FN Thomson Reuters Web of Science™ VR 1.0 PT J AU Southward, EC Schulze, A Gardiner, SL AF Southward, EC Schulze, A Gardiner, SL TI Pogonophora (Annelida): form and function SO HYDROBIOLOGIA LA English DT Article; Proceedings Paper CT Symposium on Morphology, Molecules, Evolution and Phylogeny in Polychaeta and Related Taxa CY SEP, 2002 CL Osnabruck, GERMANY DE Pogonophora; Siboglinidae; Frenulata; Vestimentifera; anatomy; ultrastructure ID TUBEWORM RIFTIA-PACHYPTILA; CHEMOAUTOTROPH SYMBIOTIC BACTERIA; MULTI-HEMOGLOBIN SYSTEM; SOUTHWEST PACIFIC-OCEAN; SEA HYDROTHERMAL VENTS; PAPUA-NEW-GUINEA; SULFIDE-BINDING; VESTIMENTIFERA SIBOGLINIDAE; EXTRACELLULAR-MATRIX; JONES POGONOPHORA AB Pogonophora, also known as Siboglinidae, are tube-dwelling marine annelids. They rely on endosymbiotic chemoautotrophic bacteria for nutrition and their anatomy and physiology are adapted to their need to obtain both oxygen and reduced sulphur compounds. Frenulate pogonophores are generally long and slender, sediment-living tubeworms; vestimentiferans are stouter, inhabitants of hydrothermal vents and cool seeps; and moniliferans or sclerolinids are very slender inhabitants of decaying wood and sulphidic sediments. The anatomy and ultrastructure of the three groups are compared and recent publications are reviewed. Annelid characters are the presence of chaetae and septa, concentrated at the hind end. The adaptations to a specialised way of life include, in particular, the chitinous tube; the anterior appendages that function as gills; the internal tissue called the trophosome, where the endosymbiotic bacteria live; and the blood vascular system that transports oxygen, sulphide and carbon dioxide to the trophosome. C1 Marine Biol Assoc United Kingdom Lab, Plymouth PL1 2PB, Devon, England. Smithsonian Marine Stn, Ft Pierce, FL 34949 USA. Bryn Mawr Coll, Dept Biol, Bryn Mawr, PA 19010 USA. RP Southward, EC (reprint author), Marine Biol Assoc United Kingdom Lab, Citadel Hill, Plymouth PL1 2PB, Devon, England. EM 100721.3720@compuserve.com; aschulze@oeb.harvard.edu RI Schulze, Anja/I-4215-2012 NR 150 TC 43 Z9 48 U1 0 U2 14 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0018-8158 J9 HYDROBIOLOGIA JI Hydrobiologia PD MAR 1 PY 2005 VL 535 BP 227 EP 251 DI 10.1007/s10750-004-4401-6 PG 25 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 946RL UT WOS:000230589800014 ER PT J AU Schulze, A Cutler, EB Giribet, G AF Schulze, A Cutler, EB Giribet, G TI Reconstructing the phylogeny of the Sipuncula SO HYDROBIOLOGIA LA English DT Article; Proceedings Paper CT Symposium on Morphology, Molecules, Evolution and Phylogeny in Polychaeta and Related Taxa CY SEP, 2002 CL Osnabruck, GERMANY DE Sipuncula; phylogeny; 18S rRNA; 28S rRNA; histone H3; Spiralia; cladistic analysis ID DEEP-SEA SEDIMENTS; ANIMAL PHYLOGENY; PHYLUM SIPUNCULA; MORPHOLOGY; SUBSTRATE; SEQUENCES; METAZOA; CYCLIOPHORA; EVOLUTION; ANNELIDA AB Sipunculans are marine spiralian worms with possible close affinities to the Mollusca or Annelida. Currently 147 species, 17 genera, 6 families, 4 orders and 2 classes are recognized. In this paper we review sipunculan morphology, anatomy, paleontological data and historical affiliations. We have conducted cladistic analyses for two data sets to elucidate the phylogenetic relationships among sipunculan species. We first analyzed the relationships among the 45 species of Phascolosomatidea with representatives of the Sipunculidea as outgroups, using 35 morphological characters. The resulting consensus tree has low resolution and branch support is low for most branches. The second analysis was based on DNA sequence data from two nuclear ribosomal genes (18S rRNA and 28S rRNA) and one nuclear protein-coding gene, histone H3. Outgroups were chosen among representative spiralians. In a third analysis, the molecular data were combined with the morphological data. Data were analyzed using parsimony as the optimality criterion and branch support evaluated with jackknifing and Bremer support values. Branch support for outgroup relationships is low but the monophyly of the Sipuncula is well supported. Within Sipuncula, the monophyly of the two major groups, Phascolosomatidea and Sipunculidea is not confirmed. Of the currently recognized families, only Themistidae appears monophyletic. The Aspidosiphonidae, Phascolosomatidae and Golfingiidae would be monophyletic with some adjustments in their definition. The Sipunculidae is clearly polyphyletic, with Sipunculus nudus as the sister group to the remaining Sipuncula, Siphonosoma cumanense the sister group to a clade containing Siphonosoma vasturn and the Phascolosomatidea, and Phascolopsis gouldi grouping within the Golfingliformes, as suggested previously by some authors. Of the genera with multiple representatives, only Phascolosoma and Themiste are monophyletic as currently defined. We are aiming to expand our current dataset with more species in our molecular database and more detailed morphological studies. C1 Harvard Univ, Museum Comparat Zool, Dept Invertebrate Zool, Cambridge, MA 02138 USA. Harvard Univ, Dept Organism & Evolutionary Biol, Cambridge, MA 02138 USA. RP Schulze, A (reprint author), Smithsonian Marine Stn, 701 Seaway Dr, Ft Pierce, FL 34949 USA. EM anjaschulze@bigfoot.com; ebcutler@earthlink.net RI Schulze, Anja/I-4215-2012; Giribet, Gonzalo/P-1086-2015 OI Giribet, Gonzalo/0000-0002-5467-8429 NR 86 TC 19 Z9 24 U1 1 U2 13 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0018-8158 EI 1573-5117 J9 HYDROBIOLOGIA JI Hydrobiologia PD MAR 1 PY 2005 VL 535 BP 277 EP 296 DI 10.1007/s10750-004-4404-3 PG 20 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 946RL UT WOS:000230589800016 ER PT J AU Krebs, E AF Krebs, E TI Another look: A diary of the Serra do Norte Expedition SO ISIS LA English DT Book Review C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20560 USA. RP Krebs, E (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, 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 2005 VL 96 IS 1 BP 128 EP 129 DI 10.1086/433015 PG 2 WC History & Philosophy Of Science SC History & Philosophy of Science GA 941NJ UT WOS:000230221200050 ER PT J AU Norris, DR Marra, PP Kyser, TK Ratcliffe, LM AF Norris, DR Marra, PP Kyser, TK Ratcliffe, LM TI Tracking habitat use of a long-distance migratory bird, the American redstart Setophaga ruticilla, using stable-carbon isotopes in cellular blood SO JOURNAL OF AVIAN BIOLOGY LA English DT Article ID DIET-TISSUE FRACTIONATION; NONBREEDING SEASON; BREEDING GROUNDS; TURNOVER; NITROGEN; WINTER; PATTERNS; WARBLERS; SEGREGATION; POPULATIONS AB The successful use of stable isotopes to track migratory animals between different seasons of the annual cycle depends, in part, on the turnover rate of isotopes in sample tissue. We examined whether stable-carbon isotopes in the blood of a long-distance migratory bird, the American redstart Setophaga ruticilla, sampled upon arrival to the temperate breeding grounds could be used to track the quality of habitat used the previous season on the tropical wintering grounds. Stable-carbon isotopes in red-blood cells sampled upon arrival (delta(13)C(RBC)) were significantly less negative relative to: 1) plasma sampled upon arrival from the same individuals, 2) red-blood cells of redstarts recaptured more than a month later on the breeding grounds, and 3) nestling feathers grown at the same breeding location. delta(13)C(RBC) was also significantly different between sexes, consistent with findings from the wintering grounds where sex-biased habitat use is known to occur. Although individuals likely integrate some isotopic signatures during migration, we provide evidence that cellular blood can be used to track the relative habitat use of migratory birds during the wintering period. Nondestructive methods of sampling stable-isotopes, such as this, are particularly useful because it provides a technique for tracking the patterns of habitat use and/or geographic location of migratory animals. Such approaches allow researchers to understand how events throughout the annual cycle interact to influence population dynamics. C1 Queens Univ, Dept Biol, Kingston, ON K7L 3N6, Canada. Queens Univ, Dept Geol Sci, Kingston, ON K7L 3N6, Canada. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Norris, DR (reprint author), Univ British Columbia, Dept Forest Sci, Ctr Appl Conservat Res, 3041-2424 Main Mall, Vancouver, BC V6T 1Z4, Canada. EM ryann@biology.queensu.ca RI Norris, Ryan/F-4720-2011 NR 38 TC 20 Z9 21 U1 0 U2 25 PU BLACKWELL MUNKSGAARD PI COPENHAGEN PA 35 NORRE SOGADE, PO BOX 2148, DK-1016 COPENHAGEN, DENMARK SN 0908-8857 J9 J AVIAN BIOL JI J. Avian Biol. PD MAR PY 2005 VL 36 IS 2 BP 164 EP 170 DI 10.1111/j.0908-8857.2005.03398.x PG 7 WC Ornithology SC Zoology GA 910UT UT WOS:000227958400010 ER PT J AU Davidar, P Puyravaud, JP Leigh, EG AF Davidar, P Puyravaud, JP Leigh, EG TI Changes in rain forest tree diversity, dominance and rarity across a seasonality gradient in the Western Ghats, India SO JOURNAL OF BIOGEOGRAPHY LA English DT Article DE alpha diversity; India; Janzen-Connell hypothesis; pest pressure; seasonality gradient; tropical rain forest; Western Ghats ID TROPICAL EVERGREEN FOREST; SPECIES-DIVERSITY; NEOTROPICAL TREE; SEED DISPERSAL; DENSITY; PATTERN; CONSEQUENCES; RECRUITMENT; MAINTENANCE; MORTALITY AB Aim We assessed the effects of latitude, altitude and climate on the alpha diversity of rain forest trees in the Western Ghats (WG) of India. We tested whether stem densities, dominance, the prevalence of rarity, and the proportion of understorey trees are significantly correlated with alpha diversity. Locatiaon The WG is a chain of mountains c. 1600 km in length, running parallel to the western coast of the Indian peninsula from above 8degrees N to almost 21degrees N latitude. Wet forests occur as a narrow strip in regions with heavy rainfall. Methods To assess tree diversity we used data from 40 small plots, < 1 ha in area, where all trees greater than or equal to 3.18 cm d.b.h. had been inventoried. These plots were distributed across 7 latitudinal degrees and at elevations between 200 and 1550 m. Fisher's alpha was used as a measure of diversity. For each plot, the proportion of trees belonging to the understorey, the proportion of trees belonging to the most abundant species in the plot, as a measure of dominance, and the proportionate representation of singletons, as a measure of rarity, were estimated, and correlated with Fisher's alpha, elevation, rainfall and seasonality. Results Annual rainfall and seasonality increased towards the north, but were not significantly correlated. Tree diversity increased significantly with decreasing seasonality. Tree diversity was not significantly correlated with stem density or with the proportion of understorey tree species, but was significantly correlated with tree dominance and rarity. Dominance increased and rarity significantly decreased with increasing seasonality. Main conclusions This study demonstrates that seasonality influences rain forest tree diversity in the WG of India. The relationship between alpha diversity, dominance and rarity lends correlative support for the Janzen-Connell pest pressure hypothesis. C1 Smithsonian Trop Res Inst, Balboa, Panama. Pondicherry Univ, Salim Ali Sch Ecol & Environm Sci, Pondicherry, India. SUNY Stony Brook, Dept Ecol & Evolut, Stony Brook, NY 11794 USA. Ctr Valbio, Ifanadiana, Fianarantsoa, Madagascar. RP Davidar, P (reprint author), Smithsonian Trop Res Inst, Box 2072, Balboa, Panama. EM davidarp@tivoli.si.edu OI Davidar, Priya/0000-0003-2463-6743 NR 53 TC 21 Z9 24 U1 2 U2 20 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0305-0270 J9 J BIOGEOGR JI J. Biogeogr. PD MAR PY 2005 VL 32 IS 3 BP 493 EP 501 DI 10.1111/j.1365-2699.2005.01165.x PG 9 WC Ecology; Geography, Physical SC Environmental Sciences & Ecology; Physical Geography GA 901XM UT WOS:000227315600011 ER PT J AU Cybulski, H Krems, RV Sadeghpour, HR Dalgarno, A Klos, J Groenenboom, GC van der Avoird, A Zgid, D Chalasinski, G AF Cybulski, H Krems, RV Sadeghpour, HR Dalgarno, A Klos, J Groenenboom, GC van der Avoird, A Zgid, D Chalasinski, G TI Interaction of NH(X (3)Sigma(-)) with He: Potential energy surface, bound states, and collisional Zeeman relaxation SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID DISCRETE VARIABLE REPRESENTATION; FINE-STRUCTURE SPECTRUM; MATRIX KOHN METHOD; ULTRACOLD MOLECULES; REACTIVE SCATTERING; GROUND-STATE; QUANTUM; SPECTROSCOPY; FIELD AB A detailed analysis of the He-NH((3)Sigma(-)) van der Waals complex is presented. We discuss ab initio calculations of the potential energy surface and fitting procedures with relevance to cold collisions, and we present accurate calculations of bound energy levels of the triatomic complex as well as collisional properties of NH molecules in a buffer gas of He-3. The influence of the external magnetic field used to trap the NH molecules and the effect of the atom-molecule interaction potential on the collisionally induced Zeeman relaxation are explored. It is shown that minute variations of the interaction potential due to different fitting procedures may alter the Zeeman relaxation rate at ultralow temperatures by as much as 50%. (C) 2005 American Institute of Physics. C1 Warsaw Univ, Dept Chem, PL-02093 Warsaw, Poland. Univ Nijmegen, Inst Theoret Chem, NSRIM, NL-6525 ED Nijmegen, Netherlands. Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. Oakland Univ, Dept Chem, Rochester, MI 48309 USA. RP Warsaw Univ, Dept Chem, PL-02093 Warsaw, Poland. EM rkrems@cfa.harvard.edu; jakl@theochem.ru.nl; gerritg@theochem.ru.nl; avda@theochem.ru.nl RI Klos, Jacek/A-6457-2008; Groenenboom, Gerrit/F-9692-2015; Cybulski, Hubert/G-3724-2014 OI Klos, Jacek/0000-0002-7407-303X; NR 43 TC 59 Z9 60 U1 1 U2 8 PU AMER INST PHYSICS PI MELVILLE PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA SN 0021-9606 EI 1089-7690 J9 J CHEM PHYS JI J. Chem. Phys. PD MAR 1 PY 2005 VL 122 IS 9 AR 094307 DI 10.1063/1.1857473 PG 8 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 904GE UT WOS:000227483300028 PM 15836128 ER PT J AU Stanley, JD AF Stanley, JD TI Growth faults, a distinct carbonate-siliciclastic interface and recent coastal evolution, NW Nile delta, Egypt SO JOURNAL OF COASTAL RESEARCH LA English DT Article DE Abu Qir Bay; Alexandria; basin subsidence; Canopus; carbonates; delta facies; depressed shelf platform; earthquakes; growth faults; Herakleion; Holocene; joint structures; kurkar; Nile River; Pleistocene; quartz; seismic profiles ID LATE QUATERNARY EVOLUTION; ALEXANDRIA REGION; SEDIMENTS; EROSION; SHELF AB A sharp, well-defined interface between a late Pleistocene carbonate sandstone ridge (kurkar) and Holocene unconsolidated coastal siliciclastic sediment has formed largely as a consequence of recent structural activity along the NW Nile delta coast at Abu Qir, Egypt. Joint patterns in the coastal kurkar exposed on land, and its irregular and dislocated configuration beneath Abu Qir Bay, suggest that the ridge east of Alexandria was stretched, down-bowed and offset in a NE direction. The ridge has subsided by growth faults to shallow depths in the bay, resulting in westward coastal regression toward the Abu Qir peninsula by headscarp retreat. Deformation of the coastal margin and development of the distinct lithological interface occurred primarily from late Pleistocene to early Holocene time, although continued subsidence and disruption of the late Quaternary section has occurred locally in the bay as recently as the first millennium C.E. Both emerged land and coastal-to-shallow bay phenomena are a probable response to readjustment at depth of the thick (> 5000 m) Mesozoic to Quaternary sediment section lying beneath the recent NW Nile delta. This shift deep within the underlying sediment pile has lowered the bay floor and likely accounts for some shallow to intermediate depth earthquakes along, and proximal to, the Alexandria to Abu Qir coastal margin. C1 Smithsonian Inst, Geoarchaeol Global Change Program, Washington, DC 20560 USA. RP Stanley, JD (reprint author), Smithsonian Inst, Geoarchaeol Global Change Program, E-205 NMNH, Washington, DC 20560 USA. NR 63 TC 2 Z9 2 U1 0 U2 2 PU COASTAL EDUCATION & RESEARCH FOUNDATION PI LAWRENCE PA 810 EAST 10TH STREET, LAWRENCE, KS 66044 USA SN 0749-0208 EI 1551-5036 J9 J COASTAL RES JI J. Coast. Res. PD SPR PY 2005 SI 42 BP 309 EP 318 PG 10 WC Environmental Sciences; Geography, Physical; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Physical Geography; Geology GA 947FU UT WOS:000230629600035 ER PT J AU Salazar, CA Jiggins, CD Arias, CF Tobler, A Bermingham, E Linares, M AF Salazar, CA Jiggins, CD Arias, CF Tobler, A Bermingham, E Linares, M TI Hybrid incompatibility is consistent with a hybrid origin of Heliconius heurippa Hewitson from its close relatives, Heliconius cydno Doubleday and Heliconius melpomene Linnaeus SO JOURNAL OF EVOLUTIONARY BIOLOGY LA English DT Article DE Dominance Theory; Haldane's rule; Heliconius; hybrid speciation; Lepidoptera ID HALDANES RULE; POSTZYGOTIC ISOLATION; REPRODUCTIVE ISOLATION; DROSOPHILA-SIMULANS; GENETIC DISSECTION; SPECIATION; BUTTERFLIES; EVOLUTION; STERILITY; DOMINANCE AB Shared ancestral variation and introgression complicates the reconstruction of phylogenetic relationships among closely related taxa. Here we use overall genomic compatibility as an alternative estimate of species relationships in a group where divergence is rapid and genetic exchange is common. Heliconius heurippa, a butterfly species endemic to Colombia, has a colour pattern genetically intermediate between H. cydno and H. melpomene: its hindwing is nearly indistinguishable from that of H. melpomene and its forewing band is an intermediate phenotype between both species. This observation has lead to the suggestion that the pattern of H. heurippa arose through hybridization. We present a genetic analysis of hybrid compatibility in crosses between the three taxa. Heliconius heurippa x H. cydno and female H. melpomene x male H. heurippa yield fertile and viable F-1 hybrids, but male H. melpomene x female H. heurippa crosses yield sterile F-1 females. In contrast, Haldane's rule has previously been detected between H. melpomene and H cydno in both directions. Therefore, H. heurippa is most closely related to H. cydno, with some evidence for introgression of genes from H. melpomene. The results are compatible with the hypothesis of a hybrid origin for H. heurippa. In addition, backcrosses using F-1 hybrid males provide evidence for a large Z(X)-chromosome effect on sterility and for recessive autosomal sterility factors as predicted by Dominance Theory. C1 Univ Los Andes, Inst Genet, Bogota, Colombia. Duke Univ, Dept Biol, Durham, NC USA. Univ Edinburgh, Inst Evolutionary Biol, Edinburgh, Midlothian, Scotland. Smithsonian Trop Res Inst, Balboa, Panama. RP Linares, M (reprint author), Univ Los Andes, Inst Genet, Cra 1-18A-70, Bogota, Colombia. EM mlinares@uniandes.edu.co RI Jiggins, Chris/B-9960-2008; Salazar, camilo/A-1647-2010; Arias, Carlos/G-2881-2016; Linares, Mauricio/I-3509-2016 OI Jiggins, Chris/0000-0002-7809-062X; Salazar, camilo/0000-0001-9217-6588; Arias, Carlos/0000-0001-5925-0985; Linares, Mauricio/0000-0002-1021-0226 FU Biotechnology and Biological Sciences Research Council [BBS/B/09074] NR 49 TC 24 Z9 27 U1 1 U2 15 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 1010-061X J9 J EVOLUTION BIOL JI J. Evol. Biol. PD MAR PY 2005 VL 18 IS 2 BP 247 EP 256 DI 10.1111/j.1420-9101.2004.00839.x PG 10 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 897PP UT WOS:000227017400001 PM 15715831 ER PT J AU Pelaez, J Lorenzini, EC AF Pelaez, J Lorenzini, EC TI Libration control of electrodynamic tethers in inclined orbit SO JOURNAL OF GUIDANCE CONTROL AND DYNAMICS LA English DT Article; Proceedings Paper CT AAS/AIAA 13th Space Flight Mechanics Meeting CY FEB 09-13, 2003 CL Ponce, PR SP AAS, Amer Inst Aeronaut & Astronaut ID PERIODIC-ORBITS; DYNAMIC INSTABILITY; DELAY FEEDBACK; STABILITY; CHAOS; KIND AB Any electrodynamic tether working in an inclined orbit is affected by a dynamic instability generated by the continuos pumping of energy from electromagnetic forces into the tether attitude motion. To overcome the difficulties associated with this instability, two control schemes have been analyzed. In both cases the background strategy is the same: we add appropriate forces to the system with the aim of converting an unstable periodic orbit of the governing equations into an asymptotically stable one. The idea is to take such a stabilized periodic orbit as the starting point for the operation of the electrodynamic tether. In the first case, the unstable periodic orbit is taken as a reference orbit. In the second one, we use a delay feedback control scheme that has been used successfully in problems with one degree of freedom. To obtain results with broad validity, some simplifying assumptions have been introduced in the analysis. Thus, we assume a rigid tether with two end masses orbiting along a circular, inclined orbit. We also assume a constant tether current that does not depend on the attitude and orbital position of the tether, and the Earth's magnetic field is modeled as a dipole aligned with the Earth's rotation axis. C1 Tech Univ Madrid, Escuela Tecn Super Ingn Aeronaut, E-28040 Madrid, Spain. Harvard Smithsonian Ctr Astrophys, Special Projects Grp, Radio & Geoastron Div, Cambridge, MA 02138 USA. RP Pelaez, J (reprint author), Tech Univ Madrid, Escuela Tecn Super Ingn Aeronaut, Pl Cardenal Cisneros 3, E-28040 Madrid, Spain. EM j.pelaez@upm.es; elorenzini@cfa.harvard.edu RI Pelaez, Jesus/M-7806-2016 OI Pelaez, Jesus/0000-0001-9755-1674 NR 16 TC 34 Z9 37 U1 1 U2 7 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0731-5090 J9 J GUID CONTROL DYNAM JI J. Guid. Control Dyn. PD MAR-APR PY 2005 VL 28 IS 2 BP 269 EP 279 DI 10.2514/1.6473 PG 11 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA 906IB UT WOS:000227633200010 ER PT J AU Henry, TJ Covell, CV Wheeler, AG AF Henry, TJ Covell, CV Wheeler, AG TI An annotated list of the plant bugs, or Miridae (Hemiptera : Heteroptera), of Kentucky SO JOURNAL OF THE NEW YORK ENTOMOLOGICAL SOCIETY LA English DT Article DE Heteroptera; Miridae; Kentucky; checklist; hosts; distributions ID HOST PLANTS; SEASONAL HISTORY; LIFE-HISTORY; DIAPHNOCORIS-CHLORIONIS; ORNAMENTAL HONEYLOCUST; ARTHROPOD FAUNA; NYMPHAL STAGES; UNITED-STATES; 5TH INSTAR; BIOLOGY AB A list of 202 species of Miridae, or plant bugs, of Kentucky is presented, based on study of more than 4,000 specimens from the University of Kentucky and University of Louisville collections and fieldwork conducted by the authors, supplemented by a review of the literature. One- hundred seventy-six species are newly recorded front the state; 26 species previously were known in Kentucky based on the most recent North American Heteroptera catalog and a few other literature sources. The Miridae in this list are arranged alphabetically by subfamily, tribe, genus, and species. Distribution, dates, host plants, depository, and number of specimens examined are provided for each species. When a Kentucky host was not recorded, literature documenting known hosts is given, along with selected papers providing biological information. C1 Smithsonian Inst, Systemat Entomol Lab, PSI, Natl Museum Nat Hist,USDA ARS, Washington, DC 20013 USA. Univ Louisville, Dept Biol, Louisville, KY 40292 USA. Clemson Univ, Dept Entomol, Clemson, SC 29634 USA. RP Henry, TJ (reprint author), Smithsonian Inst, Systemat Entomol Lab, PSI, Natl Museum Nat Hist,USDA ARS, CO POB 37012,MRC-0168, Washington, DC 20013 USA. EM thenry@sel.barc.usda.gov; covell@louisville.edu; awhlr@clemson.edu NR 78 TC 6 Z9 8 U1 0 U2 3 PU NEW YORK ENTOMOLOGICAL SOC INC PI NEW YORK PA C/O AMER MUSEUM NAT HIST 79TH & CENTRAL PARK WEST, NEW YORK, NY 10024 USA SN 0028-7199 J9 J NEW YORK ENTOMOL S JI J. N.Y. Entomol. Soc. PD SPR-SUM PY 2005 VL 113 IS 1-2 BP 24 EP 76 DI 10.1664/0028-7199(2005)113[0024:AALOTP]2.0.CO;2 PG 53 WC Entomology SC Entomology GA 969UE UT WOS:000232259700003 ER PT J AU Cooper, DV Grobler, D Bush, M Jessup, D Lance, W AF Cooper, DV Grobler, D Bush, M Jessup, D Lance, W TI Anaesthesia of nyala (Tragelaphus angasi) with a combination of thiafentanil (A3080), medetomidine and ketamine SO JOURNAL OF THE SOUTH AFRICAN VETERINARY ASSOCIATION-TYDSKRIF VAN DIE SUID-AFRIKAANSE VETERINERE VERENIGING LA English DT Article DE A3080; anaesthesia; atipamezole hydrochloride; ketamine hydrochloride; medetomidine hydrochloride; naltrexone hydrochloride; nyala; thiafentanil; Tragelaplius angasi ID IMPALA AEPYCEROS-MELAMPUS; ORYX ORYX-LEUCORYX; IMMOBILIZATION; ATIPAMEZOLE; A-3080 AB A combination of thiafentanil (A3080), medetomidine hydrochloride (MED) and ketamine hydrochloride (KET) was evaluated in 19 boma-habituated (12 female and 7 males) and 9 free-ranging nyala (7 male and 2 females) (Tragelaphus angasi) to develop a safe and reliable anaesthesia protocol. Wide dosages were used safely during this study with ranges for A3080 of 45 +/- 8 mu g/kg with MED of 69 +/- 19 mu g/kg and KET of 3.7 1.0 mg/kg (200 mg/ animal). The dosages developed on boma-habituated nyala proved to be equally effective in 9 adult free-ranging nyala (7 males and 2 females). The optimum dosage for nyala was a combination of A3080 (40-50 mu g/kg), MED (60-80 mu g/kg) plus 200 mg of KET/animal. The anaesthesia was characterised by a short induction, good muscle relaxation and mild hypoxaemia during monitoring the anaesthesia was rapidly and completely reversed by naltrexone hydrochloride (30 mg/mg of A3080) and atipamezole hydrochloride (5 mg/mg of MED) given intramuscularly. There was no mortality or morbidity associated with this protocol. C1 Conservat & Res Ctr, Smithsonian Natl Zool Pk, Front Royal, VA 22630 USA. Ezemvelo Kwa Zulu Natal Wildlife, ZA-3936 St Lucia, South Africa. S African Natl Parks, Kruger Pk, South Africa. Int Wildlife Vet Sci, Santa Cruz, CA 95060 USA. Wildlife Pharmaceut Inc, Ft Collins, CO 80524 USA. RP Bush, M (reprint author), Conservat & Res Ctr, Smithsonian Natl Zool Pk, 1500 Remount Rd, Front Royal, VA 22630 USA. EM mbush@crc.si.edu NR 20 TC 8 Z9 9 U1 1 U2 6 PU SOUTH AFRICAN VET ASSN PI MONUMENT PARK PA PO BOX 25033, MONUMENT PARK 0105, SOUTH AFRICA SN 0038-2809 J9 J S AFR VET ASSOC JI J. S. Afr. Vet. Assoc.-Tydskr. Suid-Afr. Vet. Ver. PD MAR PY 2005 VL 76 IS 1 BP 18 EP 21 PG 4 WC Veterinary Sciences SC Veterinary Sciences GA 927UE UT WOS:000229225200004 PM 15900895 ER PT J AU Launius, RD AF Launius, RD TI Wheels for the world: Henry Ford, his company, and a century of progress SO JOURNAL OF THE WEST LA English DT Book Review C1 Smithsonian Inst, Washington, DC 20560 USA. RP Launius, RD (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU J WEST INC PI MANHATTAN PA P O BOX 1009, MANHATTAN, KS 66505-1009 USA SN 0022-5169 J9 J WEST JI J. West PD SPR PY 2005 VL 44 IS 2 BP 113 EP 114 PG 2 WC History SC History GA 964AM UT WOS:000231848300105 ER PT J AU Fornara, DA Dalling, JW AF Fornara, DA Dalling, JW TI Seed bank dynamics in five Panamanian forests SO JOURNAL OF TROPICAL ECOLOGY LA English DT Article DE environmental gradient; phenology; seasonality; soil seed bank ID TROPICAL FOREST; GERMINATION; COMMUNITY; SIZE C1 Univ Statale Milano, Sez Bot Ambientale & Appl, Dipartimento Biol, Milan, Italy. Univ Illinois, Dept Plant Biol, Urbana, IL 61801 USA. Smithsonian Trop Res Inst, Balboa, Panama. RP Fornara, DA (reprint author), Univ Pretoria, Dept Zool & Entomol, Mammal Res Inst, ZA-0002 Pretoria, South Africa. EM dfornara@zoology.up.ac.za RI Fornara, Dario/J-3315-2013; OI Fornara, Dario/0000-0002-5381-0803 NR 17 TC 7 Z9 8 U1 2 U2 7 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 40 WEST 20TH ST, NEW YORK, NY 10011-4211 USA SN 0266-4674 J9 J TROP ECOL JI J. Trop. Ecol. PD MAR PY 2005 VL 21 BP 223 EP 226 DI 10.1017/S0266467404002184 PN 2 PG 4 WC Ecology SC Environmental Sciences & Ecology GA 911TO UT WOS:000228028100012 ER PT J AU Molella, A AF Molella, A TI Human-built world: How to think about technology and culture SO MINERVA LA English DT Book Review C1 Smithsonian Inst, Natl Museum Amer Hist, Lemelson Ctr Study Invent & Innovat, Washington, DC 20013 USA. RP Molella, A (reprint author), Smithsonian Inst, Natl Museum Amer Hist, Lemelson Ctr Study Invent & Innovat, Room 1016,MRC 604,POB 37012, Washington, DC 20013 USA. EM molellaa@si.edu NR 1 TC 1 Z9 1 U1 1 U2 2 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0026-4695 J9 MINERVA JI Minerva PD MAR PY 2005 VL 43 IS 1 BP 113 EP 117 DI 10.1007/s11024-004-6645-8 PG 5 WC Education & Educational Research; History & Philosophy Of Science; Social Sciences, Interdisciplinary SC Education & Educational Research; History & Philosophy of Science; Social Sciences - Other Topics GA 904RQ UT WOS:000227515800009 ER PT J AU Molella, A AF Molella, A TI American genesis: A century of invention and technological enthusiasm, 1870-1970, 2nd edition SO MINERVA LA English DT Book Review C1 Smithsonian Inst, Natl Museum Amer Hist, Lemelson Ctr Study Invent & Innovat, Washington, DC 20013 USA. RP Molella, A (reprint author), Smithsonian Inst, Natl Museum Amer Hist, Lemelson Ctr Study Invent & Innovat, Room 1016,MRC 604,POB 37012, Washington, DC 20013 USA. EM molellaa@si.edu NR 1 TC 1 Z9 1 U1 1 U2 2 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0026-4695 J9 MINERVA JI Minerva PD MAR PY 2005 VL 43 IS 1 BP 113 EP 117 DI 10.1007/s11024-004-6645-8 PG 5 WC Education & Educational Research; History & Philosophy Of Science; Social Sciences, Interdisciplinary SC Education & Educational Research; History & Philosophy of Science; Social Sciences - Other Topics GA 904RQ UT WOS:000227515800010 ER PT J AU Mallarino, R Bermingham, E Willmott, KR Whinnett, A Jiggins, CD AF Mallarino, R Bermingham, E Willmott, KR Whinnett, A Jiggins, CD TI Molecular systematics of the butterfly genus Ithomia (Lepidoptera : Ithomiinae): a composite phylogenetic hypothesis based on seven genes SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article DE Lepidoptera; mimicry; phylogeny; phylogenetic discordance; speciation ID MITOCHONDRIAL-DNA VARIATION; HISTORICAL BIOGEOGRAPHY; SWALLOWTAIL BUTTERFLIES; NUCLEAR GENE; EVOLUTION; INCONGRUENCE; NYMPHALIDAE; MORPHOLOGY; SEQUENCES; PATTERNS AB Butterflies in the nymphalid subfamily Ithomiinae are brightly colored and involved in mimicry. Here we present a phylogenetic hypothesis for 23 of the 24 species in the genus:Ithomia, based on seven different gene regions, representing 5 linkage groups and 4469 bp. We sequenced varying length regions of the following genes: (1) elongation factor 1alpha (Ef1 alpha; 1028 bp); (2) tektin (tektin; 715 bp); (3) wingless (wg; 405 bp); (4) ribosomal protein L5 (RpL5; 722 bp, exons 1, 2, 3, and introns 1 and 2); and (5) mitochondrial cytochrome oxidase I, II (Co1 and Co2 and intervening leucine tRNA; 1599 bp). The results show incongruence between some genetic loci, although when alternate topologies are compared statistically it was generally true that one topology was supported by a majority of loci sampled. This highlights the need to sample widely across the genome in order to obtain a well-supported phylogenetic hypothesis. A combined evidence topology is presented based on a Bayesian analysis of all the gene regions, except the fast-evolving RpL5. The resulting hypothesis is concordant with the most probable relationships determined from our topological comparisons, although in some parts of the tree relationships remain weakly supported. The tree suggests diversification has largely occurred within biogeographic regions such as Central America, the Amazon, the southern and northern Andes, with only occasional dispersal (or vicariance) between such regions. This phylogenetic hypothesis can now be used to investigate patterns of diversification across the genus, such as the potential role of color pattern changes in speciation. (C) 2004 Elsevier Inc. All rights reserved. C1 Univ Edinburgh, Inst Evolutionary Biol, Edinburgh EH9 3JT, Midlothian, Scotland. Smithsonian Trop Res Inst, Balboa, Panama. Nat Hist Museum, London SW7 5BD, England. UCL, Galton Lab, London NW1 2HE, England. RP Jiggins, CD (reprint author), Univ Edinburgh, Inst Evolutionary Biol, Edinburgh EH9 3JT, Midlothian, Scotland. EM chris.jiggins@ed.ac.uk RI Jiggins, Chris/B-9960-2008 OI Jiggins, Chris/0000-0002-7809-062X NR 45 TC 44 Z9 48 U1 1 U2 12 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 1055-7903 J9 MOL PHYLOGENET EVOL JI Mol. Phylogenet. Evol. PD MAR PY 2005 VL 34 IS 3 BP 625 EP 644 DI 10.1016/j.ympev.2004.10.021 PG 20 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 897UT UT WOS:000227031600014 PM 15683934 ER PT J AU Thoroughgood, TD Dhillon, VS Steeghs, D Watson, CA Buckley, DAH Littlefair, SP Smith, DA Still, M van der Heyden, KJ Warner, B AF Thoroughgood, TD Dhillon, VS Steeghs, D Watson, CA Buckley, DAH Littlefair, SP Smith, DA Still, M van der Heyden, KJ Warner, B TI The component masses of the cataclysmic variable V347 Puppis SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; binaries : eclipsing; binaries : spectroscopic; stars : individual : V347 Pup; novae, cataclysmic variables ID DW URSAE MAJORIS; X-RAY BINARIES; ACCRETION DISKS; DOPPLER TOMOGRAPHY; WHITE-DWARF; SPECTROSCOPIC OBSERVATIONS; ROCHE TOMOGRAPHY; SECONDARY STARS; SW SEXTANTIS; LOW STATE AB We present time-resolved spectroscopy and photometry of the double-lined eclipsing cataclysmic variable V347 Pup ( = LB 1800). There is evidence of irradiation on the inner hemisphere of the secondary star, which we correct for using a model to give a secondary-star radial velocity of K R = 198 +/- 5 km s(-1). The rotational velocity of the secondary star in V347 Pup is found to be v sin i = 131 +/- 5 km s(-1) and the system inclination is i = 84degrees.0 +/- 2degrees.3. From these parameters we obtain masses of M-1 = 0.63 +/- 0.04 M for the white dwarf primary and M-2 = 0.52 +/- 0.06 M for the M0.5V secondary star, giving a mass ratio of q = 0.83 +/- 0.05. On the basis of the component masses, and the spectral type and radius of the secondary star in V347 Pup, we find tentative evidence for an evolved companion. V347 Pup shows many of the characteristics of the SW Sex stars, exhibiting single-peaked emission lines, high-velocity S-wave components and phase-offsets in the radial velocity curve. We find spiral arms in the accretion disc of V347 Pup and measure the disc radius to be close to the maximum allowed in a pressureless disc. C1 Univ Sheffield, Dept Phys & Astron, Sheffield S3 7RH, S Yorkshire, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. S African Astron Observ, ZA-7935 Cape Town, South Africa. Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England. Winchester Coll, Winchester SO23 9LX, Hants, England. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Cape Town, Dept Astron, ZA-7700 Rondebosch, South Africa. RP Univ Sheffield, Dept Phys & Astron, Sheffield S3 7RH, S Yorkshire, England. EM Tim.Thoroughgood@shef.ac.uk RI Steeghs, Danny/C-5468-2009; OI Steeghs, Danny/0000-0003-0771-4746; Littlefair, Stuart/0000-0001-7221-855X NR 63 TC 12 Z9 12 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 MAR 1 PY 2005 VL 357 IS 3 BP 881 EP 894 DI 10.1111/j.1365-2966.2004.08613.x PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 898OP UT WOS:000227086400007 ER PT J AU Molina, MC DePriest, PT Lawrey, JD AF Molina, MC DePriest, PT Lawrey, JD TI Genetic variation in the widespread lichenicolous fungus Marchandiomyces corallinus SO MYCOLOGIA LA English DT Article DE basidiomycetes; host-parasite evolution; lichenicolous fungi; lichens; Marchandiomyces; rDNA sequences ID RHIZOCTONIA-SOLANI; ANASTOMOSIS GROUPS; ATHELIA-ROLFSII; DNA; DIVERSITY; SYMBIOSES; DIFFERENTIATION; IDENTIFICATION; BASIDIOMYCOTA; RELATEDNESS AB The lichenicolous basidiomycete Marchandiomyces corallinus is widely distributed in North America and Europe, where it commonly is found on a variety of lichens. Theoretically either of these characteristics, a wide geographic range or generalized host ecology, could provide opportunities for genetic differentiation within this species. To determine how genetic variation is partitioned in M. corallinus, 12 fungal isolates were obtained from locations in North America and Europe; at two locations, in Washington County, Maine, and on the Isle of Mull in Scotland, fungi also were isolated from different lichen hosts. Vegetative mycelial compatibility tests were used to determine compatibility groupings from among the isolates; in addition, several PCR amplification products (RAPD, nuITS rDNA) were obtained for each isolate. A number of distinct compatibility groups were recognizable based on geography, not host ecology. In addition compatible isolates always were restricted to either North America or Europe. However RAPD markers indicated that compatible isolates are not always genetically identical. The presence of sequence heterozygosity at specific positions indicated that the isolates are heterokaryotic and a number of distinct haplotypes could be identified based on ITS variation at three separate locations. This type of genetic variation in these fungi suggests that sexual recombination is possible and that genetic differentiation has taken place recently as a result of geographic isolation, not host switching. C1 Univ Rey Juan Carlos, Dept Matemat & Fis Aplicadas & Ciencias Nat, Escuela Super Ciencias Expt & Technol, Madrid 28933, Spain. Smithsonian Inst, Bot Sect, US Natl Herbarium, Washington, DC 20013 USA. George Mason Univ, Dept Environm Sci & Policy, Fairfax, VA 22030 USA. RP Molina, MC (reprint author), Univ Rey Juan Carlos, Dept Matemat & Fis Aplicadas & Ciencias Nat, Escuela Super Ciencias Expt & Technol, Madrid 28933, Spain. EM cmolina@escet.urjc.es RI Molina, Maria del Carmen/H-9399-2015; DePriest, Paula/K-6633-2015 OI Molina, Maria del Carmen/0000-0002-8397-5887; NR 43 TC 6 Z9 9 U1 0 U2 1 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 2005 VL 97 IS 2 BP 454 EP 463 DI 10.3852/mycologia.97.2.454 PG 10 WC Mycology SC Mycology GA 943EZ UT WOS:000230336600018 PM 16396353 ER PT J AU Wurth, MKR Pelaez-Riedl, S Wright, SJ Korner, C AF Wurth, MKR Pelaez-Riedl, S Wright, SJ Korner, C TI Non-structural carbohydrate pools in a tropical forest SO OECOLOGIA LA English DT Article DE biodiversity; carbon balance; global change; seasonality; wood reserves ID ELEVATED CARBON-DIOXIDE; NITROGEN NUTRITION; CLIMATE TREES; CO2; RESPONSES; STORAGE; GROWTH; PLANTS; LEAF; WATER AB The pool size of mobile, i.e. non-structural carbohydrates (NSC) in trees reflects the balance between net photosynthetic carbon uptake (source) and irreversible investments in structures or loss of carbon (sink). The seasonal variation of NSC concentration should reflect the sink/source relationship, provided all tissues from root to crown tops are considered. Using the Smithsonian canopy crane in Panama we studied NSC concentrations in a semi-deciduous tropical forest over 22 months. In the 9 most intensively studied species (out of the 17 investigated), we found higher NSC concentrations (starch, glucose, fructose, sucrose) across all species and organs in the dry season than in the wet season (NSC 7.2% vs 5.8% of dry matter in leaves, 8.8/6.0 in branches, 9.7/8.5 in stems, 8.3/6.4 in coarse and 3.9/2.2 in fine roots). Since this increase was due to starch only, we attribute this to drought-constrained growth (photosynthesis less affected by drought than sink activity). Species-specific phenological rhythms (leafing or fruiting) did not overturn these seasonal trends. Most of the stem volume (diameter at breast height around 40 cm) stores NSC. We present the first whole forest estimate of NSC pool size, assuming a 200 t ha(-1) forest biomass: 8% of this i.e. ca. 16 t ha(-1) is NSC, with ca. 13 t ha(-1) in stems and branches, ca. 0.5 and 2.8 t ha(-1) in leaves and roots. Starch alone (ca. 10.5 t ha(-1)) accounts for far more C than would be needed to replace the total leaf canopy without additional photosynthesis. NSC never passed through a period of significant depletion. Leaf flushing did not draw heavily upon NSC pools. Overall, the data imply a high carbon supply status of this forest and that growth during the dry season is not carbon limited. Rather, water shortage seems to limit carbon investment (new tissue formation) directly, leaving little leeway for a direct CO2 fertilization effects. C1 Univ Basel, Inst Bot, CH-4056 Basel, Switzerland. Smithsonian Trop Res Inst, Balboa, Panama. RP Korner, C (reprint author), Univ Basel, Inst Bot, Schonbeinstr 6, CH-4056 Basel, Switzerland. EM ch.koerner@unibas.ch RI Korner, Christian/B-6592-2014; Wright, Stuart/M-3311-2013 OI Wright, Stuart/0000-0003-4260-5676 NR 49 TC 135 Z9 159 U1 11 U2 77 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013 USA SN 0029-8549 J9 OECOLOGIA JI Oecologia PD MAR PY 2005 VL 143 IS 1 BP 11 EP 24 DI 10.1007/s00442-004-1773-2 PG 14 WC Ecology SC Environmental Sciences & Ecology GA 902PT UT WOS:000227369700002 PM 15578227 ER PT J AU Van Bael, SA Brawn, JD AF Van Bael, SA Brawn, JD TI The direct and indirect effects of insectivory by birds in two contrasting Neotropical forests SO OECOLOGIA LA English DT Article DE arthropods; canopy; herbivory; multitrophic interactions; predation ID FOOD-WEB COMPLEXITY; TROPHIC CASCADES; POPULATION CONTROL; PRIMARY PRODUCTIVITY; HERBIVOROUS INSECTS; COMMUNITY STRUCTURE; RELATIVE ROLES; LEAF DAMAGE; BOTTOM-UP; WHITE OAK AB A goal among community ecologists is to predict when and where trophic cascades occur. For example, several studies have shown that forest birds can limit arthropod abundances on trees, but indirect effects of bird predation (i.e. decreased arthropod damage to trees) are not always observed and their context is not well understood. Because productivity is one factor that is expected to influence trophic cascades, we compared the extent to which birds indirectly limit herbivore damage to trees in two lowland Neotropical forests that differed in seasonality of leaf production and rainfall. We compared the effects of bird predation on local arthropod densities and on damage to foliage through a controlled experiment using bird exclosures in the canopy and understory of two forests. We found that birds decreased local arthropod densities and leaf damage in the canopy of the drier site during periods of high leaf production, but not in the wetter forest where leaf production was low and sporadic throughout the year. Birds had no effect on arthropod abundances and leaf damage in the understory where leaf production and turnover rates were low. In support of these experimental interpretations, although we observed that arthropod densities were similar at the two sites, bird densities and the rate at which birds captured arthropods were greater at the drier, seasonally productive site. The influence of top-down predation by birds in limiting herbivorous insects appears to be conditional and most important when the production and turnover of leaves are comparatively high. C1 Univ Illinois, Dept Anim Biol, Urbana, IL 61801 USA. Univ Illinois, Dept Nat Resources & Environm Sci, Urbana, IL 61801 USA. RP Van Bael, SA (reprint author), Smithsonian Trop Res Inst, Apartado 2072, Ancon, Panama. EM vanbaels@si.edu NR 66 TC 23 Z9 24 U1 2 U2 21 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013 USA SN 0029-8549 J9 OECOLOGIA JI Oecologia PD MAR PY 2005 VL 143 IS 1 BP 106 EP 116 DI 10.1007/s00442-004-1774-1 PG 11 WC Ecology SC Environmental Sciences & Ecology GA 902PT UT WOS:000227369700011 PM 15586294 ER PT J AU Schmidt, BK Branch, WR AF Schmidt, BK Branch, WR TI Nests and eggs of the Black-headed Bee-eater (Merops breweri) in Gabon, with notes on other bee-eaters SO OSTRICH LA English DT Article C1 Smithsonian Inst, Div Birds, Washington, DC 20013 USA. Bayworld, ZA-6013 Humewood, South Africa. RP Schmidt, BK (reprint author), Smithsonian Inst, Div Birds, POB 37012, Washington, DC 20013 USA. EM schmidtb@si.edu NR 7 TC 1 Z9 1 U1 0 U2 2 PU BIRDLIFE SOUTH AFRICA PI GREENSIDE PA PO BOX 84394, GREENSIDE 2034, SOUTH AFRICA SN 0030-6525 J9 OSTRICH JI Ostrich PD MAR PY 2005 VL 76 IS 1-2 BP 80 EP 81 PG 2 WC Ornithology SC Zoology GA 926KH UT WOS:000229121600012 ER PT J AU Buzas, MA Hayek, LAC AF Buzas, MA Hayek, LAC TI On richness and evenness within and between communities SO PALEOBIOLOGY LA English DT Article ID SPECIES-ABUNDANCE; RELATIVE ABUNDANCE; DIVERSITY INDEXES; SHE ANALYSIS; MODELS; FORAMINIFERA; POPULATION; PARAMETERS; PATTERNS AB Although there is extraordinary interest in the quantitative measurement of species diversity, published statements on the behavior of the components of species diversity are contradictory and lead to opposite conclusions. In this paper, we demonstrate that the confusion is due to two key oversights: (1) whether or not biological sampling is carried out within or between communities; and (2) determination of the statistical distribution underlying a biological community, which is crucial for the evaluation of all of the components of diversity measurement. The problem of sampling "within" a population or community is basically distinct from the equivalent integration of structure and diversity measurement "between" differing multispecies populations. "Within-community sampling" is defined as a set of biological samples from a statistical population that has a particular statistical distribution or a constant value for the associated parameter(s). As the number of individuals increases along with the number of species, for a log series distribution, the diversity measures of Shannon's H, log series or Fisher's alpha, and Simpson's Index 1/lambda remain constant while the evenness measures of Buzas-Gibson's E and Pielou's J decrease. For a log-normal distribution, J will remain constant while E decreases and alpha, 1/lambda, and H increase. No single measure of evenness remains constant over all statistical distributions, so if constancy as a type of independence is required, the appropriate distribution must first be determined. Each species ensemble is mathematically fixed by the applicable statistical distribution. In contrast, "between-community sampling" is defined as a set of biological samples from different statistical distributions and/or the same distribution with differing parametric values. If sampling is between communities and S increases while the number of individuals remains constant, then all the other measures considered here increase. The exception is the broken stick, for which E remains constant while H, J, alpha, and 1/lambda increase. Herein we propose and justify the use of the log-series distribution (with regression on the information decomposition equation) as a null model for determination of community structure and demonstrate that the community structure of a Miocene bed at Calvert Cliffs, Maryland, is a log series by use of this new unified methodology. C1 Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA. Smithsonian Inst, Washington, DC 20560 USA. RP Buzas, MA (reprint author), Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA. EM buzas.marty@nmnh.si.edu; hayek.lee-ann@nmnh.si.edu NR 58 TC 42 Z9 45 U1 2 U2 24 PU PALEONTOLOGICAL SOC INC PI LAWRENCE PA 810 EAST 10TH ST, LAWRENCE, KS 66044 USA SN 0094-8373 J9 PALEOBIOLOGY JI Paleobiology PD SPR PY 2005 VL 31 IS 2 BP 199 EP 220 DI 10.1666/0094-8373(2005)031[0199:ORAEWA]2.0.CO;2 PG 22 WC Biodiversity Conservation; Ecology; Evolutionary Biology; Paleontology SC Biodiversity & Conservation; Environmental Sciences & Ecology; Evolutionary Biology; Paleontology GA 937HI UT WOS:000229914800002 ER PT J AU Sobrino, C Neale, PJ Lubian, LM AF Sobrino, C Neale, PJ Lubian, LM TI Interaction of UV radiation and inorganic carbon supply in the inhibition of photosynthesis: Spectral and temporal responses of two marine picoplankton SO PHOTOCHEMISTRY AND PHOTOBIOLOGY LA English DT Article ID ULTRAVIOLET-RADIATION; B RADIATION; NANNOCHLOROPSIS-GADITANA; CHLOROPHYLL FLUORESCENCE; DUNALIELLA-TERTIOLECTA; PIGMENT COMPOSITION; HIGH-CO2 CONDITIONS; CO2; PHYTOPLANKTON; EUSTIGMATOPHYCEAE AB The effect of ultraviolet radiation (UVR) on inhibition of photosynthesis was studied in two species of marine picoplankton with different carbon concentration mechanisms: Nannochloropsis gaditana Lubian possesses a bicarbonate uptake system and Nannochloris atomus Butcher a CO2 active transport system. Biological weighting functions (BWFs) for inhibition of photosynthesis by UVR and photosynthesis VS irradiance (PI) curves for photosynthetically active radiation (PAR) were estimated for both species grown with an enriched CO2 Supply (high dissolved inorganic carbon [DIC]: 1% CO2 in air) and in atmospheric CO2 levels (low DIC: 0.03% CO2). The response to UVR and PAR exposures was different in each species depending on the DIC treatment. Under PAR exposure, rates of maximum photosynthesis were similar between treatments in N. gaditana. However, the cultures growing in high DIC had lower sensitivity to UVR than the low DIC cultures. In contrast, N. atomus had higher rates of photosynthesis under PAR exposure with high DIC, but the BWFs were not significantly different between treatments. The results suggest that one or more processes in N. gaditana associated with HCO3- transport are target(s) for UV photodamage because there was relatively less UV inhibition of the high DIC-grown cultures in which inorganic carbon fixation is supplied by passive CO2 diffusion. Time courses of photochemical efficiency in PAR, during UV exposure and during subsequent recovery in PAR, were determined using a pulse amplitude modulated fluorometer. The results were consistent with the BWFs. In all time courses, a steady state was obtained after an initial decrease, consistent with a dynamic balance between damage and repair as found for other phytoplankton. However, the relationship of response to exposure showed a steep decline in activity that is consistent with a constant rate of repair. A novel feature of a model developed from a constant repair rate is an explicit threshold for photosynthetic response to UV. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. CSIC, Inst Ciencias Marinas Andalucia, Cadiz, Spain. RP Sobrino, C (reprint author), Smithsonian Environm Res Ctr, 647 Contees Wharf Rd,POB 28, Edgewater, MD 21037 USA. EM sobrinoc@si.edu RI Neale, Patrick/A-3683-2012; Sobrino, Cristina/J-3534-2012; LUBIAN, LUIS/L-7241-2014; OI Sobrino, Cristina/0000-0003-0431-1220 NR 43 TC 39 Z9 39 U1 2 U2 13 PU AMER SOC PHOTOBIOLOGY PI AUGUSTA PA BIOTECH PARK, 1021 15TH ST, SUITE 9, AUGUSTA, GA 30901-3158 USA SN 0031-8655 J9 PHOTOCHEM PHOTOBIOL JI Photochem. Photobiol. PD MAR-APR PY 2005 VL 81 IS 2 BP 384 EP 393 DI 10.1562/2004-08-27-RA-295.1 PG 10 WC Biochemistry & Molecular Biology; Biophysics SC Biochemistry & Molecular Biology; Biophysics GA 917LO UT WOS:000228463500020 PM 15538899 ER PT J AU Zhang, JY Yan, ZC Vrinceanu, D Sadeghpour, HR AF Zhang, JY Yan, ZC Vrinceanu, D Sadeghpour, HR TI Anisotropic van der Waals coefficients for He(1 S-1)-He(2 P-3) SO PHYSICAL REVIEW A LA English DT Article ID BOSE-EINSTEIN CONDENSATION; ATOMS; HELIUM AB We report on the anisotropic mass-dependent dispersion coefficients C-6(M=0,+/- 1) for He(1 S-1)-He(2 P-3) interaction using two different techniques. The first is a highly accurate Hylleraas basis-set diagonalization, while the second method is a semiempirical assessment based on tabulated oscillator strengths and available photoionization cross sections. The results from the two techniques agree to within 1.5%. C1 Univ New Brunswick, Dept Phys, Fredericton, NB E3B 5A3, Canada. Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. RP Univ New Brunswick, Dept Phys, Fredericton, NB E3B 5A3, Canada. RI Yan, Zong-Chao/F-6668-2014 NR 19 TC 8 Z9 8 U1 1 U2 4 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2469-9926 EI 2469-9934 J9 PHYS REV A JI Phys. Rev. A PD MAR PY 2005 VL 71 IS 3 AR 032712 DI 10.1103/PhysRevA.71.032712 PN A PG 5 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 919QH UT WOS:000228632100092 ER PT J AU Hirata, CM Loeb, A Afshordi, N AF Hirata, CM Loeb, A Afshordi, N TI CMB B-mode polarization from Thomson scattering in the local universe SO PHYSICAL REVIEW D LA English DT Article ID PROBE WMAP OBSERVATIONS; MICROWAVE BACKGROUND POLARIZATION; MAGELLANIC STREAM; INFLATIONARY UNIVERSE; GALACTIC HALO; ANISOTROPIES; FLATNESS; HORIZON; GALAXY; GAS AB The polarization of the cosmic microwave background (CMB) is widely recognized as a potential source of information about primordial gravitational waves. The gravitational wave contribution can be separated from the dominant CMB polarization created by density perturbations at the times of recombination and reionization because it generates both E and B polarization modes, whereas the density perturbations create only E polarization. The limits of our ability to measure gravitational waves are thus determined by statistical and systematic errors from CMB experiments, foregrounds, and nonlinear evolution effects such as gravitational lensing of the CMB. Usually it is assumed that most foregrounds can be removed because of their frequency dependence, however Thomson scattering of the CMB quadrupole by electrons in the Galaxy or nearby structures shares the blackbody frequency dependence of the CMB. If the optical depth from these nearby electrons is anisotropic, the polarization generated can include B modes even if no tensor perturbations are present. We estimate this effect for the Galactic disk and nearby extragalactic structures, and find that it contributes to the B polarization at the level of similar to(1-2) x 10(-4) mu K per logarithmic interval in multipole l for l < 30. This is well below the detectability level even for a future CMB polarization satellite and hence is negligible. Depending on its structure and extent, the Galactic corona may be a source of B-modes comparable to the residual large-scale lensing B-mode after the latter has been cleaned using lensing reconstruction techniques. For an extremely ambitious post-Planck CMB experiment, Thomson scattering in the Galactic corona is thus a potential contaminant of the gravitational wave signal; conversely, if the other foregrounds can be cleaned out, such an experiment might be able to constrain models of the corona. C1 Princeton Univ, Dept Phys, Princeton, NJ 08544 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Princeton Univ, Dept Phys, Jadwin Hall, Princeton, NJ 08544 USA. EM chirata@princeton.edu NR 39 TC 3 Z9 3 U1 0 U2 0 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2470-0010 EI 2470-0029 J9 PHYS REV D JI Phys. Rev. D PD MAR PY 2005 VL 71 IS 6 AR 063531 DI 10.1103/PhysRevD.71.063531 PG 10 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 917SS UT WOS:000228490100039 ER PT J AU Giray, T Giovanetti, M West-Eberhard, MJ AF Giray, T Giovanetti, M West-Eberhard, MJ TI Juvenile hormone, reproduction, and worker behavior in the neotropical social wasp Polistes canadensis SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE behavioral development; division of labor; methoprene; worker polyethism ID DIVISION-OF-LABOR; PRIMITIVELY EUSOCIAL WASP; HONEY-BEE; AGE POLYETHISM; POLYBIA-OCCIDENTALIS; BOMBUS-TERRESTRIS; TASK-PERFORMANCE; TEMPORAL POLYETHISM; ROPALIDIA-MARGINATA; OVARIAN DEVELOPMENT AB Previous studies of the division of labor in colonies of eusocial Hymenoptera (wasps and bees) have led to two hypotheses regarding the evolution of juvenile hormone (JH) involvement. The novel- or single-function hypothesis proposes that the role of JH has changed from an exclusively reproductive function in primitively eusocial species (those lacking morphologically distinct queen and worker castes), to an exclusively behavioral function in highly eusocial societies (those containing morphologically distinct castes). In contrast, the split-function hypothesis proposes that JH originally functioned in the regulation of both reproduction and behavior in ancestral solitary species. Then, when reproductive and brood-care tasks came to be divided between queens and workers, the effects of JH were divided as well, with JH involved in regulation of reproductive maturation of egg-laying queens, and behavioral maturation, manifested as age-correlated changes in worker tasks, of workers. We report experiments designed to test these hypotheses. After documenting age-correlated changes in worker behavior (age polyethism) in the neotropical primitively eusocial wasp Polistes canadensis, we demonstrate that experimental application of the JH analog methoprene accelerates the onset of guarding behavior, an age-correlated task, and increases the number of foraging females; and we demonstrate that JH titers correlate with both ovarian development of queens and task differentiation in workers, as predicted by the split-function hypothesis. These findings support a view of social insect evolution that sees the contrasting worker and queen phenotypes as derived via decoupling of reproductive and brood-care components of the ancestral solitary reproductive physiology. C1 Univ Puerto Rico, Dept Biol, Rio Piedras, PR 00931 USA. Smithsonian Trop Res Inst, Panama Univ, APO, AA 34002 USA. Univ Milan, Dipartimento Biol, Sez Zool & Citol, I-20133 Milan, Italy. RP Giray, T (reprint author), Univ Puerto Rico, Dept Biol, Rio Piedras, PR 00931 USA. EM tgiray2@yahoo.com RI Giray, Tugrul/K-9570-2013; GIOVANETTI, MANUELA/I-2629-2014 OI GIOVANETTI, MANUELA/0000-0001-9442-0062 NR 74 TC 80 Z9 81 U1 5 U2 32 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 1 PY 2005 VL 102 IS 9 BP 3330 EP 3335 DI 10.1073/pnas.0409560102 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 903KC UT WOS:000227423700031 PM 15728373 ER PT J AU Kewley, LJ Jansen, RA Geller, MJ AF Kewley, LJ Jansen, RA Geller, MJ TI Aperture effects on star formation rate, metallicity, and reddening SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID H-II-REGIONS; DIGITAL SKY SURVEY; GALAXY REDSHIFT SURVEY; LARGE-MAGELLANIC-CLOUD; NEARBY FIELD GALAXIES; SPIRAL GALAXIES; ABUNDANCE GRADIENTS; HII-REGIONS; LUMINOSITY FUNCTION; CHEMICAL EVOLUTION AB We use 101 galaxies selected from the Nearby Field Galaxy Survey to investigate the effect of aperture size on the star formation rate, metallicity, and reddening determinations for galaxies. Our sample includes galaxies of all Hubble types except ellipticals with global star formation rates (SFRs) ranging from 0.01 to 100 M-. yr(-1), metallicities in the range 7.9 less than or similar to log (O/H) + 12 less than or similar to 9.0, and reddening of 0 less than or similar to A(V) less than or similar to 3.3. We compare the SFR, metallicity, and reddening derived from nuclear spectra to those derived from integrated spectra. For apertures capturing <20% of the B-26 light, the differences between nuclear and global metallicity, extinction, and SFR are substantial. Late-type spiral galaxies show the largest systematic difference (similar to 0.14 dex), with nuclear metallicities greater than the global metallicities. The Sdm, Im, and Peculiar types have the largest scatter in nuclear/integrated metallicities, indicating a large range in metallicity gradients for these galaxy types, or clumpy metallicity distributions. We find little evidence for systematic differences between nuclear and global extinction estimates for any galaxy type. However, there is significant scatter between the nuclear and integrated extinction estimates for nuclear apertures containing <20% of the B-26 flux. We calculate an "expected" SFR using our nuclear spectra and apply the commonly used aperture correction method. The expected SFR overestimates the global value for early-type spirals, with large scatter for all Hubble types, particularly late types. The differences between the expected and global SFRs probably result from the assumption that the distributions of the emission-line gas and the continuum are identical. The largest scatter ( error) in the estimated SFR occurs when the aperture captures <20% of the B-26 emission. We discuss the implications of these results for metallicity- luminosity relations and star formation history studies based on fiber spectra. To reduce systematic and random errors from aperture effects, we recommend selecting samples with fibers that capture >20% of the galaxy light. For the Sloan Digital Sky Survey and the Two-Degree Field Galaxy Redshift Survey, redshifts z > 0.04 and 0.06 are required, respectively, to ensure a covering fraction >20% for galaxy sizes similar to the average size, type, and luminosity observed in our sample. Higher luminosity samples and samples containing many late-type galaxies require a larger minimum redshift to ensure that >20% of the galaxy light is enclosed by the fiber. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Arizona State Univ, Dept Phys & Astron, Tempe, AZ 85287 USA. RP Kewley, LJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-20, Cambridge, MA 02138 USA. EM lkewley@cfa.harvard.edu NR 68 TC 157 Z9 157 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6280 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD MAR PY 2005 VL 117 IS 829 BP 227 EP 244 DI 10.1086/428303 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 906EP UT WOS:000227623600002 ER PT J AU West-Eberhard, MJ AF West-Eberhard, MJ TI The maintenance of sex as a developmental trap due to sexual selection SO QUARTERLY REVIEW OF BIOLOGY LA English DT Review ID REPRODUCTION; PARASITES; EVOLUTION; RECOMBINATION AB The writings of George Williams challenged biologists to think critically about levels of selection, social behavior, and the paradox of sex, whose maintenance by recombination alone has not been convincingly demonstrated in theory or in fact. A solution is suggested by observations of the dependence of females on interaction with males, as a result of sexual selection. This, along with recombination in changing environments and DNA repair during meiosis, may contribute to a pluralistic explanation for the maintenance of sex. C1 Univ Costa Rica, Smithsonian Trop Res Inst, Care Of Escuela Biol, San Jose, Costa Rica. RP West-Eberhard, MJ (reprint author), Univ Costa Rica, Smithsonian Trop Res Inst, Care Of Escuela Biol, San Jose, Costa Rica. EM MJWE@SENT.COM NR 31 TC 5 Z9 6 U1 2 U2 8 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0033-5770 J9 Q REV BIOL JI Q. Rev. Biol. PD MAR PY 2005 VL 80 IS 1 BP 47 EP 53 DI 10.1086/431024 PG 7 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 912NI UT WOS:000228085300007 PM 15884735 ER PT J AU Arnoldi, MJ AF Arnoldi, MJ TI Playing for life: Performance in Africa in the age of AIDS SO RESEARCH IN AFRICAN LITERATURES LA English DT Book Review C1 Smithsonian Inst, Museum Nat Hist, Washington, DC 20560 USA. RP Arnoldi, MJ (reprint author), Smithsonian Inst, Museum Nat Hist, Washington, DC 20560 USA. NR 1 TC 1 Z9 1 U1 0 U2 0 PU INDIANA UNIV PRESS PI BLOOMINGTON PA 601 N MORTON STREET, BLOOMINGTON, IN 47404-3797 USA SN 0034-5210 J9 RES AFR LITERATURES JI Res. Afr. Lit. PD SPR PY 2005 VL 36 IS 1 BP 121 EP 122 DI 10.1353/ral.2005.0005 PG 2 WC Literature, African, Australian, Canadian SC Literature GA 893HL UT WOS:000226709800010 ER PT J AU Small, LM AF Small, LM TI Child of wonder - Cristian Samper's lifelong love of flora and fauna inspires creative new displays of the world's largest collection SO SMITHSONIAN LA English DT Editorial Material C1 Smithsonian Inst, Washington, DC 20560 USA. RP Small, LM (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SMITHSONIAN ASSOCIATES PI WASHINGTON PA 900 JEFFERSON DRIVE, WASHINGTON, DC 20560 USA SN 0037-7333 J9 SMITHSONIAN JI Smithsonian PD MAR PY 2005 VL 35 IS 12 BP 10 EP 10 PG 1 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA 899RT UT WOS:000227163200002 ER PT J AU Gingerich, O Voelkel, JR AF Gingerich, O Voelkel, JR TI Tycho and Kepler: Solid myth versus subtle truth SO SOCIAL RESEARCH LA English DT Article 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 3 TC 0 Z9 0 U1 0 U2 0 PU NEW SCHOOL UNIV PI NEW YORK PA GRADUATE FACULTY, 65 5TH AVE, RM 354, NEW YORK, NY 10003 USA SN 0037-783X J9 SOC RES JI Soc. Res. PD SPR PY 2005 VL 72 IS 1 BP 77 EP 106 PG 30 WC Social Sciences, Interdisciplinary SC Social Sciences - Other Topics GA 920TR UT WOS:000228713500006 ER PT J AU Riley, DR Solis, MA AF Riley, DR Solis, MA TI Keys to immatures of the sugarcane borer and Nectropical cornstalk borer from Tamaulipas, Mexico, intercepted on corn in Southeastern Texas SO SOUTHWESTERN ENTOMOLOGIST LA English DT Article AB Diatraea larvae and pupae intercepted on corn from northeastern Mexico at south Texas ports of entry were reared to adults and identified as the sugarcane borer, Dialraea saccharalis (Fabricius), and the Neotropical cornstalk borer, Dialraea lineolata (Walker). Keys to aid in the identification of larvae and pupae of these two species are presented. C1 USDA, PPQ, APHIS, Brownsville, TX USA. USDA ARS, Smithsonian Inst, Systemat Entomol Lab, Washington, DC 20013 USA. EM asolis@sel.barc.usda.gov NR 7 TC 3 Z9 3 U1 0 U2 0 PU SOUTHWESTERN ENTOMOLOGICAL SOC PI DALLAS PA 17360 COIT RD, DALLAS, TX 75252-6599 USA SN 0147-1724 J9 SOUTHWEST ENTOMOL JI Southw. Entomol. PD MAR PY 2005 VL 30 IS 1 BP 35 EP 39 PG 5 WC Entomology SC Entomology GA 971OH UT WOS:000232393300006 ER PT J AU LaPolla, JS AF LaPolla, JS TI Ancient Trophophoresy: A fossil Acropyga (Hymenoptera : Formicidae) from Dominican amber SO TRANSACTIONS OF THE AMERICAN ENTOMOLOGICAL SOCIETY LA English DT Article DE Acropyga; Formicinae; trophobiosis; ant; fossil; amber AB The discovery of several pieces of Dominican amber with Acropyga inclusions provides evidence that the trophophoretic behavior of Acropyga queens is at least 15-20 million years old. A fossil species, A. glaesaria, is described and its relationship to extant Acropyga is discussed. C1 Natl Museum Nat Hist, Dept Entomol, Smithsonian Inst, NHB, Washington, DC 20013 USA. RP LaPolla, JS (reprint author), Natl Museum Nat Hist, Dept Entomol, Smithsonian Inst, NHB, POB 37012,CE518,MRC 188, Washington, DC 20013 USA. EM lapollaj@si.edu NR 11 TC 12 Z9 12 U1 1 U2 5 PU AMER ENTOMOL SOC PI PHILADELPHIA PA 1900 BENJ FRANKLIN PARKWAY, PHILADELPHIA, PA 19103-1195 USA SN 0002-8320 J9 T AM ENTOMOL SOC JI Trans. Am. Entomol. Soc. PD MAR-JUN PY 2005 VL 131 IS 1-2 BP 21 EP 28 PG 8 WC Entomology SC Entomology GA 945LA UT WOS:000230502800002 ER PT J AU Scarbrough, AG Perez-Gelabert, DE Page, SH AF Scarbrough, AG Perez-Gelabert, DE Page, SH TI Synopsis of Leptogastrine Asilids (Diptera) from Hispaniola SO TRANSACTIONS OF THE AMERICAN ENTOMOLOGICAL SOCIETY LA English DT Article DE Diptera; Asilidae; leptogastrinae; Apachekolos; Beameromyia; Eurhabdus; Psilonyx; new species; Dominican Republic; new records AB Five leptogastrine genera, including eight new species and new records of four species, are reported front the Dominican Republic. Of these, Apachekolos Martin, Psilonyx Schiner, and Eurhabdus Aldrich are reported for the first time. Apachekolos flaventis Scarbrough and Perez-Gelabert, sp. n., A. invasus Scarbrough and Perez-Gelabert, sp. nov., A. magnus Scarbrough and Perez-Gelabert, sp. nov., A. volubilis Scarbrough and Perez-Gelabert, sp. nov., A. vultus Scarbrough and Perez-Gelabert, sp. nov., Beameromyia incisuralis Scarbrough and Page, sp. nov., Psilonyx zephyrus Scarbrough and Page, sp. nov., and Eurhabdus sororius Scarbrough and Perez-Gelabert, sp. nov., and the females of B. dicrana Scarbrough and Leptogaster lineatus Scarbrough are discovered and described. The terminalia of each species and the wings of A. clavipes (Johnson), B. incisuralis, B. dicrana, E. sororius, L. lineatus, and P zephyrus are illustrated and keys to species are included. New records of B. melana Scarbrough, B. dicrana, L. lineatus, and A. clavipes are also included. The distribution of A. clavipes, previously known from the Bahamas and Jamaica, is expanded to include Hispaniola. C1 Towson Univ, Dept Biol Sci, Baltimore, MD 21252 USA. Natl Museum Nat Hist, Dept Entomol, Smithsonian Inst, Washington, DC 20560 USA. RP Scarbrough, AG (reprint author), Towson Univ, Dept Biol Sci, 8000 York Rd, Baltimore, MD 21252 USA. EM ascarbrough@towson.edu; perez.daniel@nmsh.si.edu; spage@towson.edu NR 17 TC 2 Z9 2 U1 1 U2 1 PU AMER ENTOMOL SOC PI PHILADELPHIA PA 1900 BENJ FRANKLIN PARKWAY, PHILADELPHIA, PA 19103-1195 USA SN 0002-8320 J9 T AM ENTOMOL SOC JI Trans. Am. Entomol. Soc. PD MAR-JUN PY 2005 VL 131 IS 1-2 BP 29 EP 67 PG 39 WC Entomology SC Entomology GA 945LA UT WOS:000230502800003 ER PT J AU Smith, DR AF Smith, DR TI Aulacidae (Hymenoptera) of Northern South America, emphasizing Colombia SO TRANSACTIONS OF THE AMERICAN ENTOMOLOGICAL SOCIETY LA English DT Article AB Twelve species of Aulacidae, three Aulacus and nine Pristaulacus, are recorded from northern South America: Aulacus amazonicus (Roman), A. cephalus, n. sp., A. ochreus, n. sp., Pristaulacus absens, n. sp., A. colombianus, n. sp., P.femurrubrum, n. sp., P. haemorrhoidalis (Westwood), P. maculatus (Schletterer), R punctatus, n. sp., P. ruficeps (Westwood), R tridentatus, n. sp., and P. zonatipennis Roman. This study is based on recent collections from Colombia. Aulacus bicornutus Schletterer 1889 is a new synonym of Pristaulacus ruficeps (Westwood 185 1). The species are described and illustrated and a key is given. C1 USDA ARS, PSI, Systemat Entomol Lab, Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20013 USA. RP Smith, DR (reprint author), USDA ARS, PSI, Systemat Entomol Lab, Natl Museum Nat Hist,Smithsonian Inst, POB 37012,MRC 168, Washington, DC 20013 USA. EM dsmith@sel.barc.usda.gov NR 12 TC 14 Z9 17 U1 0 U2 1 PU AMER ENTOMOL SOC PI PHILADELPHIA PA 1900 BENJ FRANKLIN PARKWAY, PHILADELPHIA, PA 19103-1195 USA SN 0002-8320 J9 T AM ENTOMOL SOC JI Trans. Am. Entomol. Soc. PD MAR-JUN PY 2005 VL 131 IS 1-2 BP 217 EP 253 PG 37 WC Entomology SC Entomology GA 945LA UT WOS:000230502800012 ER PT J AU Rice, NH Milensky, CM AF Rice, NH Milensky, CM TI The nest and nestlings of the Wing-banded Antbird (Myrmornis torquata) from southern Guyana SO WILSON BULLETIN LA English DT Article AB The Wing-banded Antbird (Myrmornis torquata) is a poorly known suboscine passerine found in lowland Arnazonian forests. Here, we present new information about the nest and nestlings of this enigmatic species. Our findings differ from previous observations and notes on Clutch size. C1 Univ Kansas, Museum Hist Nat, Lawrence, KS 66045 USA. Univ Kansas, Dept Ecol & Evolutionary Biol, Lawrence, KS 66045 USA. Smithsonian Inst, Div Birds, Washington, DC 20013 USA. RP Rice, NH (reprint author), Univ Kansas, Museum Hist Nat, Lawrence, KS 66045 USA. EM rice@acnatsci.org NR 5 TC 1 Z9 1 U1 0 U2 0 PU WILSON ORNITHOLOGICAL SOC PI WACO PA 5400 BOSQUE BLVD, STE 680, WACO, TX 76710 USA SN 0043-5643 J9 WILSON BULL JI Wilson Bull. PD MAR PY 2005 VL 117 IS 1 BP 103 EP 105 DI 10.1676/04-071 PG 3 WC Ornithology SC Zoology GA 941BD UT WOS:000230188700014 ER PT J AU McTurk, D Spelman, L AF McTurk, D Spelman, L TI Hand-rearing and rehabilitation of orphaned wild giant otters, Pteronura brasiliensis, on the Rupununi River, Guyana, South America SO ZOO BIOLOGY LA English DT Article AB From 1985-2003, 34 orphaned giant otters, Pteronura brasiliensis, (22 males, 12 females) were hand raised for eventual return to the wild at The Karanambu Cattle Company Limited Ranch (Karanambu), on the Rupununi River, Guyana, South America. The orphans ranged in age from 2 weeks to 9 months old; most were 8-10-week-old cubs. Feeding, housing, exercising, veterinary care, and rehabilitation protocols for young giant otters were developed during this period. Six cubs died during hand-rearing; of these, four died from illness or injury, and two were killed, one by a caiman and one by another orphaned otter. Of 34 giant otters brought to Karanambu, 28 (82%) were, reared successfully to an age and condition suitable for rehabilitation, and 18 (53%) returned to the wild. Ten otters survived hand-rearing but died either before or during the process of rehabilitation. These hand-reared giant otters were killed by people (3 known, 2 presumed) or other giant otters (5), including one male otter that remained at Karanambu for several years. During rehabilitation, young giant otters chose to spend increasing amounts of time on the Rupununi River away from human care, often interacting with wild giant otters. Although long-term monitoring was not possible, Karanambu staff observed most (15 of 18) of the rehabilitated otters repeatedly, for as long as 4 years after their return to the river. The giant otter rehabilitation program at Karanambu generated new knowledge about this species, and offered visitors the opportunity to observe them. © 2005 Wiley-Liss, Inc. C1 Smithsonian Inst, Natl Zool Pk, Washington, DC 20008 USA. RP Spelman, L (reprint author), 3620 39th St,Apt F540, Washington, DC 20016 USA. EM lucy.spelman@gmail.com NR 20 TC 2 Z9 2 U1 2 U2 15 PU WILEY-LISS PI HOBOKEN PA DIV JOHN WILEY & SONS INC, 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 0733-3188 J9 ZOO BIOL JI Zoo Biol. PD MAR-APR PY 2005 VL 24 IS 2 BP 153 EP 167 DI 10.1002/zoo.20042 PG 15 WC Veterinary Sciences; Zoology SC Veterinary Sciences; Zoology GA 924DS UT WOS:000228959600005 ER PT J AU Tarou, LR Williams, J Powell, DM Tabet, R Allen, M AF Tarou, LR Williams, J Powell, DM Tabet, R Allen, M TI Behavioral preferences for bamboo in a pair of captive giant pandas (Ailuropoda melanoleuca) SO ZOO BIOLOGY LA English DT Article DE behavioral mechanisms; diet selection; foraging efficiency; giant pandas; nutrition ID SELECTION; DIET; SEPARATION; SICHUAN; WOLONG; CHINA AB Giant pandas (Ailuropoda melanoleuca) are members of the order Carnivora. Their diet, however, consists almost entirely of bamboo. Herbivores are under strong pressure to be selective in what they eat because of the low digestibility of plant material. The purpose of this study was to determine whether two captive giant pandas exhibited preferences among three species of bamboo: black (Phyllostachys nigra), bissetii (Phyllostachys bissetii), and arrow (Pseudosasa japonica). Eighteen classic choice trials were conducted in which the species were randomly paired and placed in one of two predetermined locations in the giant pandas' indoor enclosures. The pandas preferred leaves to culms or branches for each bamboo species. In the first hour of exposure, both pandas exhibited a preference for arrow bamboo. A comparison of total bamboo consumption over the course of the night indicated a strong preference for arrow bamboo by the male. The female exhibited equal preference for both arrow and bissetii over black bamboo. Further examination of feeding behavior determined that the pandas processed arrow bamboo behaviorally more efficiently than the other two species. This is the first study to experimentally assess bamboo preferences in giant pandas, and may have implications for husbandry and management programs as well as strategies for in situ conservation. © 2005 Wiley-Liss, Inc. C1 Smithsonian Inst, Natl Zool Pk, Washington, DC 20008 USA. Georgia Inst Technol, Sch Psychol, Atlanta, GA 30332 USA. Georgetown Univ, Dept Biol, Washington, DC 20057 USA. RP Tarou, LR (reprint author), Grand Valley State Univ, Dept Psychol, 1 Campus Dr,2112 AuSable Hall, Allendale, MI 49401 USA. EM taroul@gusu.edu NR 19 TC 9 Z9 9 U1 2 U2 26 PU WILEY-LISS PI HOBOKEN PA DIV JOHN WILEY & SONS INC, 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 0733-3188 J9 ZOO BIOL JI Zoo Biol. PD MAR-APR PY 2005 VL 24 IS 2 BP 177 EP 183 DI 10.1002/zoo.20038 PG 7 WC Veterinary Sciences; Zoology SC Veterinary Sciences; Zoology GA 924DS UT WOS:000228959600007 ER PT J AU Tyler, JC Santini, F AF Tyler, JC Santini, F TI A phylogeny of the fossil and extant zeiform-like fishes, Upper Cretaceous to Recent, with comments on the putative zeomorph clade (Acanthomorpha) SO ZOOLOGICA SCRIPTA LA English DT Article ID MISSING DATA; TAXA; TETRAODONTIFORMES; RECONSTRUCTION; CHARACTERS; ACCURACY AB A phylogenetic hypothesis based on 107 morphological characters is proposed for a data set of 43 taxa. Thirty-three are extant and belong to the orders Zeiformes (20 taxa), Caproiformes (2), Tetraodontiformes (2), Beryciformes (3), Stephanobervciformes (3) and Perciformes (3). Ten are fossil taxa previously assigned to the Zeiformes (3), Caproiformes (1), Tetraodontiformes (2), Perciformes (1), and to two extinct Eocene families, the Sorbinipercidae (2) and the Zorzinichthydae (1). This analysis indicates the existence of a previously undocumented clade formed by the families Sorbinipercidae + Zorzinichthyidae that may be related to the tetraodontiforms. It also shows that two uppermost Palaeocene species, Archaeozeus skamolensis and Protozeus kuehnei, sequentially represent the two most basal lineages of zeiforms, whereas the most ancient known zeiform, the Upper Cretaceous Cretazeus rinaldii, belongs within the clade of extant species in a polytomy with many other zeiform lineages. A reduced data set of 25 mostly zeiform taxa, after the removal of most outgroups, shows at least weak support for Cretazeus being nested deeply within the extant zeiforms; such a placement would indicate that at least six lineages of zeiforms were present during the Upper Cretaceous, and survived the Cretaceous/Tertiary (K/T) extinction to radiate in Cenozoic seas. C1 Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. Museum Natl Hist Nat, Dept Systemat & Evolut, CNRS, UMR 7138, F-75231 Paris, France. RP Tyler, JC (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. EM tyler.jim@nmnh.si.edu; fsantini@mnhn.hr NR 61 TC 13 Z9 15 U1 0 U2 2 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0300-3256 J9 ZOOL SCR JI Zool. Scr. PD MAR PY 2005 VL 34 IS 2 BP 157 EP 175 DI 10.1111/j.1463-6409.2005.00180.x PG 19 WC Evolutionary Biology; Zoology SC Evolutionary Biology; Zoology GA 905GE UT WOS:000227555800003 ER PT J AU Aguilar, A Emmons, ED Gharaibeh, MF Covington, AM Bozek, JD Ackerman, G Canton, S Rude, B Schlachter, AS Hinojosa, G Alvarez, I Cisneros, C McLaughlin, BM Phaneuf, RA AF Aguilar, A Emmons, ED Gharaibeh, MF Covington, AM Bozek, JD Ackerman, G Canton, S Rude, B Schlachter, AS Hinojosa, G Alvarez, I Cisneros, C McLaughlin, BM Phaneuf, RA TI Photoionization of ions of the nitrogen isoelectronic sequence: experiment and theory for F2+ and Ne3+ SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS LA English DT Article ID X-RAY SPECTROSCOPY; CROSS-SECTIONS; RADIATIVE RECOMBINATION; OSCILLATOR-STRENGTHS; HIGH-RESOLUTION; TRANSITIONS; HELIUM; OXYGEN; STATES AB Absolute photoionization measurements are reported for admixtures of the ground and metastable states of F2+ from 56.3 eV to 75.6 eV, and of Ne3+ from 89.3 eV to 113.8 eV. The S-4 degrees ground-state and the D-2 degrees and P-2 degrees metastable-state fractions present in the primary ion beams were estimated from photoion yield measurements near their respective threshold energies. Most of the observed resonance structure has been spectroscopically assigned. The measurements are compared with new R-matrix theoretical calculations and with those in the TOPbase astrophysical database. The systematic behaviour of the quantum-defect parameter is analysed as a function of the nuclear charge for four Rydberg series observed in both species, and compared to published data for O+ and N. C1 Univ Nevada, Dept Phys, Reno, NV 89557 USA. Univ Calif Berkeley, Lawrence Berkeley Lab, Berkeley, CA 94720 USA. Univ Nacl Autonoma Mexico, Ctr Ciencias Fis, Cuernavaca 62131, Morelos, Mexico. Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. Queens Univ Belfast, Sch Math & Phys, Belfast BT7 1NN, Antrim, North Ireland. RP Aguilar, A (reprint author), NIST, Atom Phys Div, 100 Bur Dr,Stop 8421, Gaithersburg, MD 20899 USA. EM phaneuf@physics.unr.edu RI Bozek, John/E-4689-2010; Bozek, John/E-9260-2010; Canton, Sophie/A-8432-2016 OI Bozek, John/0000-0001-7486-7238; NR 28 TC 10 Z9 10 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0953-4075 J9 J PHYS B-AT MOL OPT JI J. Phys. B-At. Mol. Opt. Phys. PD FEB 28 PY 2005 VL 38 IS 4 BP 343 EP 361 DI 10.1088/0953-4075/38/4/003 PG 19 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 914TD UT WOS:000228249700004 ER PT J AU Holman, MJ Murray, NW AF Holman, MJ Murray, NW TI The use of transit timing to detect terrestrial-mass extrasolar planets SO SCIENCE LA English DT Article ID GRAVITATIONAL LENSING EXPERIMENT; LUMINOSITY OBJECT TRANSITS; 3-BODY PROBLEM; GALACTIC DISK; 2001 CAMPAIGN; SEARCH; STARS; COMPANION; SYSTEM; ORBIT AB Future surveys for transiting extrasolar planets are expected to detect hundreds of jovian-mass planets and tens of terrestria-mass planets. For many of these newly discovered planets, the intervals between successive transits will be measured with an accuracy of 0.1 to 100 minutes. We show that these timing measurements will allow for the detection of additional planets in the system (not necessarily transiting) by their gravitational interaction with the transiting planet. The transit-time variations depend on the mass of the additional planets and in some cases terrestrial-mass planets will produce a measurable effect. In systems where two planets are seen to transit, the density of both planets can be determined without radial-velocity observations. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. RP Holman, MJ (reprint author), Harvard Smithsonian Ctr Astrophys, MS51,60 Garden St, Cambridge, MA 02138 USA. EM mholman@cfa.harvard.edu NR 30 TC 360 Z9 365 U1 6 U2 14 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD FEB 25 PY 2005 VL 307 IS 5713 BP 1288 EP 1291 DI 10.1126/science.1107822 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 901WP UT WOS:000227313200052 PM 15731449 ER PT J AU Inui, T Matsumoto, H Tsuru, TG Koyama, K Matsushita, S Peck, AB Tarchi, A AF Inui, T Matsumoto, H Tsuru, TG Koyama, K Matsushita, S Peck, AB Tarchi, A TI Chandra observation of the starburst galaxy NGC 2146 SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN LA English DT Article DE galaxies : active; galaxies : individual (NGC 2146); galaxies : starburst; X-rays : galaxies ID XMM-NEWTON OBSERVATIONS; X-RAY; DRIVEN SUPERWIND; BLACK-HOLE; NGC-2146; M82; EMISSION; MINISURVEY; PLASMAS AB We present six monitoring observations of the starburst galaxy NGC 2146 using, the Chandra X-ray Observatory. We detected 67 point sources in the field of view of the ACIS-S detector. Six of these sources were Ultra-Luminous X-ray Sources, the brightest of which had a luminosity of 5 x 10(39) erg s(-1). One of them, with a luminosity of 1 x 10(39) erg s(-1), is coincident with the dynamical center location, which may be a low-luminosity active galactic nucleus. We have produced a table where the positions and main characteristics of the detected sources are reported. A comparison between the positions of the X-ray sources and those detected in NIR or radio indicates no definite counterpart. We have derived a log N-log S relation and a luminosity function. The luminosity function has a slope of 0.71 above a detection limit, which is similar to those found in other starburst galaxies. Diffuse emissions were detected in both soft (0.5-2.0 keV) and hard (2.0-10.0 keV) energy bands. The spectra of the diffuse component were fitted with two (hard and soft) components. The hard power-law component, with a luminosity of similar to 4 x 10(39) erg s(-1), is likely to have originated by unresolved point sources. C1 Kyoto Univ, Dept Phys, Grad Sch Sci, Sakyo Ku, Kyoto 6068502, Japan. Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CNR, Inst Radioastron, I-40129 Bologna, Italy. Osservatorio Astrofis Cagliari, I-09012 Capoterra, CA, Italy. RP Kyoto Univ, Dept Phys, Grad Sch Sci, Sakyo Ku, Kyoto 6068502, Japan. EM inuit@cr.scphys.kyoto-u.ac.jp; matsumoto@cr.scphys.kyoto-u.ac.jp; tsuru@cr.scphys.kyoto-u.ac.jp; koyama@cr.scphys.kyoto-u.ac.jp; satoki@asiaa.sinica.edu.tw; apeck@cfa.harvard.edu; atarchi@ira.cnr.it OI Tarchi, Andrea/0000-0001-8540-3500 NR 26 TC 15 Z9 15 U1 0 U2 0 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 FEB 25 PY 2005 VL 57 IS 1 BP 135 EP 145 DI 10.1093/pasj/57.1.135 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 933IR UT WOS:000229622600011 ER PT J AU Bradshaw, GA Schore, AN Brown, JL Poole, JH Moss, CJ AF Bradshaw, GA Schore, AN Brown, JL Poole, JH Moss, CJ TI Elephant breakdown SO NATURE LA English DT Article C1 Oregon State Univ, Environm Sci Grad Programme, Corvallis, OR 97331 USA. Oregon State Univ, Dept Forest Sci, Corvallis, OR 97331 USA. Univ Calif Los Angeles, Dept Psychiat, Los Angeles, CA USA. Smithsonian Natl Zool Pk, Washington, DC USA. Amboseli Elephant Res Project, Nairobi, Kenya. RP Bradshaw, GA (reprint author), Oregon State Univ, Environm Sci Grad Programme, Corvallis, OR 97331 USA. NR 3 TC 68 Z9 69 U1 5 U2 46 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 24 PY 2005 VL 433 IS 7028 BP 807 EP 807 DI 10.1038/433807a PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 899VT UT WOS:000227174600022 PM 15729320 ER PT J AU Jenkins, LP Roberts, TP Warwick, RS Kilgard, RE Ward, MJ AF Jenkins, LP Roberts, TP Warwick, RS Kilgard, RE Ward, MJ TI An XMM-Newton view of M101 - II. Global X-ray source properties SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies : individual : M101; galaxies : spiral; X-rays : binaries; X-rays : galaxies ID HYPERNOVA REMNANT CANDIDATES; NEARBY SPIRAL GALAXIES; EXTERNAL GALAXIES; SOURCE POPULATION; BLACK-HOLES; H-2 REGIONS; H-I; EMISSION; IDENTIFICATION; STARBURST AB We present the global X-ray properties of the point source population in the grand-design spiral galaxy M101, as seen with XMM-Newton. 108 X-ray sources are detected within the D-25 ellipse of M101, of which 24 are estimated to be background galaxies. Multiwavelength cross-correlations show that 20 sources are coincident with H II regions and/or supernova remnants (SNRs), seven have identified/candidate background galaxy counterparts, six are coincident with foreground stars and one has a radio counterpart. While the spectral and timing properties of the brightest sources were presented by Jenkins et al., here we apply an X-ray colour classification scheme to split the entire source population into different types, i.e. X-ray binaries (XRBs), SNRs, absorbed sources, background sources and supersoft sources (SSSs). Approximately 60 per cent of the population can be classified as XRBs, although there is source contamination from background active galactic nuclei (AGN) in this category as they have similar spectral shapes in the X-ray regime. 15 sources have X-ray colours consistent with SNRs, three of which correlate with known SNR/H II radio sources. Another two are promising new candidates for SNRs, one is unidentified, and the remainder are a mixture of foreground stars, bright soft XRBs and AGN candidates. We also detect 14 candidate SSSs, with significant detections in the softest X-ray band (0.3-1 keV) only. 16 sources display short-term variability during the XMM-Newton observation, twelve of which fall into the XRB category, giving additional evidence of their accreting nature. Using archival Chandra and ROSAT High Resolution Imager data, we find that 40 per cent of the XMM sources show long-term variability over a baseline of up to 10 yr, and eight sources display potential transient behaviour between observations. Sources with significant flux variations between the XMM and Chandra observations show a mixture of softening and hardening with increasing luminosity. The spectral and timing properties of the sources coincident with M101 confirm that its X-ray source population is dominated by accreting XRBs. C1 Univ Leicester, Dept Phys & Astron, Xray & Observat Astron Grp, Leicester LE1 7RH, Leics, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Jenkins, LP (reprint author), Univ Leicester, Dept Phys & Astron, Xray & Observat Astron Grp, Univ Rd, Leicester LE1 7RH, Leics, England. EM lej@star.le.ac.uk OI Jenkins, Leigh/0000-0001-9464-0719 NR 56 TC 19 Z9 19 U1 0 U2 0 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB 21 PY 2005 VL 357 IS 2 BP 401 EP 419 DI 10.1111/j.1365-2966.2005.08645.x PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 895IG UT WOS:000226853700001 ER PT J AU Bianchi, S Matt, G Nicastro, F Porquet, D Dubau, J AF Bianchi, S Matt, G Nicastro, F Porquet, D Dubau, J TI Fe XXV and Fe XXVI lines from low-velocity, photoionized gas in the X-ray spectra of active galactic nuclei SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE line : formation; galaxies : Seyfert; X-rays : galaxies ID HELIUM-LIKE IONS; REFLECTION GRATING SPECTROMETER; XMM-NEWTON; INNER-SHELL; IONIZED-GAS; BLACK-HOLE; CHANDRA; IRON; SPECTROSCOPY; EMISSION AB We have calculated the equivalent widths of the absorption lines produced by Fe XXV and Fe XXVI in a Compton-thin, low-velocity photoionized material illuminated by the nuclear continuum in active galactic nuclei. The results, plotted against the ionization parameter and the column density of the gas, are a complement to those presented by Bianchi & Matt for the emission lines from the same ionic species. As an extension to the work by Bianchi & Matt, we also present a qualitative discussion on the different contributions to the He-like iron emission line complex in the regimes where recombination or resonant scattering dominates, providing a useful diagnostic tool to measure the column density of the gas. Future high-resolution missions (e. g. Astro-E2) will allow us to fully take advantage of these plasma diagnostics. In the meantime, we compare our results with an up-to-date list of Compton-thick and unobscured (at least at the iron line energy) Seyfert galaxies with emission and/or absorption lines from H- and He-like iron observed with Chandra and XMM-Newton. C1 Univ Roma Tre, Dipartimento Fis, I-00146 Rome, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. Univ Paris 11, Lab Interact Rayonnement X Avec Mat, F-91405 Orsay, France. RP Univ Roma Tre, Dipartimento Fis, Via Vasca Navale 84, I-00146 Rome, Italy. EM Stefano.Bianchi@sciops.esa.int RI Bianchi, Stefano/B-4804-2010; OI Bianchi, Stefano/0000-0002-4622-4240; Porquet, Delphine/0000-0001-9731-0352; Nicastro, Fabrizio/0000-0002-6896-1364 NR 46 TC 52 Z9 52 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 2005 VL 357 IS 2 BP 599 EP 607 DI 10.1111/j.1365-2966.2005.08661.x PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 895IG UT WOS:000226853700020 ER PT J AU Ward-Thompson, D Hartmann, L Nutter, DJ AF Ward-Thompson, D Hartmann, L Nutter, DJ TI Turbulence in Class 0 and I protostellar envelopes SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE radiative transfer; stars : formation; ISM : clouds; submillimetre ID YOUNG STELLAR OBJECTS; LINE FORMATION; STAR-FORMATION; CLOUD CORES; INFALL; PROTOSTARS; SUBMILLIMETER; COLLAPSE; CANDIDATES; B335 AB We estimate the levels of turbulence in the envelopes of class 0 and I protostars using a model based on measurements of the peak separation of double-peaked asymmetric line profiles. We use observations of 20 protostars of both class 0 and I taken in the HCO+ (J = 3-->2) line that show the classic double-peaked profile. We find that some class 0 sources show high levels of turbulence, whilst others demonstrate much lower levels. In class I protostars, we find predominantly low levels of turbulence. The observations are consistent with a scenario in which class 0 protostars form in a variety of environments and subsequently evolve into class I protostars. The data do not appear to be consistent with a recently proposed scenario in which class 0 protostars can only form in extreme environments. C1 Cardiff Univ, Dept Phys & Astron, Cardiff CF24 3YB, S Glam, Wales. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Ward-Thompson, D (reprint author), Cardiff Univ, Dept Phys & Astron, Cardiff CF24 3YB, S Glam, Wales. EM Derek.Ward-Thompson@astro.cf.ac.uk NR 30 TC 2 Z9 2 U1 0 U2 0 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB 21 PY 2005 VL 357 IS 2 BP 687 EP 690 DI 10.1111/j.1365-2966.2005.08680.x PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 895IG UT WOS:000226853700028 ER PT J AU Williams, BF Garcia, MR Kong, AKH Primini, FA Murray, SS AF Williams, BF Garcia, MR Kong, AKH Primini, FA Murray, SS TI Discovery of an X-ray nova in M31 SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; galaxies : individual (M31); X-rays : binaries ID CENTRAL REGION; XMM-NEWTON; CHANDRA; BINARIES; CAMERA AB We have obtained snapshot images of an X-ray nova in M31 from Chandra ACIS-I and the Hubble Space Telescope (HST) Advanced Camera for Surveys. The Chandra position of the X-ray nova was R: A: = 00(h)44(m)06.(s)68 +/- 1.(s)74, decl. = +41degrees12'20."0 +/- 2."31 (J2000.0). A follow-up HST observation 24 days later revealed a source at R: A. = 00(h)44(m)06.(s) 81, decl. = +41degrees12'24."0 that was B = 25.75 +/- 0.05. This optical source faded to B = 27.1 +/- 0.1 in 3 months. During this time period, the X-ray flux decayed linearly from ( 3.6 +/- 0.2) x 10(-4) to <(6.9 +/- 0.09) x 10(-5) counts cm(-2) s(-1). The HST identification of an optical source in the same region experiencing an obvious drop in brightness in concert with the X-ray nova suggests that this optical source is the counterpart of the X-ray nova. However, the precision of the X-ray position allows the possibility that the optical source is a nearby variable star. We discuss the implications of both possibilities. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Williams, BF (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM williams@head.cfa.harvard.edu; garcia@head.cfa.harvard.edu; akong@head.cfa.harvard.edu; fap@head.cfa.harvard.edu; ssm@head.cfa.harvard.edu OI Primini, Francis/0000-0002-6077-0643 NR 27 TC 10 Z9 10 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2005 VL 620 IS 2 BP 723 EP 730 DI 10.1086/427085 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 903DN UT WOS:000227405800014 ER PT J AU Snell, RL Hollenbach, D Howe, JE Neufeld, DA Kaufman, MJ Melnick, GJ Bergin, EA Wang, Z AF Snell, RL Hollenbach, D Howe, JE Neufeld, DA Kaufman, MJ Melnick, GJ Bergin, EA Wang, Z TI Detection of water in the shocked gas associated with IC 443: Constraints on shock models SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : abundances; ISM : clouds; ISM : molecules; radio lines : ISM; shock waves; supernova remnants ID SUPERNOVA REMNANT IC-443; WAVE-ASTRONOMY-SATELLITE; INTER-STELLAR SHOCKS; MOLECULE FORMATION; INFRARED-EMISSION; NOVA REMNANT; PHYSICAL PROCESSES; H-2 EMISSION; CO EMISSION; CHEMISTRY AB We have used the Submillimeter Wave Astronomy Satellite (SWAS) to observe the ground-state 1(10) --> 1(01) transition of ortho-H2O at 557 GHz in three of the shocked molecular clumps associated with the supernova remnant IC 443. We also observed simultaneously the 487 GHz line (3, 1 --> 3; 2) of O-2, the 492 GHz line (P-3(1) --> P-3(0)) of C I, and the 550 GHz line ( J = 5 --> 4) of (CO)-C-13. We detected the H2O, C I, and (CO)-C-13 lines toward the shocked clumps B, C, and G. In addition, ground-based observations of the J = 1 --> 0 transitions of CO and HCO+ were obtained. Assuming that the shocked gas has a temperature of 100 K and a density of 5 x 10(5) cm(-3), we derive SWAS beam-averaged ortho- H2O column densities of 3.2 x 10(13), 1,8 x 10(13), and 3.9 x 10(13) cm(-2) in clumps B, C, and G, respectively. Combining the SWAS results with our ground-based observations, we derive a relative abundance of ortho- H2O to CO in the postshock gas of between 2 x 10(-4) and 3 x 10(-3). On the basis of our results for H2O, published results of numerous atomic and molecular shock tracers, and archival Infrared Space Observatory (ISO) observations, we conclude that no single shock type can explain these observations. However, a combination of fast J-type shocks (similar to 100 km s(-1)) and slow C-type shocks (similar to 12 km s(-1)) or, more likely, slow J-type shocks (similar to 12 - 25 km s(-1)) can most naturally explain the postshock velocities and the emission seen in various atomic and molecular tracers. Such a superposition of shocks might be expected as the supernova remnant overtakes a clumpy interstellar medium. The fast J-type shocks provide a strong source of ultraviolet radiation, which photodissociates the H2O in the cooling ( T less than or equal to 300 K) gas behind the slow shocks and strongly affects the slow C-type shock structure by enhancing the fractional ionization. At these high ionization fractions, C-type shocks break down at speeds similar to 10 - 12 km s(-1), while faster flows will produce J-type shocks. Our model favors a preshock gas-phase abundance of oxygen not in CO that is depleted by a least a factor of 2, presumably as water ice on grain surfaces. Both freezeout of H2O and photodissociation of H2O in the postshock gas must be significant to explain the weak H2O emission seen by SWAS and ISO from the shocked and postshock gas. C1 Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. San Jose State Univ, Dept Phys, San Jose, CA 95192 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Snell, RL (reprint author), Univ Massachusetts, Dept Astron, LGRT 619,710 N Pleasant St, Amherst, MA 01003 USA. NR 58 TC 48 Z9 49 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2005 VL 620 IS 2 BP 758 EP 773 DI 10.1086/427231 PN 1 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 903DN UT WOS:000227405800017 ER PT J AU Lintott, CJ Viti, S Rawlings, JMC Williams, DA Hartquist, TW Caselli, P Zinchenko, I Myers, P AF Lintott, CJ Viti, S Rawlings, JMC Williams, DA Hartquist, TW Caselli, P Zinchenko, I Myers, P TI Molecular abundance ratios as a tracer of accelerated collapse in regions of high-mass star formation SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; stars : formation ID PRESTELLAR CORES; CLOUD CORES; EVAPORATION; EVOLUTION; EMISSION AB Recent observations suggest that the behavior of tracer species such as N2H+ and CS is significantly different in regions of high- and low-mass star formation. In the latter, N2H+ is a good tracer of mass, while CS is not. Observations show the reverse to be true in high- mass star formation regions. We use a computational chemical model to show that the abundances of these and other species may be significantly altered by a period of accelerated collapse in high- mass star-forming regions. We suggest that these results provide a potential explanation of the observations, and make predictions for the behavior of other species. C1 UCL, Dept Phys & Astron, London WC1E 6BT, England. Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy. Russian Acad Sci, Inst Appl Phys, Nizhnii Novgorod 603950, Russia. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP UCL, Dept Phys & Astron, Gower St, London WC1E 6BT, England. EM cjl@star.ucl.ac.uk OI Zinchenko, Igor/0000-0003-2793-8229 NR 18 TC 12 Z9 12 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2005 VL 620 IS 2 BP 795 EP 799 DI 10.1086/427164 PN 1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 903DN UT WOS:000227405800020 ER PT J AU De Vries, CH Myers, PC AF De Vries, CH Myers, PC TI Molecular line profile fitting with analytic radiative transfer models SO ASTROPHYSICAL JOURNAL LA English DT Article DE radiative transfer; radio lines : ISM; stars : formation ID MONTE-CARLO METHOD; PROTOSTELLAR COLLAPSE; STARLESS CORES; DENSE CORES; INFALL MOTIONS; CLOUD CORES; ROTATIONAL-EXCITATION; CS 2-1; B335; CO AB We present a study of analytic models of starless cores whose line profiles have "infall asymmetry,'' or blue-skewed shapes indicative of contracting motions. We compare the ability of two types of analytical radiative transfer models to reproduce the line profiles and infall speeds of centrally condensed starless cores whose infall speeds are spatially constant and range between 0 and 0.2 km s(-1). The model line profiles of HCO+ ( J = 1 --> 0) and HCO+ ( J = 3 --> 2) are produced by a self- consistent Monte Carlo radiative transfer code. The analytic models assume that the excitation temperature in the front of the cloud is either constant("two-layer'' model) or increases inward as a linear function of optical depth ("hill'' model). Each analytic model is matched to the line profile by rapid least-squares fitting. The blue-asymmetric line profiles with two peaks, or with a blueshifted peak and a red shifted shoulder, can be well fitted by one or both of the analytic models. Two-peak profiles are best matched by the "HILL5'' model ( a five parameter version of the hill model), with an rms error of 0.01 km s(-1), while the "TWOLAYER6'' model underestimates the infall speed by a factor of similar to2. For red-shoulder profiles, the HILL5 and TWOLAYER6 fits reproduce infall speeds equally well, with an rms error of 0.04 km s(-1). The fits are most accurate when the line has a brightness temperature greater than 3 K. Our most accurate models tend to not only reproduce the line profile shape but also match the excitation conditions along the line of sight. A better match to the line profile shape does not necessarily imply a better match to the infall speed. We provide guidance on how to minimize the risk of obtaining a poor infall speed fit. A peak signal-to-noise ratio of at least 30 in the molecular line observations is required for performing these analytic radiative transfer fits to the line profiles. Moderate amounts of depletion and beam smoothing do not adversely affect the accuracy of the infall speeds obtained from these models. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP De Vries, CH (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 53 TC 31 Z9 31 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2005 VL 620 IS 2 BP 800 EP 815 DI 10.1086/427141 PN 1 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 903DN UT WOS:000227405800021 ER PT J AU Yuan, F Cui, W Narayan, R AF Yuan, F Cui, W Narayan, R TI An accretion-jet model for black hole binaries: Interpreting the spectral and timing features of XTE J1118+480 SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; ISM : jets and outflows; stars : individual (XTE J1118+480); X-rays : stars ID ADVECTION-DOMINATED ACCRETION; RADIO/X-RAY CORRELATION; SAGITTARIUS A-ASTERISK; BROAD-BAND SPECTRUM; X-RAY; OPTICAL VARIABILITY; MULTIWAVELENGTH OBSERVATIONS; CANDIDATE XTE-J1118+480; RELATIVISTIC JETS; BURST AFTERGLOWS AB Multiwavelength observations of the black hole X-ray binary XTE J1118+480 have offered abundant spectral and timing information about the source and have thus provided serious challenges to theoretical models. We propose a coupled accretion-jet model to interpret the observations. We model the accretion flow as an outer standard thin accretion disk truncated at a transition radius by an inner hot accretion flow. The accretion flow accounts for the observed UV and X-ray emission, but it substantially underpredicts the radio and infrared fluxes, even after we allow for nonthermal electrons in the hot flow. We attribute the latter components to a jet. We model the jet emission by means of the internal shock scenario, which is widely employed for gamma-ray bursts. In our accretion-jet model of XTE J1118+480, the jet dominates the radio and infrared emission, the thin disk dominates the UV emission, and the hot flow produces most of the X-ray emission. The optical emission has contributions from all three components: jet, thin disk, and hot flow. The model qualitatively accounts for timing features, such as the intriguing positive and negative time lags between the optical and X-ray emission and the wavelength-dependent variability amplitude. C1 Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Yuan, F (reprint author), Purdue Univ, Dept Phys, 525 Western Ave, W Lafayette, IN 47907 USA. EM fyuan@physics.purdue.edu; cui@physics.purdue.edu; narayan@cfa.harvard.edu OI Narayan, Ramesh/0000-0002-1919-2730; Cui, Wei/0000-0002-6324-5772 NR 78 TC 120 Z9 123 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2005 VL 620 IS 2 BP 905 EP 914 DI 10.1086/427206 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 903DN UT WOS:000227405800029 ER PT J AU Cackett, EM Wijnands, R Heinke, CO Edmonds, PD Lewin, WHG Pooley, D Grindlay, JE Jonker, PG Miller, JM AF Cackett, EM Wijnands, R Heinke, CO Edmonds, PD Lewin, WHG Pooley, D Grindlay, JE Jonker, PG Miller, JM TI X-ray variability during the quiescent state of the neutron star X-ray transient in the globular cluster NGC 6440 SO ASTROPHYSICAL JOURNAL LA English DT Article DE globular clusters : individual (NGC 6440); stars : neutron; X-rays : binaries ID AQUILA X-1; CHANDRA OBSERVATION; THERMAL EMISSION; CENTAURUS X-4; NGC 6440; SPECTRUM; LUMINOSITY AB The globular cluster NGC 6440 is known to harbor a bright neutron star X-ray transient. We observed the globular cluster with Chandra on two occasions when the bright transient was in its quiescent state, in 2000 July and 2003 June ( both observations were made nearly 2 yr after the end of their preceding outbursts). The quiescent spectrum during the first observation is well represented by a two-component model ( a neutron star atmosphere model plus a power-law component that dominates at energies above 2 keV). During the second observation ( which was roughly of equal duration to the first observation) we found that the power-law component could no longer be detected. Our spectral fits indicate that the effective temperature of the neutron star surface was consistent between the two observations. We conclude that the effect of the change in the power-law component caused the 0.5 - 10 keV flux to be a factor of similar to 2 lower during the second observation compared to the first observation. We discuss plausible explanations for the variations, including variable residual accretion onto the neutron star magnetosphere or some variation in the interaction of the pulsar wind with the matter still outflowing from the companion star. C1 Univ St Andrews, Sch Phys & Astron, St Andrews KY16 933, Fife, Scotland. Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. MIT, Ctr Space Res, Cambridge, MA 02139 USA. RP Univ St Andrews, Sch Phys & Astron, St Andrews KY16 933, Fife, Scotland. EM emc14@st-and.ac.uk OI Heinke, Craig/0000-0003-3944-6109 NR 30 TC 26 Z9 26 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2005 VL 620 IS 2 BP 922 EP 928 DI 10.1086/427178 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 903DN UT WOS:000227405800031 ER PT J AU Millan-Gabet, R Pedretti, E Monnier, JD Schloerb, FP Traub, WA Carleton, NP Lacasse, MG Segransan, D AF Millan-Gabet, R Pedretti, E Monnier, JD Schloerb, FP Traub, WA Carleton, NP Lacasse, MG Segransan, D TI Diameters of Mira stars measured simultaneously in the J, H, and K ' near-infrared bands SO ASTROPHYSICAL JOURNAL LA English DT Article DE instrumentation : interferometers; stars : atmospheres; stars : fundamental parameters; stars : variables : other; techniques : high angular resolution ID ANGULAR SIZE MEASUREMENTS; BISPECTRUM SPECKLE INTERFEROMETRY; IOTA-INTERFEROMETER; VARIABLE-STARS; R-LEONIS; APERTURE MASKING; APPARENT SIZE; PULSATION; SPECTRA; CATALOG AB We present the first spatially resolved observations of a sample of 23 Mira stars simultaneously measured in the near-infrared J, H, and K' bands. The technique used was optical long-baseline interferometry, and we present for each star visibility amplitude measurements as a function of wavelength. We also present characteristic sizes at each spectral band, obtained by fitting the measured visibilities to a simple uniform disk model. This approach reveals the general relation J diameter < H diameter < K' diameter. C1 CALTECH, Michelson Sci Ctr, Pasadena, CA 91125 USA. Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Observ Geneva, CH-1290 Sauverny, Switzerland. RP Millan-Gabet, R (reprint author), CALTECH, Michelson Sci Ctr, MS 100-22, Pasadena, CA 91125 USA. EM rafael@ipac.caltech.edu NR 45 TC 28 Z9 28 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2005 VL 620 IS 2 BP 961 EP 969 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 903DN UT WOS:000227405800036 ER PT J AU Gaensler, BM McClure-Griffiths, NM Oey, MS Haverkorn, M Dickey, JM Green, AJ AF Gaensler, BM McClure-Griffiths, NM Oey, MS Haverkorn, M Dickey, JM Green, AJ TI A stellar wind bubble coincident with the anomalous X-ray pulsar 1E 1048.1-5937: Are magnetars formed from massive progenitors? SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : bubbles; ISM : individual (GSH 288.3-0.5-28); pulsars : individual (1E 1048.1-5937); radio lines : ISM; stars : neutron; stars : winds, outflows ID REPEATER SGR-0526-66; INTERSTELLAR BUBBLES; LUMINOUS STARS; 1E 1048.1-5937; LOSS RATES; O-STARS; FIELD; COUNTERPART; EVOLUTION; DATABASE AB We present 21 cm H I observations from the Southern Galactic Plane Survey of the field around the anomalous X-ray pulsar 1E 1048.1 - 5937, a source whose X-ray properties imply that it is a highly magnetized neutron star ( a "magnetar"). These data reveal an expanding hydrogen shell, GSH 288.3 - 0.5 - 28, centered on 1E 1048.1 - 5937, with a diameter of 35 x 23 pc (for a distance of 2.7 kpc) and an expansion velocity of approximate to7.5 km s(-1). We interpret GSH 288.3 - 0.5 - 28 as a wind bubble blown by a 30-40 M-. star, but no such central star can be readily identified. We suggest that GSH 288.3 - 0.5 - 28 is the wind bubble blown by the massive progenitor of 1E 1048.1 - 5937 and consequently propose that magnetars originate from more massive progenitors than do radio pulsars. This may be evidence that the initial spin period of a neutron star is correlated with the mass of its progenitor and implies that the magnetar birthrate is only a small fraction of that for radio pulsars. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. Univ Michigan, Dept Astron, Ann Arbor, MI 48103 USA. Univ Tasmania, Dept Phys, Hobart, Tas 7001, Australia. Univ Sydney, Sch Phys, Sydney, NSW 2006, Australia. RP Gaensler, BM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-6, Cambridge, MA 02138 USA. EM bgaensler@cfa.harvard.edu RI Gaensler, Bryan/F-8655-2010; Dickey, John/C-6156-2013; OI McClure-Griffiths, Naomi/0000-0003-2730-957X; Gaensler, Bryan/0000-0002-3382-9558 NR 54 TC 95 Z9 95 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2005 VL 620 IS 2 BP L95 EP L98 DI 10.1086/428725 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 903DP UT WOS:000227406000006 ER PT J AU Muzerolle, J Megeath, ST Flaherty, KM Gordon, KD Rieke, GH Young, ET Lada, CJ AF Muzerolle, J Megeath, ST Flaherty, KM Gordon, KD Rieke, GH Young, ET Lada, CJ TI The outburst of V1647 Orionis revealed by Spitzer SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared : stars; stars : formation; stars : pre-main-sequence ID T-TAURI STARS; YOUNG STELLAR OBJECTS; MCNEILS NEBULA; FU ORIONIS; MOLECULAR CLOUD; DISK ACCRETION; IRAS-05436-0007; EVOLUTION; AURIGA; MODELS AB We present Spitzer Space Telescope observations of V1647 Ori, the outbursting source lighting McNeil's Nebula, taken near the optical peak of the outburst in early March 2004. The source is easily detected in all Spitzer imaging bands from 3.6 to 70 mum. The fluxes at all wavelengths are roughly a factor of 15 brighter than pre-outburst levels; we measure a bolometric luminosity of 44. We posit that this event is due to an increase L, in the accretion luminosity of the source. Simple models of an accretion disk plus a tenuous envelope can qualitatively explain the observed pre- and post-outburst spectral energy distributions. The accretion activity implied by our results indicates that the outburst may be intermediate between FUor- and EXor-type events. We also report the discovery of a previously unknown mid-infrared counterpart to the nearby Herbig-Haro object HH 22. C1 Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Muzerolle, J (reprint author), Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA. EM jamesm@as.arizona.edu NR 24 TC 32 Z9 32 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2005 VL 620 IS 2 BP L107 EP L110 DI 10.1086/428832 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 903DP UT WOS:000227406000009 ER PT J AU Springel, V Di Matteo, T Hernquist, L AF Springel, V Di Matteo, T Hernquist, L TI Black holes in galaxy mergers: The formation of red elliptical galaxies SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : theory; galaxies : formation; methods : numerical ID PARTICLE HYDRODYNAMICS SIMULATIONS; DIGITAL SKY SURVEY; STAR-FORMATION; REDSHIFT GALAXIES; MINOR MERGERS; COOLING FLOWS; DEEP-FIELDS; QUASARS; MASS; PROGENITORS AB We use hydrodynamical simulations to study the color transformations induced by star formation and active galactic nuclei (AGNs) during major mergers of spiral galaxies. Our modeling accounts for radiative cooling, star formation, and supernova feedback. Moreover, we include a treatment of accretion onto supermassive black holes embedded in the nuclei of the merging galaxies. We assume that a small fraction of the bolometric luminosity of an accreting black hole couples thermally to surrounding gas, providing a feedback mechanism that regulates its growth. The encounter and coalescence of the galaxies triggers nuclear gas inflow, which fuels both a powerful starburst and strong black hole accretion. Comparing simulations with and without black holes, we show that AGN feedback can quench star formation and accretion on a short timescale, particularly in large galaxies where the black holes can drive powerful winds once they become sufficiently massive. The color evolution of the remnant differs markedly between mergers with and without central black holes. Without AGNs, gas-rich mergers lead to elliptical galaxies that remain blue owing to residual star formation, even after more than 7 Gyr have elapsed. In contrast, mergers with black holes produce elliptical galaxies that redden much faster, an effect that is more pronounced in massive remnants where a nearly complete termination of star formation occurs, allowing them to redden to u - r similar or equal to 2.3 in less than 1 Gyr. AGN feedback may thus be required to explain the population of extremely red massive early-type galaxies, and it appears to be an important driver in generating the observed bimodal color distribution of galaxies in the local universe. C1 Max Planck Inst Astrophys, D-85740 Garching, Germany. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Springel, V (reprint author), Max Planck Inst Astrophys, Karl Schwarzschild Str 1,Postfach 1523, D-85740 Garching, Germany. RI Di Matteo, Tiziana/O-4762-2014; OI Di Matteo, Tiziana/0000-0002-6462-5734; Springel, Volker/0000-0001-5976-4599 NR 35 TC 393 Z9 394 U1 0 U2 5 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2005 VL 620 IS 2 BP L79 EP L82 DI 10.1086/428772 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 903DP UT WOS:000227406000002 ER PT J AU Laurance, WF Fearnside, PM Albernaz, AKM Vasconcelos, HL Ferreira, LV AF Laurance, WF Fearnside, PM Albernaz, AKM Vasconcelos, HL Ferreira, LV TI Amazonian deforestation models - Response SO SCIENCE LA English DT Letter C1 Smithsonian Trop Res Inst, Balboa, Panama. Inst Nacl Pesquisas Espaciais, Dept Ecol, BR-69011970 Manaus, Amazonas, Brazil. Museu Paraense Emilio Goeldi, BR-66077530 Belem, Para, Brazil. Univ Fed Uberlandia, Inst Biol, BR-38400902 Uberlandia, MG, Brazil. RP Laurance, WF (reprint author), Smithsonian Trop Res Inst, Apartado 2072, Balboa, Panama. EM laurancew@tivoli.si.edu RI Laurance, William/B-2709-2012; Fearnside, Philip/D-6559-2011; Vasconcelos, Heraldo/C-3353-2013; Albernaz, Ana Luisa/K-5226-2012 OI Fearnside, Philip/0000-0003-3672-9082; Vasconcelos, Heraldo/0000-0001-6969-7131; NR 5 TC 2 Z9 3 U1 1 U2 7 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 18 PY 2005 VL 307 IS 5712 BP 1044 EP 1044 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 900ED UT WOS:000227197300021 ER PT J AU Fearnside, PM Laurance, WF Albernaz, AKM Vasconcelos, HL Ferreira, LV AF Fearnside, PM Laurance, WF Albernaz, AKM Vasconcelos, HL Ferreira, LV TI A delicate balance in Amazonia - Response SO SCIENCE LA English DT Letter ID BRAZILIAN AMAZON; ENVIRONMENT C1 Inst Nacl de Pesquisas da Amazonia, Dept Ecol, BR-69011970 Manaus, Amazonas, Brazil. Smithsonian Trop Res Inst, Balboa, Panama. Museu Paraense Emilio Goeldi, BR-66077530 Belem, Para, Brazil. Univ Fed Uberlandia, Inst Biol, BR-38400902 Uberlandia, MG, Brazil. RP Fearnside, PM (reprint author), Inst Nacl de Pesquisas da Amazonia, Dept Ecol, CP 478, BR-69011970 Manaus, Amazonas, Brazil. EM pmfearn@inpa.gov.br RI Laurance, William/B-2709-2012; Fearnside, Philip/D-6559-2011; Vasconcelos, Heraldo/C-3353-2013; Albernaz, Ana Luisa/K-5226-2012 OI Fearnside, Philip/0000-0003-3672-9082; Vasconcelos, Heraldo/0000-0001-6969-7131; NR 5 TC 6 Z9 6 U1 0 U2 3 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 18 PY 2005 VL 307 IS 5712 BP 1045 EP 1045 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 900ED UT WOS:000227197300023 ER PT J AU Laurance, WF Albernaz, AKM Fearnside, PM Vasconcelos, HL Ferreira, LV AF Laurance, WF Albernaz, AKM Fearnside, PM Vasconcelos, HL Ferreira, LV TI Underlying causes of deforestation - Response SO SCIENCE LA English DT Letter ID BRAZILIAN AMAZON; ENVIRONMENT C1 Smithsonian Trop Res Inst, Balboa, Panama. Museu Paraense Emilio Goeldi, BR-66077530 Belem, Para, Brazil. Inst Nacl de Pesquisas da Amazonia, Dept Ecol, BR-69011970 Manaus, Amazonas, Brazil. Univ Fed Uberlandia, Inst Biol, BR-38400902 Uberlandia, MG, Brazil. RP Laurance, WF (reprint author), Smithsonian Trop Res Inst, Apartado 2072, Balboa, Panama. EM laurancew@tivoli.si.edu RI Laurance, William/B-2709-2012; Fearnside, Philip/D-6559-2011; Vasconcelos, Heraldo/C-3353-2013; Albernaz, Ana Luisa/K-5226-2012 OI Fearnside, Philip/0000-0003-3672-9082; Vasconcelos, Heraldo/0000-0001-6969-7131; NR 9 TC 2 Z9 2 U1 2 U2 5 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 18 PY 2005 VL 307 IS 5712 BP 1046 EP 1047 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 900ED UT WOS:000227197300025 ER PT J AU Ghent, RR Leverington, DW Campbell, BA AF Ghent, RR Leverington, DW Campbell, BA TI Earth-based observations of radar-dark crater haloes on the Moon: Implications for regolith properties SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID LUNAR CRATERS; ARISTARCHUS REGION; 70-CM WAVELENGTH; STRATIGRAPHY; ABUNDANCE; DEPOSITS; IMBRIUM; IRON AB Earth-based radar can be used in conjunction with other data sets collected remotely or in situ to characterize the physical and chemical properties of the lunar regolith. We use previously existing and newly acquired Earth-based radar measurements at 70-cm wavelength to investigate the properties of distinctive low-return haloes surrounding 39 nearside impact craters. These haloes are distinct from the well-known optically dark haloes associated with volcanic craters or with impacts into cryptomare deposits. We examine two possible mechanisms for formation of radar-dark haloes: (1) excavation of high-TiO2, high-loss tangent basalt and (2) deposition of a mantling layer produced in the impact process that is depleted in meter-sized blocks. Comparison of the radar data with Apollo and Lunar Orbiter images indicates a general spatial correspondence between radar-dark crater haloes and radial ridged ejecta facies distal to the radar-bright crater rims. Comparison with Clementine UV/VIS multispectral data indicates no apparent spatial correlation between regions of enhanced TiO2 content and radar-dark haloes; though variations in TiO2 content may play a role for some mare craters, they are insufficient to account for the observed offsets in radar echo power. We conclude that the radar-dark haloes result from a block-poor ejecta deposit that disappears over time with meteoroid bombardment. A more detailed and comprehensive analysis of ejecta degradation processes and rates following acquisition of additional high-resolution radar data could lead to a refinement of the lunar geologic timescale. C1 Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20013 USA. Hawaii Inst Geophys & Planetol, Sch Ocean & Earth Sci & Technol, Honolulu, HI 96822 USA. Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. RP Ghent, RR (reprint author), Smithsonian Inst, Ctr Earth & Planetary Studies, MRC 315,POB 37012, Washington, DC 20013 USA. EM ghentr@nasm.si.edu NR 48 TC 35 Z9 35 U1 0 U2 9 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 FEB 16 PY 2005 VL 110 IS E2 AR E02005 DI 10.1029/2004JE002366 PG 19 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 900LA UT WOS:000227215200001 ER PT J AU Adamski, D AF Adamski, D TI Review of Glyphidocera Walsingham of Costa Rica (Lepidoptera : Gelechioidea : Glyphidoceridae) SO ZOOTAXA LA English DT Article DE Central America; Glyphidocera; Glyphidoceridae; microlepidoptera; Central America AB The genus Glyphidocera ( Glyphidoceridae) of Costa Rica is reviewed. Eighty-eight new species are described: Glyphidocera adrogantiae, G. advenae, G. aediculae, G. aedis, G. ambrosiae, G. amitae, G. ancillae, G. animae, G. arae, G. arakawae, G. arenae, G. asymmetricae, G. audaciae, G. brumae, G. burpurae, G. barbae, G. capsae, G. cauponae, G. caveae, G. cellae, G. cenae, G. cenulae, G. cerula, G. ciatae, G. clavae, G. comae, G. contionis, G. coquae, G. corniculae, G. coronae, G. cotis, G. coturnicis, G. crepidae, G. dictionis, G. diciae, G. eminetiae, G. fabulae, G. faecis, G. ferae, G. fidem, G. formae, G. gazae, G. gemmae, G. glaebae, G. gloriae, G. harenae, G. infulae, G. lanae, G. laricae, G. lawrenceae, G. lupae, G. luxuriae, G. minarum, G. notae, G. novercae, G. nubis, G. olivae, G. ollae, G. operae, G. orae, G. paenulae, G. pali, G. personae, G. pilae, G. placentae, G. plebis, G. plumae, G. positurae, G. raedae, G. ranae, G. reginae, G. rodriguezi, G. rubetae, G. sapphiri, G. sardae, G. scuticae, G. sollertiae, G. spathae, G. speculae, G. staerae, G. terrae, G. tibiae, G. umbrae, G. vappae, G. virgulae, G. vocis, G. zamia, and G. zothecuale. Glyphidocera illiterata Meyrick, 1928, from Panama; G. zophocrossa Meyrick, 1929, from Trinidad; G. vestita Walsingham, 1911, from Panama; and G. guaroa Adamski 2002, from Costa Rica are redescribed. Diagnoses, descriptions, and type information are provided for each species. Photographs of holotypes, illustrations of head, wing venation, and male and female genitalia, digitized distribution maps, and a key to all Glyphidocera found in Costa Rica are included. C1 Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Adamski, D (reprint author), Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, POB 37012,MRC-168, Washington, DC 20013 USA. EM dadamski@sel.barc.usda.gov NR 15 TC 3 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 16 PY 2005 IS 858 BP 1 EP 205 PG 205 WC Zoology SC Zoology GA 903AA UT WOS:000227396600001 ER PT J AU Lambert, TD Malcolm, JR Zimmerman, BL AF Lambert, TD Malcolm, JR Zimmerman, BL TI Effects of mahogany (Swietenia macrophylla) logging on small mammal communities, habitat structure, and seed predation in the southeastern Amazon Basin SO FOREST ECOLOGY AND MANAGEMENT LA English DT Article DE Amazon; logging; mahogany; small mammals; seed predation; forest structure ID RATS PROECHIMYS-SEMISPINOSUS; NEOTROPICAL FOREST; BRAZILIAN AMAZON; TROPICAL FOREST; RAIN-FOREST; ECOLOGY; RECRUITMENT; POPULATIONS; DISTURBANCE; DISPERSAL AB Vast areas of the Amazon have been subjected to low-intensity selective logging for high value timber species such as mahogany (Swietenia macrophylla). Although the ecological consequences of such logging are often assumed to be minimal, few studies have directly tested this assumption. In this paper we examine the effects of various intensities of mahogany logging on small mammal communities, habitat structure, and seed predation in the southeastern Amazon Basin. We sampled small mammal communities using live traps at two logged and two unlogged sites. Within each site, we established five, 1 ha sampling grids that sampled the range of logging damage (in the case of logged sites) or mahogany densities (in the case of unlogged sites). Grids were sampled with 10 trap stations on the ground, 10 in the understory (at 1-3 m in height), and five in the canopy (at approximately 10 m in height) during three, 10-night trapping sessions over the course of the 10-month study. We measured a suite of forest structure and small mammal food resource (insect and fruit abundances) variables at each station and mahogany and peanut seed predation rates were measured at five locations per grid. We captured a total of 817 individuals of eight marsupial and 17 rodent species in 29,500 trap nights. Neither mahogany density across unlogged grids nor logging damage across logged grids were significantly correlated with variation in any of the measured habitat variables, seed predation rates, or measures of small mammal resource abundance. However, site-specific means for several variables (volume of downed woodnumber of vines per tree, number of vines, number of herbaceous stems, and understory density) were higher in logged than unlogged sites, but significantly so in only two cases (number of vines per tree, volume of downed wood). When pooled, the logged grids had higher small mammal abundances and species richness than unlogged grids; however, predation of mahogany seeds and peanuts did not differ significantly between the two site types. When the two logged sites were analyzed separately, the effects of logging were found to be very different at the two sites. One of the logged sites showed few effects of logging and had similar forest structure and small mammal communities to the unlogged sites, whereas the other logged site demonstrated effects consistent with previous reports on logging, including increased small mammal abundances, increased seed predation, and decreases in seedling and sapling densities as a function of increasing levels of logging damage. This study provides evidence that the ecological consequences of mahogany logging are strongly dependent on local site features; however, the overall effects of the logging appeared to be small, suggesting that areas that have been subjected to only low-levels of logging can still make valuable contributions to conservation. (C) 2004 Elsevier B.V. All rights reserved. C1 Univ Toronto, Fac Forestry, Toronto, ON M5S 3B3, Canada. Conservat Int, Brazil Program, Washington, DC 20036 USA. RP Lambert, TD (reprint author), Smithsonian Trop Res Inst, BCI 0948 APO AA, Miami, FL 34002 USA. EM thomas.lambert@utoronto.ca NR 56 TC 30 Z9 33 U1 3 U2 30 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0378-1127 J9 FOREST ECOL MANAG JI For. Ecol. Manage. PD FEB 15 PY 2005 VL 206 IS 1-3 BP 381 EP 398 DI 10.1016/j.foreco.2004.11.012 PG 18 WC Forestry SC Forestry GA 891GL UT WOS:000226569200028 ER PT J AU Sassi, J AF Sassi, J TI To the flag: The history of the pledge of allegiance. SO LIBRARY JOURNAL LA English DT Book Review C1 Smithsonian Inst, Washington, DC 20560 USA. RP Sassi, J (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 1 TC 1 Z9 1 U1 1 U2 1 PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION PI NEW YORK PA 249 W 17TH ST, NEW YORK, NY 10011 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD FEB 15 PY 2005 VL 130 IS 3 BP 148 EP 148 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 896RZ UT WOS:000226952500185 ER PT J AU Hutchinson, A AF Hutchinson, A TI Clara's grand tour: Travels with an eighteenth-century rhinoceros. SO LIBRARY JOURNAL LA English DT Book Review C1 Smithsonian Inst Lib, Washington, DC USA. RP Hutchinson, A (reprint author), Smithsonian Inst Lib, Washington, DC USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION PI NEW YORK PA 249 W 17TH ST, NEW YORK, NY 10011 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD FEB 15 PY 2005 VL 130 IS 3 BP 155 EP 155 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 896RZ UT WOS:000226952500215 ER PT J AU Jenkins, LP Roberts, TP Ward, MJ Zezas, A AF Jenkins, LP Roberts, TP Ward, MJ Zezas, A TI XMM-Newton observations of the interacting galaxy pairs NGC 7771/0 and NGC 2342/1 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Review DE galaxies : individual : NGC 7771; galaxies : individual : NGC 2342; galaxies : ISM; galaxies : starburst; X-rays : binaries; X-rays : galaxies ID X-RAY SOURCES; LUMINOUS INFRARED GALAXIES; ACTIVE GALACTIC NUCLEI; DWARF SEYFERT NUCLEI; STAR-FORMATION RATES; 1.49 GHZ ATLAS; CHANDRA OBSERVATIONS; SPIRAL GALAXIES; STARBURST GALAXIES; ANTENNAE GALAXIES AB We present XMM-Newton X-ray observations of the interacting galaxy pairs NGC 7771 7770 and NGC 23422341. In NGC 7771, for the first time we are able to resolve the X-ray emission into a bright central source plus two bright (L-X > 10(40) erg s(-1)) ultraluminous X-ray sources(ULXs) located either end of the bar. In the bright central source (L-X similar to 10(41) erg s(-1)), the soft emission is well-modelled by a two-temperature thermal plasma with kT = 0.4/0.7 keV. The hard emission is modelled with a flat absorbed power-law (Gamma similar to 1.7, N-H similar to10(22) cm(-2)), and this together with a low-significance (1.7sigma) similar to300 eV equivalent width emission line at similar to6 keV are the first indications that NGC 7771 may host a low-luminosity AGN. For the bar ULXs, a power-law fit to X-1 is improved at the 2.5sigma level with the addition of a thermal plasma component (kT similar to 0.3 keV), while X-2 is improved only at the 1.3sigma level with the addition of a disc blackbody component with T-in similar to 0.2 keV. Both sources are variable on short time-scales implying that their emission is dominated by single accreting X-ray binaries (XRBs). The three remaining galaxies, NGC 7770, NGC 2342 and NGC 2341, have observed X-ray luminosities of 0.2, 1.8 and 0.9 x 10(41) erg s(-1), respectively (0.3- 10 keV). Their integrated spectra are also well-modelled by multi-temperature thermal plasma components with kT = 0.2- 0.7 keV, plus power-law continua with slopes of Gamma = 1.8-2.3 that are likely to represent the integrated emission of populations of XRBs as observed in other nearby merger systems. A comparison with other isolated, interacting and merging systems shows that all four galaxies follow the established correlations for starburst galaxies between X-ray, far-infrared and radio luminosities, demonstrating that their X-ray outputs are dominated by their starburst components. C1 Univ Leicester, Dept Phys & Astron, Xray & Observ Astron Grp, Leicester LE1 7RH, Leics, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Jenkins, LP (reprint author), Univ Leicester, Dept Phys & Astron, Xray & Observ Astron Grp, Univ Rd, Leicester LE1 7RH, Leics, England. EM lej@star.le.ac.uk RI Zezas, Andreas/C-7543-2011; OI Zezas, Andreas/0000-0001-8952-676X; Jenkins, Leigh/0000-0001-9464-0719 NR 105 TC 11 Z9 11 U1 0 U2 0 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB 11 PY 2005 VL 357 IS 1 BP 109 EP 123 DI 10.1111/j.1365-2966.2005.08616.x PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 894KI UT WOS:000226790100011 ER PT J AU Hannikainen, DC Charles, PA van Zyl, L Kong, AKH Homer, L Hakala, P Naylor, T Davies, MB AF Hannikainen, DC Charles, PA van Zyl, L Kong, AKH Homer, L Hakala, P Naylor, T Davies, MB TI The X-ray source population of the globular cluster M15: Chandra high-resolution imaging SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars : dwarf novae; planetary nebulae : individual : K648; globular clusters : individual : M15; X-rays : binaries ID HUBBLE-SPACE-TELESCOPE; CENTRAL DENSITY CUSP; MASS BLACK-HOLE; CATACLYSMIC VARIABLES; PLANETARY-NEBULAE; OPTICAL-IDENTIFICATION; NEUTRON-STAR; CORE; EMISSION; BINARY AB The globular cluster M15 was observed on three occasions with the High Resolution Camera on- board Chandra in 2001 in order to investigate the X- ray source population in the cluster centre. After subtraction of the two bright central sources, four faint sources were identified within 50 arcsec of the core. One of these sources is probably the planetary nebula K648, making this the first positive detection of X- rays from a planetary nebula inside a globular cluster. Another two are identified with UV variables (one previously known), which we suggest are cataclysmic variables (CVs). The nature of the fourth source is more difficult to ascertain, and we discuss whether it is possibly a quiescent soft X- ray transient or also a CV. C1 Univ Southampton, Dept Phys & Astron, Southampton SO17 1BJ, Hants, England. Univ Helsinki, Observatory, FIN-00014 Helsinki, Finland. Univ Keele, Sch Phys, Astrophys Grp, Keele ST5 5BG, Staffs, England. Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Washington, Dept Astron, Seattle, WA 98195 USA. Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England. Lund Observ, SE-22100 Lund, Sweden. RP Hannikainen, DC (reprint author), Univ Southampton, Dept Phys & Astron, Southampton SO17 1BJ, Hants, England. EM diana@astro.helsinki.fi RI Naylor, Tim /A-9465-2015 NR 71 TC 15 Z9 15 U1 0 U2 0 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB 11 PY 2005 VL 357 IS 1 BP 325 EP 332 DI 10.1111/j.1365-2966.2004.08652.x PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 894KI UT WOS:000226790100030 ER PT J AU Ellison, SL Kewley, LJ Mallen-Ornelas, G AF Ellison, SL Kewley, LJ Mallen-Ornelas, G TI Emission-line abundances of absorption-selected galaxies at z < 0.5 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies : abundances; galaxies : ISM; quasars : absorption lines ID LY-ALPHA SYSTEMS; STAR-FORMING GALAXIES; LYMAN-BREAK GALAXIES; H-II REGIONS; LUMINOSITY-METALLICITY RELATION; HIGH-REDSHIFT GALAXIES; STELLAR MASS DENSITY; INTERSTELLAR-MEDIUM; SPIRAL GALAXIES; CHEMICAL ABUNDANCES AB We have obtained optical spectra of four galaxies associated with MgII quasi- stellar object (QSO) absorbers at redshifts 0.10 < z < 0.45. We calculate the gas- phase oxygen abundance of these galaxies using the empirical R(23) strong- line method. The absolute B- band magnitudes of the galaxies span - 20.6 < M(B) < -18.3. If the metallicities lie on the R(23) upper branch (8.4 < log (O/H) + 12 < 8.9), then the metallicities of these absorption- selected galaxies span the range between 0.5 and 1.4 Z. and would be consistent with the well- known luminosity- metallicity relation for 0.10 < z < 0.45 emission- line galaxies. However, such metallicities would be 0.5- 1.0 dex higher than those observed in damped Lyman alpha systems (DLAs) via absorption-line measurements at similar redshifts. Conversely, the lower R(23) branch calibration yields metallicities Z similar to 1/7 Z., consistent with the DLA absorption metallicities at low redshifts. In this case, the absorption- selected galaxies would lie significantly lower than the luminosity-metallicity relation for emission- line galaxies at z < 0.5. We discuss the implications and possible solutions for each scenario. C1 Univ Victoria, Victoria, BC V8P 1A1, Canada. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Ellison, SL (reprint author), Univ Victoria, 3800 Finnerty Rd, Victoria, BC V8P 1A1, Canada. EM sarae@uvic.ca NR 80 TC 29 Z9 29 U1 0 U2 0 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB 11 PY 2005 VL 357 IS 1 BP 354 EP 360 DI 10.1111/j.1365-2966.2005.08674.x PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 894KI UT WOS:000226790100034 ER PT J AU Kuhlen, M Strigari, LE Zentner, AR Bullock, JS Primack, JR AF Kuhlen, M Strigari, LE Zentner, AR Bullock, JS Primack, JR TI Dark energy and dark matter haloes SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods : N-body simulations; cosmology : theory; dark matter; large-scale structure of Universe ID SURFACE BRIGHTNESS GALAXIES; HIGH-REDSHIFT SUPERNOVAE; POWER-SPECTRUM NORMALIZATION; DIGITAL SKY SURVEY; LAMBDA-CDM HALOES; ROTATION CURVES; INNER STRUCTURE; COSMOLOGICAL CONSEQUENCES; ACCELERATING UNIVERSE; LENSING STATISTICS AB We investigate the effect of dark energy on the density profiles of dark matter haloes with a suite of cosmological N- body simulations and use our results to test analytic models. We consider constant equation of state models, and allow both w greater than or equal to 1 and w < -1. Using five simulations with w ranging from 1.5 to 0.5, and with more than similar to 1600 well- resolved haloes each, we show that the halo concentration model of Bullock et al. accurately predicts the median concentrations of haloes over the range of w, halo masses and redshifts that we are capable of probing. We find that the Bullock et al. model works best when halo masses and concentrations are defined relative to an outer radius set by a cosmology- dependent virial overdensity. For a fixed power spectrum normalization and fixed- mass haloes, larger values of w lead to higher concentrations and higher halo central densities, both because collapse occurs earlier and because haloes have higher virial densities. While precise predictions of halo densities are quite sensitive to various uncertainties, we make broad comparisons to galaxy rotation curve data. At fixed power spectrum normalization (fixed sigma(8)), w > -1 quintessence models seem to exacerbate the central density problem relative to the standard w = 1 model. For example, models with w similar or equal to - 0.5 seem disfavoured by the data, which can be matched only by allowing extremely low normalizations, sigma(8) less than or similar to 0.6. Meanwhile w < -1 models help to reduce the apparent discrepancy. We confirm that the halo mass function of Jenkins et al. provides an excellent approximation to the abundance of haloes in our simulations and extend its region of validity to include models with w < -1. C1 Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. Univ Chicago, Ctr Cosmol Phys, Chicago, IL 60637 USA. Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA. RP Kuhlen, M (reprint author), Univ Calif Santa Cruz, Dept Astron & Astrophys, 1156 High St, Santa Cruz, CA 95064 USA. EM mqk@ucolick.org RI Bullock, James/K-1928-2015; OI Bullock, James/0000-0003-4298-5082; Strigari, Louis/0000-0001-5672-6079 NR 79 TC 52 Z9 52 U1 0 U2 0 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB 11 PY 2005 VL 357 IS 1 BP 387 EP 400 DI 10.1111/j.1365-2966.2005.08663.x PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 894KI UT WOS:000226790100037 ER PT J AU Krongold, Y Nicastro, F Elvis, M Brickhouse, NS Mathur, S Zezas, A AF Krongold, Y Nicastro, F Elvis, M Brickhouse, NS Mathur, S Zezas, A TI The ionized nuclear environment in NGC 985 as seen by Chandra and BeppoSAX SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : Seyfert; quasars : absorption lines; X-rays : galaxies ID ACTIVE GALACTIC NUCLEI; REFLECTION GRATING SPECTROMETER; SEYFERT-1 GALAXY NGC-7469; HUBBLE-SPACE-TELESCOPE; X-RAY SPECTROSCOPY; XMM-NEWTON; DIELECTRONIC RECOMBINATION; RING GALAXY; THEORETICAL CALCULATIONS; LABORATORY MEASUREMENTS AB We investigate the ionized environment of the Seyfert 1 galaxy NGC 985 with a new Chandra HETGS observation and an archival BeppoSAX observation. Both spectra exhibit strong residuals to a single-power-law model, indicating the presence of an ionized absorber and a soft excess. A detailed model over the Chandra data shows that the 0.6-8 keV intrinsic continuum can be well represented by a power law (Gamma approximate to 1.6) plus a blackbody component (kT = 0.1 keV). Two absorption components are clearly required to fit the absorption features observed in the Chandra spectrum. The components have a difference of 29 in ionization parameter and 3 in column density. The presence of the low-ionization component is evidenced by an Fe M-shell unresolved transition array produced by charge states vII-xIII. The high-ionization phase is required by the presence of broad absorption features arising from several blends of Fe L-shell transitions (Fe XVII-XXII). A third highly ionized component might also be present, but the data do not allow us to constrain its properties. Although poorly constrained, the outflow velocities of the components (581 +/- 206 km s(-1) for the high-ionization phase and 197 +/- 184 km s(-1) for the low-ionization one) are consistent with each other and with the outflow velocities of the absorption components observed in the UV. In addition, the low-ionization component produces significant amounts of O VI, N V, and C IV, which suggests that a single outflow produces the UV and X-ray features. The broadband (0.1-100 keV) continuum in the BeppoSAX data can be parameterized by a power law (Gamma approximate to 1.4), a blackbody (kT = 0.1 keV), and a high-energy cutoff (E-c approximate to 70 keV). An X-ray luminosity variation by a factor of 2.3 is observed between the BeppoSAX and Chandra observations ( separated by almost 3 yr). Variability in the opacity of the absorbers is detected in response to the continuum variation, but while the colder component is consistent with a simple picture of photoionization equilibrium, the ionization state of the hotter component seems to increase, while the continuum flux drops. The most striking result in our analysis is that during both the Chandra and the BeppoSAX observations, the two absorbing components appear to have the same pressure. Thus, we suggest that the absorption arises from a multiphase wind. Such a scenario can explain the change in the opacity of both absorption components during the observations, but it requires that a third, hotter component be pressure-confining the two phases. Hence, our analysis points to a three-phase medium similar to the wind found in NGC 3783, and it further suggests that such a wind might be a common characteristic in active galactic nuclei. The pressure-confining scenario requires fragmentation of the confined phases into a large number of clouds. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. RP Krongold, Y (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Zezas, Andreas/C-7543-2011; OI Zezas, Andreas/0000-0001-8952-676X; Nicastro, Fabrizio/0000-0002-6896-1364; Brickhouse, Nancy/0000-0002-8704-4473 NR 65 TC 48 Z9 48 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2005 VL 620 IS 1 BP 165 EP 182 DI 10.1086/425293 PN 1 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 895HI UT WOS:000226851300016 ER PT J AU Fields, DL Mathur, S Pogge, RW Nicastro, F Komossa, S AF Fields, DL Mathur, S Pogge, RW Nicastro, F Komossa, S TI Supersolar N/C in the narrow-line Seyfert 1 galaxy Markarian 1044 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : Seyfert; intergalactic medium; quasars : absorption lines; quasars : emission lines; quasars : individual (Markarian 1044); ultraviolet : galaxies ID ACTIVE GALACTIC NUCLEI; QUASI-STELLAR OBJECTS; X-RAY PROPERTIES; COMPLETE SAMPLE; ABSORPTION-LINES; SPECTRA; UV; ABUNDANCES AB Narrow-line Seyfert 1 galaxies (NLS1s) are known to have extreme values of a number of properties compared to active galactic nuclei (AGNs) as a class. In particular, previous emission-line studies have suggested that NLS1s are unusually metal-rich compared to broad-line AGNs of comparable luminosity. We present low- and medium-resolution spectroscopic observations of the NLS1 Mrk 1044 with the Hubble Space Telescope Imaging Spectrometer (STIS). We identify two blueshifted intrinsic absorption systems at -1145 and -295 km s(-1) relative to the systemic velocity of the galaxy. Using a simple photoionization model of the absorbing gas, we find that the strongest and best measured of the absorption systems has N/C greater than or similar to 3.9(N/C)(circle dot). We also report on the discovery of three new Lyalpha forest lines with log N-H (I) greater than or equal to 12.77. This number is consistent with the 2.6 expected in the path length to the source redshift of Mrk 1044. C1 Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. RP Fields, DL (reprint author), Ohio State Univ, Dept Astron, 140 W 18th Ave, Columbus, OH 43210 USA. EM fields@astronomy.ohio-state.edu OI Nicastro, Fabrizio/0000-0002-6896-1364 NR 31 TC 9 Z9 9 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2005 VL 620 IS 1 BP 183 EP 190 DI 10.1086/426805 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 895HI UT WOS:000226851300017 ER PT J AU Herrnstein, RM Ho, PTP AF Herrnstein, RM Ho, PTP TI The nature of the molecular environment within 5 parsecs of the Galactic center SO ASTROPHYSICAL JOURNAL LA English DT Article DE Galaxy : center; ISM : clouds; ISM : molecules; radio lines : ISM ID SAGITTARIUS-A COMPLEX; APERTURE SYNTHESIS OBSERVATIONS; HIGH-RESOLUTION OBSERVATIONS; SGR-A; CENTER REGION; INTERSTELLAR AMMONIA; IONIZED-GAS; BLACK-HOLE; CLOUD; GALAXY AB We present a detailed study of molecular gas in the central 10 pc of the Galaxy through spectral line observations of four rotation inversion transitions of NH3 made with the Very Large Array. Updated line widths and NH3 ( 1, 1) opacities are presented, and temperatures, column densities, and masses are derived for the major molecular features. We examine the impact of Sgr A East on molecular material at the Galactic center and find that there is no evidence that the expansion of this shell has moved a significant amount of the 50 km s(-1) giant molecular cloud. The western streamer, however, shows strong indications that it is composed of material swept up by the expansion of Sgr A East. Using the mass and kinematics of the western streamer, we calculate an energy of E-SN = ( 2 - 9) x 10(51) ergs for the progenitor explosion and conclude that Sgr A East was most likely produced by a single supernova. The temperature structure of molecular gas in the central similar to 20 pc is also analyzed in detail. We find that molecular gas has a " two- temperature'' structure similar to that measured on much larger scales in the Galactic center region. The largest observed line ratios, however, cannot be understood in terms of a two-temperature model and most likely result from absorption of NH3 ( 3, 3) emission by cool surface layers of clouds. By comparing the observed NH3 ( 6, 6)- to-( 3, 3) line ratios, we disentangle three distinct molecular features within a projected distance of 2 pc from Sgr A*. Gas associated with the highest line ratios shows kinematic signatures of both rotation and expansion. The southern streamer shows no significant velocity gradients and does not appear to be directly associated with either the circumnuclear disk or the nucleus. The paper concludes with a discussion of the line- of- sight arrangement of the main features in the central 10 pc. C1 Columbia Univ, Dept Astron, New York, NY 10027 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Herrnstein, RM (reprint author), Columbia Univ, Dept Astron, 550 W 120th St,Mail Code 5246, New York, NY 10027 USA. EM herrnstein@astro.columbia.edu; pho@cfa.harvard.edu NR 63 TC 45 Z9 45 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2005 VL 620 IS 1 BP 287 EP 307 DI 10.1086/426047 PN 1 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 895HI UT WOS:000226851300027 ER PT J AU Eksi, KY Alpar, MA AF Eksi, KY Alpar, MA TI Disks surviving the radiation pressure of radio pulsars SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; stars : individual (SAX J1808.4-3658, Aquila X-1); stars : neutron; X-rays : binaries ID X-RAY PULSARS; ROTATING NEUTRON STARS; SPIN-DOWN; MILLISECOND PULSAR; SAX J1808.4-3658; MAGNETIC-DIPOLE; OBLIQUE-ROTATOR; FALLBACK DISK; ACCRETION; MODEL AB The radiation pressure of a radio pulsar does not necessarily disrupt a surrounding disk. The position of the inner radius of a thin disk around a neutron star, determined by the balance of stresses, can be estimated by comparing the electromagnetic energy density generated by the neutron star as a rotating magnetic dipole in vacuum with the kinetic energy density of the disk. Inside the light cylinder, the near zone electromagnetic field is essentially the dipole magnetic field, and the inner radius is the conventional Alfven radius. Far outside the light cylinder, in the radiation zone, \E\ = \B\, and the electromagnetic energy density is (S) / c proportional to 1/ r(2), where S is the Poynting vector. Shvartsman argued that a stable equilibrium cannot be found in the radiative zone because the electromagnetic energy density dominates over the kinetic energy density, with the relative strength of the electromagnetic stresses increasing with radius. In order to check whether this is also true near the light cylinder, we employ the Deutsch global electromagnetic field solutions for rotating oblique magnetic dipoles. Near the light cylinder the electromagnetic energy density increases steeply enough with decreasing r to balance the kinetic energy density at a stable equilibrium. The transition from the near zone to the radiation zone is broad. The radiation pressure of the pulsar cannot disrupt the disk for values of the inner radius up to about twice the light cylinder radius if the rotation axis and the magnetic axis are orthogonal. This allowed range beyond the light cylinder extends much farther for small inclination angles. The mass flow rate in quiescent phases of accretion- driven millisecond pulsars can occasionally drop to values low enough that the inner radius of the disk goes beyond the light cylinder. The possibilities considered here may be relevant for the evolution of spun- up X- ray binaries into millisecond pulsars, for some transients, and for the evolution of young neutron stars if there is a fallback disk surrounding the neutron star. C1 Sabanci Univ, TR-34956 Istanbul, Turkey. RP Eksi, KY (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM yavuz@sabanciuniv.edu; alpar@sabanciuniv.edu RI Eksi, Kazim/B-6434-2014 OI Eksi, Kazim/0000-0001-5999-0553 NR 48 TC 27 Z9 27 U1 1 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2005 VL 620 IS 1 BP 390 EP 397 DI 10.1086/425959 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 895HI UT WOS:000226851300035 ER PT J AU Miller, JM Wojdowski, P Schulz, NS Marshall, HL Fabian, AC Remillard, RA Wijnands, R Lewin, WHG AF Miller, JM Wojdowski, P Schulz, NS Marshall, HL Fabian, AC Remillard, RA Wijnands, R Lewin, WHG TI Revealing the focused companion wind in Cygnus X-1 with Chandra SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; stars : individual (Cygnus X-1); X-rays : binaries; X-rays : individual (Cygnus X-1) ID X-RAY BINARIES; OPTICAL-SPECTRUM; STELLAR WIND; VELA X-1; ABSORPTION; EMISSION; FE; LINE; SPECTROSCOPY; VARIABILITY AB We have analyzed a Chandra HETGS spectrum of the Galactic black hole Cygnus X- 1, obtained at a source flux that is approximately twice that commonly observed in its persistent low- intensity, spectrally hard state. We find a myriad of absorption lines in the spectrum, including H- and He- like resonance lines from Ne, Na, Mg, and Si. We calculate a flux- weighted mean redshift of similar or equal to 100 km s(-1) and a flux- weighted mean velocity width of similar or equal to 800 km s(-1) ( FWHM) for lines from these elements. We also detect a number of transitions from Fe xviii - xxiv and Ni xix - xx in absorption; however, the identification of these lines is less certain and a greater range of shifts and breadth is measured. Our observation occurred at a binary phase of phi similar or equal to 0.76; the lines observed are consistent with absorption in an ionized region of the supergiant O9.7 Iab companion wind. The spectrum is extremely complicated: a rather large range of temperatures is implied, and it is unlikely that a narrow range of ionization parameters can account for the lines observed. Prior Chandra HETGS spectra of Cygnus X- 1 were obtained in a similar transition state ( at phi similar or equal to 0.93) and in the low/ hard state ( at phi similar or equal to 0.84). Considered together, these spectra provide evidence for a companion wind that is focused as it flows onto the black hole primary in this system. C1 MIT, Ctr Space Res, Cambridge, MA 02139 USA. MIT, Dept Phys, Cambridge, MA 02139 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Cambridge, Inst Astron, Cambridge CB3 OHA, England. RP Miller, JM (reprint author), MIT, Ctr Space Res, 70 Vassar St, Cambridge, MA 02139 USA. EM jmmiller@cfa.harvard.edu NR 37 TC 32 Z9 32 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2005 VL 620 IS 1 BP 398 EP 404 DI 10.1086/426701 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 895HI UT WOS:000226851300036 ER PT J AU Bemporad, A Poletto, G Raymond, JC Biesecker, DA Marsden, B Lamy, P Ko, YK Uzzo, M AF Bemporad, A Poletto, G Raymond, JC Biesecker, DA Marsden, B Lamy, P Ko, YK Uzzo, M TI UVCS observation of sungrazer C/2001 C2: Possible comet fragmentation and plasma-dust interactions SO ASTROPHYSICAL JOURNAL LA English DT Article DE comets : general; comets : individual (C/2001 C2); ultraviolet : general ID ULTRAVIOLET CORONAGRAPH SPECTROMETER; SOLAR MINIMUM; INNER COMA; STREAMER; MODEL; IONS; TEMPERATURES; COLLISIONS; DENSITIES; P/HALLEY AB In this paper we analyze SOHO Ultraviolet Coronagraph Spectrometer (UVCS) observations of the sungrazing comet C/2001 C2, a member of the Kreutz family, observed on 2001 February 7 at heliocentric distances of 4.98 and 3.60 R-.. This comet apparently went through sequential fragmentation events along its path: further indication of fragmentation processes is provided by UVCS observations, which show the presence of two separate tails in the 4.98 R-. data set, which we interpret as two fragments unresolved by LASCO images, one of which sublimates before reaching 3.60 R-.. The cometary hydrogen Lyalpha signal, decaying exponentially with time, has been interpreted in terms of the H2O outgassing rate and the interactions of coronal protons with atoms created by the photodissociation of water. However, one of the fragments shows an additional Lyalpha contribution, constant with time, which adds to the temporally decaying signal. This contribution has been ascribed to the sublimation of pyroxene dust grains, whose end products neutralize coronal protons via charge exchange processes. Hence, the two fragments have different composition; differences throughout the comet body may have been the primary cause for the comet fragmentation. C1 Univ Florence, Dipartimento Astron & Sci Spazio, I-50125 Florence, Italy. Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Space Environm Ctr R SE, Boulder, CO 80305 USA. CNRS, Astron Spatiale Lab, F-13376 Marseille 12, France. RP Bemporad, A (reprint author), Univ Florence, Dipartimento Astron & Sci Spazio, Largo Enrico Fermi 5, I-50125 Florence, Italy. EM bemporad@arcetri.astro.it; poletto@arcetri.astro.it; jraymond@cfa.harvard.edu OI Bemporad, Alessandro/0000-0001-5796-5653 NR 40 TC 16 Z9 16 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2005 VL 620 IS 1 BP 523 EP 536 DI 10.1086/427063 PN 1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 895HI UT WOS:000226851300051 ER PT J AU Barinovs, G van Hemert, MC Krems, R Dalgarno, A AF Barinovs, G van Hemert, MC Krems, R Dalgarno, A TI Fine-structure excitation of C+ and Si+ by atomic hydrogen SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : atoms; ISM : molecules; scattering ID POTENTIAL-ENERGY CURVES; SHAPE RESONANCES; STRUCTURE TRANSITIONS; SPECTROSCOPY; CH+; PHOTODISSOCIATION; STATES; SCATTERING; COLLISIONS; SYSTEM AB We present calculations of cross sections for fine-structure excitation in collisions of carbon and silicon ions in the P-2 state with atomic hydrogen in the ground state. The results are based on accurate calculations of CH+ and SiH+ molecular potentials, including electronic core correlation and relativistic effects. We find that the energy dependence of the excitation cross sections is largely determined by shape resonances. Our work improves on the results of previous calculations with less accurate potentials. Analytical expressions for the cooling efficiency of C+(P-2(1/2)) and Si+(P-2(1/2)) are given for the temperature interval 15 - 2000 K. C1 Leiden Univ, Leiden Inst Chem, Theoret Chem Grp, NL-2300 RA Leiden, Netherlands. Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom Mol & Opt Phys, Cambridge, MA 02138 USA. RP Barinovs, G (reprint author), Leiden Univ, Leiden Inst Chem, Theoret Chem Grp, POB 9502, NL-2300 RA Leiden, Netherlands. RI Barinovs, Girts/H-6896-2016 OI Barinovs, Girts/0000-0001-6554-367X NR 23 TC 31 Z9 31 U1 2 U2 10 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2005 VL 620 IS 1 BP 537 EP 541 DI 10.1086/426860 PN 1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 895HI UT WOS:000226851300052 ER PT J AU Aguirre, A Schaye, J Hernquist, L Kay, S Springel, V Theuns, T AF Aguirre, A Schaye, J Hernquist, L Kay, S Springel, V Theuns, T TI Confronting cosmological simulations with observations of intergalactic metals SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : formation; intergalactic medium; quasars : absorption lines ID LYMAN-ALPHA FOREST; PIXEL STATISTICS; STAR-FORMATION; GALAXY FORMATION; GALACTIC WINDS; ENRICHMENT; METALLICITY; ABSORPTION; FEEDBACK; SPECTRA AB Using the statistics of pixel optical depths, we compare H i, C iv, and C iii absorption in a set of six high- quality z similar to 3-4 different state- of- the- art cosmological simulations that include galactic outflows. We find that the simulations predict far too little C iv absorption, unless the UV background is extremely soft, and always predict far too small C iii/ C iv ratios. We note, however, that much of the enriched gas is in a phase (T similar to 10(5) - 10(7) K, rho/(rho) similar to 0.1-10, Z greater than or similar to 0.1 Z.) that should cool by metal line emission- which was not included in our simulations. When the effect of cooling is modeled, the predicted C iv absorption increases substantially, but the C iii/ C iv ratios are still far too small because the density of the enriched gas is too low. Finally, we find that the predicted metal distribution is much too inhomogeneous to reproduce the observed probability distribution of C iv absorption. These findings suggest that strong winds cannot fully explain the z less than or similar to 6 observed enrichment and that an additional ( perhaps higher z) contribution is required. C1 Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA. Inst Adv Study, Sch Nat Sci, Princeton, NJ 08540 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Sussex, Ctr Astron, Brighton BN1 9QH, E Sussex, England. Max Planck Inst Astrophys, D-85740 Munich, Germany. Univ Durham, Dept Phys, Inst Computat Cosmol, Durham DH1 3LE, England. Univ Antwerp, B-2610 Antwerp, Belgium. RP Aguirre, A (reprint author), Univ Calif Santa Cruz, Dept Phys, 1156 High St, Santa Cruz, CA 95064 USA. EM aguirre@scipp.ucsc.edu OI Schaye, Joop/0000-0002-0668-5560 NR 24 TC 39 Z9 39 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2005 VL 620 IS 1 BP L13 EP L17 DI 10.1086/428498 PN 2 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 895HL UT WOS:000226851600004 ER PT J AU Luhman, KL D'Alessio, P Calvet, N Allen, LE Hartmann, L Megeath, ST Myers, PC Fazio, GG AF Luhman, KL D'Alessio, P Calvet, N Allen, LE Hartmann, L Megeath, ST Myers, PC Fazio, GG TI Spitzer identification of the least massive known brown dwarf with a circumstellar disk SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; planetary systems : protoplanetary disks; stars : formation; stars : low-mass, brown dwarfs; stars : pre-main-sequence ID STAR-FORMING REGION; MAIN-SEQUENCE STARS; T-TAURI STARS; I DARK CLOUD; CHAMELEON I; ACCRETION DISKS; YOUNG OBJECTS; EVOLUTIONARY MODELS; TRAPEZIUM CLUSTER; GRAIN-GROWTH AB Using the Infrared Array Camera ( IRAC) aboard the Spitzer Space Telescope, we have obtained mid- infrared photometry of the least massive known brown dwarf in the Chamaeleon I star- forming region. For this young brown dwarf, OTS 44, we have constructed a spectral energy distribution ( SED) from 0.8 to 8 mum by combining the measurements at 3.6, 4.5, 5.8, and 8.0 mum from IRAC with ground- based photometry at I, J, H, and K. The resulting SED for OTS 44 exhibits significant excess emission longward of 3 mum relative to the SED expected from the photosphere of the brown dwarf. We have successfully modeled the source of this excess emission in terms of an irradiated viscous accretion disk with M less than or similar to 10(-10) M. yr(-1). With a spectral type of M9.5 and a mass of similar to 15M(Jup), OTS 44 is now the coolest and least massive brown dwarf observed to have a circumstellar disk. M Jup These measurements demonstrate that disks exist around brown dwarfs even down to the deuterium- burning mass limit and the approximate upper mass limit of extrasolar planetary companions. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Nacl Autonoma Mexico, Ctr Radioastron & Astrofis, Morelia 58089, Michoacan, Mexico. RP Luhman, KL (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM kluhman@cfa.harvard.edu; p.dalessio@astrosmo.unam.mx; ncalvet@cfa.harvard.edu; leallen@cfa.harvard.edu; lhartmann@cfa.harvard.edu; tmegeath@cfa.harvard.edu; pmyers@cfa.harvard.edu; gfazio@cfa.harvard.edu NR 54 TC 37 Z9 37 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2005 VL 620 IS 1 BP L51 EP L54 DI 10.1086/428613 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 895HL UT WOS:000226851600013 ER PT J AU Yanoviak, SP Dudley, R Kaspari, M AF Yanoviak, SP Dudley, R Kaspari, M TI Directed aerial descent in canopy ants SO NATURE LA English DT Article ID BEHAVIOR; FOREST; FLIGHT; RAIN AB Numerous non- flying arboreal vertebrates use controlled descent ( either parachuting or gliding sensu stricto(1,2)) to avoid predation or to locate resources(3 - 7), and directional control during a jump or fall is thought to be an important stage in the evolution of flight(3,8,9). Here we show that workers of the neotropical ant Cephalotes atratus L. ( Hymenoptera: Formicidae) use directed aerial descent to return to their home tree trunk with > 80% success during a fall. Videotaped falls reveal that C. atratus workers descend abdomen- first through steep glide trajectories at relatively high velocities; a field experiment shows that falling ants use visual cues to locate tree trunks before they hit the forest floor. Smaller workers of C. atratus, and smaller species of Cephalotes more generally, regain contact with their associated tree trunk over shorter vertical distances than do larger workers. Surveys of common arboreal ants suggest that directed descent occurs in most species of the tribe Cephalotini and arboreal Pseudomyrmecinae, but not in arboreal ponerimorphs or Dolichoderinae. This is the first study to document the mechanics and ecological relevance of this form of locomotion in the Earth's most diverse lineage, the insects. C1 Smithsonian Trop Res Inst, Balboa, Panama. Univ Texas, Med Branch, Galveston, TX 77555 USA. Univ Florida, Florida Med Entomol Lab, Vero Beach, FL 32962 USA. Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. Univ Oklahoma, Dept Zool, Norman, OK 73019 USA. RP Kaspari, M (reprint author), Smithsonian Trop Res Inst, POB 2072, Balboa, Panama. EM mkaspari@ou.edu OI Kaspari, Michael/0000-0002-9717-5768 NR 25 TC 63 Z9 63 U1 2 U2 22 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 10 PY 2005 VL 433 IS 7026 BP 624 EP 626 DI 10.1038/nature03254 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 895KX UT WOS:000226862000042 PM 15703745 ER PT J AU Ward, PD Botha, J Buick, R De Kock, MO Erwin, DH Garrison, GH Kirschvink, JL Smith, R AF Ward, PD Botha, J Buick, R De Kock, MO Erwin, DH Garrison, GH Kirschvink, JL Smith, R TI Abrupt and gradual extinction among Late Permian land vertebrates in the Karoo Basin, South Africa SO SCIENCE LA English DT Article ID TRIASSIC BOUNDARY; MASS EXTINCTION; STRATIGRAPHIC RANGES; CONFIDENCE-INTERVALS; EVENT; CONSTRAINTS; SUPERGROUP; PATTERNS; RECOVERY; MARINE AB The Karoo basin of South Africa exposes a succession of Upper Permian. to Lower Triassic terrestrial strata containing abundant terrestrial vertebrate fossils. Paleomagnetic/magnetostratigraphic and carbon-isotope data allow sections to be correlated across the basin. With this stratigraphy, the vertebrate fossil data show a gradual extinction in the Upper Permian punctuated by an enhanced extinction pulse at the Permian-Triassic boundary interval, particularly among the dicynodont therapsids, coinciding with negative carbon-isotope anomalies. C1 Univ Washington, Dept Biol, Seattle, WA 98195 USA. Univ Washington, Dept Earth & Space Sci, Seattle, WA 98195 USA. S African Museum, ZA-8000 Cape Town, South Africa. CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. Rand Afrikaans Univ, Dept Geol, Johannesburg, South Africa. MRC121 Smithsonian Inst, Dept Paleobiol, Washington, DC 20013 USA. RP Ward, PD (reprint author), Univ Washington, Dept Biol, Seattle, WA 98195 USA. EM argo@u.washington.edu RI Erwin, Douglas/A-9668-2009; Botha-Brink, Jennifer/N-1893-2013; OI Botha-Brink, Jennifer/0000-0001-8824-9334; Buick, Roger/0000-0003-0139-1659 NR 34 TC 159 Z9 176 U1 1 U2 28 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 4 PY 2005 VL 307 IS 5710 BP 709 EP 714 DI 10.1126/science.1107068 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 894TQ UT WOS:000226814900039 PM 15661973 ER PT J AU Nicastro, F Mathur, S Elvis, M Drake, J Fang, TT Fruscione, A Krongold, Y Marshall, H Williams, R Zezas, A AF Nicastro, F Mathur, S Elvis, M Drake, J Fang, TT Fruscione, A Krongold, Y Marshall, H Williams, R Zezas, A TI The mass of the missing baryons in the X-ray forest of the warm-hot intergalactic medium SO NATURE LA English DT Article ID PROBE WMAP OBSERVATIONS; LOW-REDSHIFT; ABSORPTION SYSTEMS; CHANDRA DETECTION; ALPHA ABSORPTION; PKS-2155-304; GALAXIES; SPECTRA; DENSITY; CLOUDS AB Recent cosmological measurements indicate that baryons comprise about four per cent of the total mass-energy density of the Universe(1,2), which is in accord with the predictions arising from studies of the production of the lightest elements(3). It is also in agreement with the actual number of baryons detected at early times (redshifts z > 2)(4,5). Close to our own epoch (z < 2), however, the number of baryons detected add up to just over half (, 55 per cent) of the number seen at z > 2 (refs 6 - 11), meaning that about similar to45 per cent are 'missing'. Here we report a determination of the mass-density of a previously undetected population of baryons, in the warm - hot phase of the intergalactic medium. We show that this mass density is consistent, within the uncertainties, with the mass density of the missing baryons. