOLOGY LA English DT Review DE Endocrine; hypothalamic-pituitary-adrenal (HPA); reproductive; methylmercury (MeHg); hypothalamic-pituitary-gonadal (HPG); hypothalamic-pituitary-thyroid (HPT); mercury (Hg); mercury chloride (HgCl2) ID CLARIAS-BATRACHUS L; WALLEYE STIZOSTEDION-VITREUM; TROUT ONCORHYNCHUS-MYKISS; CHANNA-PUNCTATUS BLOCH; FED METHYL MERCURY; HETEROPNEUSTES-FOSSILIS BLOCH; PITUITARY-HORMONE RESPONSE; METAL-CONTAMINATED WATERS; FETAL MINAMATA DISEASE; CORONARY-HEART-DISEASE AB Mercury (Hg) is well studied and research continues as our knowledge of its health risks increases. One expanding area of research not well emphasized to date is the endocrine effects of Hg. This review summarizes the existing literature on the effects of Hg on the endocrine system and identifies gaps in the knowledge. It focuses on the thyroid, adrenal, and reproductive systems, including the accumulation of Hg in the endocrine system, sex differences that are manifested with Hg exposure, reproductive effects in male and female animals including humans, and Hg effects on the thyroid and adrenal systems. We concluded that there are five main endocrine-related mechanisms of Hg across these systems: (a) accumulation in the endocrine system; (b) specific cytotoxicity in endocrine tissues; (c) changes in hormone concentrations; (d) interactions with sex hormones; and (e) up-regulation or down-regulation of enzymes within the steroidogenesis pathway. Recommendations for key areas of research to better understand how the endocrine effects of Hg affect human and wildlife health were developed, and include increasing the amount of basic biological information available about Hg and wildlife species, exploring the role of Hg in the presence of other stressors and chemicals, understanding sublethal and indirect effects of Hg on adverse outcomes, developing better methods to extrapolate effects across species, and understanding the effects of Hg on multiple organ systems following exposure of an animal. Greater inclusion of endocrine endpoints in epidemiological and field studies on humans and wildlife will also advance the research in this area. C1 [Tan, Shirlee W.; Meiller, Jesse C.; Mahaffey, Kathryn R.] US EPA, Off Sci Coordinat & Policy, Washington, DC 20460 USA. [Tan, Shirlee W.] Smithsonian Inst, Natl Zool Pk, Washington, DC 20008 USA. RP Tan, SW (reprint author), US EPA, Off Sci Coordinat & Policy, Mailcode 7203-M,1200 Penn Ave NW, Washington, DC 20460 USA. EM Tan.Shirlee@epamail.epa.gov FU American Association for the Advancement of Science; US Environmental Protection Agency; Smithsonian Institution FX The authors would like to thank Dr Kathy Shea, Dr Thomas Zoeller, Dr Katsuyuki Murata, and Dr Rebecca Klaper for critically reading individual sections and providing invaluable advice on how to better focus the paper. This paper was prepared by authors under support from or employment with the American Association for the Advancement of Science, the US Environmental Protection Agency, and the Smithsonian Institution. NR 390 TC 106 Z9 107 U1 12 U2 64 PU INFORMA HEALTHCARE PI LONDON PA TELEPHONE HOUSE, 69-77 PAUL STREET, LONDON EC2A 4LQ, ENGLAND SN 1040-8444 EI 1547-6898 J9 CRIT REV TOXICOL JI Crit. Rev. Toxicol. PY 2009 VL 39 IS 3 BP 228 EP 269 AR PII 909432267 DI 10.1080/10408440802233259 PG 42 WC Toxicology SC Toxicology GA 417SK UT WOS:000264097800002 PM 19280433 ER PT J AU Marin, I Anker, A AF Marin, Ivan Anker, Arthur TI ON THE PRESENCE OF THE PONTONIINE SHRIMP, TULEARIOCARIS HOLTHUISI HIPEAU-JACQUOTTE, 1965 (DECAPODA, PONTONIINAE) ON THE PACIFIC COAST OF PANAMA SO CRUSTACEANA LA English DT Article ID CRUSTACEA C1 [Marin, Ivan] Russian Acad Sci, AN Severtzov Inst Ecol & Evolut, Moscow 117071, Russia. [Anker, Arthur] Smithsonian Trop Res Inst, Naos Unit 0948, APO, AA 34002 USA. RP Marin, I (reprint author), Russian Acad Sci, AN Severtzov Inst Ecol & Evolut, Leninsky Prospect 33, Moscow 117071, Russia. EM coralliodecapoda@mail.ru; ankera@si.edu NR 16 TC 4 Z9 4 U1 0 U2 0 PU BRILL ACADEMIC PUBLISHERS PI LEIDEN PA PLANTIJNSTRAAT 2, P O BOX 9000, 2300 PA LEIDEN, NETHERLANDS SN 0011-216X EI 1568-5403 J9 CRUSTACEANA JI Crustaceana PY 2009 VL 82 IS 4 BP 505 EP 508 DI 10.1163/156854008X400577 PG 4 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 447TV UT WOS:000266215600011 ER PT J AU Humphreys, WF Kornicker, LS Danielopol, DL AF Humphreys, William F. Kornicker, Louis S. Danielopol, Dan L. TI ON THE ORIGIN OF DANIELOPOLINA BALTANASI SP N. (OSTRACODA, THAUMATOCYPRIDOIDEA) FROM THREE ANCHIALINE CAVES ON CHRISTMAS ISLAND, A SEAMOUNT IN THE INDIAN OCEAN SO CRUSTACEANA LA English DT Article ID WESTERN-AUSTRALIA; MARINE CAVES; DEEP-SEA; CRUSTACEA; SHRIMP; KORNICKERI; DISPERSAL; EVOLUTION; MYODOCOPA; PATTERNS AB The morphology and systematic affinities of Danielopolina sp. cf. D. kornickeri from Christmas Island, an isolated seamount in the Indian Ocean, are reassessed with the aid of new material including a juvenile male. The species is formally described as Danielopolina (Humphreysella) baltanasi sp. n., which places the species in a separate subgenus to Danielopolina ( Danielopolina) kornickeri from northwest Australia, the only other member of the genus in the Indian Ocean. In addition, the only deep-sea member of the genus, D. carolynae from the mid-Atlantic, a putative colonizer of seamounts, belongs to the subgenus Danielopolina. These findings compound theories on the distribution and dispersal of anchialine faunas. A coherent programme of molecular phylogenetic research and historical biogeographical analysis is needed to further enquiry into the enigmatic distribution of the anchialine faunas of both isolated sea mounts and epicontinental waters. Owing to the scarcity of anchialine fauna and the difficulty of access of their habitat, a global effort will be required to assemble the required specimens. C1 [Humphreys, William F.] Western Australian Museum, Collect & Res Ctr, Welshpool Dc, WA 6986, Australia. [Kornicker, Louis S.] Natl Museum Nat Hist, Dept Invertebrate Zool, Smithsonian Inst, Washington, DC 20013 USA. [Danielopol, Dan L.] Graz Univ, Inst Earth Sci, Austrian Acad Sci, Commiss Stratig & Palaeontol Res Austria, A-8010 Graz, Austria. RP Humphreys, WF (reprint author), Western Australian Museum, Collect & Res Ctr, Locked Bag 49, Welshpool Dc, WA 6986, Australia. EM bill.humphreys@museum.wa.gov.au; kornickl@si.edu; dan.danielopol@oeaw.ac.at FU Parks Australia North Christmas Island FX The two new specimens reported here were collected during a Western Australian Speleological Group expedition led by Darren Brooks and funded by Parks Australia North Christmas Island. Other expedition members, who spent up to a month searching for the sparse stygofauna in the anchialine and plateau waters of Christmas Island, were Ross Anderson, Jay Anderson, Greg Thomas, Jackie Tapper, Ian Collette, Robert Susac, and Tim Moulds. Considerable logistic support was also provided by Parks Australia North, particularly through the good offices of Mick Jeffery; while there is still much to learn of this fauna, their efforts are memorable. NR 54 TC 10 Z9 10 U1 1 U2 3 PU BRILL ACADEMIC PUBLISHERS PI LEIDEN PA PLANTIJNSTRAAT 2, P O BOX 9000, 2300 PA LEIDEN, NETHERLANDS SN 0011-216X EI 1568-5403 J9 CRUSTACEANA JI Crustaceana PY 2009 VL 82 IS 9 BP 1177 EP 1203 DI 10.1163/156854009X423157 PG 27 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 492VP UT WOS:000269690500005 ER PT B AU Bensch, F Melnick, GJ Neufeld, DA Harwit, M Snell, RL Patten, BM Tolls, V AF Bensch, F. Melnick, G. J. Neufeld, D. A. Harwit, M. Snell, R. L. Patten, B. M. Tolls, V. BE Kaufl, HU Sterken, C TI Submillimeter Wave Astronomy Satellite Observations of Comet 9P/Tempel 1 SO DEEP IMPACT AS A WORLD OBSERVATORY EVENT: SYNERGIES IN SPACE, TIME, AND WAVELENGTH SE ESO ASTROPHYSICS SYMPOSIA LA English DT Proceedings Paper CT Conference on Deep Impact as a World Observatory Event - Synergies in Space, Time and Wavelength CY AUG 07-10, 2006 CL Brussels, BELGIUM SP ESO, VUB ID DEEP-IMPACT; COMET-9P/TEMPEL-1; NUCLEUS AB We present observations of the 1(10)-1(01) ortho-water ground-state rotational transition in comet 9P/Tempel 1 made with the NASA Submillimeter Wave Astronomy Satellite (SWAS). The SWAS monitoring covered a 3-month period from June to August 2005 and included observations of the comet's activity during the collision of the Deep Impact spacecraft with the nucleus on 4 July 2005. No excess emission from the material ejected by the impactor was detected and we derive an upper limit; of 1.8 x 10(7) kg on the vaporized water ice. However, the water production rate of the comet shows large natural variations of up to a factor of three throughout the 3-month monitoring period. The total amount of water vaporized between 5 June and 1 September 2005 is 4.5 x 10(34) molecules (similar to 1.3 x 10(9) kg) and we estimate that 9P/Tempel 1. has lost as much as N similar to 10(35) molecules during its 2005 apparition. C1 [Bensch, F.; Melnick, G. J.; Patten, B. M.; Tolls, V.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Bensch, F.] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany. [Neufeld, D. A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Harwit, M.] Cornell Univ, Washington, DC 20024 USA. [Snell, R. L.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. RP Bensch, F (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM fbensch@astro.uni-bonn.de NR 10 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY BN 978-3-540-76958-3 J9 ESO ASTROPHY SYMP PY 2009 BP 221 EP + DI 10.1007/978-3-540-76959-0_28 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BIS26 UT WOS:000262404900028 ER PT S AU Mejia, LC Herre, EA Singh, AP Singh, V Vorsa, N White, JF AF Mejia, Luis C. Herre, Edward Allen Singh, Ajay P. Singh, Vartika Vorsa, Nicholi White, James F., Jr. BE White, JF Torres, MS TI Fungal Endophytes: Defensive Characteristics and Implications for Agricultural Applications SO DEFENSIVE MUTUALISM IN MICROBIAL SYMBIOSIS SE Mycology Series LA English DT Article; Book Chapter ID BEAUVERIA-BASSIANA ASCOMYCOTA; RUGULOSIN-PRODUCING ENDOPHYTE; TALL FESCUE; MOLECULAR CHARACTERIZATION; ACREMONIUM-COENOPHIALUM; SECONDARY METABOLITES; ANTIBIOTIC-ACTIVITY; DISEASE RESISTANCE; BIOLOGICAL-CONTROL; PHENOLIC-COMPOUNDS C1 [Mejia, Luis C.] Rutgers State Univ, Sch Environm & Biol Sci, Dept Plant Biol & Pathol, New Brunswick, NJ 08903 USA. [Vorsa, Nicholi] Philip E Marucci Ctr Blueberry & Cranberry Res &, Chatsworth, NJ USA. [Herre, Edward Allen] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Mejia, LC (reprint author), Rutgers State Univ, Sch Environm & Biol Sci, Dept Plant Biol & Pathol, New Brunswick, NJ 08903 USA. NR 113 TC 2 Z9 2 U1 0 U2 7 PU CRC PRESS-TAYLOR & FRANCIS GROUP PI BOCA RATON PA 6000 BROKEN SOUND PARKWAY NW, STE 300, BOCA RATON, FL 33487-2742 USA SN 0730-9597 BN 978-1-4200-6931-0 J9 MYCOL SER JI MYCOLOGY S PY 2009 VL 27 BP 367 EP 383 D2 10.1201/9781420069327 PG 17 WC Mycology SC Mycology GA BKJ99 UT WOS:000268336300022 ER PT B AU Thompson, FC AF Thompson, F. Christian BE Pape, T Bickel, D Meier, R TI NEARCTIC DIPTERA: TWENTY YEARS LATER SO DIPTERA DIVERSITY: STATUS, CHALLENGES AND TOOLS LA English DT Article; Book Chapter ID ANIMAL NAMES; REVISION; SYRPHIDAE; NORTH; TAXONOMY; FAMILY C1 ARS, Systemat Entomol Lab, PSI, USDA,Smithsonian Inst, Washington, DC 20013 USA. RP Thompson, FC (reprint author), ARS, Systemat Entomol Lab, PSI, USDA,Smithsonian Inst, NHB 0169, Washington, DC 20013 USA. EM chris.thompson@ars.usda.gov NR 184 TC 5 Z9 5 U1 0 U2 0 PU BRILL PI PA LEIDEN PA PO BOX 9000, NL-2300 PA LEIDEN, NETHERLANDS BN 978-90-04-18100-7; 978-90-04-14897-0 PY 2009 BP 3 EP 46 D2 10.1163/ej.9789004148970.I-459 PG 44 WC Biodiversity Conservation SC Biodiversity & Conservation GA BZP10 UT WOS:000302311900002 ER PT J AU Stouffer, PC Strong, C Naka, LN AF Stouffer, Philip C. Strong, Cheryl Naka, Luciano N. TI Twenty years of understorey bird extinctions from Amazonian rain forest fragments: consistent trends and landscape-mediated dynamics SO DIVERSITY AND DISTRIBUTIONS LA English DT Article DE Amazonia; bird communities; extinction; forest fragmentation; landscape dynamics; rain forest; rescue effect ID BARRO COLORADO ISLAND; INSECTIVOROUS BIRDS; LOCAL EXTINCTIONS; COSTA-RICA; COMMUNITIES; ABUNDANCE; PANAMA; PATTERNS; BRAZIL; RATES AB We analysed presence/absence data for understorey bird species in rain forest fragments sampled from 1979 through 2001. Here we consider extinctions between 1992, when most fragments had been isolated for at least 8 years, and 2001. Our objectives were to determine whether high extinction rates documented soon after isolation continued through up to 20 years after isolation, and to examine fragment size and landscape effects on extinction. Biological Dynamics of Forest Fragments Project, near Manaus, Brazil. Through 1992, birds were surveyed with standardized mist net sampling in ten 1- to 100-ha fragments. We repeated the mist net protocol in 2000-01. We also added remote taping of the dawn chorus and tape playback surveys for species captured in 1991-92 but not in 2000-01. Between 1992 and 2001, 37 species went extinct in at least one fragment. As expected, extinction rate decreased with increasing fragment size. Over 30% of species went extinct in 1-ha fragments, compared to about 5% in 100-ha fragments. Extinction followed a predictable pattern: most species lost from 100-ha fragments between 1992 and 2001 had already gone extinct in smaller fragments before 1992. Despite extinctions, fragments gained species between 1992 and 2001, apparently due to species moving through the developing second growth matrix. Fragments surrounded by old second growth had lower extinction rates than predicted based on fragment size alone. Sequential extinctions occurred for at least 20 years. Some additional species previously lost from smaller fragments may continue to go extinct in 100-ha fragments. At the same time, species assemblages in 1- and 10-ha fragments mostly reflect second-growth dynamics by 20 years after isolation. High species loss predicted from the first few years after isolation has not occurred, almost certainly because of recolonization. C1 [Stouffer, Philip C.] Louisiana State Univ, Sch Renewable Nat Resources, Baton Rouge, LA 70803 USA. [Stouffer, Philip C.] LSU AgCtr, Baton Rouge, LA 70803 USA. [Stouffer, Philip C.; Strong, Cheryl] Inst Nacl de Pesquisas da Amazonia, Smithsonian Trop Res Inst, Biol Dynam Forest Fragments Project, BR-69011 Manaus, Amazonas, Brazil. [Naka, Luciano N.] Louisiana State Univ, Museum Nat Sci, Baton Rouge, LA 70803 USA. RP Stouffer, PC (reprint author), Louisiana State Univ, Sch Renewable Nat Resources, Baton Rouge, LA 70803 USA. EM pstouffer@lsu.edu RI Naka, Luciano/G-7485-2014 NR 37 TC 36 Z9 37 U1 5 U2 33 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1366-9516 J9 DIVERS DISTRIB JI Divers. Distrib. PD JAN PY 2009 VL 15 IS 1 BP 88 EP 97 DI 10.1111/j.1472-4642.2008.00497.x PG 10 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 381FP UT WOS:000261521400009 ER EF