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. Univ Calif Berkeley, Berkeley, CA 94720 USA. Univ Nacl Autonoma Mexico, Ist Astron, Mexico City 04510, DF, Mexico. MIT, Cambridge, MA 02139 USA. RP Nicastro, F (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM fnicastro@cfa.harvard.edu RI Zezas, Andreas/C-7543-2011; OI Zezas, Andreas/0000-0001-8952-676X; Nicastro, Fabrizio/0000-0002-6896-1364 NR 27 TC 136 Z9 136 U1 0 U2 3 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD FEB 3 PY 2005 VL 433 IS 7025 BP 495 EP 498 DI 10.1038/nature03245 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 893NT UT WOS:000226727200040 PM 15690033 ER PT J AU Cueto, M D'Croz, L Mate, JL San-Martin, A Darias, J AF Cueto, M D'Croz, L Mate, JL San-Martin, A Darias, J TI Elysiapyrones from Elysia diomedea. Do such metabolites evidence an enzymatically assisted electrocyclization cascade for the biosynthesis of their bicyclo[4.2.0]octane core? SO ORGANIC LETTERS LA English DT Article ID OCTOCORAL CARIJOA-MULTIFLORA; ENDIANDRIC ACID CASCADE; PLACOBRANCHUS-OCELLATUS; BIOMIMETIC SYNTHESIS; SACOGLOSSAN MOLLUSK; TRIDACHIA-CRISPATA; ORGANIC-SYNTHESIS; MARINE MOLLUSKS; PHOTOSYNTHESIS; SNF4435C AB Biogenetically interesting polypropionate-derived metabolites 1 and 2, featuring an unprecedented skeleton, have been isolated from the sea slug Elysia diomedea. Their enantiomeric character indicates that the current spontaneous electrocyclization cascade biogenetic hypothesis for the bicyclo[4.2.0]octane core must be enzymatically aided. These compounds are isomeric with the 15-nor-9,10-deoxytridachione/15-norphotodeoxytridachione pair of metabolites and encourage speculation about their biosynthetic relationship. C1 CSIC, Inst Prod Nat & Agrobiol, San Cristobal la Laguna 38206, Tenerife, Spain. Smithsonian Trop Res Inst, Balboa, Panama. Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, Div Marine Biol & Fisheries, Miami, FL 33149 USA. Univ Chile, Fac Ciencias, Dept Quim, Santiago, Chile. RP Cueto, M (reprint author), CSIC, Inst Prod Nat & Agrobiol, Avda Astrofis F Sanchez,3, San Cristobal la Laguna 38206, Tenerife, Spain. EM jdarias@ipna.csic.es RI Cueto, MERCEDES/L-3185-2014 OI Cueto, MERCEDES/0000-0002-9112-6877 NR 30 TC 32 Z9 32 U1 0 U2 6 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 1523-7060 J9 ORG LETT JI Org. Lett. PD FEB 3 PY 2005 VL 7 IS 3 BP 415 EP 418 DI 10.1021/ol0477428 PG 4 WC Chemistry, Organic SC Chemistry GA 892VW UT WOS:000226679100015 PM 15673253 ER PT J AU Kitajima, K Mulkey, SS Wright, SJ AF Kitajima, K Mulkey, SS Wright, SJ TI Variation in crown light utilization characteristics among tropical canopy trees SO ANNALS OF BOTANY LA English DT Article; Proceedings Paper CT Symposium on Structure and Function of Plant Canopies held at the Annual Meeting of the Ecological-Society-of-Japan CY MAR, 2003 CL Tsukuba, JAPAN SP Ecol Soc Japan DE Anacardium excelsum; Antirrhoea trichantha; architecture; Castilla elastica; Cecropia longipes; crown LAI; forest canopy; leaf angle; light extinction coefficient; Luehea seemannii; photosynthesis; tropical trees ID PHOTON FLUX-DENSITY; BROAD-LEAVED FOREST; RAIN-FOREST; LEAF AGE; CARBON GAIN; PHOTOSYNTHETIC CAPACITY; NITROGEN ALLOCATION; UNDERSTORY PLANTS; STAND STRUCTURE; USE EFFICIENCY AB Background and Aims Light extinction through crowns of canopy trees determines light availability at lower levels within forests. The goal of this paper is the exploration of foliage distribution and light extinction in crowns of five canopy tree species in relation to their shoot architecture, leaf traits (mean leaf angle, life span, photosynthetic characteristics) and successional status (from pioneers to persistent). Methods Light extinction was examined at three hierarchical levels of foliage organization, the whole crown, the outermost canopy and the individual shoots, in a tropical moist forest with direct canopy access with a tower crane. Photon flux density and cumulative leaf area index (LAI) were measured at intervals of 0.25-1 m along multiple vertical transects through three to five mature tree crowns of each species to estimate light extinction coefficients (K). Results Cecropia longipes, a pioneer species with the shortest leaf life span, had crown LAI <0.5. Among the remaining four species, crown LAI ranged from 2 to 8, and species with orthotropic terminal shoots exhibited lower light extinction coefficients (0.35) than those with plagiotropic shoots (0.53-0.80). Within each type, later successional species exhibited greater maximum LAI and total light extinction. A dense layer of leaves at the outermost crown of a late successional species resulted in an average light extinction of 61 % within 0.5 m from the surface. In late successional species, leaf position within individual shoots does not predict the light availability at the individual leaf surface, which may explain their slow decline of photosynthetic capacity with leaf age and weak differentiation of sun and shade leaves. Conclusion Later-successional tree crowns, especially those with orthotropic branches, exhibit lower light extinction coefficients, but greater total LAI and total light extinction, which contribute to their efficient use of light and competitive dominance. (C) 2004 Annals of Botany Company. C1 Univ Florida, Dept Bot, Gainesville, FL 32611 USA. Smithsonian Trop Res Inst, Balboa, Panama. RP Kitajima, K (reprint author), Univ Florida, Dept Bot, Gainesville, FL 32611 USA. EM kitajima@botany.ufl.edu RI Kitajima, Kaoru/E-8877-2012; Wright, Stuart/M-3311-2013 OI Wright, Stuart/0000-0003-4260-5676 NR 79 TC 64 Z9 68 U1 3 U2 18 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 2005 VL 95 IS 3 BP 535 EP 547 DI 10.1093/aob/mci051 PG 13 WC Plant Sciences SC Plant Sciences GA 894RI UT WOS:000226808900016 PM 15585541 ER PT J AU Garnet, KN Megonigal, JP Litchfield, C Taylor, GE AF Garnet, KN Megonigal, JP Litchfield, C Taylor, GE TI Physiological control of leaf methane emission from wetland plants SO AQUATIC BOTANY LA English DT Article DE methane; wetlands; Peltandra virginica; Orontium aquaticum; Juncus effuses; Taxodium distichum ID EMERGENT AQUATIC MACROPHYTES; PHRAGMITES-AUSTRALIS; INTERNAL PRESSURIZATION; DIEL VARIATION; ATMOSPHERE; FLUX; RHIZOSPHERE; TRANSPORT; PATTERNS; RICE AB The transport of methane from the rhizosphere to the atmosphere takes place in the intercellular spaces and stomata of wetland plants, and foliar gas exchange is one of the critical steps of the transport process. The objectives of our research were to investigate: (i) variation in foliar gas exchange among four common wetland plant species (i.e., Peltandra virginica L., Orontium aquaticum L., Juncus effusus L., and Taxodium distichum L.), (ii) the role of key environmental factors (i.e., light, temperature, and carbon dioxide concentration) in controlling foliar methane emission, and (iii) physiological mechanisms underlying the variation in methane emission due to species and the environment. Experiments were conducted in an instantaneous, flow-through gas-exchange system that operated on a mass balance approach and concurrently measured foliar fluxes of methane, water vapor, and carbon dioxide. The chamber system allowed for the control of light, temperature, humidity, and carbon dioxide concentration. Diel patterns of methane emission varied among species, with daylight emissions from P virginica and O. aquaticum 2-4 times those of J. effusus and T distichum in saturating light. Foliar methane emission from P. virginica (1.80 mu mol m(-2) s(-1)) under ambient daylight conditions was an order of magnitude higher than that of the other three species (similar to 0.20 mu mol m(-2) s(-1)). As leaf temperature was increased by 10 degrees C, methane emission increased by a factor of 1.5-2.2, and the temperature effect was independent of stomatal conductance. When data were pooled among the four species, varying the light and carbon dioxide concentrations in a stepwise manner produced changes in foliar methane emission that were associated with stomatal conductance (r(2) = 0.52). To scale our observations to other wetland plant species, a stepwise multiple regression model is offered that incorporates stomatal conductance and net carbon dioxide assimilation to estimate instantaneous methane emission from foliar surfaces. The model indicates that changes in stomatal conductance affect methane emission three times more than equivalent changes in net carbon dioxide assimilation. (c) 2004 Elsevier B.V. All rights reserved. C1 George Mason Univ, Sch Computat Sci, Fairfax, VA 22030 USA. Smithsonian Environm Res Ctr, Smithsonian Inst, Edgewater, MD 21037 USA. George Mason Univ, Dept Environm Sci & Policy, Manassas, VA 22030 USA. RP Garnet, KN (reprint author), George Mason Univ, Sch Computat Sci, 5C3,4400 Univ Dr, Fairfax, VA 22030 USA. EM kgarnet@gmu.edu NR 36 TC 30 Z9 34 U1 6 U2 39 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0304-3770 J9 AQUAT BOT JI Aquat. Bot. PD FEB PY 2005 VL 81 IS 2 BP 141 EP 155 DI 10.1016/j.aquabot.2004.10.003 PG 15 WC Plant Sciences; Marine & Freshwater Biology SC Plant Sciences; Marine & Freshwater Biology GA 908UQ UT WOS:000227816100002 ER PT J AU Rose, JA Arimoto, N Caldwell, N Schiavon, RP Vazdekis, A Yamada, Y AF Rose, JA Arimoto, N Caldwell, N Schiavon, RP Vazdekis, A Yamada, Y TI Radial age and metal abundance gradients in the stellar content of M32 SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies : elliptical and lenticular, cD; galaxies : evolution ID EARLY-TYPE GALAXIES; COLOR-MAGNITUDE DIAGRAM; GIANT BRANCH STARS; POPULATION SYNTHESIS; EMPIRICAL CALIBRATION; ELLIPTICAL GALAXIES; SPECTRAL-RESOLUTION; ABSORPTION FEATURES; SURFACE PHOTOMETRY; FEATURE INDEXES AB We present long-slit spectroscopy of the elliptical galaxy M32, obtained with the 8 in Subaru telescope at Mauna Kea, the 1.5 m Tillinghast telescope at the F. L. Whipple Observatory, and the 4 in Mayall telescope at the Kitt Peak National Observatory. The spectra cover the Lick index red spectral region, as well as higher order Balmer lines in the blue. Spectra have been taken with the slit offset from the nucleus to avoid scattered-light contamination from the bright nucleus of M32. An analysis of numerous absorption features, particularly involving the Hgamma and Hbeta Balmer lines, reveals that systematic radial trends are evident in the integrated spectrum of M32. Population synthesis models indicate a radial change in both the age and chemical composition of the light-weighted mean stellar population in M32, from the nucleus out to 33", i.e., an approximately 1.0 effective radius, R-e. Specifically, the light-weighted mean stellar population at 1R(e) is older by similar to3 Gyr and more metal-poor by about -0.25 dex in [Fe/H] than the central value of similar to4 Gyr and [Fe/H] similar to0.0. We show that this apparent population trend cannot be attributed to a varying contribution from either hot stars or emission-line contamination. The increase in age and decrease in metal abundance with radius are sufficiently well matched to explain the flat radial color profiles previously observed in M32. In addition, the ratio of Mg to Fe abundance, [Mg/Fe], increases from about -0.25 in the nucleus to about -0.08 at 1R(e) Finally, we find spuriously pronounced line-strength gradients in the Mayall data that are an artifact of scattered light from the bright nucleus. Scattered-light issues may explain the lack of consistency among previously published studies of radial line strength gradients in M32. C1 Univ N Carolina, Dept Phys & Astron, Chapel Hill, NC 27599 USA. Natl Astron Observ, Tokyo 181, Japan. Smithsonian Inst, FL Whipple Observ, Amado, AZ 85645 USA. Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA. Inst Astrofis Canarias, Tenerife, Spain. RP Rose, JA (reprint author), Univ N Carolina, Dept Phys & Astron, Chapel Hill, NC 27599 USA. EM jim@physics.unc.edu; arimoto@optik.mtk.nao.ac.jp; caldwell@flwo99.sao.arizona.edu; ripisc@virginia.edu; vazdekis@ll.iac.es; yyamada@optik.mtk.nao.ac.jp NR 70 TC 40 Z9 40 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD FEB PY 2005 VL 129 IS 2 BP 712 EP 728 DI 10.1086/427136 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 895HY UT WOS:000226852900012 ER PT J AU Hernandez, J Calvet, N Hartmann, L Briceno, C Sicilia-Aguilar, A Berlind, P AF Hernandez, J Calvet, N Hartmann, L Briceno, C Sicilia-Aguilar, A Berlind, P TI Herbig Ae/Be stars in nearby OB associations SO ASTRONOMICAL JOURNAL LA English DT Article DE Hertzsprung-Russell diagram; open clusters and associations : general; stars : emission-line, Be; stars : pre-main-sequence ID INTERMEDIATE-MASS STARS; T-TAURI STARS; MAIN-SEQUENCE EVOLUTION; ORION MOLECULAR CLOUD; CIRCUMSTELLAR DISKS; HIGH-RESOLUTION; STELLAR POPULATION; HIPPARCOS CATALOG; INTERNAL MOTIONS; INTRINSIC COLORS AB We have carried out a study of the early-type stars in nearby OB associations spanning an age range of similar to3-16 Myr, with the aim of determining the fraction of stars that belong to the Herbig Ae/Be class. We studied the B, A, and F stars in the nearby (less than or equal to500 pc) OB associations Upper Scorpius, Perseus OB2, Lacerta OB1, and Orion OB1, with membership determined from Hipparcos data. We also included in our study the early-type stars in the Trumpler 37 cluster, part of the Cep OB2 association. We obtained spectra for 440 Hipparcos stars in these associations, from which we determined accurate spectral types, visual extinctions, effective temperatures, luminosities and masses, using Hipparcos photometry. Using colors corrected for reddening, we find that the Herbig Ae/Be stars and the classical Be (CBe) stars occupy clearly different regions in the JHK diagram. Thus, we use the location on the JHK diagram, as well as the presence of emission lines and of strong 12 pm flux relative to the visual, to identify the Herbig Ae/Be stars in the associations. We find that the Herbig Ae/Be stars constitute a small fraction of the early-type stellar population even in the younger associations. Comparing the data from associations with different ages and assuming that the near-infrared excess in the Herbig Ae/Be stars arises from optically thick dusty inner disks, we determined the evolution of the inner disk frequency with age. We find that the inner disk frequency in the age range 3-10 Myr in intermediate-mass stars is lower than that in the low-mass stars (<1 M-circle dot); in particular, it is a factor of similar to10 lower at similar to3 Myr. This indicates that the timescales for disk evolution are much shorter in the intermediate-mass stars, which could be a consequence of more efficient mechanisms of inner disk dispersal (viscous evolution, dust growth, and settling toward the midplane). C1 CIDA, Merida 5101, Venezuela. Univ Los Andes, Merida 5101, Venezuela. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Hernandez, J (reprint author), CIDA, Apdo Postal 264, Merida 5101, Venezuela. EM jesush@cida.ve; ncalvet@cfa.harvard.edu; hartmann@cfa.harvard.edu; briceno@cida.ve; pberlind@cfa.harvard.edu NR 92 TC 127 Z9 128 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD FEB PY 2005 VL 129 IS 2 BP 856 EP 871 DI 10.1086/426918 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 895HY UT WOS:000226852900021 ER PT J AU Briceno, C Calvet, N Hernandez, J Vivas, AK Hartmann, L Downes, JJ Berlind, P AF Briceno, C Calvet, N Hernandez, J Vivas, AK Hartmann, L Downes, JJ Berlind, P TI The cida variability survey of orion OB1. I. The low-mass population of ORI OB1A and 1B SO ASTRONOMICAL JOURNAL LA English DT Article ID T-TAURI STARS; EMISSION-LINE STARS; MAIN-SEQUENCE STARS; YOUNG STELLAR POPULATION; HERBIG AE/BE STARS; MOLECULAR CLOUD; FORMING REGION; HYDRAE ASSOCIATION; TRAPEZIUM CLUSTER; VARIABLE-STARS AB We present results of a large-scale, multiepoch optical survey of the Orion OB1 association, carried out with the QUEST camera at the Venezuela National Astronomical Observatory. We identify for the first time the widely spread low-mass, young population in the Ori OB1a and OB1b subassociations. Candidate members were picked up by their variability in the V band and position in color-magnitude diagrams. We obtained spectra to confirm membership. In a 2 region spanning similar to68 deg(2), we found 197 new young stars; of these, 56 are located in the Ori OB1a subassociation and 141 in Ori OB1b. The spatial distribution of the low-mass young stars is spatially coincident with that of the high-mass members but suggests a much sharper edge to the association. Comparison with the spatial extent of molecular gas and extinction maps indicates that the subassociation Ori OB1b is concentrated within a ringlike structure of radius similar to2degrees(similar to15 pc at 440 pc), centered roughly on the star epsilon Ori in the Orion belt. The ring is apparent in (CO)-C-13 and corresponds to a region with an extinction A(nu) greater than or equal to 1. The stars exhibiting strong Halpha emission, an indicator of active accretion, are found along this ring, whereas the center is populated with weak Ha.-emitting stars. In contrast, Ori OB1a is located in a region devoid of gas and dust. We identify a grouping of stars within a similar to3 deg(2) area located in Ori OB1a, roughly clustered around the B2 star 25 Ori. The Herbig Ae/Be star V346 Ori is also associated with this grouping, which could be an older analog of sigma Ori. Using several sets of evolutionary tracks, we find an age of 710 Myr for Ori OB1a and of similar to4-6 Myr for Ori OB1b, consistent with previous estimates from OB stars. Indicators such as the equivalent width of Halpha and near-IR excesses show that the number of accreting low-mass stars decreases sharply between Ori OB1b and Ori OB1a. These results indicate that although a substantial fraction of accreting disks remain at ages similar to5 Myr, inner disks are essentially dissipated by 10 Myr. C1 Ctr Invest Astron, Merida 5101A, Venezuela. Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. Univ Los Andes, Postgrad Fis Fundamental, Merida, Venezuela. Cent Univ Venezuela, Postgrad Fis, Caracas, Venezuela. RP Ctr Invest Astron, Apdo Postal 264, Merida 5101A, Venezuela. EM briceno@cida.ve; ncalvet@cfa.harvard.edu; avivas@cida.ve; hartmann@cfa.harvard.edu; jesush@cida.ve; pberlin@cfa.harvard.edu NR 85 TC 88 Z9 88 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 FEB PY 2005 VL 129 IS 2 BP 907 EP 926 DI 10.1086/426911 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 895HY UT WOS:000226852900025 ER PT J AU Calvet, N Briceno, C Hernandez, J Hoyer, S Hartmann, L Sicilia-Acuilar, A Megeath, ST D'Alessio, P AF Calvet, N Briceno, C Hernandez, J Hoyer, S Hartmann, L Sicilia-Acuilar, A Megeath, ST D'Alessio, P TI Disk evolution in the Orion OB1 association SO ASTRONOMICAL JOURNAL LA English DT Article ID T-TAURI-STARS; SPECTRAL ENERGY-DISTRIBUTIONS; INTERMEDIATE-MASS STARS; MAIN-SEQUENCE TRACKS; ACCRETION DISKS; STELLAR POPULATION; FORMING REGION; YOUNG OBJECTS; CIRCUMSTELLAR DISKS; INFRARED-EMISSION AB We analyze multiband photometry of a subsample of low-mass stars in the associations Ori OB1a and 1b discovered during the Centro de Investigaciones de Astronomia (CIDA) Orion Variability Survey, which have ages of 7-10 and 3-5 Myr, respectively. We obtained UBVRCIC photometry at Mount Hopkins for six classical T Tauri stars (CTTSs) and 26 weak T Tauri stars (WTTSs) in Ori OB1a and for 21 CTTSs and two WTTSs in Ori OB1b. We also obtained L-band photometry for 14 CTTSs at Mount Hopkins and 10 and 18 mum photometry with OSCIR at Gemini for six CTTSs; of these, all six were detected at 10 pm, whereas only one was detected at 18 mum. We estimate mass accretion rates from the excess luminosity at U and find that they are consistent with determinations for a number of other associations, with or without high-mass star formation. The observed decrease of mass accretion rate with age is qualitatively consistent with predictions of viscous evolution of accretion disks, although other factors can also play a role in slowing accretion rates. We compare the excesses over photospheric fluxes in H - K, K - L, and K - N with the younger sample of Taurus and find an overall decrease of disk emission from Taurus to Ori OB1b to Ori OB1a. This decrease implies that significant grain growth and settling toward the midplane has taken place in the inner disks of Ori OB1. We compare the spectral energy distribution of the star detected at both 10 and IS mum with disk models for similar stellar and accretion parameters. We find that the low fluxes shortward of 18 mum of this Ori OB1b star cannot be due to the smaller disk radius expected from viscous evolution in the presence of the far-ultraviolet radiation fields from the OB stars in the association. Instead, we find that the disk of this star is essentially a flat disk, with little if any flaring, indicating a significant degree of dust settling toward the midplane, as expected from dust evolution in protoplanetary disks. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. Ctr Invest Astron, Merida 5101A, Venezuela. Pontificia Univ Catolica Chile, Santiago 22, Chile. Ctr Radioastron & Astrofis, Morelia 58089, Michoacan, Mexico. RP Calvet, N (reprint author), Smithsonian Astrophys Observ, Mail Stop 42, Cambridge, MA 02138 USA. EM nealvet@cfa.harvard.edu; briceno@cida.ve; jesush@cida.ve; hartmann@cfa.harvard.edu; avivas@cida.ve NR 70 TC 50 Z9 50 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD FEB PY 2005 VL 129 IS 2 BP 935 EP 946 DI 10.1086/426910 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 895HY UT WOS:000226852900027 ER PT J AU Rodriguez-Gil, P Torres, MAP AF Rodriguez-Gil, P Torres, MAP TI Time-resolved photometry of the nova remnants DM Gem, CP Lac, GI Mon, V400 Per, CT Ser and XX Tau SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE accretion, accretion discs; stars : binaries : close; novae, cataclysmic variables ID FAINT CATACLYSMIC VARIABLES; OLD NOVAE; SPECTROSCOPIC CONFIRMATION; STAR; SUPERHUMPS; DISCOVERY; NORTHERN AB We present the first results of a photometric survey of poorly studied nova remnants in the Northern Hemisphere. The main results are as follows: DM Gem shows a modulation at 0.123 d (probably linked to the orbit) and rapid variations at similar to22 min. A moderate resolution spectrum taken at the time of the photometric observations shows intense He II lambda4686 and Bowen emission, characteristic of an intermediate polar or a SW Sex star. Variability at 0.127 d and intense flickering (or quasi-periodic oscillations) are the main features of the light curve of CP Lac. A 0.1-mag dip lasting for similar to45 min is observed in GI Mon, which could be an eclipse. A clear modulation (probably related to the orbital motion) either at 0.179 d or 0.152 d is observed in the B-band light curve of V400 Per. The results for CT Ser point to an orbital period close to 0.16 d. Intense flickering is also characteristic of this old nova. Finally, XX Tau shows a possible periodic signal near 0.14 d and displays fast variability at similar to24 min. Its brightness seems to be modulated at similar to5 d. We relate this long periodicity to the motion of an eccentric/tilted accretion disc in the binary. C1 Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. Inst Astrofis Canarias, San Cristobal la Laguna 38205, Spain. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Coll, Dept Phys, Cork, Ireland. RP Rodriguez-Gil, P (reprint author), Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. EM Pablo.Rodriguez-Gil@warwick.ac.uk RI Rodriguez-Gil, Pablo/H-7709-2015 OI Rodriguez-Gil, Pablo/0000-0002-4717-5102 NR 41 TC 9 Z9 9 U1 0 U2 0 PU E D P SCIENCES 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 2005 VL 431 IS 1 BP 289 EP 296 DI 10.1051/0004-6361:20041112 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 897WI UT WOS:000227036100026 ER PT J AU Wilson, BA Dame, TM Masheder, MRW Thaddeus, P AF Wilson, BA Dame, TM Masheder, MRW Thaddeus, P TI A uniform CO survey of the molecular clouds in Orion and Monoceros SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM : clouds; ISM : structure; ISM : kinematics and dynamics; ISM : general ID REFLECTION NEBULAE; INFRARED OBSERVATIONS; EXPANDING SHELL; OB1 ASSOCIATION; CARBON-MONOXIDE; OUTFLOW; STARS; R2; ERIDANUS; POPULATION AB We report the results of a new large scale survey of the Orion-Monoceros complex of molecular clouds made in the J = 1 --> 0 line of (CO)-C-12 with the Harvard-Smithsonian 1.2 m millimetre-wave telescope. The survey consists of 52 288 uniformly spaced spectra that cover an area of 432 deg(2) on the sky and represent the most sensitive large-scale survey of the region to date. Distances to the constituent molecular clouds of the complex, estimated from an analysis of foreground and background stars, have provided information on the three dimensional structure of the entire complex. C1 Univ Bristol, Bristol, Avon, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Wilson, BA (reprint author), Univ Bristol, Tyndall Ave, Bristol, Avon, England. EM awilson@cfa.harvard.edu; tmdame@cfa.harvard.edu NR 58 TC 97 Z9 97 U1 0 U2 1 PU E D P SCIENCES 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 2005 VL 430 IS 2 BP 523 EP 539 DI 10.1051/0004-6361:20035943 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 889TE UT WOS:000226464700020 ER PT J AU Mediavilla, E Munoz, JA Kochanek, CS Falco, EE Arribas, S Motta, V AF Mediavilla, E Munoz, JA Kochanek, CS Falco, EE Arribas, S Motta, V TI The first precise determination of an optical-far-ultraviolet extinction curve beyond the local group (z=0.83) SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; gravitational lensing; quasars : individual (SBS 0909+532) ID SMALL-MAGELLANIC-CLOUD; GRAIN-SIZE DISTRIBUTIONS; ACTIVE GALACTIC NUCLEI; INTERSTELLAR DUST; MILKY-WAY; HIGH-REDSHIFT; GALAXIES; SUPERNOVAE; SPECTRA; DENSITY AB We present the optical-far-ultraviolet extinction curve of the dust in the lens galaxy of the gravitational lens system SBS 0909+ 532 (z = 0.83). Extending our previous optical-UV estimate (from lambda(0)(-1) similar to2 to 5 mum(-1)) into the far ultraviolet (from lambda(0)(-1) similar to 5 to 8 mum(-1)) is crucial for comparing with the extinction curves measured for Local Group galaxies in the spectral region where the differences are greatest. The SBS 0909+ 532 curve is similar to that of the LMC2 supershell, with a weaker 2175 Angstrom feature and a steeper rise into the UV than that observed in the Milky Way. The shapes of the extinction curve inferred from the quasar continuum and emission lines are in very good agreement. There is, however, a 0.6 +/- 0.1 mag offset in the implied magnification of the source that can be interpreted as differential magnification due to microlensing of the compact accretion disk producing the continuum emission by the stars in the lens galaxy. There is no evidence for a wavelength dependence on the microlensing effect except for a similar to2 sigma shift near the Mg II emission line. If this difference were confirmed, it could be used to probe the emission profile of the quasar accretion disk. C1 Inst Astrofis Canarias, Tenerife 38200, Spain. Univ Valencia, Dept Astron & Astrofis, E-46100 Valencia, Spain. Ohio State Univ, Dept Astron, Columbus, OH 43221 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Space Telescope Sci Inst, Baltimore, MD 20852 USA. Fac Ciencias, Dept Astron, Montevideo 11400, Uruguay. RP Mediavilla, E (reprint author), Inst Astrofis Canarias, Via Lactea S-N, Tenerife 38200, Spain. NR 31 TC 23 Z9 23 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2005 VL 619 IS 2 BP 749 EP 754 DI 10.1086/426579 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 891NZ UT WOS:000226589100009 ER PT J AU Dopita, MA Groves, BA Fischera, J Sutherland, RS Tuffs, RJ Popescu, CC Kewley, LJ Reuland, M Leitherer, C AF Dopita, MA Groves, BA Fischera, J Sutherland, RS Tuffs, RJ Popescu, CC Kewley, LJ Reuland, M Leitherer, C TI Modeling the pan-spectral energy distribution of starburst galaxies. I. The role of ISM pressure and the molecular cloud dissipation timescale SO ASTROPHYSICAL JOURNAL LA English DT Review DE dust, extinction; galaxies : general; galaxies : starburst; HII regions; infrared : galaxies; radio continuum : galaxies; ultraviolet : galaxies ID STAR-FORMATION RATES; LUMINOUS INFRARED GALAXIES; LYMAN CONTINUUM EXTINCTION; ALPHA EMITTING GALAXIES; LARGE-MAGELLANIC-CLOUD; SPIRAL GALAXIES; RADIO-EMISSION; TEMPERATURE-FLUCTUATIONS; INTERSTELLAR GRAINS; HIGH-REDSHIFT AB In this paper, we combine the stellar spectral synthesis code STARBURST99, the nebular modeling code MAPPINGS IIIq, a one-dimensional dynamical evolution model of H II regions around massive clusters of young stars, and a simplified model of synchrotron emissivity to produce purely theoretical self-consistent synthetic spectral energy distributions (SEDs) for ( solar metallicity) starbursts lasting similar to 10(8) yr. These SEDs extend from the Lyman limit to beyond 21 cm. We find that two ISM parameters control the form of the SED: the pressure in the diffuse phase of the ISM ( or, equivalently, its density), and the molecular cloud dissipation timescale. In particular, the shape of the far-infrared ( dust re-emission) bump is strongly dependent on the mean pressure in the star-forming or starburst galaxy. This can explain the range of far-infrared (FIR) colors seen in starburst galaxies. In the case of objects of composite excitation, such diagrams potentially provide a means of estimating the fraction of the FIR emission that is contributed by an active nucleus. We present detailed SED fits to Arp 220 and NGC 6240, and we give the predicted colors for starburst galaxies derived from our models for the IRAS and the Spitzer Space Telescope MIPS and IRAC instruments. Our models reproduce the spread in observed colors of starburst galaxies. From both the SED fits and the color : color diagrams, we infer the presence of a population of compact and ultracompact H II regions around single OB stars or small OB clusters. Finally, we present absolute calibrations to convert observed fluxes into star formation rates in the UV (GALEX), at optical wavelengths (Halpha), and in the IR ( IRAS or Spitzer). We show that 25 mum fluxes are particularly valuable as star formation indicators, since they largely eliminate one of the parameters controlling the IR SED. C1 Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. Max Planck Inst Kernphys, D-69117 Heidelberg, Germany. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Sterrewacht Leiden, NL-2300 RA Leiden, Netherlands. Space Telescope Sci Inst, Baltimore, MD 21218 USA. RP Australian Natl Univ, Res Sch Astron & Astrophys, Cotter Rd, Weston, ACT 2611, Australia. EM Michael.Dopita@anu.edu.au RI Dopita, Michael/P-5413-2014 OI Dopita, Michael/0000-0003-0922-4986 NR 150 TC 117 Z9 117 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 2005 VL 619 IS 2 BP 755 EP 778 DI 10.1086/423948 PN 1 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 891NZ UT WOS:000226589100010 ER PT J AU Gottlieb, CA Thorwirth, S McCarthy, MC Thaddeus, P AF Gottlieb, CA Thorwirth, S McCarthy, MC Thaddeus, P TI The radio spectra of S-3 and S-4 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : molecules; molecular data; molecular processes; radio lines : ISM; stars : formation ID MOLECULAR LINE SURVEY; S-BEARING MOLECULES; IOS PELE PLUME; SAGITTARIUS B2; ROTATIONAL SPECTRUM; GEOMETRICAL STRUCTURE; OBSERVATIONAL DATA; ORION-KL; 263 GHZ; SULFUR AB The pure rotational spectra of the polar asymmetric top molecules S-3 and S-4 have recently been observed in the laboratory for the first time. Approximately 150 transitions of S-3 between 10 and 458 GHz and a similar number for S-4 between 6 and 271 GHz have been measured. Many transitions of both molecules are accessible with existing telescopes across the entire radio band. The most interesting astronomical lines to 300 GHz are calculated here from the derived spectroscopic constants to an uncertainty of 1 km s(-1) or better in equivalent radial velocity, and even at 700 GHz uncertainties are probably worse by only an order of magnitude. Both S-3 and S-4 are plausible candidates for detection in Galactic molecular sources, the atmosphere of the Jovian moon Io, and comets. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Harvard Univ, Div Engn & Appl Sci, Cambridge, MA 02138 USA. RP Gottlieb, CA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM cgottlieb@cfa.harvard.edu RI Thorwirth, Sven/C-6217-2011; OI Thorwirth, Sven/0000-0001-8200-6710; McCarthy, Michael/0000-0001-9142-0008 NR 35 TC 5 Z9 5 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2005 VL 619 IS 2 BP 939 EP 944 DI 10.1086/426711 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 891NZ UT WOS:000226589100022 ER PT J AU Lee, CF Ho, PTP White, SM AF Lee, CF Ho, PTP White, SM TI Molecular line observations of IRAM 04191+1522 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : individual (IRAM 04191+1522); ISM : jets and outflows; stars : formation ID STAR-FORMATION; PROTOSTAR IRAM-04191; CLOUD CORES; JET-DRIVEN; ROTATION; COLLAPSE; OUTFLOW; INFALL; N2H+; DYNAMICS AB We have mapped the CO, HCO+, CS, and N2H+ emission around a low-luminosity Class 0 source IRAM 04191+1522 in the Taurus molecular cloud using the Berkeley-Illinois-Maryland Association array. A bipolar molecular outflow is seen in CO, HCO+, and CS emission originating from around the IRAM source, while a flattened envelope is seen in N2H+ emission surrounding the waist of the molecular outflow around the IRAM source. Outflow, rotation, and probably infall are seen around the Class 0 source, indicating a complicated context for star formation in the earliest stages. The N2H+ envelope is a thick clumpy torus with a tenuous outer part and a ringlike dense inner edge. The dense inner edge has a mean radius of 10", or 1400 AU. The outer part of the torus exhibits differential rotation, and the infalling material appears to carry angular momentum inward toward the central source. The region surrounded by the inner edge of the torus may have a solid-body rotation. The envelope may result from the collapse of a rotating, magnetized toroid toward the central source. Outflow motion is seen in the outer part of the inner edge of the torus, probably due to an interaction with the molecular outflow. Two armlike structures are seen extending out from the inner edge in the torus. One of them is clearly seen with the velocity increasing roughly linearly with the distance. The HCO+ emission around the source may trace the central core around the source, showing a velocity structure connecting to that of the outer part of the torus. The molecular outflow is best seen in CO. It is bipolar with both a southwest and a northeast lobe. Two internal structures are seen along the main outflow axis within the lobes: ( 1) a strong CO emission at similar to20" to the northeast of the IRAM source, likely tracing an internal bow shock driven by a collimated, episodic jet and ( 2) a linear HCO+ structure of similar to50" length at low blueshifted velocity to the southwest of the IRAM source, requiring some interaction with a jet to be produced. In addition, a dense condensation is also seen in HCO+ and CS to the south of the IRAM source, likely representing a recent strong outflow interaction. C1 Harvard Smithsonian Ctr Astrophys, Hilo, HI 96720 USA. Univ Maryland, Dept Astron, College Pk, MD 20742 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Harvard Smithsonian Ctr Astrophys, Submillimeter Array,645 N Aohoku Pl, Hilo, HI 96720 USA. EM cflee@cfa.harvard.edu; ho@cfa.harvard.edu; white@astro.umd.edu NR 33 TC 22 Z9 22 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2005 VL 619 IS 2 BP 948 EP 958 DI 10.1086/426780 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 891NZ UT WOS:000226589100024 ER PT J AU Jang-Condell, H Sasselov, DD AF Jang-Condell, H Sasselov, DD TI Type I migration in a nonisothermal protoplanetary disk SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; planetary systems : formation; planetary systems : protoplanetary disks ID ACCRETION DISKS; YOUNG OBJECTS; LINDBLAD RESONANCES; WAVE EXCITATION; DENSITY WAVES; GASEOUS DISK; PLANET; MASS; SYSTEMS; NEBULA AB We calculate rates of type I migration of protoplanets in a nonisothermal three-dimensional protoplanetary disk, building on planet-disk models developed in previous work. We find that including the vertical thickness of the disk results in a decrease in the type I migration rate by a factor of similar to2 from that of a two-dimensional disk. The vertical temperature variation has only a modest effect on migration rates, since the torques at the midplane are weighted heavily because both the density and the perturbing potential are maximized at the midplane. However, temperature perturbations resulting from shadowing and illumination at the disk's surface can decrease the migration rate by up to another factor of 2 for planets at the gap-opening threshold at distances for which viscous heating is minimal. This would help to resolve the timescale mismatch between the standard core-accretion scenario for planet formation and the survival of planets and could help explain some of the rich diversity of planetary systems already observed. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Jang-Condell, H (reprint author), Carnegie Inst Washington, Dept Terr Magnetism, 5241 Broad Branch Rd NW, Washington, DC 20015 USA. EM hannah@dtm.ciw.edu; dsasselov@cfa.harvard.edu OI Jang-Condell, Hannah/0000-0002-7639-1322 NR 23 TC 24 Z9 24 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2005 VL 619 IS 2 BP 1123 EP 1131 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 891NZ UT WOS:000226589100042 ER PT J AU Vasquez, AM Raymond, JC AF Vasquez, AM Raymond, JC TI Oxygen abundance in coronal streamers SO ASTROPHYSICAL JOURNAL LA English DT Article DE solar wind; Sun : abundances; Sun : corona; Sun : UV radiation ID WHOLE SUN MONTH; SLOW SOLAR-WIND; OUTFLOW VELOCITIES; ELEMENTAL ABUNDANCES; ENERGETIC PARTICLES; TEMPERATURE; MINIMUM; HOLE; SPECTROMETER; MODEL AB In a previous work we developed a stationary proton-electron MHD model of the solar corona, suitable for the minimum-activity epochs. In the present work, we use empirically derived information from the past solar minimum for the oxygen parameters ( temperatures and outflow velocity) to develop an oxygen model in the frame of our previous model. Solar and Heliospheric Observatory UVCS observations of past minimum coronal streamers in the O VI lambda1032 and O VI lambda1037 lines have revealed that oxygen abundances are very much depleted within the stable closed-field regions of the quiescent streamers. This characteristic appears as a relatively dark region, often seen in the core of the quiescent equatorial streamers when imaged in oxygen lines. Using the oxygen abundance as a free parameter, we compute the expected O vi line emissivities from our models and synthesize images considering the projection effects in detail. We find here that, in order to obtain oxygen images with dark streamer cores similar to those observed, very low element abundances have to be assumed. The required depletion factors are lower than previous estimates that do not account for projection effects, which is especially important at 1.75 R-circle dot and higher. C1 Inst Astron & Fis Espacio, RA-1428 Buenos Aires, DF, Argentina. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Buenos Aires, Dept Phys, RA-1053 Buenos Aires, DF, Argentina. RP Vasquez, AM (reprint author), Inst Astron & Fis Espacio, CC 67,Suc 28, RA-1428 Buenos Aires, DF, Argentina. EM albert@iafe.uba.ar NR 35 TC 15 Z9 15 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2005 VL 619 IS 2 BP 1132 EP 1141 DI 10.1086/426776 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 891NZ UT WOS:000226589100043 ER PT J AU Barth, AJ Greene, JE Ho, LC AF Barth, AJ Greene, JE Ho, LC TI Dwarf Seyfert 1 nuclei and the low-mass end of the M-BH-sigma relation SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : kinematics and dynamics; galaxies : nuclei; galaxies : Seyfert ID ACTIVE GALACTIC NUCLEI; BLACK-HOLE MASS; VELOCITY DISPERSION; GALAXIES; QUASARS; KINEMATICS; HOSTS; BULGE AB To examine the relationship between black hole mass and host galaxy velocity dispersion for low black hole masses, we have measured the velocity dispersions of 15 Seyfert 1 galaxies from the recent catalog of Greene & Ho. These Seyfert galaxies were selected from the Sloan Digital Sky Survey to have estimated black hole masses below 10(6) M-.. The data are consistent with a straightforward downward extrapolation of the local M-BH-sigma relation, indicating that this correlation extends over a range of more than 4 orders of magnitude in black hole mass. The rms scatter of the sample about the extrapolated M-BH-sigma relation is 0.57 dex, consistent with the expected scatter of single-epoch mass estimates for Seyfert 1 galaxies. C1 Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. RP Barth, AJ (reprint author), Univ Calif Irvine, Dept Phys & Astron, 4129 Frederick Reines Hall, Irvine, CA 92697 USA. EM barth@uci.edu; jgreene@cfa.harvard.edu; lho@ociw.edu NR 29 TC 124 Z9 125 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2005 VL 619 IS 2 BP L151 EP L154 DI 10.1086/428365 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 891OB UT WOS:000226589300007 ER PT J AU Stark, AA Lee, Y AF Stark, AA Lee, Y TI The scale height of giant molecular clouds is less than that of smaller clouds SO ASTROPHYSICAL JOURNAL LA English DT Article DE Galaxy : structure; ISM : clouds; ISM : molecules ID GALAXY; DISK AB An antenna temperature thresholding algorithm is used on the Bell Laboratories (CO)-C-13 J = 1 --> 0 Milky Way Survey to create a catalog of 1400 molecular clouds. Of these, 281 clouds are selected for having well- determined kinematic distances. The scale height, luminosity, internal velocity dispersion, and size of the cloud sample are analyzed to show that clouds smaller than similar to10(5.5) M-. have a scale height which is about 35 pc, roughly independent of cloud mass, while larger clouds, the giant molecular clouds, have a reduced scale height which declines with increasing cloud mass. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Korea Astron Observ, Taeduk Radio Astron Observ, Taejon 305348, South Korea. RP Stark, AA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM aas@cfa.harvard.edu; yulee@trao.re.kr OI Stark, Antony/0000-0002-2718-9996 NR 17 TC 19 Z9 19 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2005 VL 619 IS 2 BP L159 EP L162 DI 10.1086/427936 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 891OB UT WOS:000226589300009 ER PT J AU Cranmer, SR van Ballegooijen, AA AF Cranmer, SR van Ballegooijen, AA TI On the generation, propagation, and reflection of Alfven waves from the solar photosphere to the distant heliosphere SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Review DE MHD; solar wind; Sun : atmospheric motions; Sun : corona; turbulence; waves ID MAGNETIC-FLUX TUBES; CORONAL HEATING MECHANISMS; LONGITUDINAL-TRANSVERSE WAVES; STELLAR CONVECTION ZONES; PERIOD ACOUSTIC-WAVES; LOW-FREQUENCY WAVES; BAND BRIGHT POINTS; TRANSITION REGION; QUIET-SUN; MAGNETOHYDRODYNAMIC TURBULENCE AB We present a comprehensive model of the global properties of Alfven waves in the solar atmosphere and the fast solar wind. Linear non-WKB wave transport equations are solved from the photosphere to a distance past the orbit of the Earth, and for wave periods ranging from 3 s to 3 days. We derive a radially varying power spectrum of kinetic and magnetic energy fluctuations for waves propagating in both directions along a superradially expanding magnetic flux tube. This work differs from previous models in three major ways. ( 1) In the chromosphere and low corona, the successive merging of flux tubes on granular and supergranular scales is described using a two-dimensional magnetostatic model of a network element. Below a critical flux-tube merging height the waves are modeled as thin-tube kink modes, and we assume that all of the kink-mode wave energy is transformed into volume-filling Alfven waves above the merging height. ( 2) The frequency power spectrum of horizontal motions is specified only at the photosphere, based on prior analyses of G-band bright point kinematics. Everywhere else in the model the amplitudes of outward and inward propagating waves are computed with no free parameters. We find that the wave amplitudes in the corona agree well with off-limb nonthermal line-width constraints. ( 3) Nonlinear turbulent damping is applied to the results of the linear model using a phenomenological energy loss term. A single choice for the normalization of the turbulent outer-scale length produces both the right amount of damping at large distances ( to agree with in situ measurements) and the right amount of heating in the extended corona ( to agree with empirically constrained solar wind acceleration models). In the corona, the modeled heating rate differs by more than an order of magnitude from a rate based on isotropic Kolmogorov turbulence. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Cranmer, Steven/0000-0002-3699-3134 NR 215 TC 211 Z9 213 U1 3 U2 14 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 EI 1538-4365 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD FEB PY 2005 VL 156 IS 2 BP 265 EP 293 DI 10.1086/426507 PG 29 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 890JZ UT WOS:000226508800009 ER PT J AU Adey, WH Hayek, LAC AF Adey, WH Hayek, LAC TI The biogeographic structure of the western North Atlantic rocky intertidal SO CRYPTOGAMIE ALGOLOGIE LA English DT Article DE benthic invertebrates; biogeography; biogeographic model testing; community structure; marine algae; quantitative ecological analysis; rocky intertidal; western North Atlantic ID ICE; NEWFOUNDLAND; PATTERNS AB The shallow water, coastal flora and fauna from Cape Cod to southern Labrador in the northwestern North Atlantic have been biogeographically regarded as a single unit, although the northern half has been only weakly sampled. The recent "Adey/Steneck biogeographic model" for the subtidal has shown the northern half of this coast as a core Subarctic Region, while the southern half is mixed Boreal/Subarctic (the North Atlantic Boreal being centered in the British Isles). In this study, quantitative sampling, and statistical and graphic analyses of the dominant intertidal biota shows the two areas to be quite different based on species biomass or number of individuals/m(2). Ascophyllum nodosum, highly dominant in the southern part of the area becomes an occasional in the north, with Fucus vesiculosus in part replacing it, while Fucus distichus, a minor species in the south, becomes a dominating element on the northern rocky shores. The ubiquitous, intertidal, understory of the bushy-red alga Chondrus crispus and its associated algae in the Gulf of Maine and Nova Scotia, virtually disappears in the northern half of the region, being replaced by the large, filiform, brown alga Chordaria flagelliformis and its complex of ecologically-associated species. The characteristic, intertidal mollusc fauna shows a parallel change, with the abundant Littorina littorea of the southern coast being replaced by L. saxatilis northwards. Those species dominating the intertidal coastal biota surrounding the Strait of Belle Isle (center of the Subarctic core) provide 85% of the number/area/biomass count, but are only 13% of that count in the Gulf of Maine. These results provide further support for the Adey/Steneck theoretical model and demonstrate the necessity for using quantitative area/biomass data, as opposed to only species presence/absence data, in biogeographic analyses. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA. RP Adey, WH (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, NHB-166,POB 37012, Washington, DC 20013 USA. EM adeyw@nmnh.si.edu NR 24 TC 23 Z9 25 U1 3 U2 17 PU ADAC-CRYPTOGAMIE PI PARIS PA 12 RUE DE BUFFON, 75005 PARIS, FRANCE SN 0181-1568 J9 CRYPTOGAMIE ALGOL JI Cryptogam. Algol. PD FEB PY 2005 VL 26 IS 1 BP 35 EP 66 PG 32 WC Plant Sciences; Marine & Freshwater Biology SC Plant Sciences; Marine & Freshwater Biology GA 908XF UT WOS:000227822800002 ER PT J AU Leon-Alvarez, D Norris, JN AF Leon-Alvarez, D Norris, JN TI Terminology and position of reproductive structures in crustose brown algae: Misapplication, confusion and clarification SO CRYPTOGAMIE ALGOLOGIE LA English DT Article DE crustose algae; morphology; Phaeophyceae; Ralfsiaceae; reproductive structures; taxonomy ID PHAEOPHYCEAE; RALFSIACEAE AB The different meanings and applications of the terms used to describe important taxonomic characters and to distinguish some species, genera, and families of Phaeophyceae are discussed. The position of reproductive structures on the thallus of crustose brown algae is considered a critical character but has been misapplied or interpreted differently by some investigators. The meaning of the terms "lateral" and "terminal" sometimes varies as used by different authors, as does the usage of "paraphyses" and "stalks." For example, the position of the reproductive structure, lateral vs. terminal, and its relative position to the paraphyses, reproductive or vegetative filaments, and stalks have often not been clearly stated or defined. We propose restricted meanings and specific definitions for these terms in order to standardize their usage in algal systematics, and to simplify their use in comparative tables, numerical taxonomy, and morphological and phylogenetic analyses, etc.... C1 Univ Nacl Autonoma Mexico, Herbario Fac Ciencias, Secc Algas, Mexico City 04510, DF, Mexico. Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA. RP Leon-Alvarez, D (reprint author), Univ Nacl Autonoma Mexico, Herbario Fac Ciencias, Secc Algas, AP 70-592, Mexico City 04510, DF, Mexico. EM dla@hp.fciencias.unam.mx NR 30 TC 4 Z9 4 U1 0 U2 2 PU ADAC-CRYPTOGAMIE PI PARIS PA 12 RUE DE BUFFON, 75005 PARIS, FRANCE SN 0181-1568 J9 CRYPTOGAMIE ALGOL JI Cryptogam. Algol. PD FEB PY 2005 VL 26 IS 1 BP 91 EP 102 PG 12 WC Plant Sciences; Marine & Freshwater Biology SC Plant Sciences; Marine & Freshwater Biology GA 908XF UT WOS:000227822800005 ER PT J AU King, RS Baker, ME Whigham, DF Weller, DE Jordan, TE Kazyak, PF Hurd, MK AF King, RS Baker, ME Whigham, DF Weller, DE Jordan, TE Kazyak, PF Hurd, MK TI Spatial considerations for linking watershed land cover to ecological indicators in streams SO ECOLOGICAL APPLICATIONS LA English DT Article DE agriculture; bioassessment; distance weighting; ecological thresholds; land-cover collinearity; land use; macroinvertebrates; nitrate-nitrogen; nutrients; spatial autocorrelation; urbanization; water quality ID DIGITAL ELEVATION DATA; CHESAPEAKE BAY; NUTRIENT DISCHARGES; LANDSCAPE METRICS; BIOTIC INTEGRITY; MANTEL TEST; QUALITY; MODELS; SCALE; AUTOCORRELATION AB Watershed land cover is widely used as a predictor of stream-ecosystem condition. However, numerous spatial factors can confound the interpretation of correlative analyses between land cover and stream indicators, particularly at broad spatial scales. We used a stream-monitoring data set collected from the Coastal Plain of Maryland, USA to address analytical challenges presented by (1) collinearity of land-cover class percentages, (2) spatial autocorrelation of land cover and stream data, (3) intercorrelations among and spatial autocorrelation within abiotic intermediaries that link land cover to stream biota, and (4) spatial arrangement of land cover within watersheds. We focused on two commonly measured stream indicators, nitrate-nitrogen (NO3-N) and macroinvertebrate assemblages, to evaluate how different spatial considerations may influence results. Partial correlation analysis of land-cover percentages revealed that simple correlations described relationships that could not be separated from the effects of other land-cover classes or relationships that changed substantially when the influences of other land-cover classes were taken into account. Partial Mantel tests showed that all land-cover percentages were spatially autocorrelated, and this spatial phenomenon accounted for much of the variation in macroinvertebrate assemblages that could naively be attributed to certain classes (e.g., percentage cropland). We extended our use of partial Mantel tests into a path-analytical framework and identified several independent pathways between percentage developed land and instream measurements after factoring out spatial autocorrelation and other confounding variables; however, under these conditions, percentage cropland was only linked to nitrate-N. Further analyses revealed that spatial arrangement of land cover, as measured by areal buffers and distance weighting, influenced the amount of developed land, resulting in a threshold change in macroinvertebrate-assemblage composition. Moreover, distance-weighted percentage cropland improved predictions of stream nitrate-N concentrations in small watersheds, but not in medium or large ones. Collectively, this series of analyses clarified the magnitude and critical scales of effects of different land-cover classes on Coastal Plain stream ecosystems and may serve as an analytical framework for other studies. Our results suggest that greater emphasis should be placed on these important spatial considerations; otherwise, we risk obscuring the relationships between watershed land cover and the condition of stream ecosystems. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Maryland Dept Nat Resources, Monitoring & Nontidal Assessment Div, Annapolis, MD 21401 USA. RP King, RS (reprint author), Baylor Univ, Dept Biol, Ctr Reservior & Aquat Syst Res, 1 Bear Pl 97388, Waco, TX 76798 USA. EM Ryan_S_King@baylor.edu RI Baker, Matthew/I-2839-2014; OI Baker, Matthew/0000-0001-5069-0204; Weller, Donald/0000-0002-7629-5437; Whigham, Dennis/0000-0003-1488-820X NR 72 TC 244 Z9 267 U1 18 U2 146 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1707 H ST NW, STE 400, WASHINGTON, DC 20006-3915 USA SN 1051-0761 J9 ECOL APPL JI Ecol. Appl. PD FEB PY 2005 VL 15 IS 1 BP 137 EP 153 DI 10.1890/04-0481 PG 17 WC Ecology; Environmental Sciences SC Environmental Sciences & Ecology GA 899BU UT WOS:000227120700012 ER PT J AU Asquith, NM Mejia-Chang, M AF Asquith, NM Mejia-Chang, M TI Mammals, edge effects, and the loss of tropical forest diversity SO ECOLOGY LA English DT Article DE agouti; Burro Colorado Island, Panama; Dasyprocta spp.; edge effects; irrigation experiments; island biogeography; Proechimys semispinosus; Protium panamense; seed dispersal; seedling herbivory; spiny rat; tropical forest diversity ID PROECHIMYS-SEMISPINOSUS; TREE DIVERSITY; SPINY RATS; DIPTERYX-PANAMENSIS; NEOTROPICAL FORESTS; GUSTAVIA-SUPERBA; SEED DISPERSAL; RAIN-FORESTS; PANAMA; RECRUITMENT AB Relative to the surrounding mainland forests, a subset of tree species dominates wind-exposed, forested islands in Gatun Lake, Panama. We explored how tree diversity in these fragments has been affected by (1) impoverishment of the mammal community and (2) changes in abiotic conditions following island formation ca. 90 years ago. To test effects of changes in the mammal community, we assessed seed and seedling survival for nine tree species in five forests: small islands with no mammals; small islands with spiny rats but no larger mammals; medium islands (intermediate mammal community); Barro Colorado Island (intermittently present puma and jaguar); and mainland forests (intact mammal community). To test effects of abiotic stress, we chose experimental sites at wind-exposed, wind-protected, and interior forest sites. We predicted that fragments with less diverse mammal communities would be characterized by (1) fewer seeds dispersed and cached, (2) lower long-term seed survival, and (3) higher rates of seedling herbivory by mammals. Where alteration of the environment has caused greater exposure to dry-season winds, we predicted that (4) germination and seedling establishment and (5) dry-season seedling survival would be low. Further, we expected that (6) dry-season seedling survival would increase if soil moisture levels were raised, but that (7) wet-season seedling survival is independent of wind exposure. In the larger forests, seed and seedling survival were low, and differences in mammal community composition had little effect. Small islands that supported only rats had the same low seed survival as larger forests. Elimination of all mammals resulted in much higher seed survival, and slightly higher seedling survival. Germination and seedling survival were lower at wind-exposed than at protected sites, but irrigation had no effect on dry-season seedling survival. It appears that the dominant species on Gatun Lake fragments have passed through a series of filters: seeds must first avoid being eaten by spiny rats, survive the first dry season, and then avoid seedling herbivory by rats. Biotic and abiotic factors determine seedling survival in tropical forests; synergistic changes in these factors can thus lead to dramatic losses of diversity. C1 Duke Univ, Dept Zool, Durham, NC 27708 USA. Smithsonian Trop Res Inst, Balboa, Panama. RP Asquith, NM (reprint author), Conservat Int, Reg Conservat Strateg Grp, 1919 M St NW, Washington, DC 20036 USA. EM nigelasquith@yahoo.com NR 40 TC 32 Z9 34 U1 5 U2 39 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1707 H ST NW, STE 400, WASHINGTON, DC 20006-3915 USA SN 0012-9658 J9 ECOLOGY JI Ecology PD FEB PY 2005 VL 86 IS 2 BP 379 EP 390 DI 10.1890/03-0575 PG 12 WC Ecology SC Environmental Sciences & Ecology GA 906IM UT WOS:000227634400015 ER PT J AU Hubbell, SP AF Hubbell, SP TI Neutral theory in community ecology and the hypothesis of functional equivalence SO FUNCTIONAL ECOLOGY LA English DT Editorial Material ID RELATIVE SPECIES ABUNDANCE; RECRUITMENT LIMITATION; DEPENDENT RECRUITMENT; NEOTROPICAL FOREST; PLANT-COMMUNITIES; TROPICAL TREES; COEXISTENCE; COMPETITION; DIVERSITY; CONSEQUENCES C1 Univ Georgia, Dept Plant Biol, Athens, GA 30605 USA. Smithsonian Trop Res Inst, Balboa, Panama. RP Univ Georgia, Dept Plant Biol, Athens, GA 30605 USA. EM shubbell@plantbio.uga.edu NR 55 TC 288 Z9 323 U1 24 U2 209 PU WILEY PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0269-8463 EI 1365-2435 J9 FUNCT ECOL JI Funct. Ecol. PD FEB PY 2005 VL 19 IS 1 BP 166 EP 172 DI 10.1111/j.0269-8463.2005.00965.x PG 7 WC Ecology SC Environmental Sciences & Ecology GA 906VJ UT WOS:000227672000022 ER PT J AU Harlow, GE Sorensen, SS AF Harlow, GE Sorensen, SS TI Jade (Nephrite and Jadeitite) and Serpentinite: Metasomatic connections SO INTERNATIONAL GEOLOGY REVIEW LA English DT Review ID MOTAGUA FAULT ZONE; ITOIGAWA-OHMI-DISTRICT; SUBDUCTION-ZONE; NORTHWESTERN MYANMAR; NIIGATA PREFECTURE; METAMORPHIC ROCKS; CATALINA SCHIST; STABLE ISOTOPE; SOLID-SOLUTION; OCEANIC-CRUST AB The lapidary term "jade" refers to two very tough, virtually monomineralic rocks used for ornamental carvings or gems. Both have metasomatic origins that are intimately connected with their host serpentinite bodies and convergent-margin petrotectonics. Amphibole jade is nephrite, a tremolite-actinolite rock with a felted, microcrystalline habit; pyroxene jade is jadeite rock (Jadeitite), which varies from micro- to macrocrystalline textures. Most nephrite occurs along fault contacts between serpentinite and mafic to felsic igneous rocks or metagraywacke in obduction settings. It forms by Ca- and Si-rich, aqueous fluid-mediated metasomatic replacement of serpentinite, typically antigorite, at greenschist-facies or lower P-T conditions. Other nephrite bodies reflect contact metasomatic replacement of dolomite by Si-rich aqueous fluids during felsic pluton emplacement. Like most nephrite, jadeitite is hosted by antigorite-dominated serpentinite bodies. However, these serpentinites are associated with HP/LT metamorphic terranes, in which jadeitite occurs as isolated tabular bodies or tectonized blocks. Based on textural evidence, particularly clear from cathodoluminescence studies, nearly all jadeitite bodies appear to have formed originally as vein crystallization of an aqueous fluid, most readily interpreted as Na-Al-Si-rich fluid at HP/LT conditions in subduction/collisional settings. The host serpentinite influences jadeitite compositions by lowering fluid a(SiO2) during serpentinization, and contributing Ca + Mg +/- Cr to late-stage jadeitite-forming fluids. Thus, although both types of jade form in convergent-margin tectonic settings, jade has two distinct primary modes of origin: (1) by siliceous replacement of already serpentinized ultramafic rock at low-P, low- to moderate-T conditions following obduction (nephrite); or (2) by the interaction of serpentinizing peridotite and Na-Al-Si fluids at HP/LT conditions during active subduction/collision (jadeitite). C1 Amer Museum Nat Hist, Dept Earth & Planetary Sci, New York, NY 10024 USA. NMNH, Smithsonian Inst, Dept Mineral Sci, Washington, DC 20013 USA. RP Harlow, GE (reprint author), Amer Museum Nat Hist, Dept Earth & Planetary Sci, 79th & Cent Pk W, New York, NY 10024 USA. EM gharlow@amnh.org NR 140 TC 79 Z9 91 U1 0 U2 33 PU V H WINSTON & SON INC PI PALM BEACH PA 360 SOUTH OCEAN BLVD, PH-B, PALM BEACH, FL 33480 USA SN 0020-6814 J9 INT GEOL REV JI Int. Geol. Rev. PD FEB PY 2005 VL 47 IS 2 BP 113 EP 146 DI 10.2747/0020-6814.47.2.113 PG 34 WC Geology SC Geology GA 895EX UT WOS:000226844800001 ER PT J AU Cruz-Angon, A Greenberg, R AF Cruz-Angon, A Greenberg, R TI Are epiphytes important for birds in coffee plantations? An experimental assessment SO JOURNAL OF APPLIED ECOLOGY LA English DT Article DE biodiversity; birds; community structure; shade coffee management; vascular epiphytes ID SHADE COFFEE; FORAGING BEHAVIOR; SPECIES RICHNESS; MIGRATORY BIRDS; CLOUD FOREST; GREAT TITS; MEXICO; FRAGMENTATION; POPULATIONS; FRUGIVORY AB 1. Coffee is produced in tropical regions of the world, largely in Latin America. Coffee cultivation techniques range from traditional systems, where coffee grows under a diverse canopy of shade trees (shade-coffee plantations), to modern systems, where coffee grows without any type of shade (sun-coffee plantations). Shade-coffee plantations provide refuge for forest fauna in otherwise deforested landscapes. The conservation value of these agro-ecosystems depends upon their structural and floristic diversity. 2. The way coffee producers manage the vegetation, including the epiphytic component, may profoundly affect the value of plantations for conserving biological diversity. Shade-coffee certification programmes have emerged to verify that coffee advertised as 'shade grown' is actually grown on highly biodiverse plantations. Although these programmes universally encourage epiphyte protection from pruning (a common practice), there has been no experimental evaluation of the importance of epiphytes in supporting faunal diversity. We report the effect of experimentally removing epiphytes on the bird assemblage in a shade-coffee farm near Coatepec, Veracruz, Mexico. 3. We established two matching pairs of epiphyte removal and control plots. We compared bird diversity and abundance, based on daily censuses during the breeding and non-breeding season. We used existing information on the way in which birds use epiphytes as foraging and nesting substrates to explain the presence of different species in plots with epiphytes. 4. Plots without epiphytes tended to be less diverse than plots with epiphytes, but rarefaction analysis and ANOVA showed no significant differences in species richness between treatments in any of the seasons. Mean bird abundance was significantly higher in plots with epiphytes during both seasons, and a multidimensional scaling analysis showed that bird community structure differed between the two treatments. 5. Eighteen forest bird species were significantly more abundant in plots with epiphytes. Three non-forest species were more common in plots without epiphytes. Resident bird species that used epiphytes as a nesting substrate were significantly more abundant in plots with epiphytes. 6. When epiphytes are removed, canopy cover, foraging substrates, nest sites and nest materials are eliminated and microclimatic conditions change. This could increase predation on adult birds and nests, increase intra- and interspecific competition, and decrease individual survivorship. 7. Synthesis and applications. This is the first experimental assessment of the importance of epiphytes for birds. Shade-coffee plantations with epiphytes maintain higher abundance and diversity of the inhabitant bird fauna than plantations without epiphytes. This study reinforces the value of positive epiphyte management as an important factor in shade-grown coffee certification, where the goal is to promote biodiversity conservation. C1 Inst Ecol, AC Dept Ecol Func, Xalapa 91070, Veracruz, Mexico. Natl Zool Pk, Smithsonian Migratory Bird Ctr, Washington, DC 20008 USA. RP Inst Ecol, AC Dept Ecol Func, Km 2-5 Antigua Carretera Coatepec,315, Xalapa 91070, Veracruz, Mexico. EM angon@ecologia.edu.mx NR 65 TC 57 Z9 61 U1 2 U2 42 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0021-8901 EI 1365-2664 J9 J APPL ECOL JI J. Appl. Ecol. PD FEB PY 2005 VL 42 IS 1 BP 150 EP 159 DI 10.1111/j.1365-2664.2004.00983.x PG 10 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 899VZ UT WOS:000227175200016 ER PT J AU Mora, C Robertson, DR AF Mora, C Robertson, DR TI Factors shaping the range-size frequency distribution of the endemic fish fauna of the Tropical Eastern Pacific SO JOURNAL OF BIOGEOGRAPHY LA English DT Article DE dispersal; geography; habitat fragmentation; habitat usage; isolation; range-size frequency distribution; shorefishes; Tropical Eastern Pacific ID CORAL-REEFS; BIODIVERSITY HOTSPOTS; GEOGRAPHIC RANGE; SPECIES RICHNESS; CONSERVATION; PATTERNS; RECRUITMENT; POPULATIONS; MECHANISMS; DIVERSITY AB Aim To assess the effect of habitat fragmentation and isolation in determining the range-size frequency distribution (RFD) of the shorefish fauna endemic to a discrete biogeographical region. Location The Tropical Eastern Pacific (TEP). Methods Habitat isolation represents the separation between oceanic islands and the continental shore of the TEP and habitat fragmentation the degree of spatial continuity of habitats (i.e. reefs, soft bottom, nearshore waters) along the continental coast of the TEP. The effects of habitat isolation and fragmentation were quantified by comparing the RFDs of (1) the species found on oceanic islands vs. the continental shore, and (2) species on the continental shore that use different habitat types. Results The RFD of the entire TEP fauna was bimodal, with peaks at both small- and large-range ends of the spectrum. The small-range peak was due almost entirely to island species and the large-range peak due mainly to species found in both the continental shore and oceanic islands. RFDs varied among species using different habitats on the continental shore: reef-fishes had a right-skewed RFD, soft-bottom species a flat RFD, and coastal-pelagic fishes a left-skewed RFD. Main conclusions Variation in dispersal capabilities associated with habitat isolation and fragmentation in the TEP appears to be the main mechanism contributing to differences among RFD structure, although variation in tolerances arising from the dynamic regional environment may contribute to some patterns. Because diversity patterns are strongly affected by RFD structure, it is now evident that the insular and continental components of a fauna should be treated separately when analysing such patterns. Furthermore, contrasts in RFD structure among species using different habitats demonstrate that a full understanding of the causes of diversity patterns requires analyses of complete regional faunas in relation to regional geography. C1 Univ Windsor, Dept Biol, Windsor, ON N9B 3P4, Canada. Smithsonian Trop Res Inst, Balboa, Panama. RP Mora, C (reprint author), Univ Windsor, Dept Biol, 401 Sunset, Windsor, ON N9B 3P4, Canada. EM moracamilo@hotmail.com NR 49 TC 26 Z9 27 U1 0 U2 17 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0305-0270 J9 J BIOGEOGR JI J. Biogeogr. PD FEB PY 2005 VL 32 IS 2 BP 277 EP 286 DI 10.1111/j.1365-2699.2004.01155.x PG 10 WC Ecology; Geography, Physical SC Environmental Sciences & Ecology; Physical Geography GA 889WA UT WOS:000226472300009 ER PT J AU Hall, MC Stiling, P Moon, DC Drake, BG Hunter, MD AF Hall, MC Stiling, P Moon, DC Drake, BG Hunter, MD TI Effects of elevated CO2 on foliar quality and herbivore damage in a scrub oak ecosystem SO JOURNAL OF CHEMICAL ECOLOGY LA English DT Article DE elevated CO2; Quercus myrtifolia; Quercus chapmanii; Quercus geminata; Galactia elliottii; herbivory; nitrogen fixer; Kennedy Space Center ID CARBON-DIOXIDE ATMOSPHERES; INSECT HERBIVORE; PLANT-RESPONSES; DECIDUOUS TREES; JUNONIA-COENIA; LEAF QUALITY; GROWTH; FOREST; AVAILABILITY; LEPIDOPTERA AB Atmospheric CO2 concentrations have increased exponentially over the last century and continuing increases are expected to have significant effects on ecosystems. We investigated the interactions among atmospheric CO2, foliar quality, and herbivory within a scrub oak community at the Kennedy Space Center, Florida. Sixteen plots of open-top chambers were followed; eight of which were exposed to ambient levels of CO2 (350 ppm), and eight of which were exposed to elevated levels of CO2 (700 ppm). We focused on three oak species, Quercus geminata, Quercus myrtifolia, Quercus chapmanii, and one nitrogen fixing legume, Galactia elliottii. There were declines in overall nitrogen and increases in C:N ratios under elevated CO2. Total carbon, phenolics (condensed tannins, hydrolyzable tannins, total phenolics) and fiber (cellulose, hemicellulose, lignin) did not change under elevated CO2 across plant species. Plant species differed in their relative foliar chemistries over time, however, the only consistent differences were higher nitrogen concentrations and lower C: N ratios in the nitrogen fixer when compared to the oak species. Under elevated CO2, damage by herbivores decreased for four of the six insect groups investigated. The overall declines in both foliar quality and herbivory under elevated CO2 treatments suggest that damage to plants may decline as atmospheric CO2 levels continue to rise. C1 Univ Georgia, Inst Ecol, Athens, GA 30602 USA. Univ S Florida, Dept Biol, Tampa, FL 33620 USA. Univ N Florida, Dept Biol, Jacksonville, FL 32224 USA. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Hall, MC (reprint author), Univ Georgia, Inst Ecol, Athens, GA 30602 USA. EM mchall@uga.edu NR 65 TC 24 Z9 27 U1 1 U2 17 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0098-0331 J9 J CHEM ECOL JI J. Chem. Ecol. PD FEB PY 2005 VL 31 IS 2 BP 267 EP 286 DI 10.1007/s10886-005-1340-2 PG 20 WC Biochemistry & Molecular Biology; Ecology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology GA 903SA UT WOS:000227444700004 PM 15856783 ER PT J AU Schotte, M AF Schotte, M TI Brian Frederick Kensley - 17 April 1944-19 January 2004 SO JOURNAL OF CRUSTACEAN BIOLOGY LA English DT Biographical-Item C1 Smithsonian Inst, Dept Invertebrate Zool, Washington, DC 20013 USA. RP Schotte, M (reprint author), Smithsonian Inst, Dept Invertebrate Zool, Washington, DC 20013 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU CRUSTACEAN SOC PI SAN ANTONIO PA 840 EAST MULBERRY, SAN ANTONIO, TX 78212 USA SN 0278-0372 J9 J CRUSTACEAN BIOL JI J. Crustac. Biol. PD FEB PY 2005 VL 25 IS 1 BP 165 EP 174 DI 10.1651/0278-0372(2005)025[0165:BFKAJ]2.0.CO;2 PG 10 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 903AR UT WOS:000227398300019 ER PT J AU Yoshino, K Parkinson, WH Ito, K Matsui, T AF Yoshino, K Parkinson, WH Ito, K Matsui, T TI Absolute absorption cross-section measurements of Schumann-Runge continuum of O-2 at 90 and 295 K SO JOURNAL OF MOLECULAR SPECTROSCOPY LA English DT Article DE oxygen; continuum; cross-section ID MOLECULAR-OXYGEN; TEMPERATURE-DEPENDENCE; REGION; PHOTOABSORPTION; BANDS; NM AB Laboratory measurements of the absorption cross-section of the Schumann-Runge continuum of O-2 at the temperatures 90 and 295 K have been made in the wavelength region 130-175 urn. The absolute absorption cross-sections at the same temperatures have been measured at several discrete wavelengths through the region. The absolute cross-sections of the O-2 continuum have been used to put relative cross-sections on a firm absolute basis throughout the region 130-175 nm. These recalibrated cross-sections are available as numerical compilations. (C) 2004 Elsevier Inc. All rights reserved. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. KEK, Photon Factory, Tsukuba, Ibaraki 305, Japan. RP Yoshino, K (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM kyoshino@cfa.harvard.edu NR 18 TC 36 Z9 36 U1 0 U2 5 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0022-2852 J9 J MOL SPECTROSC JI J. Mol. Spectrosc. PD FEB PY 2005 VL 229 IS 2 BP 238 EP 243 DI 10.1016/j.jms.2004.08.020 PG 6 WC Physics, Atomic, Molecular & Chemical; Spectroscopy SC Physics; Spectroscopy GA 887FV UT WOS:000226291900011 ER PT J AU Pecio, A Burns, JR Weitzman, SH AF Pecio, A Burns, JR Weitzman, SH TI Sperm and spermatozeugma ultrastructure in the inseminating species Tyttocharax cochui, T-tambopatensis, and Scopaeocharax rhinodus (Pisces : Teleostei : Characidae : Glandulocaudinae : Xenurobryconini) SO JOURNAL OF MORPHOLOGY LA English DT Article DE insemination; internal fertilization; spermatozeugmata; sperm ultrastructure; Tyttocharax; Scopaeocharax ID MIMAGONIATES-BARBERI TELEOSTEI; FINE-STRUCTURE; FISHES TELEOSTEI; TESTIS; CHARACIFORMES; CELLS; SPERMIOGENESIS; MORPHOLOGY; MOTILITY AB This article presents the scanning and transmission electron microscopy of the spermatozoa and sperm packets of three inseminating species of the glandulocaudine tribe Xenurobryconini. All three species, Scopaeocharax rhinodus, Tyttocharax cochui, and T. tambopatensis produce unencapsulated sperm packets (= spermatozeugmata) of similar morphology. The external anterior surface of each spermatozeugma is comprised of elongate sperm heads arranged in parallel, and the posterior part is made up of tightly packed flagella. The interior of the anterior portion consists of alternating layers of sperm heads and flagella. The remarkable integrity of each packet appears to be maintained through an electron-dense secretion seen among all parts of the cells. Spermatozeugma formation takes place within the spermatocysts at the end of spermiogenesis and at spermiation fully formed packets are released. Morphology of the mature spermatozoa was similar in all three species. Each nucleus is elongate, flattened along most of its length, and tapers at either end. The two centrioles are nearly parallel to one another and are located just anterior to the nucleus. Elongate mitochondria are located along the nucleus. The single flagellum, which lacks axonemal fins, is initially contained within a short cytoplasmic collar. Accessory microtubules run parallel to the long axis of the nucleus just beneath the plasma membrane. During spermiogenesis, no nuclear rotation occurs and the cytoplasmic canal containing the flagellum elongates along with the nucleus. However, prior to spermiation all but the anterior portion of the collar degenerates. The sperm modifications observed in these species are discussed as adaptations to the unique reproductive habit of insemination. (C) 2004 Wiley-Liss, Inc. C1 George Washington Univ, Dept Sci Biol, Washington, DC 20052 USA. Jagiellonian Univ, Inst Zool, Dept Comparat Med, Krakow, Poland. Smithsonian Inst, Museum Natl Hist Nat, Dept Zool, Washington, DC 20560 USA. RP Burns, JR (reprint author), George Washington Univ, Dept Sci Biol, 2023 G St NW, Washington, DC 20052 USA. EM jrburns@gwu.edu NR 39 TC 17 Z9 18 U1 0 U2 1 PU WILEY-LISS PI HOBOKEN PA DIV JOHN WILEY & SONS INC, 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 0362-2525 J9 J MORPHOL JI J. Morphol. PD FEB PY 2005 VL 263 IS 2 BP 216 EP 226 DI 10.1002/jmor.10299 PG 11 WC Anatomy & Morphology SC Anatomy & Morphology GA 889OG UT WOS:000226451700005 PM 15593307 ER PT J AU Hussein, AA Barberena, I Correa, M Coley, PD Solis, PN Gupta, MP AF Hussein, AA Barberena, I Correa, M Coley, PD Solis, PN Gupta, MP TI Cytotoxic flavonol glycosides from Triplaris cumingiana SO JOURNAL OF NATURAL PRODUCTS LA English DT Article AB Three new compounds, 2-(3,4-dihydroxyphenyl)-5,7-dihydroxy-4-oxo-4H-chromen-3-yl-4,6-bis-O-beta-D-(3,4,5-trihydroxybenzoyl)glucopyranoside (1), 5,7-dihydroxy-2-(4-hydroxyphenyl)-4-oxo-4H-chromen-3-yl-5-O-alpha-L-(3,4,5-trihydroxybenzoyl)arabinofuranoside (2), and 2-hydroxy-4-O-alpha-L-(3,5,7-trihydroxy-4-oxo-4H-chromen-2-yl)phenylarabinofuranoside (3), were isolated from the young leaves of Triplaris cumingiana, together with two known compounds, quercetin 3-O-alpha-L-(5"-O-galloyl)arabinofuranoside (4) and quercetin 3-O-beta-D-(6"-O-galloyl)glucopyranoside (5). The structures of 1-3 were established by spectroscopic methods. Compounds 1-5 were evaluated for their cytotoxic activities against the MCF-7, H-460, and SF-268 human cancer cell lines. C1 Univ Panama, Fac Farm, CIFLORPAN, Panama City, Panama. Smithsonian Trop Res Inst, Panama City, Panama. Univ Utah, Dept Biol, Salt Lake City, UT 84112 USA. RP Gupta, MP (reprint author), Univ Panama, Fac Farm, CIFLORPAN, Apartado 10767,Estafeta Univ, Panama City, Panama. EM cytedqff@ancon.up.ac.pa OI Gupta, Mahabir/0000-0002-9302-7864; Hussein, Ahmed/0000-0002-3877-9959 FU FIC NIH HHS [1U01 TW 01021-01] NR 11 TC 11 Z9 11 U1 2 U2 5 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0163-3864 J9 J NAT PROD JI J. Nat. Prod. PD FEB PY 2005 VL 68 IS 2 BP 231 EP 233 DI 10.1021/np049803g PG 3 WC Plant Sciences; Chemistry, Medicinal; Pharmacology & Pharmacy SC Plant Sciences; Pharmacology & Pharmacy GA 901VF UT WOS:000227309500015 PM 15730249 ER PT J AU Kooistra, WHCF Verbruggen, H AF Kooistra, WHCF Verbruggen, H TI Genetic patterns in the calcified tropical seaweeds Halimeda opuntia, H-distorta, H-hederacea, and H-minima (Bryopsidales, Chlorophyta) provide insights in species boundaries and interoceanic dispersal SO JOURNAL OF PHYCOLOGY LA English DT Article DE calcareous algae; cryptic species; cognate; dispersal; Halimeda; H. distorta; H. hederacea; H. opuntia; introduced species; ITS; morphology; phylogeny; phylogeography; SSU rDNA; taxonomy ID GREEN-ALGAE; CORAL-REEFS; EVOLUTION; REPRODUCTION; CAULERPALES; SPECIATION; LINEAGES; PACIFIC; ECOLOGY; DNA AB The section Opuntia within the green seaweed genus Halimeda includes sprawling and pendant thalli composed of strongly calcified segments. Within this section, identification of Atlantic material is straightforward, but Indo-Pacific material is often difficult to key out. This is particularly true for specimens resembling H. opuntia, H. distorta, and H. hederacea; many specimens do not fit any type or are morphologically intermediate. The goals of the present study are to define morphologically and genetically distinct groups among such specimens and to assess phylogeographic patterns within these groups. Specimens were collected throughout the geographical and morphological range. Sequences of H. minima and H. gracilis were included as outgroups. Two morphological groups were discerned within the ingroup; the first fit H. opuntia, whereas most specimens in the second group, referred to as the distorta-hederacea complex, did not fit any species description unambiguously. The latter were subdivided into two subgroups corresponding more or less to H. hederacea and H. distorta, yet intermediates between these morphs existed. A phylogeny inferred from partial nuclear rDNA sequences showed one lineage with H. opuntia and a second one containing the distorta-hederacea complex, thus corroborating the two major morphological groups. The distorta-hederacea complex contained two clades that show only partial correspondence with the morphological subgroups. Therefore, H. hederacea is synonymized with H. distorta. Phylogeographic structure within H. opuntia indicated that this species dispersed from the Indo-Pacific into the Atlantic. Fossil records of the species also show occurrence at Pacific sites throughout the last 10(5) years and a sudden appearance in the Caribbean and Bahamas during the last millennium. C1 State Univ Ghent, Phycol Res Grp, B-9000 Ghent, Belgium. Smithsonian Trop Res Inst, Balboa, Panama. RP Verbruggen, H (reprint author), State Univ Ghent, Phycol Res Grp, B-9000 Ghent, Belgium. EM heroen.verbruggen@ugent.be RI Verbruggen, Heroen/C-6951-2009; OI Verbruggen, Heroen/0000-0002-6305-4749; Kooistra, Wiebe/0000-0002-8641-9739 NR 48 TC 20 Z9 24 U1 0 U2 6 PU BLACKWELL PUBLISHING INC PI MALDEN PA 350 MAIN ST, MALDEN, MA 02148 USA SN 0022-3646 J9 J PHYCOL JI J. Phycol. PD FEB PY 2005 VL 41 IS 1 BP 177 EP 187 DI 10.1111/j.1529-8817.2005.04095.x PG 11 WC Plant Sciences; Marine & Freshwater Biology SC Plant Sciences; Marine & Freshwater Biology GA 894KT UT WOS:000226791300017 ER PT J AU Chaparro, OR Saldivia, CL Pereda, SV Segura, CJ Montiel, YA Collin, R AF Chaparro, OR Saldivia, CL Pereda, SV Segura, CJ Montiel, YA Collin, R TI The reproductive cycle and development of Crepipatella fecunda (Gastropoda : Calyptraeidae) from southern Chile SO JOURNAL OF THE MARINE BIOLOGICAL ASSOCIATION OF THE UNITED KINGDOM LA English DT Article ID CREPIDULA-CONVEXA SAY; SEX-CHANGE; PROSOBRANCHIA; CAPACITY; PATTERNS; GALLARDO; MODES AB Crepipatella fecunda is a benthic, primarily suspension-feeding gastropod that occurs in great abundance along the Chilean coast. It is a protandrous species whose reproduction involves brooding of an encapsulated embryonic stage followed by the release of free-living planktotrophic larvae. Because its close sister species, C. dilatala, co-occurs with C. fecunda, understanding the details of reproduction in this species might shed light on differences in reproductive features that correlate with divergences in mode of development. In southern Chile, brooding occurs throughout the year except for May and June, and each female produces 3-7 broods. The smallest brooding female was 28.2 mm in shell length and the largest was 56.3 mm. All full-grown eggs from the ovary are deposited at one time In a single brood, and only smaller oocytes remain in the gonad after the female finishes ovopositing. Those females that host pinnotherid crabs do not deposit eggs. All the eggs develop into embryos whose intracapsular development is similar to Crepidula fornicata and Crepipatella. lingulata. Planktotrophic larvae hatch at a mean shell length of 329.5 mu m (SD=27.09) after 4-5 weeks. During the pelagic stage the shell and velum of the larvae grow, but little other morphological development is visible externally. The pelagic stage lasts for 15-16 days at 17 degrees C, during which the larvae grow similar to 20.7 mu m d(-1). Observations of cultured larvae and protoconchs of field-collected juveniles show that settlement Occurs when the larvae reach a shell-length of 650 mu m (SD=28.3 mu m). C1 Univ Austral Chile, Inst Biol Marina, Valdivia 567, Chile. Smithsonian Trop Res Inst, Unit 0948, APO AA, Miami, FL 34002 USA. RP Chaparro, OR (reprint author), Univ Austral Chile, Inst Biol Marina, Valdivia 567, Chile. EM ochaparr@uach.cl RI Chaparro, Oscar/A-5070-2009; Collin, Rachel/G-2001-2010; Segura, Cristian/C-1306-2010 NR 20 TC 21 Z9 21 U1 1 U2 4 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 40 WEST 20TH ST, NEW YORK, NY 10011-4211 USA SN 0025-3154 J9 J MAR BIOL ASSOC UK JI J. Mar. Biol. Assoc. U.K. PD FEB PY 2005 VL 85 IS 1 BP 157 EP 161 DI 10.1017/S0025315405010982h PG 5 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 911OS UT WOS:000228014500021 ER PT J AU Phillips, DE Novikova, I Wang, CYT Walsworth, RL Crescimanno, M AF Phillips, DE Novikova, I Wang, CYT Walsworth, RL Crescimanno, M TI Modulation-induced frequency shifts in a coherent-population-trapping-based atomic clock SO JOURNAL OF THE OPTICAL SOCIETY OF AMERICA B-OPTICAL PHYSICS LA English DT Article ID RESONANCES; REFERENCES/; STANDARDS; VAPOR AB We investigate systematic errors associated with a common modulation technique used for phase-sensitive detection of a coherent-population-trapping (CPT) resonance. In particular, we show that modification of the CPT resonance line shape due to the presence of off-resonant fields leads to frequency shifts that may limit the stability of CPT-based atomic clocks. We also demonstrate that an alternative demodulation technique greatly reduces these effects. (C) 2005 Optical Society of America. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Youngstown State Univ, Dept Phys & Astron, Youngstown, OH 44555 USA. RP Phillips, DE (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM dphil@cfa.harvard.edu RI Novikova, Irina/B-9041-2008 NR 14 TC 12 Z9 14 U1 1 U2 5 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 0740-3224 J9 J OPT SOC AM B JI J. Opt. Soc. Am. B-Opt. Phys. PD FEB PY 2005 VL 22 IS 2 BP 305 EP 310 DI 10.1364/JOSAB.22.000305 PG 6 WC Optics SC Optics GA 896XM UT WOS:000226967800001 ER PT J AU Schroll, S AF Schroll, S TI Magnum stories. Phaidon. SO LIBRARY JOURNAL LA English DT Book Review C1 Smithsonian Inst Libs, Washington, DC USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION PI NEW YORK PA 249 W 17TH ST, NEW YORK, NY 10011 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD FEB 1 PY 2005 VL 130 IS 2 BP 76 EP + PG 2 WC Information Science & Library Science SC Information Science & Library Science GA 891WQ UT WOS:000226612100126 ER PT J AU Wang, RP Rosen, MS Candela, D Mair, RW Walsworth, RL AF Wang, RP Rosen, MS Candela, D Mair, RW Walsworth, RL TI Study of gas-fluidization dynamics with laser-polarized Xe-129 SO MAGNETIC RESONANCE IMAGING LA English DT Article; Proceedings Paper CT 7th International Conference on Magnetic Resonance in Porous Media (MRPM7) CY JUL 04-08, 2004 CL Palaiseau, FRANCE DE laser-polarized xenon; fluidization; granular media; T-2* contrast; gas dispersion ID DIFFUSION; EXCHANGE AB We report initial NMR studies of gas dynamics in a particle bed fluidized by laser-polarized xenon (Xe-129) gas. We have made preliminary measurements of two important characteristics: gas exchange between the bubble and emulsion phases and the gas velocity distribution in the bed. We used T-2* contrast to differentiate the bubble and emulsion phases by choosing solid particles with large magnetic susceptibility. Experimental tests demonstrated that this method was successful in eliminating Xe-129 magnetization in the emulsion phase, which enabled us to observe the time dependence of the bubble magnetization. By employing the pulsed field gradient method, we also measured the gas velocity distribution within the bed. These results clearly show the onset of bubbling and can be used to deduce information about gas and particle motion in the fluidized bed. (c) 2005 Elsevier Inc. All rights reserved. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. MIT, Dept Nucl Engn, Cambridge, MA 02139 USA. Univ Massachusetts, Dept Phys, Amherst, MA 01003 USA. RP Mair, RW (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM rmair@cfa.harvard.edu NR 20 TC 17 Z9 17 U1 0 U2 7 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0730-725X J9 MAGN RESON IMAGING JI Magn. Reson. Imaging PD FEB PY 2005 VL 23 IS 2 SI SI BP 203 EP 207 DI 10.1016/j.mri.2004.11.012 PG 5 WC Radiology, Nuclear Medicine & Medical Imaging SC Radiology, Nuclear Medicine & Medical Imaging GA 920AD UT WOS:000228658400013 PM 15833613 ER PT J AU Wang, RP Pavlin, T Rosen, MS Mair, RW Cory, DG Walsworth, RL AF Wang, RP Pavlin, T Rosen, MS Mair, RW Cory, DG Walsworth, RL TI Xenon NMR measurements of permeability and tortuosity in reservoir rocks SO MAGNETIC RESONANCE IMAGING LA English DT Article; Proceedings Paper CT 7th International Conference on Magnetic Resonance in Porous Media (MRPM7) CY JUL 04-08, 2004 CL Palaiseau, FRANCE DE gas flow; laser-polarized xenon; permeability; porous media flow; tortuosity ID POLARIZED NOBLE-GAS AB In this work we present measurements of permeability, effective porosity and tortuosity on a variety of rock samples using NMR/MRI of thermal and laser-polarized gas. Permeability and effective porosity are measured simultaneously using MRI to monitor the inflow of laser-polarized xenon into the rock core. Tortuosity is determined from measurements of the time-dependent diffusion coefficient using thermal xenon in sealed samples. The initial results from a limited number of rocks indicate inverse correlations between tortuosity and both effective porosity and permeability. Further studies to widen the number of types of rocks studied may eventually aid in explaining the poorly understood connection between permeability and tortuosity of rock cores. (c) 2005 Elsevier Inc. All rights reserved. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. MIT, Dept Nucl Engn, Cambridge, MA 02139 USA. RP Pavlin, T (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM tpavlin@cfa.harvard.edu NR 6 TC 22 Z9 23 U1 0 U2 4 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0730-725X J9 MAGN RESON IMAGING JI Magn. Reson. Imaging PD FEB PY 2005 VL 23 IS 2 SI SI BP 329 EP 331 DI 10.1016/j.mri.2004.11.044 PG 3 WC Radiology, Nuclear Medicine & Medical Imaging SC Radiology, Nuclear Medicine & Medical Imaging GA 920AD UT WOS:000228658400038 PM 15833638 ER PT J AU Duda, TF Kohn, AJ AF Duda, TF Kohn, AJ TI Species-level phylogeography and evolutionary history of the hyperdiverse marine gastropod genus Conus SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article DE biogoegrahy; molecular phylogeny; fossil record; evolutionary history; Conus ID TROPICAL EASTERN PACIFIC; DNA-SEQUENCE DATA; MITOCHONDRIAL-DNA; POPULATION-STRUCTURE; PANAMA; SUBSTITUTION; DIVERGENCE; PHYLOGENY; ISTHMUS; SEA AB Phylogenetic and paleontological analyses are combined to reveal patterns of species origination and divergence and to define the significance of potential and actual barriers to dispersal in Conus, a species-rich genus of predatory gastropods distributed throughout the world's tropical oceans. Species-level phylogenetic hypotheses are based on nucleotide sequences from the nuclear calmodulin and mitochondrial 16S rRNA genes of 138 Conus species from the Indo-Pacific, eastern Pacific, and Atlantic Ocean regions. Results indicate that extant species descend from two major lineages that diverged at least 33 mya. Their geographic distributions suggest that one clade originated in the Indo-Pacific and the other in the eastern Pacific + western Atlantic. Impediments to dispersal between the western Atlantic and Indian Oceans and the central and eastern Pacific Ocean may have promoted this early separation of Indo-Pacific and eastern Pacific + western Atlantic lineages of Conus. However, because both clades contain both Indo-Pacific and eastern Pacific + western Atlantic species, migrations must have occurred between these regions; at least four migration events took place between regions at different times. In at least three cases, incursions between regions appear to have crossed the East Pacific Barrier. The paleontological record illustrates that distinct sets of Conus species inhabited the Indo-Pacific, eastern Pacific + western Atlantic, and eastern Atlantic + former Tethys Realm in the Tertiary, as is the case today. The ranges of 1% of fossil species (N = 841) spanned more than one of these regions throughout the evolutionary history of this group. (C) 2004 Elsevier Inc. All rights reserved. C1 Smithsonian Trop Res Inst, Naos Marine Lab, Balboa, Ancon, Panama. Univ Washington, Dept Biol, Seattle, WA 98195 USA. RP Duda, TF (reprint author), Univ Michigan, Dept Ecol & Evolutionary Biol, 1109 Geddes Ave, Ann Arbor, MI 48103 USA. EM tfduda@umich.edu NR 62 TC 100 Z9 100 U1 1 U2 10 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 1055-7903 J9 MOL PHYLOGENET EVOL JI Mol. Phylogenet. Evol. PD FEB PY 2005 VL 34 IS 2 BP 257 EP 272 DI 10.1016/j.ympev.2004.09.012 PG 16 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 886UQ UT WOS:000226258600002 PM 15619440 ER PT J AU Liu, HP Hershler, R AF Liu, HP Hershler, R TI Molecular systematics and radiation of western North American nymphophiline gastropods SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article DE gastropods; Hydrobiidae; Pyrgulopsis; western North America; molecular systematics; mtDNA ID MITOCHONDRIAL-DNA SEQUENCES; FRESH-WATER SNAIL; GENUS PYRGULOPSIS; PHYLOGENETIC-RELATIONSHIPS; HYDROBIIDAE GASTROPODA; AQUATIC GASTROPODS; RAPID RADIATION; RIVER-BASIN; RISSOOIDEA; CALIFORNIA AB Three mitochondrial DNA (mtDNA) markers were used to infer the phylogenetic relationships of the morphologically diverse, species rich, and poorly understood western North American aquatic gastropod genus Pyrgulopsis (Hydrobiidae: Nymphophilinae). Sequences were obtained from 62 of 124 currently recognized species of Pyrgulopsis and representatives of four related genera of North American nymphophilines. Separate and combined analyses of the mtDNA datasets recovered a well supported clade composed of Pyrgulopsis and two other North American nymphophiline genera (Floridobia, Nymphophilus) consistent with the results of a prior study based on a single gene and with anatomical evidence suggesting that these taxa form a monophyletic group. Phylogenetic relationships among lineages of Pyrgulopsis were little resolved in our analyses and provided no obvious basis for splitting this large genus into multiple genera. The little differentiated Mexican genus Nymphophilus was consistently placed within Pyrgulopsis in our trees and is formally synonymized with it herein. Pyrgulopsis was also depicted as paraphyletic with respect to Floridobia in some of our trees while in others the latter was sister to a Nymphophilus + Pyrgulopsis clade. Based on these equivocal results and the morphological and geographical divergence of eastern North American Floridobia relative to Pyrgulopsis, we recommend that the former be maintained as a separate genus. The short, weakly supported branches within Pyrgulopsis and the noncongruence between our molecular phylogenetic hypotheses and geographical groupings of species are attributed to an early rapid diversification of the genus, perhaps triggered by the complex changes in western topography which occurred during the late Tertiary. Our results also indicate that penial morphologies used to define species groups of Pyrgulopsis have been subject to striking convergence throughout the West, suggesting another compelling facet of the radiation of these snails. (C) 2004 Elsevier Inc. All rights reserved. C1 Smithsonian Inst, Dept Zool, Washington, DC 20013 USA. Univ Denver, Dept Biol Sci, Denver, CO 80208 USA. RP Hershler, R (reprint author), Smithsonian Inst, Dept Zool, POB 37012,NHB W-305,MRC 163, Washington, DC 20013 USA. EM hershler.robert@nmnh.si.edu NR 81 TC 35 Z9 35 U1 0 U2 4 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 2005 VL 34 IS 2 BP 284 EP 298 DI 10.1016/j.ympev.2004.09.013 PG 15 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 886UQ UT WOS:000226258600004 PM 15619442 ER PT J AU Hosseini, BH Sadeghpour, HR Balakrishnan, N AF Hosseini, BH Sadeghpour, HR Balakrishnan, N TI Control of polarized iodine atom branching ratio in NaI photodissociation SO PHYSICAL REVIEW A LA English DT Article ID BOSE-EINSTEIN CONDENSATION; WAVE-PACKET DYNAMICS; MOLECULAR PHOTODISSOCIATION; CHEMICAL-REACTION; LASER-PULSE; FEMTOSECOND; MOTION; TRANSITION; STATES; PREDISSOCIATION AB We report branching ratios between the ground and excited states of iodine atoms in the photodissociation of sodium iodide. We employ wave packet propagation techniques to study the optimal production of polarized iodine atoms and find experimentally realizable laser parameters to control the outcome. Application of a learning algorithm shows that the product branching can be controlled by suitably varying the time delay, the chirp, and the relative phase of the pump and control laser pulses. Periodic modulation of the polarized iodine atom branching ratio as a function of the delay between the firing of the two ultrashort laser pulses provides interesting insights into the photodissociation process. C1 Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. Univ Heidelberg, Fak Phys & Astron, Heidelberg, Germany. Univ Nevada, Dept Chem, Las Vegas, NV 89154 USA. RP Hosseini, BH (reprint author), Harvard Smithsonian Ctr Astrophys, ITAMP, 60 Garden St, Cambridge, MA 02138 USA. EM bhadjiho@cfa.harvard.edu NR 42 TC 15 Z9 16 U1 1 U2 4 PU AMERICAN 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 FEB PY 2005 VL 71 IS 2 AR 023402 DI 10.1103/PhysRevA.71.023402 PG 7 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 904GK UT WOS:000227483900077 ER PT J AU Stein, DL Felley, JD Vecchione, M AF Stein, DL Felley, JD Vecchione, M TI ROV observations of benthic fishes in the Northwind and Canada Basins, Arctic Ocean SO POLAR BIOLOGY LA English DT Article AB Abyssal and midslope Arctic benthic fishes were sampled nonquantitatively by still photography and videography from a remotely operated vehicle (ROV) between 13 August and 7 September 2002. Species diversity was low: only six putative species were seen, including Lycodes frigidus Collett 1879, Lycodes sp., Rhodichthys regina Collett 1879, Paraliparis bathybius (Collett 1879), Raja (Amblyraja) hyperborea Collett 1879, and Cottunculus species diversity varied among stations sampled. An analysis of 1-min segments of videotape from one long ROV dive suggested that habitat selection by demersal nekton in these environments may be associated with the presence, absence, or density of other benthic animals. C1 NOAA, NMFS, Natl Systemat Lab,Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. Smithsonian Inst, Off Chief Informat Officer, Washington, DC 20560 USA. RP Stein, DL (reprint author), NOAA, NMFS, Natl Systemat Lab,Smithsonian Inst, Natl Museum Nat Hist, MRC-153,POB 37012, Washington, DC 20013 USA. EM steind@si.edu NR 13 TC 12 Z9 15 U1 0 U2 6 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013 USA SN 0722-4060 J9 POLAR BIOL JI Polar Biol. PD FEB PY 2005 VL 28 IS 3 BP 232 EP 237 DI 10.1007/s00300-004-0696-z PG 6 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 898AS UT WOS:000227048700008 ER PT J AU Clarke, HD Funk, VA AF Clarke, HD Funk, VA TI Using checklists and collections data to investigate plant diversity: II. An analysis of five florulas from northeastern South America SO PROCEEDINGS OF THE ACADEMY OF NATURAL SCIENCES OF PHILADELPHIA LA English DT Article ID TREE SPECIES RICHNESS; AMAZONIAN FORESTS; PATTERNS AB Five plant checklists from areas on and adjacent to the Guiana Shield were analyzed and used to test hypotheses of the salient properties of the flora of northeastern South America. Newly available checklists of Iwokrama, Mabura Hill, and Kaieteur Falls (all three in Guyana), Central French Guiana, and Reserva Ducke near Manaus, Brazil were compiled and their nomenclatural synonymies standardized. Data from checklists provide an attractive alternative to transect or plot data because they are based on rigorously determined plants of all habit types rather than the sterile vouchers of tree species often used in plot or transect studies. Descriptive data were compiled from the checklists regarding diversity, overlap, and endemism. Ranking of diversity at the family level was subjected to Kendall's coefficient of concordance of ranks test and Spearman rank correlation coefficients to evaluate similarities among the five sites. A UPGMA dendrogram was created from data for the presence or absence of species shared by two or more sites. The results indicate strong similarity among the three sites in Guyana and between Central French Guiana and Reserva Ducke, supporting a model of plant distributions determined by the presence or absence of sandstone or white sands rather than disjunct between the Roraima sandstone formation ("Guiana Highland") and other areas of the Guiana Shield. Relatively little overlap was found even between adjacent areas with ostensibly very similar abiotic environments, indicating that plant diversity will not necessarily be protected by conserving representative areas selected on the basis of general characteristics. C1 Univ N Carolina, Dept Biol, Asheville, NC 28804 USA. Smithsonian Inst, US Natl Herbarium, Washington, DC 20013 USA. RP Clarke, HD (reprint author), Univ N Carolina, Dept Biol, CPO 2440, Asheville, NC 28804 USA. EM dclarke@unca.edu; Funk.Vicki@NMNH.SI.EDU NR 35 TC 9 Z9 10 U1 0 U2 2 PU ACAD NATURAL SCIENCES PHILA PI PHILADELPHIA PA SCIENTIFIC PUBLICATIONS, 1900 BENJ FRANKLIN PKWY, PHILADELPHIA, PA 19103-1195 USA SN 0097-3157 J9 P ACAD NAT SCI PHILA JI Proc. Acad. Nat. Sci. Phila. PD FEB PY 2005 VL 154 BP 29 EP 37 DI 10.1635/0097-3157(2004)154[0029:UCACDT]2.0.CO;2 PG 9 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 950AH UT WOS:000230829500003 ER PT J AU von Braun, K Lee, BL Seager, S Yee, HKC Mallen-Ornelas, G Gladders, MD AF von Braun, K Lee, BL Seager, S Yee, HKC Mallen-Ornelas, G Gladders, MD TI Searching for planetary transits in Galactic open clusters: EXPLORE/OC SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID GRAVITATIONAL LENSING EXPERIMENT; LUMINOSITY OBJECT TRANSITS; IMAGE SUBTRACTION PHOTOMETRY; EXTRASOLAR PLANETS; INFRARED OBSERVATIONS; SECONDARY ECLIPSE; EXTENSIVE SEARCH; STELLAR-SYSTEMS; VARIABLE-STARS; 2001 CAMPAIGN AB Open clusters potentially provide an ideal environment for the search for transiting extrasolar planets, since they feature a relatively large number of stars of the same known age and metallicity at the same distance. With this motivation, over a dozen open clusters are now being monitored by four different groups. We review the motivations and challenges for open cluster transit surveys for short-period giant planets. Our photometric monitoring survey of Galactic southern open clusters, the Extrasolar Planet Occultation Research/Open Clusters (EXPLORE/OC) project, was designed with the goals of maximizing the chance of finding and characterizing planets and of providing a statistically valuable astrophysical result in the case of no detections. We use the EXPLORE/OC data from two open clusters, NGC 2660 and NGC 6208, to illustrate some of the largely unrecognized issues facing open cluster surveys, including severe contamination by Galactic field stars (>80%) and the relatively low number of cluster members for which high-precision photometry can be obtained. We discuss how a careful selection of open cluster targets under a wide range of criteria such as cluster richness, observability, distance, and age can meet the challenges, maximizing chances to detect planet transits. In addition, we present the EXPLORE/OC observing strategy to optimize planet detection, which includes high-cadence observing and continuously observing individual clusters rather than alternating between targets. C1 Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC 20015 USA. Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H8, Canada. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. RP von Braun, K (reprint author), Carnegie Inst Washington, Dept Terr Magnetism, 5241 Broad Branch Rd NW, Washington, DC 20015 USA. EM kaspar@dtm.ciw.edu; blee@astro.utoronto.ca; seager@dtm.ciw.edu; hyee@astro.utoronto.ca; gmalleno@cfa.harvard.edu; gladders@ociw.edu NR 89 TC 28 Z9 28 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 2005 VL 117 IS 828 BP 141 EP 159 DI 10.1086/427982 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 902UI UT WOS:000227381700003 ER PT J AU Small, LM AF Small, LM TI Our adaptable ancestors SO SMITHSONIAN LA English DT Editorial Material C1 Smithsonian Inst, Washington, DC 20560 USA. RP Small, LM (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 0 TC 1 Z9 1 U1 0 U2 0 PU SMITHSONIAN ASSOCIATES PI WASHINGTON PA 900 JEFFERSON DRIVE, WASHINGTON, DC 20560 USA SN 0037-7333 J9 SMITHSONIAN JI Smithsonian PD FEB PY 2005 VL 35 IS 11 BP 12 EP 12 PG 1 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA 890EV UT WOS:000226495400002 ER PT J AU Fabbiano, G AF Fabbiano, G TI Astronomy - The hunt for intermediate-mass black holes SO SCIENCE LA English DT Editorial Material ID X-RAY SOURCES; STAR-CLUSTERS; GALAXIES C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Fabbiano, G (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM pepi@head.cfa.harvard.edu NR 16 TC 15 Z9 18 U1 0 U2 0 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 JAN 28 PY 2005 VL 307 IS 5709 BP 533 EP 534 DI 10.1126/science.1107110 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 893BJ UT WOS:000226694000035 PM 15681375 ER PT J AU Ascasibar, Y Binney, J AF Ascasibar, Y Binney, J TI Numerical estimation of densities SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods : data analysis; methods : numerical; galaxies : haloes; galaxies : kinematics and dynamics; dark matter ID SMOOTHED PARTICLE HYDRODYNAMICS; DARK-MATTER HALOES; PHASE-SPACE STRUCTURE; COSMOLOGICAL SIMULATIONS; GALAXY; CLUSTERS; CODE; TREE; SPH AB We present a novel technique, dubbed FIESTAS, to estimate the underlying density field from a discrete set of sample points in an arbitrary multidimensional space. FIESTAS assigns a volume to each point by means of a binary tree. Density is then computed by integrating over an adaptive kernel. As a first test, we construct several Monte Carlo realizations of a Hernquist profile and recover the particle density in both real and phase space. At a given point, Poisson noise causes the unsmoothed estimates to fluctuate by a factor of similar to2 regardless of the number of particles. This spread can be reduced to about 1 dex (similar to26 per cent) by our smoothing procedure. The density range over which the estimates are unbiased widens as the particle number increases. Our tests show that real-space densities obtained with an SPH kernel are significantly more biased than those yielded by FIESTAS. In phase space, about 10 times more particles are required in order to achieve a similar accuracy. As a second application we have estimated phase-space densities in a dark matter halo from a cosmological simulation. We confirm the results of Arad, Dekel & Klypin that the highest values of f are all associated with substructure rather than the main halo, and that the volume function v (f) similar to f(-2.5) over about four orders of magnitude in f. We show that a modified version of the toy model proposed by Arad et al. explains this result and suggests that the departures of v (f) from power-law form are not mere numerical artefacts. We conclude that our algorithm accurately measures the phase-space density up to the limit where discreteness effects render the simulation itself unreliable. Computationally, FIESTAS is orders of magnitude faster than the method based on Delaunay tessellation that Arad et al. employed, making it practicable to recover smoothed density estimates for sets of 10(9) points in six dimensions. C1 Theoret Phys, Oxford OX1 3NP, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Ascasibar, Y (reprint author), Theoret Phys, 1 Keble Rd, Oxford OX1 3NP, England. EM yago@thphys.ox.ac.uk OI Ascasibar Sequeiros, Yago/0000-0003-1577-2479; Binney, James/0000-0002-1926-2436 NR 30 TC 53 Z9 53 U1 2 U2 2 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JAN 21 PY 2005 VL 356 IS 3 BP 872 EP 882 DI 10.1111/j.1365-2966.2004.08480.x PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 889DE UT WOS:000226422900007 ER PT J AU Sun, M Vikhlinin, A Forman, W Jones, C Murray, SS AF Sun, M Vikhlinin, A Forman, W Jones, C Murray, SS TI The survival and destruction of X-ray coronae of early-type galaxies in rich cluster environments: A case study of A1367 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : clusters : general; galaxies : clusters : individual (A1367); galaxies : individual (NGC 3842, NGC 3837); magnetic fields; X-rays : galaxies ID DYNAMICALLY YOUNG CLUSTER; ELLIPTIC GALAXIES; LUMINOSITY FUNCTION; ABELL CLUSTERS; CHANDRA VIEW; MASS-LOSS; HOT GAS; EMISSION; MERGERS; SAMPLE AB A new Chandra observation of the northwest region of the galaxy cluster A1367 reveals four cool galaxy coronae (0.4-1.0 keV) embedded in the hot (5-6 keV) intracluster medium (ICM). While the large coronae of NGC 3842 and NGC 3837 appear symmetric and relaxed, the galaxy coronae of the less than or similar toL* galaxies (NGC 3841 and CGCG 97090) are disturbed and being stripped. Massive galaxies, generally with dense cooling cores, are better able to resist ram pressure stripping and survive in rich environments than less than or similar toL* galaxies, whose galactic coronae are generally much less dense. The survival of these cool coronae implies that thermal conduction from the hot surrounding ICM has to be suppressed by a factor of at least 60 at the corona boundary. Within the galaxy coronae of NGC 3842 and NGC 3837, stellar mass loss or heat conduction with the Spitzer value may be sufficient to balance radiative cooling. Energy deposition at the ends of collimated jets may heat the outer coronae but allow the survival of a small, dense gas core (e.g., NGC 3842 in A1367 and NGC 4874 in the Coma Cluster). The surviving X-ray coronae become significantly smaller and fainter with the increasing ambient pressure. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Sun, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM msun@cfa.harvard.edu NR 27 TC 28 Z9 28 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2005 VL 619 IS 1 BP 169 EP 177 DI 10.1086/425298 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 890KA UT WOS:000226508900015 ER PT J AU McIntosh, DH Zabludoff, AI Rix, HW Caldwell, N AF McIntosh, DH Zabludoff, AI Rix, HW Caldwell, N TI Testing the universality of the (U-V) color-magnitude relations for nearby clusters of galaxies SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : observations; galaxies : clusters : general; galaxies : clusters : individual (A85, A496, A754); galaxies : elliptical and lenticular, cD; galaxies : evolution; galaxies : photometry ID BUTCHER-OEMLER CLUSTERS; HUBBLE-SPACE-TELESCOPE; STAR-FORMATION RATES; DISTANT CLUSTERS; RICH CLUSTERS; S0 GALAXIES; SURFACE PHOTOMETRY; ELLIPTIC GALAXIES; SPIRAL GALAXIES; BLUE GALAXIES AB We present a detailed (U - V) color-magnitude relation (CMR) analysis for three local (z < 0.06) clusters of galaxies. From square-degree imaging of the Abell clusters A85, A496, and A754, we select 637 galaxies down to L &SIM; 0.1L(V)* with spectroscopic membership, which minimizes uncertain field contamination corrections. To characterize the degree of CMR uniformity among nearby clusters, we use a maximum likelihood technique to quantify the CMR properties of the red galaxies in each cluster. We find that these clusters have similar CMRs with a mean color of (U - V) = 1.40 at M-V = -20 + 5 log(10)h and narrow limits of intrinsic color scatter [0.047, 0.079] and slope [-0.094, -0.075]. If we restrict our analysis to the core cluster population of red galaxies, the resulting CMRs are in close agreement with that of the Coma Cluster, the only local cluster with a rest-frame (U - V) CMR determination of comparable precision. Therefore, the CMR uniformity of present-day clusters spans a fairly wide range of cluster masses. We test how sensitive the CMR uniformity is to variations in color aperture size and sample selection, and we find at most slightly wider limits of scatter [0.047, 0.112] and slope [-0.104, -0.054]. This upper limit for (U - V) scatter is consistent with the bulk of the stellar populations of red cluster galaxies forming before z = 1.2, with a maximum age spread of 5.2 Gyr. In addition, we note that using colors from apertures containing equal fractions of galactic light does not remove the CMR slope and that none of the slopes exhibit a break as claimed by Metcalf and coworkers. Our findings expand the single Coma data point and provide a much needed z = 0 baseline for comparisons to high-redshift cluster CMRs at the same rest-frame wavelengths. The range in CMR scatter that we find among nearby clusters is consistent with the values reported for clusters at higher redshifts, further suggesting that there has been little evolution in the stellar populations of red-sequence cluster galaxies out to at least z &SIM; 1. To identify the most recently accreted cluster galaxies, we divide each cluster's membership into three galaxy populations based on (U - V) color relative to the well-defined CMR. Blue and moderately blue galaxies make up 18% - 23% by number of each cluster population more luminous than 0.1L*. Our color-magnitude division should represent a rough time since cluster accretion. In testing this hypothesis, we find that blue galaxies are spatially, kinematically, and morphologically distinct from red cluster galaxies. Even in projection, the blue galaxies reside toward the outskirts of the cluster and appear to avoid the inner half-megaparsec, in contrast with the increasing density of red-sequence galaxies toward the cluster center. In addition, the blue galaxies have velocity distributions relative to the cluster rest frame that are flatter, and some have different means, compared to the roughly Gaussian distribution of red member velocities. Members with the bluest colors tend to be disklike or irregular in appearance compared to the red galaxies, which have mostly early-type (E/S0) morphologies. Moderately blue cluster galaxies may be an intermediate mix with a fraction of small bulge-to-disk ratio S0s, yet these require closer scrutiny. The spatial, kinematic, and morphological distinctions between blue and red cluster galaxies provide further evidence that CMR-relative color is related to time since cluster infall and that bluer members are indeed the most recently accreted field spirals as expected in a hierarchical univers C1 Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Max Planck Inst Astron, D-69117 Heidelberg, Germany. Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP McIntosh, DH (reprint author), Univ Massachusetts, Dept Astron, 710 N Pleasant St, Amherst, MA 01003 USA. EM dmac@hamerkop.astro.umass.edu NR 100 TC 34 Z9 34 U1 0 U2 5 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2005 VL 619 IS 1 BP 193 EP 217 DI 10.1086/426473 PN 1 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 890KA UT WOS:000226508900017 ER PT J AU Crapsi, A Caselli, P Walmsley, CM Myers, PC Tafalla, M Lee, CW Bourke, TL AF Crapsi, A Caselli, P Walmsley, CM Myers, PC Tafalla, M Lee, CW Bourke, TL TI Probing the evolutionary status of starless cores through N2H+ and N2D+ observations SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : clouds; ISM : evolution; ISM : kinematics and dynamics; ISM : molecules; stars : formation ID MOLECULAR CLOUD CORES; RADIO-ASTRONOMICAL SPECTROSCOPY; COLLAPSING PRESTELLAR CORES; PRE-STELLAR CORES; DARK CLOUDS; DEUTERIUM FRACTIONATION; INTERSTELLAR CLOUDS; INFALL MOTIONS; DENSE CORES; AMBIPOLAR DIFFUSION AB We have undertaken a survey of N2H+ and N2D+ toward 31 low-mass starless cores using the IRAM 30 m telescope. Our main objective has been to determine the abundance ratio of N2D+ and N2H+ toward the nuclei of these cores and thus to obtain estimates of the degree of deuterium enrichment, a symptom of advanced chemical evolution according to current models. We find that the N(N2D+)/N(N2H+) ratio is larger in more "centrally concentrated cores'' with larger peak H-2 and N2H+ column density than the sample mean. The deuterium enrichment in starless cores is presently ascribed to depletion of CO in the high density (>3 x 10(4) cm(-3)) core nucleus. To substantiate this picture, we compare our results with observations in dust emission at 1.2 mm and in two transitions of (CO)-O-18. We find a good correlation between deuterium fractionation and N((CO)-O-18)/N(H-2)(1.2 mm) for the nuclei of 14 starless cores. We thus identified a set of properties that characterize the most evolved, or "prestellar,'' starless cores. These are higher N2H+ and N2D+ column densities, higher N(N2D+)/N(N2H+), more pronounced CO depletion, broader N2H+ lines with infall asymmetry, higher central H-2 column densities, and a more compact density profile than in the average core. We conclude that this combination of properties gives a reliable indication of the evolutionary state of the core. Seven cores in our sample (L1521F, Oph D, L429, L694, L183, L1544, and TMC 2) show the majority of these features and thus are believed to be closer to forming a protostar than are the other members of our sample. Finally, we note that the subsample of Taurus cores behaves more homogeneously than the total sample, an indication that the external environment could play an important role in the core evolution. C1 Univ Florence, Dipartimento Astron & Sci Spazio, I-50125 Florence, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Osserv Astrofis Arcetri, Ist Nazl Astrofis, I-50125 Florence, Italy. Observ Astron Nacl IGN, E-28014 Madrid, Spain. Korea Astron Observ, Taejon 305348, South Korea. Harvard Smithsonian Ctr Astrophys, Submillimeter Array Project, Hilo, HI 96720 USA. RP Crapsi, A (reprint author), Univ Florence, Dipartimento Astron & Sci Spazio, Largo Enrico Fermi 5, I-50125 Florence, Italy. NR 80 TC 185 Z9 185 U1 0 U2 4 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2005 VL 619 IS 1 BP 379 EP 406 DI 10.1086/426472 PN 1 PG 28 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 890KA UT WOS:000226508900030 ER PT J AU Wijnands, R Homan, J Heinke, CO Miller, JM Lewin, WHG AF Wijnands, R Homan, J Heinke, CO Miller, JM Lewin, WHG TI Chandra observations of the accretion-driven millisecond X-ray pulsars XTE J0929-314 and XTE J1751-305 in quiescence SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; stars : individual (XTE J0929-314); stars : neutron; X-rays : stars ID NEUTRON-STAR; SAX J1808.4-3658; MAGNETIC-FIELD; XTE J1751-305; KS 1731-260; XMM-NEWTON; TRANSIENTS; DISCOVERY; OUTBURST; BINARY AB We observed the accretion-driven millisecond X-ray pulsars XTE J0929 - 314 and XTE J1751 - 305 in their quiescent states using Chandra. From XTE J0929 - 314 we detected 22 source photons ( in the energy range 0.3 - 8 keV) in similar to24.4 ks, resulting in a background- corrected time-averaged count rate of (9 x 2) x 10(-4) counts s(-1). The small number of photons detected did not allow for a detailed spectral analysis of the quiescent spectrum, but we can demonstrate that the spectrum is harder than simple thermal emission, which is what is usually presumed to arise from a cooling neutron star that has been heated during the outbursts. Assuming a power-law model for the time-averaged ( averaged over the whole observation) X-ray spectrum, we obtain a power-law index of 1,8(-0.5)(+0.6) and an unabsorbed X-ray flux of 6(-2)(+4) x 10(-15) ergs s(-1) cm(-2) ( for the energy range 0.5 - 10 keV), resulting in a 0.5 - 10 keV X-ray luminosity of 7(-2)(+5) x 10(31) (d/10 kpc)(2) ergs s(-1), with d the distance toward the source in kiloparsecs. No thermal component could be detected; such a component contributed at most 30% to the 0.5 - 10 keV flux. Variability in the count rate of XTE J0929 - 314 was observed at the 95% confidence level. We did not conclusively detect XTE J1751 - 305 in our similar to43 ks observation, with 0.5 - 10 keV flux upper limits between 0.2 and 2.7 x 10(-14) ergs s(-1) cm(-2) depending on assumed spectral shape, resulting in 0.5 - 10 keV luminosity upper limits of (0.2-2) x 10(32) (d/8 kpc)(2) ergs s(-1). We compare our results with those obtained for other neutron star X-ray transients in their quiescent state, and in particular with the quiescent properties of SAX J1808.4 - 3658. Using simple accretion disk physics in combination with our measured quiescent luminosity of XTE J0929 - 314 and the luminosity upper limits of XTE J1751 - 305 and the known spin frequency of the neutron stars, we can constrain the magnetic field of the neutron stars in XTE J0929 - 314 and XTE J1751 - 305 to be less than 3 x 10(9) (d/10 kpc) and (3-7) x 10(8) (d/8 kpc) G (depending on assumed spectral shape of the quiescent spectrum), respectively. C1 Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. MIT, Ctr Space Res, Cambridge, MA 02139 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02139 USA. Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA. RP Wijnands, R (reprint author), Univ Amsterdam, Astron Inst Anton Pannekoek, Kruislaan 403, NL-1098 SJ Amsterdam, Netherlands. EM rudy@science.uva.nl; jeroen@space.mit.edu; cheinke@head.cfa.harvard.edu; jmmiller@head.cfa.harvard.edu; lewin@space.mit.edu OI Heinke, Craig/0000-0003-3944-6109 NR 41 TC 31 Z9 31 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2005 VL 619 IS 1 BP 492 EP 502 DI 10.1086/426379 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 890KA UT WOS:000226508900038 ER PT J AU Torres, G Konacki, M Sasselov, DD Jha, S AF Torres, G Konacki, M Sasselov, DD Jha, S TI Testing blend scenarios for extrasolar transiting planet candidates. II. OGLE-TR-56 SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : eclipsing; line : profiles; planetary systems; stars : evolution; stars : individual (OGLE-TR-56); techniques : radial velocities ID GRAVITATIONAL LENSING EXPERIMENT; LUMINOSITY OBJECT TRANSITS; EVOLUTIONARY MODELS; GALACTIC DISK; ABSOLUTE DIMENSIONS; GIANT PLANETS; 2001 CAMPAIGN; HOT JUPITERS; MASS STARS; 51 PEGASI AB We reexamine the photometric and spectroscopic evidence available for the star OGLE-TR-56, recently discovered to harbor a giant planet presenting transits and orbiting with a period of 1.21 days. We investigate the possibility that the observational signatures reported might be the result of "blending'' with the light of an eclipsing binary along the same line of sight. Using techniques developed earlier we perform fits to the light curve under a variety of blend configurations, subject to all observational constraints, and we infer further properties of these possible blends. We then carry out realistic end-to-end simulations based on those properties in order to quantify the spectral line asymmetries and radial velocity variations expected from such scenarios. We confront these calculations with the observations. The results from these models are clearly inconsistent with the measured radial velocity and bisector span variations, ruling out blends and confirming the planetary nature of the companion. The example of OGLE-TR-56 serves to illustrate the sort of tests that can and should be performed on transiting planet candidates to eliminate the possibility of "false positives'' and, in particular, line-of-sight contamination from eclipsing binaries. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. RP Torres, G (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM gtorres@cfa.harvard.edu RI Konacki, Maciej/A-1220-2007 NR 46 TC 51 Z9 51 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2005 VL 619 IS 1 BP 558 EP 569 DI 10.1086/426496 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 890KA UT WOS:000226508900044 ER PT J AU Sanders, D Baron-Szabo, RC AF Sanders, D Baron-Szabo, RC TI Scleractinian assemblages under sediment input: their characteristics and relation to the nutrient input concept SO PALAEOGEOGRAPHY PALAEOCLIMATOLOGY PALAEOECOLOGY LA English DT Review DE corals; reefs; siltation; turbidity; nutrients; bioerosion; encrustation ID GREAT-BARRIER-REEF; NORTHERN CALCAREOUS ALPS; CORAL MONTASTREA-ANNULARIS; SOUTH-CENTRAL PYRENEES; COMMUNITY STRUCTURE; BUILDING CORALS; FRINGING REEFS; DISCOVERY BAY; PHASE-SHIFTS; DEPOSITIONAL-ENVIRONMENTS AB In the geological record, scleractinian-dominated "turbid-water" bioconstructions that accumulated under substantial terrigenous input, along with shallow neritic marls rich in well-preserved corals are common. These occurrences indicate that beyond some threshold, the ecologic and taphonomic effects of sedimentation prevail over the effects of nutrification. Field data and experiments on recent corals show that some taxa cope well with terrigenous turbidity and sedimentation, and acclimate to increased heterotrophy. Colonial corals resilient to sediment input commonly are massive to platy forms of high skeletal plasticity and with large polypars, to effectively reject sediment, or are branched species providing a very small sedimentation area cleaned by feeble currents, or small-polyped massive taxa that tolerate intermittent veneering by sediment. These corals may comprise "siltation assemblages" of recent turbid-water reefs and level-bottoms, in siliciclastic environments. Conversely, excess input of even low amounts of dissolved inorganic nutrients into clear waters adversely affects many coral species. Fossil turbid-water bioconstructions (TWB) were situated in inner shelf to shore zone settings or near storm wave base on shelves or ramps, did not stack into reef complexes, mostly show a cluster to segment fabric, are scarce in or devoid of frame pores with marine cement, and lacked a high carbonate slope. Relative to fossil "clear-water" buildups preserved in pure limestone successions, fossil TWB contain (moderately) diverse coral assemblages, with an increased proportion of sediment-resistant forms. Aside from coral behaviour that is elusive in fossils, the sediment resistance of corals was mainly determined by colony shape and polypar size, but small-polyped, sediment-tolerant corals became common since the Early Cretaceous. Late Jurassic to Cretaceous turbid-water coral assemblages are dominated by plocoid or thamnasterioid forms; corresponding Cainozoic assemblages consist mainly of cerioid and plocoid taxa. In fossil TWB, bioerosion and encrustation are similar or higher than in contemporaneous clear-water buildups. Under higher sediment input, accumulation of discrete TWB was quenched, and level-bottoms of both corals and soft-substrate biota formed. In the resulting "coral marls", depending on turbidity, sedimentation and substrate stability, the coral fauna consists largely of both solitary corals and (mainly) sediment-resistant pseudocolonial/colonial forms, or is dominated by solitary corals. Many corals show growth "anomalies" resulting from partial mortality due to episodic, rapid sedimentation and unstable substrate. In coral marl environments, because of terrigenous input, nutrient levels probably were elevated, yet macroboring and encrustation are very scarce. Beyond some threshold of terrigenous sediment input and accumulation, the ecologic and taphonomic effects of sedimentation and unstable substrate prevail over the effects of nutrient enrichment. During the Meso-Cainozoic evolution of scleractinians, increasing photoautotrophy and progressive invasion of oligotrophic environments is in contrast to a Late Cretaceous to Cainozoic increase in the relative number of reefs in marginal-marine/siliciclastic settings. This trend may be explained by second-order sea-level fall and shrinking of epicontinental carbonate seas and isolated platforms, driving corals to more narrow, attached shelves, and by a wider total trophic range in which distinct coral assemblages can thrive, as a result of coral evolution and diversification. (C) 2004 Elsevier B.V. All rights reserved. C1 Univ Innsbruck, Fac Geo & Atmospher Sci, A-6020 Innsbruck, Austria. Natl Museum Nat Hist, Dept Invertebrate Zool, Smithsonian Inst, Washington, DC 20560 USA. RP Sanders, D (reprint author), Univ Innsbruck, Fac Geo & Atmospher Sci, Innrain 52, A-6020 Innsbruck, Austria. EM Diethard.G.Sanders@uibk.ac.at; RoseBaron@web.de NR 261 TC 73 Z9 80 U1 2 U2 28 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0031-0182 J9 PALAEOGEOGR PALAEOCL JI Paleogeogr. Paleoclimatol. Paleoecol. PD JAN 20 PY 2005 VL 216 IS 1-2 BP 139 EP 181 DI 10.1016/j.palaeo.2004.10.008 PG 43 WC Geography, Physical; Geosciences, Multidisciplinary; Paleontology SC Physical Geography; Geology; Paleontology GA 887OH UT WOS:000226314900007 ER PT J AU Choi, Y Wang, YH Zeng, T Martin, RV Kurosu, TP Chance, K AF Choi, Y Wang, YH Zeng, T Martin, RV Kurosu, TP Chance, K TI Evidence of lightning NOx and convective transport of pollutants in satellite observations over North America SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID UNITED-STATES; REACTIVE NITROGEN; FOREST-FIRES; OZONE; MODEL; CHEMISTRY; GOME; CO; PARAMETERIZATIONS; RETRIEVAL AB [1] Column observations of NO2 by GOME and CO by MOPITT over North America and surrounding oceans for April 2000 are analyzed using a regional chemical transport model. Transient enhancements in these measurements due to lightning NOx production or convective transport are examined. Evidence is found for lightning enhancements of NO2 over the continent and western North Atlantic and for convective transport enhancements of CO over the ocean. The two independent satellite measurements show consistent enhancements related to convective events. Model results suggest that the enhancements are particularly large in the lower troposphere due to convective downdrafts of lightning NOx and shallow convection of CO, implying that low- altitude aircraft in situ observations are potentially critical for evaluating the model simulations and validating satellite observations of these transient features. C1 Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA. Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 3J5, Canada. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Choi, Y (reprint author), Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA. RI Martin, Randall/A-2051-2008; Wang, Yuhang/B-5578-2014; Martin, Randall/C-1205-2014; OI Martin, Randall/0000-0003-2632-8402; Chance, Kelly/0000-0002-7339-7577 NR 23 TC 62 Z9 64 U1 1 U2 7 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JAN 19 PY 2005 VL 32 IS 2 AR L02805 DI 10.1029/2004GL021436 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 891JV UT WOS:000226578100004 ER PT J AU Lemaitre, R Watabe, H AF Lemaitre, R Watabe, H TI Pagurus ikedai (Crustacea : Anomura : Paguridae), a new hermit crab species of the bernhardus group from Japanese waters SO ZOOTAXA LA English DT Article DE hermit crab; Paguridae; Pagurus; new species; bernhardus group; Tokyo Submarine Canyon; Japan ID TOMOPAGURUS CRUSTACEA; DECAPODA; GENUS; PYLOPAGURUS; MCLAUGHLIN; REVISION; GENERA AB A new species of Paguridae, Pagurus ikedai, from the Tokyo Submarine Canyon and vicinity, Japan, is described and fully illustrated, including information on live coloration. This new species is distinguished primarily by size and shape of the chelipeds, in particular the massiveness of the left, and the presence in some males of a papilla or very short sexual tube on the right coxa of the fifth pereopod and a papilla on the coxa of the left. It is assigned to the bernhardus group which now includes eight species. C1 Smithsonian Inst, Natl Museum Amer Hist, Dept Zool, Washington, DC 20013 USA. Univ Tokyo, Ocean Res Inst, Tokyo 1648639, Japan. RP Lemaitre, R (reprint author), Smithsonian Inst, Natl Museum Amer Hist, Dept Zool, MRC 163,POB 37012, Washington, DC 20013 USA. EM lemaitre.rafael@nmnh.si.edu; watabe@ori.u-tokyo.ac.jp NR 23 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 JAN 17 PY 2005 IS 819 BP 1 EP 12 PG 12 WC Zoology SC Zoology GA 890BZ UT WOS:000226488000001 ER PT J AU Kurtz, MJ Eichhorn, G Accomazzi, A Grant, C Demleitner, M Murray, SS Martimbeau, N Elwell, B AF Kurtz, MJ Eichhorn, G Accomazzi, A Grant, C Demleitner, M Murray, SS Martimbeau, N Elwell, B TI The bibliometric properties of article readership information SO JOURNAL OF THE AMERICAN SOCIETY FOR INFORMATION SCIENCE AND TECHNOLOGY LA English DT Article ID ASTROPHYSICS DATA SYSTEM; CITATION ANALYSIS; DIGITAL LIBRARY; JOURNAL USE; HALF-LIFE; OBSOLESCENCE; IMPACT; TIME; PUBLICATION AB Digital libraries such as the NASA Astrophysics Data System (Kurtz et al., 2005) permit the easy accumulation of a new type of bibliometric measure, the number of electronic accesses ("reads") of individual articles. We explore various aspects of this new measure. We examine the obsolescence function as measured by actual reads and show that it can be well fit by the sum of four exponentials with very different time constants. We compare the obsolescence function as measured by readership with the obsolescence function as measured by citations. We find that the citation function is proportional to the sum of two of the components of the readership function. This proves that the normative theory of citation is true in the mean. We further examine in detail the similarities and differences among the citation rate, the readership rate, and the total citations for individual articles, and discuss some of the causes. Using the number of reads as a bibliometric measure for individuals, we introduce the read-cite diagram to provide a two-dimensional view of an individual's scientific productivity. We develop a simple model to account for an individual's reads and cites and use it to show that the position of a person in the read-cite diagram is a function of age, innate productivity, and work history. We show the age biases of both reads and cites and develop two new bibliometric measures which have substantially less age bias than citations: SumProd, a weighted sum of total citations and the readership rate, intended to show the total productivity of an individual; and Read10, the readership rate for articles published in the last 10 years, intended to show an individual's current productivity. We also discuss the effect of normalization (dividing by the number of authors on a paper) on these statistics. We apply SumProd and Read10 using new, nonparametric techniques to compare the quality of different astronomical research organizations. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kurtz, MJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM kurtz@cfa.harvard.edu RI Eichhorn, Guenther/C-9480-2009; KURTZ, Michael /B-3890-2009; OI Eichhorn, Guenther/0000-0002-3032-1978; Grant, Carolyn/0000-0003-4424-7366; Kurtz, Michael/0000-0002-6949-0090; Accomazzi, Alberto/0000-0002-4110-3511 NR 40 TC 64 Z9 64 U1 6 U2 23 PU JOHN WILEY & SONS INC PI HOBOKEN PA 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 1532-2882 J9 J AM SOC INF SCI TEC JI J. Am. Soc. Inf. Sci. Technol. PD JAN 15 PY 2005 VL 56 IS 2 BP 111 EP 128 DI 10.1002/asi.20096 PG 18 WC Computer Science, Information Systems; Information Science & Library Science SC Computer Science; Information Science & Library Science GA 890JU UT WOS:000226508300002 ER PT J AU Krems, RV Klos, J Rode, MF Szczesniak, MM Chalasinski, G Dalgarno, A AF Krems, RV Klos, J Rode, MF Szczesniak, MM Chalasinski, G Dalgarno, A TI Suppression of angular forces in collisions of non-S-state transition metal atoms SO PHYSICAL REVIEW LETTERS LA English DT Article ID BOSE-EINSTEIN CONDENSATE; BASIS-SETS; RESONANCES AB Angular momentum transfer is expected to occur rapidly in collisions of atoms in states of nonzero angular momenta due to the large torque of angular forces. We show that despite the presence of internal angular momenta transition metal atoms interact in collisions with helium effectively as spherical atoms and angular momentum transfer is slow. Thus, magnetic trapping and sympathetic cooling of transition metal atoms to ultracold temperatures should be readily achievable. Our results open up new avenues of research with a broad class of ultracold atoms. C1 Harvard Univ, Dept Phys, Harvard MIT Ctr Ultracold Atoms, Cambridge, MA 02138 USA. Oakland Univ, Dept Chem, Rochester, MI 48309 USA. Warsaw Univ, Fac Chem, PL-02093 Warsaw, Poland. Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom Mol & Opt Phys, Cambridge, MA 02138 USA. RP Krems, RV (reprint author), Harvard Univ, Dept Phys, Harvard MIT Ctr Ultracold Atoms, Cambridge, MA 02138 USA. RI Klos, Jacek/A-6457-2008; Rode, Michal/A-4370-2017 OI Klos, Jacek/0000-0002-7407-303X; Rode, Michal/0000-0003-0416-8305 NR 25 TC 47 Z9 47 U1 0 U2 3 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 J9 PHYS REV LETT JI Phys. Rev. Lett. PD JAN 14 PY 2005 VL 94 IS 1 AR 013202 DI 10.1103/PhysRevLett.94.013202 PG 4 WC Physics, Multidisciplinary SC Physics GA 887LQ UT WOS:000226308000029 PM 15698078 ER PT J AU Segal, D Granger, BE Sadeghpour, HR Kral, P Shapiro, M AF Segal, D Granger, BE Sadeghpour, HR Kral, P Shapiro, M TI Tunable bands of electronic image states in nanowire lattices SO PHYSICAL REVIEW LETTERS LA English DT Article ID CARBON NANOTUBES AB We demonstrate that suspended arrays of parallel nanowires support bound electron image states with rich band structures. Surprisingly, these Bloch states can be highly detached from the surfaces of the nanowires, similar to the single-tube wave functions. This is because an electron hovering in such a periodic lattice of nanowires is influenced by a Coulombic-like attraction and a centrifugal repulsion, which are both central symmetric around each wire. These novel states could be used in building of waveguides, mirrors, and storage places for Rydberg-like electrons. C1 Weizmann Inst Sci, Dept Chem Phys, IL-76100 Rehovot, Israel. Univ British Columbia, Dept Chem, Vancouver, BC V6T 1Z1, Canada. Santa Clara Univ, Dept Phys, Santa Clara, CA 95053 USA. Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. RP Segal, D (reprint author), Weizmann Inst Sci, Dept Chem Phys, IL-76100 Rehovot, Israel. NR 18 TC 10 Z9 10 U1 2 U2 3 PU AMERICAN 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 14 PY 2005 VL 94 IS 1 AR 016402 DI 10.1103/PhysRevLett.94.016402 PG 4 WC Physics, Multidisciplinary SC Physics GA 887LQ UT WOS:000226308000056 PM 15698105 ER PT J AU Rappaport, SA Podsiadlowski, P Pfahl, E AF Rappaport, SA Podsiadlowski, P Pfahl, E TI Stellar-mass black hole binaries as ultraluminous X-ray sources SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; black hole physics; binaries : general; stars : neutron; X-rays : binaries ID ANTENNAE GALAXIES NGC-4038/4039; DISC INSTABILITY MODEL; CHANDRA OBSERVATIONS; LUMINOSITY FUNCTION; OBSERVATIONAL APPEARANCE; SOURCE POPULATION; ACCRETION DISKS; CARTWHEEL RING; STAR-FORMATION; ORBITAL DECAY AB Ultraluminous X-ray sources (ULXs) with L-x > 10(39) erg s(-1) have been discovered in great numbers in external galaxies with ROSAT, Chandra and XMM-Newton. The central question regarding this important class of sources is whether they represent an extension in the luminosity function of binary X-ray sources containing neutron stars and stellar-mass black holes (BHs), or a new class of objects, e. g. systems containing intermediate-mass BHs (100-1000 M-.). We have carried out a theoretical study to test whether a large fraction of the ULXs, especially those in galaxies with recent star formation activity, can be explained with binary systems containing stellar-mass BHs. To this end, we have applied a unique set of binary evolution models for BH X-ray binaries, coupled to a binary population synthesis code, to model the ULXs observed in external galaxies. We find that for donor stars with initial masses greater than or similar to10 M-. the mass transfer driven by the normal nuclear evolution of the donor star is sufficient to potentially power most ULXs. This is the case during core hydrogen burning and, to an even more pronounced degree, while the donor star ascends the giant branch, although the latter phases last only 5 per cent of the main-sequence phase. We show that with only a modest violation of the Eddington limit, e. g. a factor of 10, both the numbers and properties of the majority of the ULXs can be reproduced. One of our conclusions is that if stellar-mass BH binaries account for a significant fraction of ULXs in star-forming galaxies, then the rate of formation of such systems is similar to3 x 10(-7) yr(-1) normalized to a core-collapse supernova rate of 0.01 yr(-1). C1 MIT 37 602B, Dept Phys, Cambridge, MA 02139 USA. Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Rappaport, SA (reprint author), MIT 37 602B, Dept Phys, 77 Massachusetts Ave, Cambridge, MA 02139 USA. EM sar@mit.edu; podsi@astro.ox.ac.uk; epfahl@cfa.harvard.edu NR 69 TC 77 Z9 77 U1 0 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JAN 11 PY 2005 VL 356 IS 2 BP 401 EP 414 DI 10.1111/j.1365-2966.2004.08489.x PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 882OW UT WOS:000225949200001 ER PT J AU Kovacs, G Bakos, G Noyes, RW AF Kovacs, G Bakos, G Noyes, RW TI A trend filtering algorithm for wide-field variability surveys SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods : data analysis; surveys; planetary systems; stars : variables : other ID IMAGE SUBTRACTION; TRANSITS; PHOTOMETRY; PLANET; STARS AB We show that various systematics related to certain instrumental effects and data reduction anomalies in wide-field variability surveys can be efficiently corrected by a trend filtering algorithm (TFA) applied to the photometric time-series produced by standard data pipelines. Statistical tests, performed on the data base of the HAT Network project, show that by the application of this filtering method the cumulative detection probability of periodic transits increases by up to 0.4 for variables brighter than 11 mag, with a trend of increasing efficiency toward brighter magnitudes. We also show that the TFA can be used for the reconstruction of periodic signals by iteratively filtering out systematic distortions. C1 Konkoly Observ Budapest, H-1525 Budapest, Hungary. Harvard Smithsonian Ctr Astrophys CfA, Cambridge, MA 02138 USA. RP Kovacs, G (reprint author), Konkoly Observ Budapest, POB 67, H-1525 Budapest, Hungary. EM kovacs@konkoly.hu; gbakos@cfa.harvard.edu; noyes@cfa.harvard.edu NR 17 TC 170 Z9 170 U1 0 U2 1 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JAN 11 PY 2005 VL 356 IS 2 BP 557 EP 567 DI 10.1111/j.1365-2966.2004.08479.x PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 882OW UT WOS:000225949200013 ER PT J AU Jonker, PG Steeghs, D Nelemans, G van der Klis, M AF Jonker, PG Steeghs, D Nelemans, G van der Klis, M TI The radial velocity of the companion star in the low-mass X-ray binary 2S 0921-630: limits on the mass of the compact object SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion : accretion discs; binaries : general; stars : individual : 2S 0921-630; stars : neutron; X-rays : binaries ID NEUTRON-STAR; 2S 0921-630; BLACK-HOLE; PULSARS; SPECTROSCOPY; 2S0921-630; SYSTEMS AB In this paper we report on optical spectroscopic observations of the low-mass X-ray binary 2S 0921-630 obtained with the Very Large Telescope. We found sinusoidal radial velocity variations of the companion star with a semi-amplitude of 99.1 +/- 3.1 km s(-1) modulated on a period of 9.006 +/- 0.007 d, consistent with the orbital period found previously for this source, and a systemic velocity of 44.4 +/- 2.4 km s(-1). Owing to X-ray irradiation, the centre of light measured by the absorption lines from the companion star is probably shifted with respect to the centre of mass. We try to correct for this using the so-called K-correction. Conservatively applying the maximum correction possible and using the previously measured rotational velocity of the companion star, we find a lower limit to the mass of the compact object in 2S 0921-630 of M-X sin(3) i > 1.90 +/- 0.25 M. (1sigma errors). The inclination in this system is well constrained since partial eclipses have been observed in X-ray and optical bands. For inclinations in the range 60degrees < i < 90degrees we find 1.90 +/- 0.25 < M-X < 2.9 +/- 0.4 M.. However, using this maximum K-correction we find that the ratio between the mass of the companion star and that of the compact object, q, is 1.32 +/- 0.37, implying super-Eddington mass-transfer rates; however, evidence for that has not been found in 2S 0921-630. We conclude that the compact object in 2S 0921-630 is either a (massive) neutron star or a low-mass black hole. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. RP Jonker, PG (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM pjonker@cfa.harvard.edu RI Nelemans, Gijs/D-3177-2012; Steeghs, Danny/C-5468-2009 OI Nelemans, Gijs/0000-0002-0752-2974; Steeghs, Danny/0000-0003-0771-4746 NR 30 TC 25 Z9 27 U1 0 U2 0 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JAN 11 PY 2005 VL 356 IS 2 BP 621 EP 626 DI 10.1111/j.1365-2966.2004.08476.x PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 882OW UT WOS:000225949200019 ER PT J AU Kondratko, PT Greenhill, LJ Moran, JM AF Kondratko, PT Greenhill, LJ Moran, JM TI Evidence for a geometrically thick self-gravitating accretion disk in NGC 3079 SO ASTROPHYSICAL JOURNAL LA English DT Review DE galaxies : active; galaxies : individual (NGC 3079); galaxies : Seyfert; galaxies : starburst; ISM : jets and outflows; masers ID ACTIVE GALACTIC NUCLEI; H2O MASER EMISSION; COMPACT RADIO-SOURCES; LARGE-SCALE OUTFLOWS; ON SEYFERT-GALAXIES; STAR-FORMING DISK; SUPERMASSIVE BLACK-HOLES; RESOLUTION X-RAY; MOLECULAR CLOUDS; CIRCINUS GALAXY AB We have mapped, for the first time, the full velocity extent of the water maser emission in NGC 3079. The largely north-south distribution of emission, aligned with a kiloparsec-scale molecular disk, and the segregation of blueshifted and redshifted emission on the sky are suggestive of a nearly edge-on molecular disk on parsec scales. Positions and line-of-sight velocities of blueshifted and redshifted maser emission are consistent with a central mass of similar to2 x 10(6) M-circle dot enclosed within a radius of similar to0.4 pc. The corresponding mean mass density of 10(6.8) M-circle dot pc(-3) is suggestive of a central black hole, which is consistent with the detection of hard X-ray excess (20-100 keV) and an Fe Kalpha line from the nucleus. Because the rotation curve traced by the maser emission is flat, the mass of the parsec-scale disk is significant with respect to the central mass. Since the velocity dispersion of the maser features does not decrease with radius and constitutes a large fraction of the orbital velocity, the disk is probably thick and flared. The rotation curve and the physical conditions necessary to support maser emission imply a Toomre Q-parameter that is much less than1. Thus, the disk is most likely clumpy, and we argue that it is probably forming stars. Overall, the accretion disk in NGC 3079 stands in contrast to the compact, thin, warped, differentially rotating disk in the archetypal maser galaxy NGC 4258. We have also mapped radio continuum emission in the vicinity of the disk and identify a new, time-variable, nonthermal component ( E) that is not collinear with the previously imaged putative jet. Based on the large luminosity and the unusually steep spectrum (alpha < -2.1), we exclude a radio supernova as the progenitor of E. However, because its spectrum is consistent with an aging electron energy distribution, E might be a rapidly cooling remnant, which may indicate that the jet axis wobbles. Alternatively, considering its location, the component might mark a shock in a wide-angle outflow that is interacting with a dense ambient medium. In this context, masers at high latitudes above the disk, mapped in this and previous studies, may be tracing an inward extension of the kiloparsec-scale bipolar wide-angle outflow previously observed along the galactic minor axis. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kondratko, PT (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM pkondrat@cfa.harvard.edu OI Moran, James/0000-0002-3882-4414 NR 124 TC 79 Z9 79 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 2005 VL 618 IS 2 BP 618 EP 634 DI 10.1086/426101 PN 1 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 887GM UT WOS:000226293800007 ER PT J AU Matsushita, S Kawabe, R Kohno, K Matsumoto, H Tsuru, TG Vila-Vilaro, B AF Matsushita, S Kawabe, R Kohno, K Matsumoto, H Tsuru, TG Vila-Vilaro, B TI Starburst at the expanding molecular superbubble in M82: Self-induced starburst at the inner edge of the superbubble SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : individual (M82, NGC 3034); galaxies : ISM; galaxies : starburst; ISM : bubbles; radio lines : galaxies ID INITIAL MASS FUNCTION; PROPAGATING STAR-FORMATION; HUBBLE-SPACE-TELESCOPE; HIGH-RESOLUTION CAMERA; H-II REGIONS; GALAXY M82; MIDINFRARED SPECTROSCOPY; CONTINUUM OBSERVATIONS; INTERACTING GALAXIES; INTERSTELLAR-MEDIUM AB We present high spatial resolution (2."3; 1."9 or 43 pc x 36 pc at D = 3.9 Mpc) 100 GHz millimeter-wave continuum emission observations with the Nobeyama Millimeter Array toward an expanding molecular superbubble in the central region of M82. The 100 GHz continuum image, which is dominated by free-free emission, revealed that the four strongest peaks are concentrated at the inner edge of the superbubble along the galactic disk. The production rates of Lyman continuum photons calculated from 100 GHz continuum flux at these peaks are an order of magnitude higher than those from the most massive star-forming regions in our Galaxy. At these regions, high-velocity ionized gas (traced by H41alpha and [Ne II]) can be seen, and H(2)O and OH masers are also concentrated. The center of the superbubble, on the other hand, is weak in molecular and free-free emissions and strong in diffuse hard X-ray emission. These observations suggest that a strong starburst produced energetic explosions and the resulting plasma and superbubble expansions and induced the present starburst regions traced by our 100 GHz continuum observations at the inner edge of the molecular superbubble. These results, therefore, provide the first clear evidence of self-induced starburst in external galaxies. The starburst at the center of the superbubble, on the other hand, is beginning to cease because of a lack of molecular gas. This kind of intense starburst seems to have occurred several times within 10(6)-10(7) yr in the central region of M82. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Natl Astron Observ Japan, Tokyo 1818588, Japan. Univ Tokyo, Inst Astron, Tokyo 1810015, Japan. Kyoto Univ, Fac Sci, Dept Phys, Sakyo Ku, Kyoto 6068502, Japan. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. RP Matsushita, S (reprint author), Acad Sinica, Inst Astron & Astrophys, POB 23141, Taipei 106, Taiwan. EM smatsushita@cfa.harvard.edu NR 98 TC 21 Z9 21 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 2005 VL 618 IS 2 BP 712 EP 722 DI 10.1086/425408 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 887GM UT WOS:000226293800015 ER PT J AU Lazendic, JS Slane, PO Hughes, JP Chen, Y Dame, TM AF Lazendic, JS Slane, PO Hughes, JP Chen, Y Dame, TM TI Chandra detection of ejecta in the small-diameter supernova remnant G349.7+0.2 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : individual (G349.7+0.2); radiation mechanisms : thermal; supernova remnants; X-rays : ISM ID LARGE-MAGELLANIC-CLOUD; GALACTIC PLANE SURVEY; MHZ MASER EMISSION; X-RAY SPECTROSCOPY; INTERSTELLAR-MEDIUM; MOLECULAR CLOUDS; DENSITY GRADIENT; MORPHOLOGY; N132D; EVOLUTION AB We present high-resolution X-ray observations of the small-diameter supernova remnant (SNR) G349.7+0.2 with Chandra. The overall SNR spectrum can be described by two spectral components. The soft component is in ionization equilibrium and has a temperature of approximate to0.8 keV; the hard spectral component has a temperature of approximate to1.4 keV, an ionization timescale of approximate to5 x 10(11) cm(-3) s, and enhanced abundances of Si. The spatially resolved spectral modeling shows that S may also be enhanced, at least in some regions. The enhanced abundances clearly point to the presence of an ejecta component in this remnant. Using the available H I and CO data toward G349.7+0.2 we derive a column density of approximate to7 x 10(22) cm(-2) along the line of sight to the SNR, which is consistent with our X-ray data. The X-ray morphology of G349.7+0.2 is strikingly similar to that at radio wavelengths - an irregular shell with a brighter eastern side - which is consistent with expansion in a medium with a large-scale density gradient. The remnant is known to be interacting with a molecular cloud (from the presence of OH (1720 MHz) masers), but this interaction is probably limited to the central portion of the SNR, as seen in SNR IC443. We found that H I clouds are present in the SNR region, which supports the notion that G349.7+0.2 belongs to a class of remnants evolving in the intercloud medium (such are IC 443 and W44), which is also responsible for the remnant's morphology. G349.7+0.2 does not have the mixed-morphology found for other maser-emitting SNRs studied to date in X-rays, but its morphology can be explained by a projection model for mixed-morphology SNRs. We have identified a point source close to the center of the SNR with a luminosity of L-X(0.5-10.0 keV) similar to (0.2-2.3) x 10(34) d(22) ergs s(-1), which is consistent with that of the compact central objects found in a few other Galactic SNRs. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. Nanjing Univ, Dept Astron, Nanjing 210093, Peoples R China. RP Lazendic, JS (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 39 TC 30 Z9 30 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 2005 VL 618 IS 2 BP 733 EP 743 DI 10.1086/426114 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 887GM UT WOS:000226293800017 ER PT J AU Luhman, KL Lada, EA Muench, AA Elston, RJ AF Luhman, KL Lada, EA Muench, AA Elston, RJ TI Flamingos spectroscopy of new low-mass members of the young cluster IC 348 SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared : stars; stars : evolution; stars : formation; stars : low-mass, brown dwarfs; stars : pre-main-sequence ID INFRARED CLASSIFICATION SPECTROSCOPY; FUNDAMENTAL MK STANDARDS; LATE M-DWARFS; BROWN DWARFS; IC 348; EVOLUTIONARY MODELS; STAR-FORMATION; BAND SPECTRA; LUMINOSITY; CANDIDATES AB We present spectroscopy of candidate stellar and substellar members of the young cluster IC 348. Using the Florida Multi-Object Imaging Near-Infrared Grism Observational Spectrometer with the 4 m telescope at Kitt Peak National Observatory, we have obtained multiobject moderate-resolution (R = 1000) J- and H-band spectra of 66 infrared sources (H = 12-17) toward IC 348, many of which are difficult to observe spectroscopically at optical wavelengths (I > 20) because they are highly reddened and/or intrinsically cool and red. We have also observed 19 known cluster members that have optical spectral types available from previous work. By using these latter sources as the spectral classification standards, we have identified 14 new members of the cluster with types M2-M6 in the sample of 66 new objects. Two additional objects exhibit types later than M8.5 but cannot be conclusively classified as either field dwarfs or cluster members with available data. We have estimated extinctions, luminosities, and effective temperatures for these 16 M-type objects, placed them on the H-R diagram, and used the evolutionary models of Chabrier & Baraffe to estimate their masses. If the two candidates at later than M8.5 are indeed members, they should be among the least massive known brown dwarfs in IC 348 (M/M(circle dot)similar to0.01). C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Florida, Dept Astron, Gainesville, FL 32611 USA. RP Luhman, KL (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM kluhman@cfa.harvard.edu OI Muench, August/0000-0003-0666-6367 NR 24 TC 34 Z9 35 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 2005 VL 618 IS 2 BP 810 EP 816 DI 10.1086/426052 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 887GM UT WOS:000226293800023 ER PT J AU Zimmerman, ER Narayan, R McClintock, JE Miller, JM AF Zimmerman, ER Narayan, R McClintock, JE Miller, JM TI Multitemperature blackbody spectra of thin accretion disks with and without a zero-torque inner boundary condition SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; stars : individual (4U 1543-47, GRO J1655-40, XTE J1550-564); X-rays : binaries; X-rays : stars ID ADVECTION-DOMINATED ACCRETION; X-RAY BINARIES; MICROQUASAR GRO J1655-40; MARGINALLY STABLE ORBIT; ACTIVE GALACTIC NUCLEI; OPTICAL OBSERVATIONS; TIMING EXPLORER; HOLE ACCRETION; XTE J1550-564; CYGNUS X-1 AB The standard spectral model for analyzing the soft component of thermal emission from a thin accretion disk around a black hole is the multitemperature blackbody model. The widely used implementation of this model, which is known as diskbb, assumes nonzero torque at the inner edge of the accretion disk. This assumption is contrary to the classic and current literature on thin-disk accretion, which advocates the use of a zero-torque boundary condition. Consequently, we have written code for a zero-torque model, ezdiskbb, which we compare to the nonzero-torque model diskbb by fitting Rossi X-Ray Timing Explorer spectra of three well-known black hole binaries: 4U 1543-47, XTE J1550-564, and GRO J1655-40. The chief difference we find is that the zero-torque model gives a value for the inner disk radius that is approximate to2.2 times smaller than the value given by diskbb. This result has important implications, especially for the determination of black hole angular momentum and mass accretion rate. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Zimmerman, ER (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 55 TC 50 Z9 51 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 2005 VL 618 IS 2 BP 832 EP 844 DI 10.1086/426071 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 887GM UT WOS:000226293800026 ER PT J AU Grindlay, JE Chou, Y Bloser, PF Narita, T AF Grindlay, JE Chou, Y Bloser, PF Narita, T TI EXITE2 observation of the SIGMA source GRS 1227+025 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; gamma rays : observations; novae, cataclysmic variables; quasars : individual (3C 273); X-rays : galaxies ID CZT DETECTORS; AE AQUARII; 3C-273; VARIABILITY; PROPELLER AB We report the second-generation Energetic X-Ray Imaging Telescope Experiment (EXITE2) hard X-ray imaging of the sky around 3C 273. A 2 hr observation on 1997 May 8 shows a similar to260 mcrab source detected at similar to4 sigma in each of two bands (50-70 and 70-93 keV) and located similar to30' from 3C 273 and consistent in position with the Granat SIGMA source GRS 1227+025. The EXITE2 spectrum is consistent with a power law with photon index 3 and large low-energy absorption, as indicated by the SIGMA results. No source was detected in more sensitive follow-up EXITE2 observations in 2000 and 2001 with 3 sigma upper limits of 190 and 65 mcrab, respectively. Comparison with the flux detected by SIGMA shows the source to be highly variable, suggesting it may be nonthermal and beamed and thus the first example of a "type 2'' (absorbed) blazar. Alternatively, it might be an unprecedented very highly absorbed binary system undergoing accretion-disk instability outbursts, possibly either a magnetic cataclysmic variable or a black hole X-ray nova. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Natl Cent Univ, Chungli 32054, Taiwan. Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA. Coll Holy Cross, Worcester, MA 01610 USA. RP Grindlay, JE (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jgrindlay@cfa.harvard.edu RI Chou, Yi/C-4922-2008 OI Chou, Yi/0000-0002-8584-2092 NR 25 TC 2 Z9 2 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 2005 VL 618 IS 2 BP 852 EP 855 DI 10.1086/383457 PN 1 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 887GM UT WOS:000226293800028 ER PT J AU Chou, Y Bloser, PF Grindlay, JE Narita, T AF Chou, Y Bloser, PF Grindlay, JE Narita, T TI Observations of Cygnus X-1 with the EXITE2 hard X-ray balloon payload SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars : individual (Cygnus X-1); X-rays : binaries; X-rays : individual (Cygnus X-1) ID BLACK-HOLE CANDIDATES; SPECTRAL VARIABILITY; X-1; TELESCOPE; COMPTONIZATION; ASTRONOMY AB We present results from the second-generation Energetic X-ray Imaging Telescope (EXITE2) observations of the black hole X-ray binary Cyg X-1 during the experiment's 1997 and 2001 flights. The EXITE2 phoswich [NaI(Tl)/CsI(Na)] detector is designed to image cosmic X-ray sources in the hard X-ray band by using the coded-aperture imaging technique from a high-altitude scientific balloon. The sky image reconstruction methodology used for EXITE2 is also discussed in detail. Background reduction (PSD rejection), subtractive flat-fielding, pixel shuffling, and image functions are introduced. During the observations from the EXITE2 1997 and 2001 flights, Cyg X-1 is easily detected in the 37-237 keV energy range. During the 1997 observations, the spectrum is well fitted by a Comptonization model. The spectral signatures and the observed 100 keV flux, together with the RXTE ASM light curve, indicate that the source was in the typical low state during this observation. Evidence is seen for hard X-ray variability on timescales on the order of 10 minutes. During the 2001 flight the spectrum is best fit by an extended power law with no observable cutoff. This is possible evidence of a transition to the high state, which is indeed seen in the RXTE ASM light curve shortly after our observation. C1 Natl Cent Univ, Grad Inst Astron, Jung Li City 320, Tuoyuan, Taiwan. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Coll Holy Cross, Dept Phys, Worcester, MA 01610 USA. RP Chou, Y (reprint author), Natl Cent Univ, Grad Inst Astron, 300 Jung Da Rd, Jung Li City 320, Tuoyuan, Taiwan. EM yichou@astro.ncu.edu.tw; bloser@milkyway.gsfc.nasa.gov; josh@head-cfa.harvard.edu; tnarita@holycross.edu RI Chou, Yi/C-4922-2008 OI Chou, Yi/0000-0002-8584-2092 NR 32 TC 4 Z9 4 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 2005 VL 618 IS 2 BP 856 EP 865 DI 10.1086/383078 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 887GM UT WOS:000226293800029 ER PT J AU Wijnands, R Heinke, CO Pooley, D Edmonds, PD Lewin, WHG Grindlay, JE Jonker, PG Miller, JM AF Wijnands, R Heinke, CO Pooley, D Edmonds, PD Lewin, WHG Grindlay, JE Jonker, PG Miller, JM TI The hard quiescent spectrum of the neutron star X-ray transient EXO 1745-248 in the globular cluster Terzan 5 SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; globular clusters : individual (Terzan 5); stars : individual (EXO 1745-248); X-rays : stars ID CHANDRA OBSERVATION; THERMAL EMISSION; SAX J1808.4-3658; CENTAURUS X-4; BINARY; PULSAR; DISCOVERY; CORE; LUMINOSITY; NGC-6440 AB We present a Chandra observation of the globular cluster Terzan 5 during times when the neutron star X-ray transient EXO 1745-248 located in this cluster was in its quiescent state. We detected the quiescent system with a (0.5-10 keV) luminosity of similar to2 x 10(33) ergs s(-1). This is similar to several other neutron-star transients observed in their quiescent states. However, the quiescent X-ray spectrum of EXO 1745-248 was dominated by a hard power-law component instead of the soft component that usually dominates the quiescent emission of other neutron star X-ray transients. This soft component could not conclusively be detected in EXO 1745-248, and we conclude that it contributed at most 10% of the quiescent flux in the energy range 0.5-10 keV. EXO 1745-248 is only the second known neutron-star transient whose quiescent spectrum is dominated by the hard component (SAX J1808.4-3658 is the other one). We discuss possible explanations for this unusual behavior of EXO 1745-248, its relationship to other quiescent neutron-star systems, and the impact of our results on understanding quiescent X-ray binaries. We also discuss the implications of our results on the way that the low-luminosity X-ray sources in globular clusters are classified. C1 Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02139 USA. MIT, Ctr Space Res, Cambridge, MA 02139 USA. Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. RP Wijnands, R (reprint author), Univ Amsterdam, Astron Inst Anton Pannekoek, Kruislaan 403, NL-1098 SJ Amsterdam, Netherlands. EM rudy@science.uva.nl OI Heinke, Craig/0000-0003-3944-6109 NR 45 TC 46 Z9 46 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 2005 VL 618 IS 2 BP 883 EP 890 DI 10.1086/426127 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 887GM UT WOS:000226293800032 ER PT J AU Young, PR Dupree, AK Espey, BR Kenyon, SJ Ake, TB AF Young, PR Dupree, AK Espey, BR Kenyon, SJ Ake, TB TI Far Ultraviolet Spectroscopic Explorer observations of the symbiotic star AG Draconis SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : symbiotic; line : identification; stars : individual (AG Draconis); stars : winds, outflows; ultraviolet : stars ID PHOTOIONIZATION CROSS-SECTIONS; RECOMBINATION LINE-INTENSITIES; EXPERIMENTAL LEVEL VALUES; EMISSION-LINES; IUE OBSERVATIONS; ISOELECTRONIC SEQUENCE; OPTICAL OBSERVATIONS; EXTREME-ULTRAVIOLET; N=2 CONFIGURATIONS; RATE COEFFICIENTS AB Spectra of the bright symbiotic star AG Draconis (BD + 67degrees922) in the wavelength range 905-1187 Angstrom obtained with the Far Ultraviolet Spectroscopic Explorer (FUSE) are presented. The spectra show a number of narrow, nebular emission lines, together with a uniform continuum from the hot component of the system, and numerous interstellar absorption lines. We infer the existence of Ne VIII in the AG Dra nebula through the identification of the Ne VII lambda973.3 recombination line. The emission-line spectrum is dominated by intense lines of O VI but also shows weaker lines from highly ionized ions including Ne V, Ne VI, S IV, and S VI. Members of the He II Balmer series can be identified up to n = 20. Lines of Fe II and Fe III fluoresced by O VI lambda1032 are identified at wavelengths 1141.172 and 1142.429 Angstrom, respectively. The emission lines are shown to be produced in a plasma with an electron temperature of 20,000-30,000 K, photoionized by the white dwarf. The Ne VI lambda997/lambda999 ratio shows that this ion and all others except perhaps Ne VII are formed at least 300 white dwarf radii from the white dwarf. Revised wavelengths for the Ne V 2s(2)2p(2) P-3(0,1)-2s2p(3) S-5(2) and Ne VI 2s(2)2p P-2-2s2p(2) P-4 transitions are published. C1 Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. Rutherford Appleton Lab, Didcot OX11 0QX, Oxon, England. Univ Dublin Trinity Coll, Dept Phys, Dublin 2, Ireland. Dublin Inst Adv Studies, Astrophys Sect, Dublin 2, Ireland. Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. Comp Sci Corp, Lanham, MD 20706 USA. RP Young, PR (reprint author), Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. OI Espey, Brian/0000-0002-2457-1380; Kenyon, Scott/0000-0003-0214-609X NR 52 TC 21 Z9 21 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 2005 VL 618 IS 2 BP 891 EP 907 DI 10.1086/426045 PN 1 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 887GM UT WOS:000226293800033 ER PT J AU Han, CH Gaudi, BS An, JH Gould, A AF Han, CH Gaudi, BS An, JH Gould, A TI Microlensing detection and characterization of wide-separation planets SO ASTROPHYSICAL JOURNAL LA English DT Article DE gravitational lensing; planetary systems; planets and satellites : general ID EXTRASOLAR PLANETS; GRAVITATIONAL LENS; HIGH-MAGNIFICATION; GALACTIC BULGE; EVENTS; SYSTEMS; COMPANIONS; CHANNEL; BINARY; STARS AB With their excellent photometric precision and dramatic increase in monitoring frequency, future microlensing survey experiments are expected to be sensitive to very short timescale, isolated events caused by free-floating and wide-separation planets with masses as low as a few lunar masses. The scientific value of these detections would be greatly enhanced if their nature (bound or unbound) could be accurately characterized and if the planet masses could be measured. Here we present a comprehensive discussion of the ability of microlensing to detect and characterize wide-separation planets. We estimate the probability of measuring the planetary Einstein radius theta(E,p) for bound and free-floating planets; this is one of the two additional observables required to measure the planet mass. We carry out detailed simulations of the planetary events expected in next-generation surveys and estimate the resulting uncertainty in theta(E,p) for these events. We show that, for main-sequence sources and Jupiter-mass planets, the caustic structure of wide-separation planets with projected separations of less than or similar to20 AU substantially increases the probability of measuring the dimensionless source size and thus determining theta(E,p) compared to the case of unbound planets. In this limit where the source is much smaller than the caustic, the effective cross section to measure theta(E,p) to 10% is similar to25% larger than the full width of the caustic. Measurement of the lens parallax is possible for low-mass planetary events through combined observations from the ground and a satellite located in an L2 orbit; this would complete the mass measurements for such wide-separation planets. Finally, short-duration events caused by bound planets can be routinely distinguished from those caused by free-floating planets for planet-star separations less than or similar to20 AU from either the deviations due to the planetary caustic or (more often) the low-amplitude bump from the magnification due to the parent star. C1 Chungbuk Natl Univ, Inst Basic Sci Res, Dept Phys, Chonju 361763, South Korea. Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. RP Han, CH (reprint author), Chungbuk Natl Univ, Inst Basic Sci Res, Dept Phys, Chonju 361763, South Korea. EM cheongho@astroph.chungbuk.ac.kr; sgaudi@cfa.harvard.edu; jin@ast.cam.ac.uk; gould@astronomy.ohio-state.edu RI Gaudi, Bernard/I-7732-2012 NR 32 TC 19 Z9 19 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 2005 VL 618 IS 2 BP 962 EP 972 DI 10.1086/426115 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 887GM UT WOS:000226293800039 ER PT J AU Lie-Svendsen, O Esser, R AF Lie-Svendsen, O Esser, R TI Modeling the energy budget of solar wind minor ions: Implications for temperatures and abundances SO ASTROPHYSICAL JOURNAL LA English DT Article DE solar wind; Sun : abundances; Sun : corona ID POLAR CORONAL HOLES; DIFFERENTIAL FLOW SPEEDS; SPECTRAL-LINE PROFILES; ELEMENT FRACTIONATION; CYCLOTRON-RESONANCE; TRANSPORT-EQUATIONS; CHARGE STATES; CHROMOSPHERE; HELIUM; ACCELERATION AB The outflow of oxygen and silicon ions in the solar wind has been studied using a model that extends from the chromosphere into interplanetary space, with emphasis on understanding the energy budget of the minor ions. The model solves coupled gyrotropic transport equations, which account for temperature anisotropies and heat conduction, for all charge states, and includes ionization and recombination. The minor ions are heated with a constant heating rate per particle in the corona. In the transition region the thermal force causes minor ions to flow faster than protons, with an abundance that can be less than half of the chromospheric abundance. The ions quite suddenly decouple from the proton flow in the corona, and above this point the ion flow is independent of the proton flow. For high heating rates the coronal abundance is comparable to the chromospheric abundance, the ion terminal wind speed is high, and most of the deposited energy is lost into the solar wind. Low heating rates lead to very large coronal abundances and a low terminal flow speed, and the main energy loss is then through collisions with protons and electrons in the corona. The heavy ions become much hotter than protons in the corona, even without preferential heating of the ions. However, preferential heating is necessary to prevent a large abundance enhancement in the corona and to achieve flow speeds close to the speeds observed by the Ultraviolet Coronagraph Spectrometer (UVCS) on the Solar and Heliospheric Observatory (SOHO). The abundance enhancement implies that lowering the heating rate per particle in general leads to an increase in the total energy flux absorbed by the ions. C1 Norwegian Def Res Estab, NO-2027 Kjeller, Norway. Univ Tromso, Dept Phys, NO-9037 Tromso, Norway. Univ Oslo, Inst Theoret Astrophys, NO-0315 Oslo, Norway. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Lie-Svendsen, O (reprint author), Norwegian Def Res Estab, POB 25, NO-2027 Kjeller, Norway. EM oystein.lie-svendsen@ffi.no; ruth.esser@phys.uit.no NR 33 TC 18 Z9 18 U1 1 U2 8 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 2005 VL 618 IS 2 BP 1057 EP 1073 PN 1 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 887GM UT WOS:000226293800049 ER PT J AU Miller, JM Homan, J AF Miller, JM Homan, J TI Evidence for a link between Fe K alpha emission-line strength and quasi-periodic oscillation phase in a black hole SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; binaries : general; black hole physics; relativity ID X-RAY BINARIES; XTE J1550-564; GRO J1655-40; IRON LINE; STATES; DISK; X-1 AB In X-ray binaries, the frequencies revealed in X-ray quasi-periodic oscillations (QPOs) are often interpreted as characteristic frequencies in the inner accretion disk, although the exact oscillation mechanism is unknown at present. Broadened Fe Kalpha lines are also excellent diagnostics of the inner accretion flow, if their broadening is indeed due to inner disk reflection. Here we present two cases where the flux and equivalent width of the Fe Kalpha emission lines in spectra of the Galactic black hole GRS 1915+105 vary with the phase of strong 1 and 2 Hz QPOs in the X-ray flux. These results provide strong evidence that both QPOs and the Fe Kalpha lines originate in the inner disk. If the 1 Hz QPO is only a Keplerian orbital frequency, the QPO comes from a distance of from (84 +/- 26) R-Schw the black hole; the 2 Hz QPO implies a radius of (50 +/- 15) R-Schw. At these radii, relativistic shaping of a disk line is inevitable. Moreover, the link holds in radio-bright and radio-faint phases, signaling that in systems like GRS 1915 + 105, the Fe Kalpha line is a disk line and not a jet line as per SS 433. A particularly interesting possibility is that a stable warp in the inner disk, e.g., due to Lense-Thirring precession, may produce the observed QPOs and line modulations. More broadly, the Fe K-QPO link provides an unprecedented mechanism for revealing the inner accretion flow and relativistic regime in accreting systems, in that it gives two measures of radius: for a given disk QPO model, the frequency translates into a specific radius, and relativistic line models yield radii directly. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. MIT, Ctr Space Res, Cambridge, MA 02139 USA. MIT, Dept Phys, Cambridge, MA 02139 USA. RP Miller, JM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jmmiller@cfa.harvard.edu; jeroen@space.mit.edu NR 22 TC 34 Z9 35 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 2005 VL 618 IS 2 BP L107 EP L110 DI 10.1086/427775 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 887GO UT WOS:000226294000012 ER PT J AU Yoshida, N Furlanetto, SR Hernquist, L AF Yoshida, N Furlanetto, SR Hernquist, L TI The temperature structure of the warm-hot intergalactic medium SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : theory; intergalactic medium ID X-RAY-CLUSTERS; SUPERNOVA-REMNANTS; CYGNUS LOOP; EMISSION; SHOCKS; DISCOVERY; FILAMENT; SPECTRA; FOREST AB We study the temperature structure of the intergalactic medium (IGM) using a large cosmological N-body/ smoothed particle hydrodynamics simulation. We employ a two-temperature model for the thermal evolution of the ionized gas, in which we include explicitly the relaxation process between electrons and ions. In the diffuse, hot IGM, the relaxation time is comparable to the age of the universe, and hence the electron temperature in postshock regions remains significantly smaller than the ion temperature. We show that, at the present epoch, a large fraction of the warm-hot intergalactic medium (WHIM) has a well-developed two-temperature structure, with typical temperature differences of order a few. Consequently, the fraction of metals in various ionization states such as O VI, O VII, and O VIII, as well as their line emissivities, can differ locally by more than an order of magnitude from those computed with a single-temperature model, especially in gas with T similar to 10(7) K. It is thus necessary to follow the evolution of the electron temperature explicitly to determine absorption and emission by the WHIM. Although equipartition is nearly achieved in the denser intracluster medium, we find an appreciable systematic deviation between the gas mass weighted electron temperature and the mean temperature even at half the virial radii of clusters. There is thus a reservoir of warm (T-e < 1 keV) gas in and around massive clusters. Our results imply that relaxation processes need to be considered in describing and interpreting observational data from existing X-ray telescopes as well as from future missions designed to detect the WHIM, such as the Diffuse Intergalactic Oxygen Surveyor and the Missing Baryon Explorer. C1 Nagoya Univ, Dept Phys, Chikusa Ku, Nagoya, Aichi 4646082, Japan. CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Yoshida, N (reprint author), Nagoya Univ, Dept Phys, Chikusa Ku, Nagoya, Aichi 4646082, Japan. RI Yoshida, Naoki/A-4305-2011 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 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 2005 VL 618 IS 2 BP L91 EP L94 DI 10.1086/427874 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 887GO UT WOS:000226294000008 ER PT J AU Lee, TG Rochow, C Martin, R Clark, TK Forrey, RC Balakrishnan, N Stancil, PC Schultz, DR Dalgarno, A Ferland, GJ AF Lee, TG Rochow, C Martin, R Clark, TK Forrey, RC Balakrishnan, N Stancil, PC Schultz, DR Dalgarno, A Ferland, GJ TI Close-coupling calculations of low-energy inelastic and elastic processes in He-4 collisions with H-2: A comparative study of two potential energy surfaces SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID RO-VIBRATIONAL TRANSITIONS; ATOM-MOLECULE COLLISIONS; RATE CONSTANTS; CROSS-SECTIONS; RELAXATION; SCATTERING; COLD; TEMPERATURES; DIFFRACTION; EXCITATION AB The two most recently published potential energy surfaces (PESs) for the HeH2 complex, the so-called MR (Muchnick and Russek) and BMP (Boothroyd, Martin, and Peterson) surfaces, are quantitatively evaluated and compared through the investigation of atom-diatom collision processes. The BMP surface is expected to be an improvement, approaching chemical accuracy, over all conformations of the PES compared to that of the MR surface. We found significant differences in inelastic rovibrational cross sections computed on the two surfaces for processes dominated by large changes in target rotational angular momentum. In particular, the H-2(nu=1,j=0) total quenching cross section computed using the BMP potential was found to be a factor of 1000 larger than that obtained with the MR surface. A lesser discrepancy persists over a large range of energies from the ultracold to thermal and occurs for other low-lying initial rovibrational levels. The MR surface was used in previous calculations of the H-2(nu=1,j=0) quenching rate coefficient and gave results in close agreement with the experimental data of Audibert which were obtained for temperatures between 50 and 300 K. Examination of the rovibronic coupling matrix elements, which are obtained following a Legendre expansion of the PES, suggests that the magnitude of the anisotropy of the BMP potential is too large in the interaction region. However, cross sections for elastic and pure rotational processes obtained from the two PESs differ typically by less than a factor of 2. The small differences may be ascribed to the long-range and anharmonic components of the PESs. Exceptions occur for (nu=10,j=0) and (nu=11,j=1) where significant enhancements have been found for the low-energy quenching and elastic cross sections due to zero-energy resonances in the BMP PES which are not present in the MR potential. (C) 2005 American Institute of Physics. C1 Univ Kentucky, Dept Phys & Astron, Lexington, KY 40506 USA. Oak Ridge Natl Lab, Div Phys, Oak Ridge, TN 37831 USA. Penn State Univ, Berks Lehigh Valley Coll, Dept Phys, Reading, PA 19610 USA. Univ Nevada, Dept Chem, Las Vegas, NV 89154 USA. Univ Georgia, Dept Phys & Astron, Athens, GA 30602 USA. Univ Georgia, Ctr Simulat Phys, Athens, GA 30602 USA. Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. RP Lee, TG (reprint author), Univ Kentucky, Dept Phys & Astron, Lexington, KY 40506 USA. RI Lee, Teck Ghee/D-5037-2012 OI Lee, Teck Ghee/0000-0001-9472-3194 NR 51 TC 17 Z9 18 U1 1 U2 5 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 8 PY 2005 VL 122 IS 2 AR 024307 DI 10.1063/1.1833351 PG 9 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 893DH UT WOS:000226699000024 PM 15638586 ER PT J AU Latychev, K Mitrovica, JX Tamisiea, ME Tromp, J Moucha, R AF Latychev, K Mitrovica, JX Tamisiea, ME Tromp, J Moucha, R TI Influence of lithospheric thickness variations on 3-D crustal velocities due to glacial isostatic adjustment SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID SEA-LEVEL CHANGE; MANTLE VISCOSITY; HORIZONTAL MOTIONS; NORTHERN EUROPE; EARTH; MODEL; FENNOSCANDIA; DEFORMATION; RHEOLOGY; ICE-3G AB Predictions of 3-D crustal velocities driven by glacial isostatic adjustment (GIA) have generally been based on spherically symmetric Earth models. We adopt a finite-volume formulation to explore the impact of lateral variations in elastic plate strength, including lithospheric thickness changes across the continent-ocean interface and plate boundary weak zones, on these predictions. Weak zones introduce horizontal rate perturbations with a plate scale coherency and amplitudes reaching 1-2 mm/yr; radial velocity perturbations can be as large, but are geographically isolated to the weak zones (specifically, the North Atlantic Ridge). A discontinuity in ocean-continent lithospheric thickness significantly impacts rates along continental margins (order 1 mm/yr for radial rates and generally about half this for tangential rates). We conclude that lateral variations in lithospheric strength should be included in future GIA analyzes of space-geodetic survey results and in assessing the impact of GIA on the stability of geodetic reference frames. C1 Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CALTECH, Seismol Lab, Pasadena, CA 91125 USA. RP Latychev, K (reprint author), Univ Toronto, Dept Phys, 60 St George St, Toronto, ON M5S 1A7, Canada. EM latychev@physics.utoronto.ca RI Tromp, Jeroen/B-6185-2015 OI Tromp, Jeroen/0000-0002-2742-8299 NR 20 TC 13 Z9 13 U1 1 U2 8 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JAN 7 PY 2005 VL 32 IS 1 AR L01304 DI 10.1029/2004GL021454 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 890KS UT WOS:000226510700004 ER PT J AU Narayan, R Quataert, E AF Narayan, R Quataert, E TI Black hole accretion SO SCIENCE LA English DT Review ID GAMMA-RAY BURSTS; ELECTROMAGNETIC EXTRACTION; MAGNETICALLY DRIVEN; RADIO-SOURCES; FLOWS; GALAXY; JETS; MODELS; ENERGY; DISKS AB Black holes are most often detected by the radiation produced when they gravitationally pull in surrounding gas, in a process called accretion. The efficiency with which the hot gas radiates its thermal energy strongly influences the geometry and dynamics of the accretion flow. Both radiatively efficient thin disks and radiatively inefficient thick disks are observed. When the accreting gas gets close to the central black hole, the radiation it produces becomes sensitive to the spin of the hole and the presence of an event horizon. Analysis of the luminosities and spectra of accreting black holes has yielded tantalizing evidence for both rotating holes and event horizons. Numerical simulations imply that the relativistic jets often seen from accreting black holes may be powered in part by the spin of the hole. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. RP Narayan, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM narayan@cfa.harvard.edu; eliot@astron.berkeley.edu OI Narayan, Ramesh/0000-0002-1919-2730 NR 61 TC 32 Z9 32 U1 1 U2 1 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 JAN 7 PY 2005 VL 307 IS 5706 BP 77 EP 80 DI 10.1126/science.1105746 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 886GG UT WOS:000226214300038 PM 15637269 ER PT J AU Harrison, RD AF Harrison, RD TI Destructive fires are not just Indonesia's problem SO NATURE LA English DT Letter C1 Smithsonian Trop Res Inst, Ancon, Panama. RP Harrison, RD (reprint author), Smithsonian Trop Res Inst, Apartado Postal 2072,Balboa Ave, Ancon, Panama. NR 1 TC 0 Z9 0 U1 0 U2 1 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 EI 1476-4687 J9 NATURE JI Nature PD JAN 6 PY 2005 VL 433 IS 7021 BP 13 EP 13 DI 10.1038/433013a PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 884WJ UT WOS:000226117100011 ER PT J AU McNamara, BR Nulsen, PEJ Wise, MW Rafferty, DA Carilli, C Sarazin, CL Blanton, EL AF McNamara, BR Nulsen, PEJ Wise, MW Rafferty, DA Carilli, C Sarazin, CL Blanton, EL TI The heating of gas in a galaxy cluster by X-ray cavities and large-scale shock fronts SO NATURE LA English DT Article ID COOLING FLOWS; RADIO-SOURCES; BLACK-HOLES; SKY SURVEY; ENERGY; MODELS AB Most of the baryons in galaxy clusters reside between the galaxies in a hot, tenuous gas(1). The densest gas in their centres should cool and accrete onto giant central galaxies at rates of 10-1,000 solar masses per year(1). No viable repository for this gas, such as clouds or new stars, has been found(1). New X-ray observations, however, have revealed far less cooling below X-ray temperatures than expected(2), altering the previously accepted picture of cooling flows. As a result, most of the gas must be heated to and maintained at temperatures above similar to2 keV (ref. 3). The most promising heating mechanism is powerful radio jets emanating from supermassive black holes in the central galaxies of clusters(4). Here we report the discovery of giant cavities and shock fronts in a distant (z=0.22) cluster caused by an interaction between a radio source and the hot gas surrounding it. The energy involved is similar to6x10(61) erg, the most powerful radio outburst known. This is enough energy to quench a cooling flow for several Gyr, and to provide similar to1/3 keV per particle of heat to the surrounding cluster. C1 Ohio Univ, Clippinger Labs, Inst Astrophys, Athens, OH 45701 USA. Ohio Univ, Clippinger Labs, Dept Phys & Astron, Athens, OH 45701 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. MIT, Ctr Space Res, Cambridge, MA 02139 USA. Natl Radio Astron Observ, Very Large Array, Socorro, NM 87801 USA. Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA. Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA. RP McNamara, BR (reprint author), Ohio Univ, Clippinger Labs, Inst Astrophys, Athens, OH 45701 USA. EM mcnamarb@ohio.edu RI Blanton, Elizabeth/H-4501-2014 NR 29 TC 250 Z9 250 U1 1 U2 5 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD JAN 6 PY 2005 VL 433 IS 7021 BP 45 EP 47 DI 10.1038/nature03202 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 884WJ UT WOS:000226117100030 PM 15635404 ER PT J AU Hall, JPW Willmott, KR Busby, RC AF Hall, JPW Willmott, KR Busby, RC TI Five new Penaincisalia species (Lepidoptera : Lycaenidae : Eumaeini) from the Andes of southern Ecuador and northern Peru SO ZOOTAXA LA English DT Article DE Andes; cloud forest; Ecuador; hilltopping; Penaincisalia; Peru ID BUTTERFLIES AB Five new species of Penaincisalia (Lycaenidae: Eumaeini) are described from the high Andes of southern Ecuador and northern Peru: P. caeruleanota Hall & Willmott n. sp., P. juliae Hall & Willmott n. sp., P. andreae Busby & Hall n. sp., P. libertada Hall n. sp. and P. ismaeli Busby & Hall n. sp.. We present brief discussions on their systematic placement within the genus and on their adult ecology. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20560 USA. Nat Hist Museum, Dept Entomol, London SW7 5BD, England. RP Hall, JPW (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20560 USA. NR 25 TC 10 Z9 15 U1 0 U2 1 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD JAN 5 PY 2005 IS 797 BP 1 EP 20 PG 20 WC Zoology SC Zoology GA 887CL UT WOS:000226280700001 ER PT J AU Davis, JLD Eckert-Mills, MG Young-Williams, AC Hines, AH Zohar, Y AF Davis, JLD Eckert-Mills, MG Young-Williams, AC Hines, AH Zohar, Y TI Morphological conditioning of a hatchery-raised invertebrate, Callinectes sapidus, to improve field survivorship after release SO AQUACULTURE LA English DT Article DE stock enhancement; decapod; Callinectes sapidus; lateral spines; carapace color ID TROUT ONCORHYNCHUS-MYKISS; CONCH STROMBUS-GIGAS; JUVENILE QUEEN CONCH; CHESAPEAKE-BAY; COHO SALMON; BLUE-CRAB; AGONISTIC BEHAVIOR; STOCK ENHANCEMENT; WILD ANCESTRY; RED DRUM AB For recruitment-limited, severely depleted fishery stocks, stock enhancement may become an important technique in the return of population sizes to sustainable levels. Aquaculture-reared individuals, however, may face some disadvantages upon release into the wild due to differences between natural conditions and the hatchery. The goal of this study was to test whether field survivorship of hatchery-raised blue crabs, Callinectes sapidus, could be improved by simple conditioning steps, taking advantage of phenotypic plasticity in certain traits. This species is currently the focus of a preliminary stock enhancement program in the Chesapeake Bay. Results indicate that unconditioned hatchery crabs had lower survivorship than wild crabs in the field and differed in carapace color and lateral spine length. Both traits were plastic. Carapace color was changeable within 1-2 days, without a molt, upon the exposure of crabs to new substrates. However, colors within the range produced in this study did not significantly affect survivorship in a field or a laboratory experiment. Change in spine length required exposure to predators for 1-4 weeks. Exposure to fish predators resulted in increased spine length, though exposure to adult blue crabs had no significant effect. Crabs with lengthened spines had significantly higher survivorship in both laboratory and field experiments, suggesting that this feature may be one on which to focus large-scale conditioning efforts. Results of this study suggest a level of phenotypic plasticity that may contribute to the blue crab's ability to take advantage of multiple estuarine habitat types. On a more applied level, results of this study suggest that at least some deficiencies in hatchery-raised organisms can be alleviated and would likely lead to improved success and efficiency of stock enhancement efforts. Similar studies on other hatchery-raised invertebrates and finfishes may also lead to improvements in their enhancement programs. (C) 2004 Elsevier B.V. All rights reserved. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Univ Maryland, Inst Biotechnol, Ctr Marine Biotechnol, Baltimore, MD 21202 USA. RP Davis, JLD (reprint author), Smithsonian Environm Res Ctr, 647 Contees Wharf Rd, Edgewater, MD 21037 USA. EM janalddavis@yahoo.com NR 39 TC 32 Z9 37 U1 0 U2 10 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0044-8486 J9 AQUACULTURE JI Aquaculture PD JAN 3 PY 2005 VL 243 IS 1-4 BP 147 EP 158 DI 10.1016/j.aquaculture.2004.09.027 PG 12 WC Fisheries; Marine & Freshwater Biology SC Fisheries; Marine & Freshwater Biology GA 887MM UT WOS:000226310200015 ER PT B AU Gingerich, O AF Gingerich, O BE Turatto, M Benetti, S Zampieri, L Shea, W TI Tycho Brahe and the Nova of 1572 SO 1604-2004: Supernovae as Cosmological Lighthouses SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Conference on 1604-2004 - Supernovae as Cosmological Lighthouses CY JUN 15-19, 2004 CL Univ Degli Studi Padova, Padua, ITALY HO Univ Degli Studi Padova AB The brilliant Nova of 1572 marked the beginning of the end of Aristotelian cosmology and provided the defining moment when the young Tycho Brahe became a professional astronomer. He received more than a ton of gold from the Danish king to build his Uraniborg Observatory. His instruments, the finest produced in the pre-telescopic age, enabled him to establish that both the nova and the Comet of 1577 lay beyond the moon, contrary to Aristotle's teaching. His major attempt to establish the distance to Mars (in order to distinguish between the Ptolemaic and Copernican cosmologies) failed, but left, in its wake a magnificently accurate set of data that enabled Kepler to make the greatest advance in celestial mechanics since Copernicus himself. 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 12 TC 2 Z9 2 U1 0 U2 1 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-209-1 J9 ASTR SOC P PY 2005 VL 342 BP 3 EP 12 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BDX50 UT WOS:000235953000001 ER PT B AU Matheson, T AF Matheson, T BE Turatto, M Benetti, S Zampieri, L Shea, W TI The supernovae associated with gamma-ray bursts SO 1604-2004: SUPERNOVAE AS COSMOLOGICAL LIGHTHOUSES SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT Conference on 1604-2004 - Supernovae as Cosmological Lighthouses CY JUN 15-19, 2004 CL Univ Degli Studi Padova, Padua, ITALY HO Univ Degli Studi Padova ID 25 APRIL 1998; IC HYPERNOVA SN-2003DH/GRB-030329; OPTICAL SPECTROSCOPY; SN 1998BW; AFTERGLOW; GRB-030329; PROGENITOR; GRB-021004; GRB-011121; PHOTOMETRY AB Supernovae were long suspected as possible progenitors of gammaray bursts. The arguments relied on circumstantial evidence. Several recent gamma-ray bursts, notably GRB 030329, have provided direct, spectroscopic evidence that supernovae and gamma-ray bursts are related. The supernovae associated with gamma-ray bursts are all of Type Ic, implying a compact progenitor, which has implications for gamma-ray burst models. Other peculiar Type le supernovae may help to expand understanding of the mechanisms involved. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Matheson, T (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM tmatheso@cfa.harvard.edu NR 44 TC 1 Z9 1 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-209-1 J9 ASTR SOC P PY 2005 VL 342 BP 309 EP 314 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BDX50 UT WOS:000235953000059 ER PT S AU Phillips, DF Novikova, I Zibrov, S Smallwood, C Taichenachev, AV Yudin, VI Walsworth, RL Zibrov, AS AF Phillips, David F. Novikova, Irina Zibrov, Sergei Smallwood, Chris Taichenachev, Aleksei V. Yudin, Valeriy I. Walsworth, Ronald L. Zibrov, Alexander S. GP IEEE TI A novel absorption resonance for atomic clocks SO 2005 IEEE International Frequency Control Symposium and Exhibition SE PROCEEDINGS OF THE IEEE INTERNATIONAL FREQUENCY CONTROL SYMPOSIUM LA English DT Proceedings Paper CT IEEE International Frequency Control Symposium and Exposition CY AUG 29-31, 2005 CL Vancouver, CANADA ID POPULATION-TRAPPING RESONANCES; FREQUENCY STANDARDS; SHIFTS; LINES; RB-85 AB We report an experimental study of an all-optical three-photon-absorption resonance (known as an "N-resonance") and discuss its potential application as an alternative to atomic clocks based on coherent population trapping (CPT). We present measurements of the N-resonance contrast, width and light shift for Rb-87 under various conditions including both D-1 and D-2 optical transitions. Under conditions such that first-order light shifts cancel, we observe promising short-term frequency stability (approximate to 1.5 x 10(-11) tau(-1/2)) for an N-resonance on the D-1 transition of Rb-87 vapor. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Phillips, DF (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Taichenachev, Aleksei/K-7065-2015; Zibrov, Sergei/M-6400-2015; Zibrov, Alexander/G-7419-2014 OI Taichenachev, Aleksei/0000-0003-2273-0066; NR 20 TC 0 Z9 0 U1 0 U2 1 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 1075-6787 BN 0-7803-9052-0 J9 P IEEE INT FREQ CONT PY 2005 BP 767 EP 773 DI 10.1109/FREQ.2005.1574031 PG 7 WC Engineering, Electrical & Electronic; Instruments & Instrumentation; Physics, Applied SC Engineering; Instruments & Instrumentation; Physics GA BEG11 UT WOS:000237191500137 ER PT J AU Giannini, NP Kalko, EKV AF Giannini, NP Kalko, EKV TI The guild structure of animalivorous leaf-nosed bats of Barro Colorado Island, Panama, revisited SO ACTA CHIROPTEROLOGICA LA English DT Article DE Panama; Phyllostomidae; feeding habits; tropical forest; ecomorphology ID FORAGING BEHAVIOR; CHROTOPTERUS-AURITUS; INSECTIVOROUS BATS; TRACHOPS-CIRRHOSUS; PHYLLOSTOMID BATS; DIETARY OVERLAP; GLEANING BATS; FOOD-HABITS; MORPHOLOGY; ECOLOGY AB We examined data sets on dietary composition of a rich (15 species) assemblage of animal-eating Neotropical leaf-nosed bats (Phyllostomidae: Phyllostominae) that occur syntopically on Barro Colorado Island, Panama. Our aim was to test previously postulated trophic structure of phyllostomines in the light of alternative analytical techniques and new data. The trophic structure of this assemblage, according to new results from Correspondence Analysis, has two main trends of variation: a gradient of increased carnivory (axis 1) and a gradient involving plant and arthropod consumption (axis 2). This rejects previous hypotheses of this guild in which the structure was described as a complex of many independent discrete resources. Although all data sets agree that coleopterans as a group are an important food item for most species, Phyllostominae bats are not typically durophageous; i.e., they lack cranial and dental adaptations for rapid processing of hard-shelled arthropods as found in other bat families. Furthermore, insectivory varies inversely with body size, and is gradually replaced by carnivory in association with increasing mass and limited dental modifications. Together with CA results, this suggests that carnivory is an extreme of animalivory rather than. a qualitatively distinct feeding habit among Phyllostominae bats. This conclusion fits biomechanical data that indicate that carnivorous bats are bigger and only modestly modified versions of soft-insect specialists. C1 Amer Museum Nat Hist, Dept Mammal, New York, NY 10024 USA. Smithsonian Trop Res Inst, Balboa, Panama. Univ Ulm, Dept Expt Ecol, D-89069 Ulm, Germany. RP Amer Museum Nat Hist, Dept Mammal, Cent Pk W 79th St, New York, NY 10024 USA. EM norberto@amnh.org NR 70 TC 25 Z9 26 U1 2 U2 20 PU MUSEUM & INST ZOOLOGY PAS-POLISH ACAD SCIENCES PI WARSAW PA WILCZA STREET 64, 00-679 WARSAW, POLAND SN 1508-1109 EI 1733-5329 J9 ACTA CHIROPTEROL JI Acta Chiropt. PY 2005 VL 7 IS 1 BP 131 EP 146 DI 10.3161/1733-5329(2005)7[131:TGSOAL]2.0.CO;2 PG 16 WC Zoology SC Zoology GA 951IR UT WOS:000230923500013 ER PT J AU Arroyo-Cabrales, J Kalko, EKV LaVal, RK Maldonado, JE Medellin, RA Polaco, OJ Rodriguez-Herrera, B AF Arroyo-Cabrales, J Kalko, EKV LaVal, RK Maldonado, JE Medellin, RA Polaco, OJ Rodriguez-Herrera, B TI Rediscovery of the Mexican flat-headed bat Myotis planiceps (Vespertilionidae) SO ACTA CHIROPTEROLOGICA LA English DT Article DE flat-headed bat; Myotis; critically endangered; Mexico; new records ID ECHOLOCATION; PLASTICITY C1 INAH, Subdirect Lab & Apoyo Acad, Mexico City 06060, DF, Mexico. Programa Para Conservac Murcielagos Mexico, Mexico City 10400, DF, Mexico. Univ Ulm, Dept Expt Ecol, D-89069 Ulm, Germany. Smithsonian Trop Res Inst, Balboa, Panama. Programa Conservac Mucrielagos Costa Rica, Moneverde, Costa Rica. Natl Zool Pk, Genet Program, Washington, DC 20008 USA. Univ Nacl Autonoma Mexico, Inst Ecol, Mexico City 04510, DF, Mexico. RP Arroyo-Cabrales, J (reprint author), INAH, Subdirect Lab & Apoyo Acad, Moneda 16,Co Ctr, Mexico City 06060, DF, Mexico. EM arromatu5@yahoo.com.mx NR 9 TC 2 Z9 3 U1 1 U2 3 PU POLISH ACAD OF SCIENCES PI WARSAW PA MUSEUM & INST ZOOLOGY WILCZA 64, 00-679 WARSAW, POLAND SN 1508-1109 J9 ACTA CHIROPTEROL JI Acta Chiropt. PY 2005 VL 7 IS 2 BP 309 EP 314 DI 10.3161/1733-5329(2005)7[309:ROTMFB]2.0.CO;2 PG 6 WC Zoology SC Zoology GA 994HT UT WOS:000234022700010 ER PT S AU Spurr, R Stamnes, K Eide, H Li, W Stamnes, J AF Spurr, R Stamnes, K Eide, H Li, W Stamnes, J BE Frouin, RJ Kawamura, H Pan, D TI Analytic Jacobians for ocean color retrieval: linearization of the coupled atmosphere-ocean discrete ordinate model SO ACTIVE AND PASSIVE REMOTE SENSING OF THE OCEANS SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Active and Passive Remote Sensing of the Oceans CY NOV 08-09, 2004 CL Honolulu, HI SP SPIE DE remote sensing; radiative transfer; weighting functions; ocean color ID RADIATIVE-TRANSFER; LAYERED MEDIA; ALGORITHM; ACCURATE; SYSTEM; SEAWIFS; RADIANCE AB Recent work has shown the need for accurate treatment of radiative transfer in ocean color retrieval. The plane-parallel coupled atmosphere-ocean discrete ordinate model CAO-DISORT has been used to investigate the validity of current approximative inverse methods and to study new techniques for improved ocean color retrieval. In this paper we show that CAO-DISORT is fully differentiable with respect to its input optical properties, so that we can define analytic Jacobians with respect to any profile element in the atmosphere and ocean. A single call to the linearized model will produce radiances and Jacobians at arbitrary optical depth and viewing geometry in either medium. The model also has a pseudo-spherical treatment for solar beam attenuation in a curved atmosphere. The linearized model can be used directly in iterative least-squares retrievals requiring forward model simulations of backscatter measurements and their parameter derivatives; there is no need for approximations involving an atmospheric correction. We demonstrate the model's new capability by performing closed-loop least squares fitting to simultaneously retrieve the aerosol optical thickness and marine chlorophyll concentration from a set of 6 synthetic measurements at SeaWifs wavelengths. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Spurr, R (reprint author), Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. NR 17 TC 0 Z9 0 U1 0 U2 1 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5617-9 J9 P SOC PHOTO-OPT INS PY 2005 VL 5656 BP 33 EP 44 DI 10.1117/12.577855 PG 12 WC Oceanography; Remote Sensing SC Oceanography; Remote Sensing GA BBT02 UT WOS:000227659900004 ER PT S AU Novikova, I Klein, M Phillips, DF Walsworth, RL AF Novikova, I Klein, M Phillips, DF Walsworth, RL BE Coufal, HJ Hasan, ZU Craig, AE TI Optimizing stored light efficiency in vapor cells SO Advanced Optical and Quantum Memories and Computing II SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Advanced Optical and Quantum Memories and Computing II CY JAN 25-26, 2005 CL San Jose, CA SP SPIE DE electromagnetically induced transparency; slow light; stored light; vapor cell; buffer gas ID ELECTROMAGNETICALLY INDUCED TRANSPARENCY; QUANTUM COMMUNICATION; ATOMIC ENSEMBLES; PHOTON STATES; GENERATION; RELAXATION; STORAGE; MEMORY; CAVITY; LASER AB We present a preliminary experimental study of slow and stored light in Rb vapor cells under the conditions of electromagnetically induced transparency (EIT). We study the efficiency of light storage as a function of pulse duration, storage time, retrieval field intensity, etc. We demonstrate that atomic diffusion in-and-out of the laser beam plays an important role not well described by previous analysis. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Novikova, I (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 33 TC 11 Z9 11 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 0-8194-5709-4 J9 P SOC PHOTO-OPT INS PY 2005 VL 5735 BP 87 EP 97 DI 10.1117/12.601719 PG 11 WC Optics SC Optics GA BCI58 UT WOS:000229604200010 ER PT S AU Chu, X Dalgarno, A AF Chu, X Dalgarno, A BE Stroke, HH TI Polarizabilities of P-3 atoms and van der Waals coefficients for their interaction with helium atoms SO ADVANCES IN ATOMIC MOLECULAR, AND OPTICAL PHYSICS, VOL 51 SE Advances In Atomic Molecular and Optical Physics LA English DT Review; Book Chapter ID ELECTRIC-DIPOLE POLARIZABILITIES; MILLIKELVIN TEMPERATURES; STATES; CALCIUM AB Time-dependent density functional theory with self-interaction correction is applied to obtain the scalar and tensor dynamic polarizabilities of atoms in P-3 states. The static polarizabilities are in good agreement with previous values. The dynamic polarizabilities are then used to evaluate the leading term in the long range interaction between the P-3 atoms and helium. They are significant in determining the likelihood that the P-3 atoms can be trapped in a helium buffer gas. C1 Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. RP Chu, X (reprint author), Harvard Smithsonian Ctr Astrophys, ITAMP, 60 Garden St, Cambridge, MA 02138 USA. NR 21 TC 4 Z9 4 U1 0 U2 4 PU ELSEVIER ACADEMIC PRESS INC PI SAN DIEGO PA 525 B STREET, SUITE 1900, SAN DIEGO, CA 92101-4495 USA SN 1049-250X BN 0-12-003851-X J9 ADV ATOM MOL OPT PHY JI Adv. Atom. Mol. Opt. Phys. PY 2005 VL 51 BP 83 EP 91 DI 10.1016/S1049-250X(05)51014-0 PG 9 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA BDT09 UT WOS:000235191900004 ER PT J AU Philpott, SM AF Philpott, SM TI Changes in arboreal ant populations following pruning of coffee shade-treesin Chiapas, Mexico SO AGROFORESTRY SYSTEMS LA English DT Article DE Azteca; biological control; Camponotus; Chiapas; Management system; Mexico ID TROPICAL AGROECOSYSTEM; SPECIES RICHNESS; BIODIVERSITY; PLANTATIONS; TRANSFORMATION; MANAGEMENT; SYSTEMS; FOREST AB Reducing or eliminating shade cover in coffee (Coffea arabica L.) agroforestry systems affects fungal disease and pest outbreaks, coffee yields, and can result in biodiversity loss of important predators, such as ants. Less dramatic changes in shade structure or composition may also affect ants. Shade tree pruning, a common management practice in shaded coffee systems, has unknown consequences for ant communities. The effects of pruning on arboreal ant communities were investigated by measuring ant abundance, distribution, and species richness in the short (1 week) and long-term (6 months) after shade tree pruning in one 25 x 50 m plot. Shade tree pruning significantly affected the distribution and abundance of two of the most common ant species (Azteca instabilis F. Smith and Camponotus senex textor Forel), and in general did not affect other ants. After pruning, C. senex textor ants were 80% more abundant on coffee plants and shade trees, whereas A. instabilis abundance dropped by 40% on coffee plants and 73% on shade trees after pruning. Additionally, C. senex textor were significantly more widespread, whereas A. instabilis distributions were more restricted. The effects of pruning were strong over the short-term, but were not evident over the long-term. Shade tree pruning did not affect ant diversity. Thus shade tree pruning largely affected certain aspects of arboreal ant communities in one coffee agroforestry system, with important implications for biological control. C1 Univ Michigan, Dept Ecol & Evolutionary Biol, Ann Arbor, MI 48109 USA. RP Philpott, SM (reprint author), Smithsonian Inst, Natl Zool Pk, Smithsonian Migratory Bird Ctr, Washington, DC 20008 USA. EM sphilpot@umich.edu RI Philpott, Stacy/F-2330-2011 NR 15 TC 16 Z9 17 U1 0 U2 14 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0167-4366 J9 AGROFOREST SYST JI Agrofor. Syst. PD JAN PY 2005 VL 64 IS 3 BP 219 EP 224 DI 10.1007/s10457-004-2372-2 PG 6 WC Agronomy; Forestry SC Agriculture; Forestry GA 945HC UT WOS:000230492600005 ER PT J AU Lyman, RL O'Brien, MJ Schiffer, MB AF Lyman, RL O'Brien, MJ Schiffer, MB TI Publishing archaeology in Science and Scientific American, 1940-2003 SO AMERICAN ANTIQUITY LA English DT Article ID ARCHEOLOGY; ORIGINS; DOMESTICATION; ANTHROPOLOGY; ARTIFACTS; WORLD; PREHISTORY; HYDRATION; CULTURES; ALEUTS AB Many new, or processual, archaeologists of the 1960s argued that Americanist archaeology became scientific only in the 1960s. The hypothesis that the rate of publication of archaeological research in Science and Scientific American increased after about 1965. as new archaeologists sought to demonstrate to their peers and other scientists that archaeology was indeed a science, is disconfirmed. The rate of archaeological publication in these journals increased after 1955 because the effort to be more scientific attributed to the processualists began earlier Higher publication rates in both journals appear to have been influenced by oil increased amount of archaeological research. a higher rate of archaeological publication generally, and increased funding. The hypothesis that editorial choice has strongly influenced what has been published in Science is confirmed: articles focusing on multidisciplinary topics rather than oil narrow archaeological ones dominate the list of titles over the period,from 1940 through 2003. C1 Univ Missouri, Dept Anthropol, Columbia, MO 65211 USA. Univ Arizona, Dept Anthropol, Tucson, AZ 85721 USA. Smithsonian Inst, Amer Museum Nat Hist, Res Associate Lemelson Ctr, Washington, DC 20560 USA. RP Lyman, RL (reprint author), Univ Missouri, Dept Anthropol, 107 Swallow Hall, Columbia, MO 65211 USA. NR 70 TC 1 Z9 1 U1 0 U2 4 PU SOC AMER ARCHAEOLOGY PI WASHINGTON PA 900 SECOND ST., NE STE 12, WASHINGTON, DC 20002-3557 USA SN 0002-7316 J9 AM ANTIQUITY JI Am. Antiq. PD JAN PY 2005 VL 70 IS 1 BP 157 EP 167 PG 11 WC Anthropology; Archaeology SC Anthropology; Archaeology GA 893HA UT WOS:000226708700010 ER PT J AU Samuel, R Kathriarachchi, H Hoffmann, P Barfuss, MHJ Wurdack, KJ Davis, CC Chase, MW AF Samuel, R Kathriarachchi, H Hoffmann, P Barfuss, MHJ Wurdack, KJ Davis, CC Chase, MW TI Molecular phylogenetics of phyllanthaceae: Evidence from plastid Matk and nuclear PHYC sequences SO AMERICAN JOURNAL OF BOTANY LA English DT Article DE Malpighiales; matK; molecular phylogenetics; Phyllanthaceae; PHYC; systematics ID ANGIOSPERM PHYLOGENY; FLOWERING PLANTS; RBCL SEQUENCES; GENE-SEQUENCES; DNA-SEQUENCES; PHYTOCHROME; EVOLUTION; SAXIFRAGACEAE; MALPIGHIACEAE; EUPHORBIACEAE AB Plastid matK and a fragment of the low-copy nuclear gene PHYC were sequenced for 30 genera of Phyllanthaceae to evaluate tribal and generic delimitation. Resolution and bootstrap percentages obtained with matK are higher than that of PHYC but both regions show nearly identical phylogenetic patterns. Phylogenetic relationships inferred from the independent and combined data are congruent and differ from previous, morphology-based classifications but are highly concordant with those of the plastid gene rbcL previously published. Phyllanthaceae is monophyletic and gives rise to two well-resolved clades (T and F) that could be recognized as subfamilies. DNA sequence data for Keayodendron and Zimmermanniopsis are presented for the first time. Keayodendron is misplaced in tribe Phyllantheae and belongs to the Bridelia alliance. Zimmermanniopsis is sister to Zimmermannia. Phyllanthus and Cleistanthus are paraphyletic. Savia and Phyllanthus subgenus Kirganelia are not monophyletic. C1 Univ Vienna, Bot Inst & Bot Garten, A-1030 Vienna, Austria. Royal Bot Gardens, Herbarium, Richmond TW9 3AB, Surrey, England. Smithsonian Inst, Dept Bot, Washington, DC 20013 USA. Smithsonian Inst, Lab Analyt Biol, Washington, DC 20013 USA. Univ Michigan Herbarium, Dept Ecol & Evolut Biol, Ann Arbor, MI 48108 USA. Royal Bot Gardens, Jodrell Lab, Richmond TW9 3DS, Surrey, England. RP Samuel, R (reprint author), Univ Vienna, Bot Inst & Bot Garten, Rennweg 14, A-1030 Vienna, Austria. EM mary.rosabella.samuel@univie.ac.at RI Chase, Mark /A-6642-2011 NR 58 TC 67 Z9 80 U1 0 U2 7 PU BOTANICAL SOC AMER INC PI ST LOUIS PA PO BOX 299, ST LOUIS, MO 63166-0299 USA SN 0002-9122 J9 AM J BOT JI Am. J. Bot. PD JAN PY 2005 VL 92 IS 1 BP 132 EP 141 DI 10.3732/ajb.92.1.132 PG 10 WC Plant Sciences SC Plant Sciences GA 890JK UT WOS:000226507300017 PM 21652393 ER PT J AU Kress, WJ Liu, AZ Newman, M Li, QJ AF Kress, WJ Liu, AZ Newman, M Li, QJ TI The molecular phylogeny of Alpinia (Zingiberaceae): A complex and polyphyletic genus of gingers SO AMERICAN JOURNAL OF BOTANY LA English DT Article DE Alpinia; flexistyly; gingers; ITS; matK; phylogeny; tropical; Zingiberaceae ID SEQUENCE DATA; MATK; DNA; CLASSIFICATION; ALPINIOIDEAE; TREES AB Alpinia is the largest, most widespread, and most taxonomically complex genus in the Zingiberaceae with 230 species occurring throughout tropical and subtropical Asia. Species of Alpinia often predominate in the understory of forests. while others are important ornamentals and medicinals. Investigations of the evolutionary relationships of a subset of species of Alpinia using DNA sequeace-based methods specifically test the monophyly of the genus and the validity of the previous classifications. Seventy-two species of , 27 non-Alpinia species in the subfamily Alpinioideae, eight species in the subfamily Zingiberoideae, one species in the subfamily Tamijioidae, and three species in the outgroup genus Siphonochilus (Siphonochiloideae) were sequenced for die plastid matK region and the nuclear internal transcribed spacer (ITS) loci. Parsimony analyse's of both individual and combined data sec, identified six polyphyletic clades containing species of Alpinia distributed across the tribe Alpiniea. These results, were Supported by a Bayesian analysis of the combined data set. Except in a few specific cases. these monophyletic groupings of species do not correspond with either Schumann's (1904) or Smith's (1990) classification of the genus. Here we build on previous molecular analyses of the Alpinioideae and propose the next steps necessary to recognize new generic boundaries in the Alpinieae. C1 US Natl Herbarium, Dept Bot, Museum Natl Hist Nat, Smithsonian Inst, Washington, DC 20013 USA. Chinese Acad Sci, Xishuangbanna Trop Bot Garden, Mengla 666303, Yunnan, Peoples R China. Royal Bot Gardens, Edinburgh EH3 5LR, Midlothian, Scotland. RP Kress, WJ (reprint author), US Natl Herbarium, Dept Bot, Museum Natl Hist Nat, Smithsonian Inst, POB 37012,MRC-166, Washington, DC 20013 USA. EM kress.j@si.edu RI Liu, aizhong/F-1770-2010 NR 46 TC 57 Z9 81 U1 3 U2 9 PU BOTANICAL SOC AMER INC PI ST LOUIS PA PO BOX 299, ST LOUIS, MO 63166-0299 USA SN 0002-9122 J9 AM J BOT JI Am. J. Bot. PD JAN PY 2005 VL 92 IS 1 BP 167 EP 178 DI 10.3732/ajb.92.1.167 PG 12 WC Plant Sciences SC Plant Sciences GA 890JK UT WOS:000226507300019 PM 21652395 ER PT J AU Mulhern, DM Jones, EB AF Mulhern, DM Jones, EB TI Test of revised method of age estimation from the auricular surface of the ilium SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Article DE skeletal aging; innominate; Terry Collection; Huntington Collection ID SKELETAL AGE; OS-PUBIS; DEATH AB The objective of this paper is to test a revised method of age estimation based on the morphology of the auricular surface recently proposed by Buckberry and Chamberlain ([2002] Am. J. Phys. Anthropol. 119:231-239). The study sample consists of 309 individuals of known sex, age, and race from the Terry and Huntington Collections. Auricular surfaces were scored using the revised technique to determine whether it is equally applicable to both sexes as well as blacks and whites. The auricular surfaces of the same individuals were also scored using the original method of auricular surface scoring developed by Lovejoy et al. ([1985] Am. J. Phys. Anthropol. 68:15-28) to determine whether the revised technique is comparable to the original method in terms of accuracy. Results show that the revised method is equally applicable to males and females as well as blacks and whites. The revised method is less accurate than the original method for individuals between 20-49 years of age, but more accurate for individuals between 50-69 years of age. (C) 2004 Wiley-Liss, Inc. C1 Smithsonian Inst, Dept Anthropol, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Mulhern, DM (reprint author), Smithsonian Inst, Dept Anthropol, Natl Museum Nat Hist, POB 37012,MRC 138, Washington, DC 20013 USA. EM mulhern.dawn@nmnh.si.edu NR 13 TC 37 Z9 38 U1 0 U2 7 PU WILEY-LISS PI HOBOKEN PA DIV JOHN WILEY & SONS INC, 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PD JAN PY 2005 VL 126 IS 1 BP 61 EP 65 DI 10.1002/ajpa.10410 PG 5 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 878SC UT WOS:000225666100006 PM 15386244 ER PT J AU Freid, D Spradley, MK Jantz, RL Ousley, SD AF Freid, D Spradley, MK Jantz, RL Ousley, SD TI The truth is out there: how NOT to use FORDISC. SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract C1 Univ Tennessee, Dept Anthropol, Knoxville, TN 37996 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Repatriat Osteol Lab, Washington, DC 20560 USA. NR 0 TC 3 Z9 3 U1 0 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 2005 SU 40 BP 103 EP 103 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 900KX UT WOS:000227214900163 ER PT J AU Jones, EB Mulhern, DM AF Jones, EB Mulhern, DM TI Interpersonal violence at Hawikku: Interpreting perimortem trauma. SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract C1 Smithsonian Inst, Dept Anthropol, NMNH, Repatriat Osteol Lab, 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 2005 SU 40 BP 123 EP 123 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 900KX UT WOS:000227214900240 ER PT J AU London, MR Wilczak, CA Dudar, JC Ousley, SD AF London, MR Wilczak, CA Dudar, JC Ousley, SD TI Congenital and developmental defects of the vertebral column in samples from Hawikku and Puye, New Mexico. SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Repatriat Osteol Lab, Washington, DC 20560 USA. Univ Maryland, Dept Anthropol, College Pk, MD 20742 USA. NR 0 TC 0 Z9 0 U1 0 U2 2 PU WILEY-LISS PI HOBOKEN PA DIV JOHN WILEY & SONS INC, 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2005 SU 40 BP 140 EP 140 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 900KX UT WOS:000227214900305 ER PT J AU Megyesi, MS Ubelaker, DH Sauer, N AF Megyesi, MS Ubelaker, DH Sauer, N TI A test of the Lamendin aging method on two historic skeletal samples. SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract C1 Michigan State Univ, Dept Anthropol, E Lansing, MI 48824 USA. Smithsonian Inst, Dept Anthropol, NMNH, 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 2005 SU 40 BP 150 EP 151 PG 2 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 900KX UT WOS:000227214900346 ER PT J AU Mulhern, DM Ortner, DJ Wilczak, CA Jones, EB AF Mulhern, DM Ortner, DJ Wilczak, CA Jones, EB TI Interpreting skeletal lesions at Hawikku: evidence for mycotic infection. SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract C1 Smithsonian Inst, Dept Anthropol, NMNH, 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 2005 SU 40 BP 154 EP 154 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 900KX UT WOS:000227214900360 ER PT J AU Ortner, DJ AF Ortner, DJ TI Ales Hrdlicka and the founding of the AJPA: 1918. SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract C1 Smithsonian Inst, Natl Museum Nat Hist, 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 2005 SU 40 BP 161 EP 162 PG 2 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 900KX UT WOS:000227214900387 ER PT J AU Wilczak, CA Ousley, SD AF Wilczak, CA Ousley, SD TI Questioning the relationship of cranial deformation to ossicle formation: results from Hawikku. SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract C1 Smithsonian Inst, Repatriat Osteol Lab, Dept Anthropol, Museum Natl Hist Nat, Washington, DC 20560 USA. Univ Maryland, Dept Anthropol, College Pk, MD 20742 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 2005 SU 40 BP 222 EP 222 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 900KX UT WOS:000227214900622 ER PT J AU Heyer, WR Murphy, JB AF Heyer, W. Ronald Murphy, James B. BE Lannoo, M TI Declining Amphibian Populations Task Force SO AMPHIBIAN DECLINES: THE CONSERVATION STATUS OF UNITED STATES SPECIES LA English DT Editorial Material; Book Chapter C1 [Heyer, W. Ronald] Smithsonian Inst, Dept Vertebrate Zool, Natl Museum Nat Hist, Washington, DC 20560 USA. [Murphy, James B.] Smithsonian Inst, Dept Herpetol, Washington, DC 20560 USA. RP Heyer, WR (reprint author), Smithsonian Inst, Dept Vertebrate Zool, Natl Museum Nat Hist, Washington, DC 20560 USA. NR 0 TC 3 Z9 5 U1 0 U2 2 PU UNIV CALIFORNIA PRESS PI BERKELEY PA 2120 BERKELEY WAY, BERKELEY, CA 94720 USA BN 978-0-520-92943-2 PY 2005 BP 17 EP 21 PG 5 WC Zoology SC Zoology GA BXA51 UT WOS:000295537400006 ER PT J AU Beasley, VR Faeh, SA Wikoff, B Staehle, C Eisold, J Nichols, D Cole, R Schotthoefer, AM Greenwell, M Brown, LE AF Beasley, Val R. Faeh, Sandra A. Wikoff, Brigit Staehle, Craig Eisold, Joyce Nichols, Donald Cole, Rebecca Schotthoefer, Anna M. Greenwell, Martin Brown, Lauren E. BE Lannoo, M TI Risk Factors and Declines in Northern Cricket Frogs (Acris crepitans) SO AMPHIBIAN DECLINES: THE CONSERVATION STATUS OF UNITED STATES SPECIES LA English DT Article; Book Chapter C1 [Beasley, Val R.; Faeh, Sandra A.; Wikoff, Brigit; Staehle, Craig; Eisold, Joyce] Univ Illinois, Coll Vet Med, Dept Vet Biosci, Urbana, IL 61801 USA. [Brown, Lauren E.] Illinois State Univ, Dept Biol Sci, Normal, IL 61761 USA. [Cole, Rebecca] USGS Natl Wildlife Hlth Ctr, Madison, WI USA. [Greenwell, Martin] John G Shedd Aquarium, Chicago, IL USA. [Nichols, Donald] Smithsonian Inst, Dept Pathol, Washington, DC 20560 USA. [Schotthoefer, Anna M.] Univ Illinois, Coll Vet Med, Dept Pathobiol, Urbana, IL 61801 USA. RP Beasley, VR (reprint author), Univ Illinois, Coll Vet Med, Dept Vet Biosci, Urbana, IL 61801 USA. NR 0 TC 24 Z9 27 U1 0 U2 5 PU UNIV CALIFORNIA PRESS PI BERKELEY PA 2120 BERKELEY WAY, BERKELEY, CA 94720 USA BN 978-0-520-92943-2 PY 2005 BP 75 EP 86 PG 12 WC Zoology SC Zoology GA BXA51 UT WOS:000295537400014 ER PT J AU Paredes, R Jones, IL Boness, DJ AF Paredes, R Jones, IL Boness, DJ TI Reduced parental care, compensatory behaviour and reproductive costs of thick-billed murres equipped with data loggers SO ANIMAL BEHAVIOUR LA English DT Article ID FORAGING TRIP DURATION; GUILLEMOTS URIA-LOMVIA; TIME-DEPTH RECORDERS; ANTARCTIC FUR SEALS; DIVING BEHAVIOR; BIPARENTAL CARE; SATELLITE TRANSMITTERS; INSTRUMENT ATTACHMENT; RADIO TRANSMITTERS; SEX-DIFFERENCES AB Theoretical models predict that in species with obligate biparental care, individuals will partially compensate for decreased parental effort by their partners as a stable evolutionary strategy. Full compensation may occur when breeding success is an accelerating function of parental effort, especially in long-lived bird species. We experimentally examined the effect of time-depth recorders (TDRs) on body mass and parental behaviour of thick-billed murres, Uria lomvia, and evaluated the effect of TDRs as handicaps to test whether individuals compensate for decreased partner effort and whether compensation is sex biased. Compared with control birds, TDR-equipped birds had reduced body mass, offspring attendance, number of foraging trips and feeding rates, and males had increased foraging trip duration. in general, males lost mass at a higher rate and made longer foraging trips than females. Partners of TDR-equipped birds compensated for their mates' reduced parental effort by increasing offspring attendance and by increasing chick provisioning above average rates of control birds. Although partners of TDR-equipped birds fully compensated for their mates' reduced offspring attendance (i.e. chicks were never observed to be left unattended), total provisioning rates of pairs with a TDR-equipped bird ((X) over bar +/-SE=4.38+/-0.26 meals/day) were significantly lower than those of control pairs (5.74+/-0.31 meals/day). However, fledgling success of control and TDR-equipped birds did not differ between reproductive seasons. TDR-equipped birds also had a significantly lower rate of return to breed than their non-TDR-equipped partners or control birds, and those that did return the following season were more likely to change mates (32%) compared with controls (0%). Taken together, our results underline the need to quantify the effects of monitoring equipment used to measure seabirds' activities, and indicate the ability of female and male thick-billed murres to compensate for reduced partner effort due to handicapping-Compensator behaviour seems to be a necessary response of this single-brooded species to ensure current breeding success; however, it may affect the stability of pair bonds in some individuals. (C) 2004 The Association for the Study of Animal Behaviour. Published by Elsevier Ltd. All rights reserved. C1 Mem Univ Newfoundland, Dept Biol, St John, NF A1B 3X9, Canada. Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, Washington, DC 20008 USA. RP Paredes, R (reprint author), Mem Univ Newfoundland, Dept Biol, St John, NF A1B 3X9, Canada. EM u92rp@mun.ca NR 83 TC 76 Z9 79 U1 7 U2 42 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0003-3472 EI 1095-8282 J9 ANIM BEHAV JI Anim. Behav. PD JAN PY 2005 VL 69 BP 197 EP 208 DI 10.1016/j.anbehav.2003.12.029 PN 1 PG 12 WC Behavioral Sciences; Zoology SC Behavioral Sciences; Zoology GA 888RO UT WOS:000226392100022 ER PT J AU Steiner, WE AF Steiner, WE TI Two new species of three-horned Hypogena from Peru (Coleoptera : Tenebrionidae) SO ANNALES ZOOLOGICI LA English DT Article DE Coleoptera; Tenebrionidae; Hypogena; new species; Peru AB Two new distinctive species of the darkling beetle genus Hypogena Dejean (Coleoptera: Tenebrionidae) are described from unique males, H. triceratops sp. nov., and H. cat sp. nov. Both are named in honor of tenebrionid specialist Charles A. Triplehorn. Images of the holotypes are provided, with comparisons to other known three-horned species of the genus. Both specimens were collected at the Rio Tambopata Reserve, Madre de Dios, Peru. C1 Smithsonian Inst, Dept Entomol, Washington, DC 20560 USA. RP Steiner, WE (reprint author), Smithsonian Inst, Dept Entomol, NHB 187, Washington, DC 20560 USA. NR 4 TC 1 Z9 1 U1 0 U2 0 PU POLISH ACAD OF SCIENCES PI WARSAW PA MUSEUM & INST ZOOLOGY WILCZA 64, 00-679 WARSAW, POLAND SN 0003-4541 J9 ANN ZOOL JI Ann. Zool. PY 2005 VL 55 IS 4 BP 571 EP 574 PG 4 WC Entomology SC Entomology GA 009VE UT WOS:000235140700006 ER PT J AU Fessler, DMT Haley, KJ Lal, RD AF Fessler, DMT Haley, KJ Lal, RD TI Sexual dimorphism in foot length proportionate to stature SO ANNALS OF HUMAN BIOLOGY LA English DT Article DE foot length; stature; sexual dimorphism ID BLUNT ABDOMINAL-TRAUMA; PHYSICAL ATTRACTIVENESS; SHOE DESIGN; PREGNANCY; DIMENSIONS; EVOLUTION; SELECTION; HEIGHT; WOMEN; FOOTPRINTS AB Background: The preponderance of existing results suggests that, relative to stature, women have smaller feet than men. However, several investigations indicate that the relationship between foot length and stature may be curvilinear, a pattern that, due to the dimorphic nature of stature, would mask the true direction of pedal sexual dimorphism in published results. Aim: The study aimed to determine whether proportionate foot length is sexually dimorphic and, if so, the nature of that dimorphism. Materials and methods: Surveying genetically disparate populations ( USA, Turkey, and Native North and Central American), we examined data from three previous anthropometric studies ( Davis 1990, Parham et al. 1992, Ozaslan et al. 2003) and foot tracings from the Steggerda Collection at the US National Museum of Health and Medicine. Analyses explored sex differences in the ratio between foot length and stature, and tested for nonlinearity. Results: Although varying in degree across populations, proportionate to stature, female foot length is consistently smaller than male foot length. Conclusion: Given the biomechanical challenges posed by pregnancy, smaller female proportionate foot length is somewhat surprising, as foot length affects dorsoventral stability. It is possible that the observed pattern reflects intersexual selection for small female foot size, a cue of youth and nulliparity. C1 Univ Calif Los Angeles, Dept Anthropol, Los Angeles, CA 90095 USA. Univ Calif Los Angeles, Ctr Behav Evolut & Culture, Los Angeles, CA 90095 USA. NIH, Dewitt Stetten Jr Museum Med Res, Bethesda, MD 20892 USA. Smithsonian Ctr Educ & Museum Studies, Washington, DC 20013 USA. RP Fessler, DMT (reprint author), Univ Calif Los Angeles, Dept Anthropol, 341 haines hall, Los Angeles, CA 90095 USA. EM dfessler@anthro.ucla.edu RI Fessler, Daniel/G-8485-2012 NR 55 TC 48 Z9 48 U1 1 U2 6 PU INFORMA HEALTHCARE PI LONDON PA TELEPHONE HOUSE, 69-77 PAUL STREET, LONDON EC2A 4LQ, ENGLAND SN 0301-4460 J9 ANN HUM BIOL JI Ann. Hum. Biol. PD JAN-FEB PY 2005 VL 32 IS 1 BP 44 EP 59 DI 10.1080/03014460400027581 PG 16 WC Anthropology; Biology; Public, Environmental & Occupational Health SC Anthropology; Life Sciences & Biomedicine - Other Topics; Public, Environmental & Occupational Health GA 906WK UT WOS:000227675100005 PM 15788354 ER PT J AU Finot, VL Peterson, PM Zuloaga, FO Soreng, RJ Matthei, O AF Finot, VL Peterson, PM Zuloaga, FO Soreng, RJ Matthei, O TI A revision of Trisetum (Poaceae : Pooideae : Aveninae) in South America SO ANNALS OF THE MISSOURI BOTANICAL GARDEN LA English DT Article DE Aveninae; Gramineae; Poaceae; Pooideae; Trisetum AB A taxonomic treatment of Trisetum Pers. for South America, is given. Eighteen species and six varieties of Trisetum are recognized in South America. Chile (14 species, 3 varieties) and Argentina (12 species, 5 varieties) have the greatest number of taxa in the genus. Two varieties. T. barbinode var. selerophyllum and T. longiglume var. glabratum. are endemic to Argentina, whereas T. macbridei and T. nancaguense are known only from Chile. Trisetum andinum is endemic to Ecuador, T. macbridei is endemic to Peru. and T. foliosum is endemic to Venezuela. A total of four species are found in Ecuador and Peru, and there are two species in Venezuela and Colombia. The following new species are described and illustrated: Trisetum mattheii Finol and T. nancoguense Finot, from Chile, and T. pyramidatum Louis-described and illustrated: ex Finot. from Chile and Argentina. The following two flew combinations are made: T. barbinode var. Scerophyllum (Hack. ex Stuck.) Finot and T. spicatum var. cumingii (Nees ex Steud.) Finol. A key for distinguishing the species and varieties of Trisetum in South America is given. The names Koeleria cumingii Nees ex Steud., Trisetum sect. Anaulacoa Louis-Marie. Trisetum sect. Aulacoa Louis-Marie, Trisetum subg. Heterolytrum Louis-Marie, Trisetum subg. Isolytrum Louis-Marie, Trisetum subsect. Koeleriformia Louis-Marie, Trisetum subsect. Sphenopholidea Louis-Marie. Trisetum malacophyllum Steud., Triselum variabile E. Desv., and Trisetum variabile var. vilescens E. Desv. are lectolypified. C1 Univ Concepcion, Fac Agron, Chillan, Chile. Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, Washington, DC 20013 USA. Inst Bot Darwin, San Isidro, Argentina. RP Finot, VL (reprint author), Univ Concepcion, Fac Agron, Casilla 537, Chillan, Chile. EM vifinot@udec.cl; peterson@si.edu; fzuloaga@darwin.edu.ar; sorengr@si.edu NR 54 TC 6 Z9 14 U1 2 U2 2 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 2005 VL 92 IS 4 BP 533 EP 568 PG 36 WC Plant Sciences SC Plant Sciences GA 998LR UT WOS:000234320700003 ER PT J AU Marsden, BG AF Marsden, BG TI Sungrazing comets SO ANNUAL REVIEW OF ASTRONOMY AND ASTROPHYSICS SE Annual Review of Astronomy and Astrophysics LA English DT Review; Book Chapter DE Kreutz Group; Kracht Group; Marsden Group; Meyer Group; SOHO; sungrazer ID IKEYA-SEKI 1965F; PERIHELION PASSAGE; ORBITAL EVOLUTION; SOLAR; SUN; FRAGMENTATION; ORIGIN; SPECTRUM; TAILS; MODEL AB After centuries of speculation that the early records of observations of bright comets near the sun involved repeated returns of a single sungrazing object, there came in the 1880s the realization, first by Kirkwood, and then most notably by Kreutz, that the observations could be explained by the existence of a group of related comets that had separated from each other at some earlier perihelion passage. After the appearance of further bright sungrazers in the mid-twentieth century, attempts were made to understand the specific manner in which the various members of this Kreutz Group of comets had evolved from each other. Beginning in 1979, coronagraphic observations from space allowed the detection of numerous additional Kreutz members that were completely vaporized as they grazed the sun. Since 1996, the Solar and Heliospheric Observatory (SOHO) coronagraphs have revealed some 700 of these comets, giving rise to the thought that there is a constant stream of small members, much of the break-up having occurred instead near aphelion and even quite recently. Whereas consideration of break-up only near perihelion requires that the observed dispersion of the orbital parameters would take many millennia, recent calculations have shown that the evolution can be substantially sped up by allowing fragments to be rotationally spun off at heliocentric distances of many tens of AU. The SOHO observations have also allowed the recognition of three other substantial groups of sungrazing comets, as well as some pairs arriving only hours apart. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM bmarsden@cfa.harvard.edu NR 97 TC 30 Z9 30 U1 0 U2 6 PU ANNUAL REVIEWS PI PALO ALTO PA 4139 EL CAMINO WAY, PO BOX 10139, PALO ALTO, CA 94303-0139 USA SN 0066-4146 J9 ANNU REV ASTRON ASTR JI Annu. Rev. Astron. Astrophys. PY 2005 VL 43 BP 75 EP 102 DI 10.1146/annurev.astro.43.072103.150554 PG 28 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 972EZ UT WOS:000232438300004 ER PT S AU Mueller, UG Gerardo, NM Aanen, DK Six, DL Schultz, TR AF Mueller, UG Gerardo, NM Aanen, DK Six, DL Schultz, TR TI The evolution of agriculture in insects SO ANNUAL REVIEW OF ECOLOGY EVOLUTION AND SYSTEMATICS SE Annual Review of Ecology Evolution and Systematics LA English DT Review; Book Chapter DE attini; macrotermitinae; mutualism; symbiosis; xyleborini ID FUNGUS-GROWING ANTS; ATTA-SEXDENS-RUBROPILOSA; SYMBIOTIC FUNGI; AMBROSIA BEETLES; MICROBIAL INTERACTIONS; PHYLOGENETIC ANALYSIS; TRIPARTITE MUTUALISM; MULTILINE CULTIVARS; BIOLOGICAL-CONTROL; GENETIC-VARIATION AB Agriculture has evolved independently in three insect orders: once in ants, once in termites, and seven times in ambrosia beetles. Although these insect farmers are in some ways quite different from each other, in many more ways they are remarkably similar, suggesting convergent evolution. All propagate their cultivars as clonal monocultures within their nests and, in most cases, clonally across many farmer generations as well. Long-term clonal monoculture presents special problems for disease control, but insect farmers have evolved a combination of strategies to manage crop diseases: They (a) sequester their gardens from the environment; (b) monitor gardens intensively, controlling pathogens early in disease outbreaks; (c) occasionally access population-level reservoirs of genetically variable cultivars, even while propagating clonal monocultures across many farmer generations; and (d) manage, in addition to the primary cultivars, an array of "auxiliary" microbes providing disease suppression and other services. Rather than growing a single cultivar solely for nutrition, insect farmers appear to cultivate, and possibly "artificially select" for, integrated crop-microbe consortia. Indeed, crop domestication in the context of coevolving and codomesticated microbial consortia may explain the 50-million year old agricultural success of insect farmers. C1 Univ Texas, Sect Integrat Biol, Austin, TX 78712 USA. Smithsonian Trop Res Inst, Balboa, Panama. Univ Arizona, Dept Ecol & Evolutionary Biol, Tucson, AZ 85721 USA. Univ Copenhagen, Inst Biol, Dept Populat Biol, DK-2100 Copenhagen, Denmark. Univ Montana, Dept Ecosyst & Conservat Sci, Missoula, MT 59812 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20013 USA. RP Mueller, UG (reprint author), Univ Texas, Sect Integrat Biol, Austin, TX 78712 USA. EM umueller@mail.utexas.edu; ngerardo@email.arizona.edu; dkaanen@bi.ku.dk; diana.six@cfc.umt.edu; schultz@lab.si.edu NR 138 TC 218 Z9 223 U1 25 U2 143 PU ANNUAL REVIEWS PI PALO ALTO PA 4139 EL CAMINO WAY, PO BOX 10139, PALO ALTO, CA 94303-0139 USA SN 1543-592X BN 978-0-8243-1436-1 J9 ANNU REV ECOL EVOL S JI Annu. Rev. Ecol. Evol. Syst. PY 2005 VL 36 BP 563 EP 595 DI 10.1146/annurev.ecolsys.36.102003.152626 PG 37 WC Ecology; Evolutionary Biology SC Environmental Sciences & Ecology; Evolutionary Biology GA 003LY UT WOS:000234684900024 ER PT S AU Lewinsohn, TM Novotny, V Basset, Y AF Lewinsohn, TM Novotny, V Basset, Y TI Insects on plants: Diversity of herbivore assemblages revisited SO ANNUAL REVIEW OF ECOLOGY EVOLUTION AND SYSTEMATICS SE Annual Review of Ecology Evolution and Systematics LA English DT Review; Book Chapter DE herbivory; insect-plant interactions; tropical insects; local and regional richness; species diversity ID PAPUA-NEW-GUINEA; TROPICAL RAIN-FORESTS; SPECIES RICHNESS; PHYTOPHAGOUS INSECTS; HOST-PLANT; COMMUNITY ECOLOGY; GLOBAL PATTERNS; CLIMATE-CHANGE; DRY FOREST; FOOD-WEB AB The diversity and composition of herbivore assemblages was a favored theme for community ecology in the 1970s and culminated in 1984 with Insects on Plants by Strong, Lawton and Southwood. We scrutinize findings since then, considering analyses of country-wide insect-host catalogs, field studies of local herbivore communities, and comparative studies at different spatial scales. Studies in tropical forests have advanced significantly and offer new insights into stratification and host specialization of herbivores. Comparative and long-term data sets are still scarce, which limits assessment of general patterns in herbivore richness and assemblage structure. Methods of community phylogenetic analysis, complex networks, spatial and among-host diversity partitioning, and metacommunity models represent promising approaches for future work. C1 Univ Estadual Campinas, Inst Biol, Lab Interacoes Insetos Plantas, Campinas, Brazil. CAS, Inst Entomol, Prague, Czech Republic. Univ S Bohemia, Fac Biol, Ceske Budejovice, Czech Republic. Smithsonian Trop Res Inst, Balboa, Panama. RP Lewinsohn, TM (reprint author), Univ Estadual Campinas, Inst Biol, Lab Interacoes Insetos Plantas, Campinas, Brazil. EM thomasl@unicamp.br; novotny@entu.cas.cz; bassety@tivoli.si.edu RI Basset, Yves/B-6642-2014; Novotny, Vojtech/G-9434-2014; Lewinsohn, Thomas/D-5880-2012 OI Novotny, Vojtech/0000-0001-7918-8023; Lewinsohn, Thomas/0000-0001-5950-5343 NR 133 TC 132 Z9 140 U1 11 U2 101 PU ANNUAL REVIEWS PI PALO ALTO PA 4139 EL CAMINO WAY, PO BOX 10139, PALO ALTO, CA 94303-0139 USA SN 1543-592X BN 978-0-8243-1436-1 J9 ANNU REV ECOL EVOL S JI Annu. Rev. Ecol. Evol. Syst. PY 2005 VL 36 BP 597 EP 620 DI 10.1146/annurev.ecolsys.36.091704.175520 PG 24 WC Ecology; Evolutionary Biology SC Environmental Sciences & Ecology; Evolutionary Biology GA 003LY UT WOS:000234684900025 ER PT B AU Selinsky, P AF Selinsky, Page BE Kealhofer, L TI A PRELIMINARY REPORT ON THE HUMAN SKELETAL MATERIAL FROM GORDION'S LOWER TOWN AREA SO ARCHAEOLOGY OF MIDAS AND THE PHRYGIANS: RECENT WORK AT GORDION LA English DT Article; Book Chapter C1 [Selinsky, Page] Smithsonian Inst, Natl Museum Nat Hist, Collect Management Dept, Washington, DC 20560 USA. [Selinsky, Page] Smithsonian Inst, Natl Museum Nat Hist, Phys Anthropol Sect, Washington, DC 20560 USA. RP Selinsky, P (reprint author), Univ Penn, Philadelphia, PA 19104 USA. NR 0 TC 3 Z9 3 U1 0 U2 0 PU UNIV PENNSYLVANIA MUSEUM ARCHAEOLOGY & ANTHROPOLOGY PI PHILADELPHIA PA 3260 SOUTH STREET, PHILADELPHIA, PA 19104-6324 USA BN 978-1-931707-76-3 PY 2005 BP 117 EP 123 PG 7 WC Archaeology SC Archaeology GA BLF62 UT WOS:000270073500009 ER PT B AU Unruh, J Johnson, JS AF Unruh, Julie Johnson, Jessica S. BE Kealhofer, L TI RECENT CONSERVATION RESEARCH Soluble Salts in Gordion Ceramics SO ARCHAEOLOGY OF MIDAS AND THE PHRYGIANS: RECENT WORK AT GORDION LA English DT Article; Book Chapter C1 [Unruh, Julie] Smithsonian Inst, Conservat Labs, Washington, DC 20560 USA. [Unruh, Julie] Royal Ontario Museum, Conservat Labs, Toronto, ON, Canada. [Unruh, Julie] Brooklyn Museum Art, Conservat Labs, Brooklyn, NY USA. [Unruh, Julie] Agora Excavat Athens, Conservat Labs, Athens, Greece. RP Unruh, J (reprint author), Arizona State Museum, Tucson, AZ 85721 USA. NR 0 TC 1 Z9 1 U1 0 U2 0 PU UNIV PENNSYLVANIA MUSEUM ARCHAEOLOGY & ANTHROPOLOGY PI PHILADELPHIA PA 3260 SOUTH STREET, PHILADELPHIA, PA 19104-6324 USA BN 978-1-931707-76-3 PY 2005 BP 204 EP 214 PG 11 WC Archaeology SC Archaeology GA BLF62 UT WOS:000270073500016 ER PT B AU Mamajek, EE AF Mamajek, EE BE Seidelmann, PK Monet, AKB TI Proper motions as an underutilized tool for estimating distances and ages for nearby, young stars SO ASTROMETRY IN THE AGE OF THE NEXT GENERATION OF LARGE TELESCOPES SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT Meeting of Astrometry in the Age of the Next Generation of Large Telescopes CY OCT 18-20, 2004 CL Lowell Observ, Flagstaff, AZ HO Lowell Observ ID MAIN-SEQUENCE STARS; OB ASSOCIATION AB The recent availability of accurate proper motion catalogs for millions of stars on the sky (e.g. Tycho-2, UCAC) can benefit projects for which age estimates are needed for stars that are plausibly young (< 100 Myr) and within a few hundred pc of the Sun. Here I summarize how accurate proper motions have been useful in (1) identifying new, nearby, post-T Tauri star populations, and (2) estimating distances to young field stars which are lacking trigonometric parallax measurements. The later enables the calculation of stellar luminosities and isochronal ages - two critical quantities for investigations of the evolution of star/planet/disk systems. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Mamajek, EE (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-42, Cambridge, MA 02138 USA. NR 16 TC 1 Z9 1 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-205-9 J9 ASTR SOC P PY 2005 VL 338 BP 280 EP 283 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BDJ24 UT WOS:000233747900042 ER PT B AU Primini, F Noble, M AF Primini, F Noble, M CA CXC Sci Data Syst Grp BE Shopbell, PL Briton, MC Ebert, R TI Extending the capabilities of CIAO with S-Lang-based tools SO Astronomical Data Analysis Software and Systems XIV, Proceedings SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 14th Annual Conference for Astronomical Data Analysis Software and Systems CY OCT 24-27, 2004 CL Calif Inst Technol, Pasadena, CA HO Calif Inst Technol AB We demonstrate a number of tools that extend the capabilities of the Chandra X-Ray Center's data analysis software system CIAO(3). These tools were developed using S-Lang(4), an interpreted language and multi-platform programmer's library that may be easily embedded into other applications. The S-Lang interpreter's C-like syntax and sophisticated vector and array manipulation capabilities allow rapid development by scientists of programs that meet their individual analysis needs. C1 Harvard Smithsonian Ctr Astrophys, Chandra Xray Ctr, Cambridge, MA 02138 USA. RP Primini, F (reprint author), Harvard Smithsonian Ctr Astrophys, Chandra Xray Ctr, 60 Garden St, Cambridge, MA 02138 USA. NR 2 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 1-58381-215-6 J9 ASTR SOC P PY 2005 VL 347 BP 17 EP 21 PG 5 WC Astronomy & Astrophysics; Computer Science, Information Systems; Computer Science, Interdisciplinary Applications SC Astronomy & Astrophysics; Computer Science GA BEE16 UT WOS:000236909500004 ER PT B AU Burke, DJ Siemiginowska, A Doe, S Nguyen, D AF Burke, DJ Siemiginowska, A Doe, S Nguyen, D BE Shopbell, PL Briton, MC Ebert, R TI Extending and enhancing the capabilities of the Sherpa modeling and fitting tool with S-Lang SO Astronomical Data Analysis Software and Systems XIV, Proceedings SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 14th Annual Conference for Astronomical Data Analysis Software and Systems CY OCT 24-27, 2004 CL Calif Inst Technol, Pasadena, CA HO Calif Inst Technol AB Sherpa is the fitting and modeling tool of the Chandra Interactive Analysis of Observations (CIAO(1)) package. It is designed to allow users to fit the 1D (e.g., spectra, luminosity functions) and 2D datasets (e.g., images) obtained from the Chandra X-ray Observatory(2) and other telescopes. The S-Lang programming language has been embedded into CIAO, which allows users the ability to access numerical data calculated by Sherpa. We present two examples of how S-Lang has been used to enhance and extend Sherpa's capabilities. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Burke, DJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 5 TC 2 Z9 2 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-215-6 J9 ASTR SOC P PY 2005 VL 347 BP 105 EP 109 PG 5 WC Astronomy & Astrophysics; Computer Science, Information Systems; Computer Science, Interdisciplinary Applications SC Astronomy & Astrophysics; Computer Science GA BEE16 UT WOS:000236909500019 ER PT B AU Joye, WA Mandel, E AF Joye, WA Mandel, E BE Shopbell, PL Briton, MC Ebert, R TI The development of SAOImage DS9: Lessons learned from a small but successful software project SO Astronomical Data Analysis Software and Systems XIV, Proceedings SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 14th Annual Conference for Astronomical Data Analysis Software and Systems CY OCT 24-27, 2004 CL Calif Inst Technol, Pasadena, CA HO Calif Inst Technol AB We present a discussion of lessons learned during the development of SAOImage DS9. Starting with general observations on scientific software development, we discuss our design and implementation cycle, allocation of effort and resources, keys to our success, overall strategies that have worked well (and those that have not), and future challenges. We hope our experience will be of use to other small software development projects. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Joye, WA (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. NR 2 TC 4 Z9 4 U1 0 U2 1 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-215-6 J9 ASTR SOC P PY 2005 VL 347 BP 110 EP 113 PG 4 WC Astronomy & Astrophysics; Computer Science, Information Systems; Computer Science, Interdisciplinary Applications SC Astronomy & Astrophysics; Computer Science GA BEE16 UT WOS:000236909500020 ER PT B AU Mink, DJ Wyatt, WF Roll, JB Tokarz, SP Conroy, MA Caldwell, N Kurtz, MJ Geller, MJ AF Mink, DJ Wyatt, WF Roll, JB Tokarz, SP Conroy, MA Caldwell, N Kurtz, MJ Geller, MJ BE Shopbell, PL Briton, MC Ebert, R TI Creating data that never die: Building a spectrograph data pipeline in the virtual observatory era SO Astronomical Data Analysis Software and Systems XIV, Proceedings SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 14th Annual Conference for Astronomical Data Analysis Software and Systems CY OCT 24-27, 2004 CL Calif Inst Technol, Pasadena, CA HO Calif Inst Technol AB Data pipelines for modern complex astronomical instruments do not begin when the data is taken and end when it is delivered to the user. Information must flow between the observatory and the observer from the time a project is conceived and between the observatory and the world well past the time when the original observers have extracted all the information they want from the data. For the 300-fiber Hectospec low dispersion spectrograph on the MMT, the SAO Telescope Data Center is constructing a data pipeline which provides assistance from preparing and submitting observing proposals through observation, reduction, and analysis to publication and an afterlife in the Virtual Observatory. We will describe our semi-automatic pipeline and how it has evolved over the first nine months of operation. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Mink, DJ (reprint author), Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RI KURTZ, Michael /B-3890-2009 NR 7 TC 4 Z9 4 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-215-6 J9 ASTR SOC P PY 2005 VL 347 BP 228 EP 232 PG 5 WC Astronomy & Astrophysics; Computer Science, Information Systems; Computer Science, Interdisciplinary Applications SC Astronomy & Astrophysics; Computer Science GA BEE16 UT WOS:000236909500043 ER PT B AU Blecksmith, S Bright, J Rots, AH Winkelman, S Green, P Yukita, M AF Blecksmith, S Bright, J Rots, AH Winkelman, S Green, P Yukita, M BE Shopbell, PL Briton, MC Ebert, R TI The Chandra bibliography database: Bibliographic statistics SO Astronomical Data Analysis Software and Systems XIV, Proceedings SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 14th Annual Conference for Astronomical Data Analysis Software and Systems CY OCT 24-27, 2004 CL Calif Inst Technol, Pasadena, CA HO Calif Inst Technol AB We have started to generate and catalog bibliographic statistics for the Chandra mission. As a result, the databases associated with the Chandra bibliography continue to expand in scope and purpose. Publication data, including number of citations, are collected for each Chandra proposal and stored in the bibliography database. Scientific metrics based on these data are computed monthly and stored in the metrics database for trending analysis of publication statistics. The design of the system and some results for illustration are presented. In addition, we have discovered some unexpected operational uses for the bibliographic database which will also be discussed. C1 Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, Chandra Xray Ctr, Cambridge, MA 02138 USA. RP Blecksmith, S (reprint author), Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, Chandra Xray Ctr, 60 Garden St, Cambridge, MA 02138 USA. RI Yukita, Mihoko/E-4135-2017 NR 0 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-215-6 J9 ASTR SOC P PY 2005 VL 347 BP 380 EP 384 PG 5 WC Astronomy & Astrophysics; Computer Science, Information Systems; Computer Science, Interdisciplinary Applications SC Astronomy & Astrophysics; Computer Science GA BEE16 UT WOS:000236909500074 ER PT B AU Galle, EC Burke, DJ Stawarz, C Fruscione, A AF Galle, EC Burke, DJ Stawarz, C Fruscione, A BE Shopbell, PL Briton, MC Ebert, R TI The CIAO website unveiled SO Astronomical Data Analysis Software and Systems XIV, Proceedings SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 14th Annual Conference for Astronomical Data Analysis Software and Systems CY OCT 24-27, 2004 CL Calif Inst Technol, Pasadena, CA HO Calif Inst Technol AB The Chandra Interactive Analysis of Observations (CIAO) website is the primary resource for users of the CIAO software package. Several hundred pages of content are written in XML, allowing for a baseline set of text from which many types of documentation may be created. Development and production (i.e., public) HTML versions of the site are generated from the XML via conversion scripts and XSL stylesheets. We present an overview of the back-end of the CIAO website, including custom markup tags; stylesheets, and CSS. The success of the project led to the use of this system in maintaining five websites at the Chandra X-ray Center (CXC). C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Galle, EC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 0 TC 1 Z9 1 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-215-6 J9 ASTR SOC P PY 2005 VL 347 BP 473 EP 477 PG 5 WC Astronomy & Astrophysics; Computer Science, Information Systems; Computer Science, Interdisciplinary Applications SC Astronomy & Astrophysics; Computer Science GA BEE16 UT WOS:000236909500092 ER PT B AU McCollough, ML Rots, AH AF McCollough, ML Rots, AH BE Shopbell, PL Briton, MC Ebert, R TI The impact of the ACIS readout streak and pileup on Chandra Source detection SO Astronomical Data Analysis Software and Systems XIV, Proceedings SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 14th Annual Conference for Astronomical Data Analysis Software and Systems CY OCT 24-27, 2004 CL Calif Inst Technol, Pasadena, CA HO Calif Inst Technol AB As part of the development of the Chandra Level 3 (L3) data products (Chandra Source catalog) the impacts of the ACIS Readout Streak and Pileup have been examined. A method has been developed which allows us to determine, for a given observation, which columns of the ACIS CCDs are impacted by Readout Streaks, resulting in the detection of false sources. A discussion is given of how to use this information to prevent false detections and how to identify and determine the characteristics of real sources located in the Readout Streak. The implications of this for the creation of L3 products are discussed. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP McCollough, ML (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. NR 1 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 1-58381-215-6 J9 ASTR SOC P PY 2005 VL 347 BP 478 EP 482 PG 5 WC Astronomy & Astrophysics; Computer Science, Information Systems; Computer Science, Interdisciplinary Applications SC Astronomy & Astrophysics; Computer Science GA BEE16 UT WOS:000236909500093 ER PT B AU Phelps, MWL AF Phelps, MWL BE Shopbell, PL Briton, MC Ebert, R TI Building a general purpose Beowulf cluster for astrophysics research SO Astronomical Data Analysis Software and Systems XIV, Proceedings SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 14th Annual Conference for Astronomical Data Analysis Software and Systems CY OCT 24-27, 2004 CL Calif Inst Technol, Pasadena, CA HO Calif Inst Technol AB The challenges of designing and deploying a high performance, Linux based, Beowulf cluster for use by many departments and projects are covered. Considerations include hardware, infrastructure (space, cooling, networking, etc.), and software; particularly scheduling systems. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Phelps, MWL (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-215-6 J9 ASTR SOC P PY 2005 VL 347 BP 548 EP 549 PG 2 WC Astronomy & Astrophysics; Computer Science, Information Systems; Computer Science, Interdisciplinary Applications SC Astronomy & Astrophysics; Computer Science GA BEE16 UT WOS:000236909500107 ER PT J AU Wu, Y Zhang, Q Chen, H Yang, C Wei, Y Ho, PTP AF Wu, Y Zhang, Q Chen, H Yang, C Wei, Y Ho, PTP TI CO J=2-1 maps of bipolar outflows in massive star-forming regions SO ASTRONOMICAL JOURNAL LA English DT Article DE ISM : jets and outflows; ISM : kinematics and dynamics; ISM : molecules; masers; stars : formation ID YOUNG STELLAR OBJECTS; HERBIG-HARO OBJECTS; HIGH-VELOCITY GAS; H-II-REGIONS; MOLECULAR LINE EMISSION; H2O MASER; HIGH-RESOLUTION; HII-REGIONS; CEPHEUS-A; CONTINUUM EMISSION AB Using the eight-beam array receiver of the NRAO 12 m telescope, we mapped the CO = J 2-1 emission toward 11 high-mass star-forming regions. In the sample, four are previously detected outflows in the CO = J 1-0 line, and seven are outflow candidates. A total of six bipolar outflows were identified in the CO = J 2-1 line. For the remaining five sources, including one previously detected bipolar outflow, the CO = J 2-1 emission shows multiple velocity components. Therefore, high-velocity line wings or bipolar structure cannot be identified. The CO = J 2-1 spectra of the four of the nonbipolar outflow sources exhibit broad-line emission due to the blending of weak velocity components. The complex CO spectra underscore the importance of large-scale mapping in identifying outflows. Compared with the outflows detected with the CO = J 1-0 line, the CO = J 2-1 outflows often have broader line wings and smaller spatial extents, indicating that the high-velocity gas measured with the CO = J 2-1 line arises from warm regions closer to the central source. The masses in the outflows range from a few to 60 M(circle dot). The linear momenta in the outflows are as large as a few hundred M(circle dot)km s(-1). Both parameters are much larger than the typical values in low-mass outflows. The average dynamic timescale of the outflows is 2 x 10(4) yr. The driving sources of the bipolar outflows are also identified. All bipolar outflows detected have a near-infrared source, except for IRAS 23385+6053, and all are associated with centimeter or millimeter continuum emission, except for IRAS 22506+5549. We investigated the correlation between the outflow parameters and the properties of the driving source. The outflow luminosity and mechanical force correlate with the bolometric luminosity of the star. However, the mechanical force required to drive a CO outflow is more than an order of magnitude higher than the radiation pressure from the star. We reexamined the relation between the mass entrainment rate of the outflows and the bolometric luminosity of the central source with an up-to-date sample. Results show that the mass outflow rate increases with increasing bolometric luminosity, suggesting that the mass outflow rate is related to the luminosity of the central source. C1 Peking Univ, CAS PKU Joint Beijing Astrophys Ctr, Dept Astron, Beijing 100871, Peoples R China. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Arizona, Dept Astron, Tucson, AZ 85721 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Columbia Univ, Dept Astron, New York, NY 10027 USA. RP Wu, Y (reprint author), Peking Univ, CAS PKU Joint Beijing Astrophys Ctr, Dept Astron, Beijing 100871, Peoples R China. EM yfwu@bac.pku.edu.cn; qzhang@cfa.harvard.edu; hua_chen@net.com; cyyang@astro.columbia.edu OI Zhang, Qizhou/0000-0003-2384-6589 NR 80 TC 30 Z9 31 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 JAN PY 2005 VL 129 IS 1 BP 330 EP 347 DI 10.1086/426361 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 885BK UT WOS:000226130800023 ER PT J AU Sicilia-Aguilar, A Hartmann, LW Szentgyorgyi, AH Fabricant, DG Furesz, G Roll, J Conroy, MA Calvet, N Tokarz, S Hernandez, J AF Sicilia-Aguilar, A Hartmann, LW Szentgyorgyi, AH Fabricant, DG Furesz, G Roll, J Conroy, MA Calvet, N Tokarz, S Hernandez, J TI Accretion, kinematics, and rotation in the Orion Nebula cluster: Initial results from Hectochelle SO ASTRONOMICAL JOURNAL LA English DT Article DE accretion, accretion disks; line : profiles; stars : pre-main-sequence; stars : rotation ID T-TAURI STARS; EMISSION-LINE DIAGNOSTICS; MAIN-SEQUENCE STARS; HERBIG-HARO OBJECTS; LOW-MASS STARS; MAGNETOSPHERIC ACCRETION; CIRCUMSTELLAR DISKS; TRAPEZIUM CLUSTER; CONVERTED MMT; YOUNG CLUSTERS AB We present results from high-resolution spectra of 237 stars in the Orion Nebula cluster ( ONC) obtained during two engineering runs with the Hectochelle multifiber echelle spectrograph on the 6.5 m MMT. The ONC is the nearest populous young (age similar to1 Myr) cluster and is therefore an important object for studies of the evolution of protoplanetary disks. Using the high spectral resolution of Hectochelle, we are able to distinguish stellar accretion and wind emission-line profiles from nebular emission lines and identify accreting members of the cluster from Halpha profiles with greater accuracy than previously possible. We find 15 new members on the basis of Li lambda6707 absorption and Halpha emission. Line profiles of Halpha of some objects that are not too contaminated by nebular emission show features characteristic of mass inflow and ejection. We also present rotational velocities as part of an initial investigation into angular momentum evolution of very young stars, confirming a difference between classical T Tauri stars and weak-line T Tauri stars that had been found from period analysis. Finally, we present an initial study of the radial velocity dispersion of the brighter stars in the central cluster. The very small dispersion derived, less than or equal to1.8 km s(-1), is in good agreement with estimates from proper motions. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Hungarian Acad Sci, Konkoly Observ, H-1525 Budapest, Hungary. Univ Szeged, Dept Expt Phys, H-6723 Szeged, Hungary. Univ Los Andes, Merida 5101A, Venezuela. Ctr Invest Astron, Merida 5101A, Venezuela. RP Sicilia-Aguilar, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM asicilia@cfa.harvard.edu NR 53 TC 53 Z9 54 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 2005 VL 129 IS 1 BP 363 EP 381 DI 10.1086/426327 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 885BK UT WOS:000226130800026 ER PT J AU Carney, BW Latham, DW Laird, JB AF Carney, BW Latham, DW Laird, JB TI Metal-poor field blue stragglers: More evidence for mass transfer SO ASTRONOMICAL JOURNAL LA English DT Article DE binaries : spectroscopic; blue stragglers; Galaxy : halo ID PROPER-MOTION STARS; SUBGIANT CH-STARS; 40 SPECTROSCOPIC BINARIES; GLOBULAR-CLUSTER M3; MAIN-SEQUENCE STARS; HIGH-VELOCITY STARS; LONG-LIVED STARS; SOLAR-TYPE STARS; HALO-STARS; LITHIUM ABUNDANCE AB We report radial velocity studies of five candidate metal-poor field blue stragglers, all known to be deficient in lithium. Four of the five stars are single-lined spectroscopic binaries, with periods ranging from 302 to 840 days, and low orbital eccentricities, in agreement with similar behavior found for other blue straggler candidates by Preston & Sneden and Carney et al. The limited data available for lithium abundances indicate that all blue straggler binaries have depleted lithium, but that constant velocity stars generally have normal lithium abundances. This suggests that the "lithium gap'' for hot metal-poor main-sequence stars may not exist or lies at higher temperatures than found in the Hyades. Our results and those of Preston & Sneden show higher values of v(rot) sin i for the binary stars than those of comparable temperature constant velocity stars. The orbital periods are too long for tidal effects to be important, implying that spin-up during mass transfer when the orbital separations and periods were smaller is the cause of the enhanced rotation. The mass function distribution is steeper for the blue straggler binary stars than that of lower mass single-lined spectroscopic binaries, indicating a narrower range in secondary masses. We argue that if all secondaries are white dwarfs with the same mass, it is probably around 0.55 M-circle dot. The models of Rappaport et al., applied to white dwarf secondaries, suggest that the orbital elements of all metal-poor binary blue stragglers are consistent with stable mass transfer, with the possible exception of G202-65. C1 Univ N Carolina, Dept Phys & Astron, Chapel Hill, NC 27599 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Bowling Green State Univ, Dept Phys & Astron, Bowling Green, OH 43403 USA. RP Carney, BW (reprint author), Univ N Carolina, Dept Phys & Astron, Chapel Hill, NC 27599 USA. EM bruce@physics.unc.edu; dlatham@cfa.harvard.edu; laird@tycho.bgsu.edu NR 70 TC 45 Z9 46 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD JAN PY 2005 VL 129 IS 1 BP 466 EP 479 DI 10.1086/426566 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 885BK UT WOS:000226130800034 ER PT B AU Rao, R Marrone, DP AF Rao, R. Marrone, D. P. BE Adamson, A Aspin, C Davis, CJ Fujiyoshi, T TI Polarization with the submillimeter array (SMA) SO Astronomical Polarimetry: Current Status and Future Directions SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Meeting on Astronomical Polarimetry - Current Status and Future Directions CY MAR 15-19, 2004 CL Waikoloa, HI ID UNDERSTANDING RADIO POLARIMETRY AB Polarimetry at far-infrared, submillimeter and millimeter wavelengths is an important probe of the magnetic field structure in astronomical sources. Most previous polarization observations have been conducted with single dish telescopes which have limited angular resolution (greater than 10"). Interferometer arrays can provide higher angular resolution (about 1"), but current arrays can only make polarization observations at frequencies up to 230 GHz. We present here the details of a proposed 345 GHz polarimetry system for the Submillimeter Array, an 8-element interferometer on Mauna Kea. This system will provide the first submillimeter polarization images at high angular resolution. Initial results from full-system tests in April and May 2004 are reported. Scientific observations have also begun and should expand over the remainder of the Year. In the future the Submillimeter Array will be upgraded with dual polarization capable receivers and thus become a powerful instrument for mapping the magnetic field structure. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Rao, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 5 TC 2 Z9 2 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-210-5 J9 ASTR SOC P PY 2005 VL 343 BP 59 EP 63 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BEI32 UT WOS:000237315100009 ER PT B AU Shinnaga, H Moran, JM Young, KH Ho, PTP AF Shinnaga, Hiroko Moran, James M. Young, Ken H. Ho, Paul T. P. BE Adamson, A Aspin, C Davis, CJ Fujiyoshi, T TI Interferometric observations of the SiO high J transition maser associated with VY Canis Majoris with the Submillimeter Array SO Astronomical Polarimetry: Current Status and Future Directions SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Meeting on Astronomical Polarimetry - Current Status and Future Directions CY MAR 15-19, 2004 CL Waikoloa, HI ID ASTROPHYSICAL MASERS; STARS; SUPERGIANTS AB We imaged the SiO maser emission of J = 5 - 4 in the v = 1 state associated with the peculiar red supergiant VY Canis Majoris using the partially completed Submillimeter Array. We identified seven maser components and measured the relative positions at sub-arcsecond scale in the high J transition for the first time. We have also measured the polarization of these maser components. The strongest maser feature has a linear polarization of similar to 60%, and its direction of polarization is approximately aligned with the bipolar axis. Such a high degree of polarization suggests that radiative pumping is probably responsible for the maser inversion. Five of the other maser features have significant linear polarization. C1 Harvard Smithsonian Ctr Astrophys, Hilo, HI 96720 USA. RP Shinnaga, H (reprint author), Harvard Smithsonian Ctr Astrophys, 645 N Aohoku Pl,Univ Pk, Hilo, HI 96720 USA. NR 15 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 1-58381-210-5 J9 ASTR SOC P PY 2005 VL 343 BP 265 EP 269 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BEI32 UT WOS:000237315100058 ER PT J AU Green, DWE AF Green, DWE TI A new look at the position of the 1604 Supernova (V843 Ophiuchi) SO ASTRONOMISCHE NACHRICHTEN LA English DT Article DE supemovae : individual (V843 Oph); astrometry; supemova remnants; methods : data analysis; history and philosophy of astronomy ID KEPLERS SUPERNOVA; REMNANT AB The position of the supemova of 1604 (V843 Oph) is re-assessed, with relevant discussion pertaining to the present-day remnant, 3C 358. C1 Univ Durham, Dept Phys, Durham, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Green, DWE (reprint author), Univ Durham, Dept Phys, Durham, England. EM dgreen@cfa.harvard.edu NR 49 TC 1 Z9 1 U1 0 U2 1 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA PO BOX 10 11 61, D-69451 WEINHEIM, GERMANY SN 0004-6337 J9 ASTRON NACHR JI Astro. Nachr. PY 2005 VL 326 IS 2 BP 101 EP 111 DI 10.1002/asna.200410345 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 903FK UT WOS:000227410800003 ER PT J AU Covey, KR Greene, TP Doppmann, GW Lada, CJ Wilking, BA AF Covey, KR Greene, TP Doppmann, GW Lada, CJ Wilking, BA TI Searching for proto-brown dwarfs: Extending near IR spectroscopy of protostars below the hydrogen burning limit SO ASTRONOMISCHE NACHRICHTEN LA English DT Article; Proceedings Paper CT Ultralow-Mass Star Formation and Evolution Workshop CY JUN 28-JUL 01, 2005 CL La Palma, SPAIN DE stars : formation; stars : low-mass, brown dwarfs; stars : pre-main sequence; stars : rotation ID INITIAL MASS FUNCTION; NEAR-INFRARED SPECTRA; TAURUS-AURIGA; T-TAURI; K-BAND; STARS; LUMINOSITY; ACCRETION; CLUSTER; OBJECTS AB Recent observations of nearby star forming regions have offered evidence that young brown dwarfs undergo a period of mass accretion analogous to the T Tauri phase observed in young stars. Brown dwarf analogs to stellar protostars, however, have yet to be definitively observed. These young, accreting objects would shed light on the nature of the dominant brown dwarf formation process, as well as provide ideal laboratories to investigate the dependence of the accretion mechanism on protostellar mass. Recent near infrared surveys have identified candidate proto-brown dwarfs and characterized low mass protostars in nearby star forming regions. These techniques allow near infrared spectra to diagnose the effective temperature, accretion luminosity, magnetic field strength and rotation velocity of young low mass stars across the stellar/substellar boundary. The lowest mass proto-brown dwarfs (M<40 M-Jup), however, will prove challenging to observe given current near IR observational capabilities. C1 Univ Washington, Dept Astron, Seattle, WA 98195 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Assoc Univ Res Astron Inc, So Operat Ctr, Gemini Observ, La Serena, Chile. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Missouri, Dept Phys & Astron, St Louis, MO 63121 USA. RP Covey, KR (reprint author), Univ Washington, Dept Astron, Box 351580, Seattle, WA 98195 USA. EM covey@astro.washington.edu OI Covey, Kevin/0000-0001-6914-7797 NR 33 TC 0 Z9 0 U1 0 U2 1 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA PO BOX 10 11 61, D-69451 WEINHEIM, GERMANY SN 0004-6337 J9 ASTRON NACHR JI Astro. Nachr. PY 2005 VL 326 IS 10 BP 886 EP 890 DI 10.1002/asna.200510462 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 000AT UT WOS:000234434000005 ER PT J AU Mohanty, S Basri, G Jayawardhana, R AF Mohanty, S Basri, G Jayawardhana, R TI Accretion in brown dwarfs down to nearly planetary masses SO ASTRONOMISCHE NACHRICHTEN LA English DT Article; Proceedings Paper CT Ultralow-Mass Star Formation and Evolution Workshop CY JUN 28-JUL 01, 2005 CL La Palma, SPAIN DE stars : low-mass, brown dwarfs; stars : formation ID T-TAURI PHASE; DISK ACCRETION; STARS; OBJECTS AB We show that in accreting ultra low-mass stars and brown dwarfs, the CaII lambda 8662 emission line flux correlates remarkably well with the mass accretion rate (M), just as it does in higher mass classical T Thuri stars (CTTs). A straightforward measurement of the CaII flux thus provides an easier M determination technique than detailed modeling of the H alpha emission line profile (except at the very lowest accretion rates, where CaII does not appear to be in emission for ultra low-mass objects, and H alpha modeling is required). Using optical high-resolution spectra, we infer M from CaII emission for young ultra low-mass objects down to nearly the deuterium-burning (planetary-mass) limit. Our results, in combination with previous determinations of M in CTTs, illustrate that the accretion rate declines steeply with mass, roughly as M proportional to M-*(2) (albeit with considerable scatter). A similar relationship has been suggested by previous studies; we extend it down to nearly the planetary regime. The physical reason for this phenomenon is not yet clear; we discuss various possible mechanisms. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H8, Canada. RP Mohanty, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM smohanty@cfa.harvard.edu NR 12 TC 8 Z9 8 U1 0 U2 1 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA PO BOX 10 11 61, D-69451 WEINHEIM, GERMANY SN 0004-6337 J9 ASTRON NACHR JI Astro. Nachr. PY 2005 VL 326 IS 10 BP 891 EP 894 DI 10.1002/asna.200510450 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 000AT UT WOS:000234434000006 ER PT J AU Jones, HRA Viti, S Tennyson, J Barber, B Harris, G Pickering, JC Blackwell-Whitehead, R Champion, JP Allard, F Hauschildt, PH Jorgensen, UG Ehrenfreund, P Stachowska, E Ludwig, HG Martin, EL Pavlenko, Y Lyubchik, Y Kurucz, RL AF Jones, HRA Viti, S Tennyson, J Barber, B Harris, G Pickering, JC Blackwell-Whitehead, R Champion, JP Allard, F Hauschildt, PH Jorgensen, UG Ehrenfreund, P Stachowska, E Ludwig, HG Martin, EL Pavlenko, Y Lyubchik, Y Kurucz, RL TI Status of the physics of substellar objects project SO ASTRONOMISCHE NACHRICHTEN LA English DT Article; Proceedings Paper CT Ultralow-Mass Star Formation and Evolution Workshop CY JUN 28-JUL 01, 2005 CL La Palma, SPAIN DE stars : structure; planets : extrasolar ID BROWN DWARF; NEUTRAL MANGANESE; MODEL ATMOSPHERES; LINE LIST; LOW-MASS; STARS; SPECTRA; METALLICITY; DISCOVERY; COMPANION AB A full understanding of the properties of substellar objects is one of the major challenges facing astrophysics. Since their discovery in 1995, hundreds of brown dwarfs and extrasolar planets have been discovered. While these discoveries have enabled important comparisons with theory, observational progress has been much more rapid than the theoretical understanding of cool atmospheres. The reliable determination of mass, abundances, gravities and temperatures is not yet possible. The key problem is that substellar objects emit their observable radiation in the infrared region of the spectrum where our knowledge of atomic, molecular and line broadening data is poor. Here we report on the status of our PoSSO (Physics of SubStellar Objects) project. In order to understand brown dwarfs and extrasolar planets increasing more like those in our solar system, we are studying a wide range of processes. Here we give an update on the project and sketch an outline of atoms, molecules and processes requiring study. C1 Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. UCL, Dept Phys & Astron, London WC1E 6BT, England. Univ London Imperial Coll Sci Technol & Med, Blackett Lab, London, England. Univ Bourgogne, Phys Lab, Dijon, France. Ctr Rech Astron Lyon, Lyon, France. Hamburger Sternwarte, Hamburg, Germany. Niels Bohr Inst, DK-2100 Copenhagen, Denmark. Univ Amsterdam, Amsterdam, Netherlands. Poznan Univ Tech, Poznan, Poland. Lund Observ, S-22100 Lund, Sweden. Inst Astrofis Canarias, Tenerife, Spain. Ukrainian Acad Sci, Main Astron Observ, UA-252127 Kiev, Ukraine. Harvard Smithsonian Ctr Astrophys, Ctr Astrophys, Cambridge, MA USA. RP Jones, HRA (reprint author), Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. EM hraj@star.herts.ac.uk RI Champion, Jean-Paul/C-3963-2009; Pavlenko, Yakiv/D-7457-2011; Tennyson, Jonathan/I-2222-2012; Stachowska, Ewa/H-9792-2014 OI Pavlenko, Yakiv/0000-0002-7615-4028; Tennyson, Jonathan/0000-0002-4994-5238; NR 29 TC 8 Z9 8 U1 3 U2 8 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA BOSCHSTRASSE 12, D-69469 WEINHEIM, GERMANY SN 0004-6337 J9 ASTRON NACHR JI Astro. Nachr. PY 2005 VL 326 IS 10 BP 920 EP 924 DI 10.1002/asna.200510463 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 000AT UT WOS:000234434000012 ER PT J AU Zhang, YY Bohringer, H Mellier, Y Soucail, G Forman, A AF Zhang, YY Bohringer, H Mellier, Y Soucail, G Forman, A TI XMM-Newton study of the lensing cluster of galaxies CL 0024+17 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies : clusters : individual : CL 0024+17; cosmology : dark matter; gravitational lensing; cosmology : observations; X-rays : galaxies : clusters ID X-RAY-CLUSTERS; FIELD SPECTROSCOPIC SURVEY; MASS-TEMPERATURE RELATION; HUBBLE-SPACE-TELESCOPE; DISTANT CLUSTERS; NEARBY CLUSTERS; T RELATION; SCALING PROJECT; DENSITY PROFILE; CL 0024+1654 AB We present a detailed gravitational mass measurement based on the XMM-Newton imaging spectroscopy analysis of the lensing cluster of galaxies CL 0024+ 17 at z = 0.395. The emission appears approximately symmetric. However, on the scale of r similar to 3.3' some indication of elongation is visible in the northwest-southeast (NW-SE) direction from the hardness ratio map (HRM). Within 3', we measure a global gas temperature of 3.52 +/- 0.17 keV, metallicity of 0.22 +/- 0.07, and bolometric luminosity of 2.9 +/- 0.1 x 10(44) h(70)(-2) erg s(-1). We derive a temperature distribution with an isothermal temperature of 3.9 keV to a radius of 1.5' and a temperature gradient in the outskirts (1.3' < r < 3'). Under the assumption of hydrostatic equilibrium, we measure gravitational mass and gas mass fraction to be M-200 = 2.0 +/- 0.3 x 10(14) h(70)(- 1) M-. and f(gas) = 0.20 +/- 0.03 h(70)(-3/2) at r(200) = 1.05 h(70)(-1) Mpc using the observed temperature profile. The complex structure in the core region is the key to explaining the discrepancy in gravitational mass determined from XMM-Newton X-ray observations and HST optical lensing measurements. C1 Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. Inst Astrophys, F-75014 Paris, France. Observ Midi Pyrenees, Astrophys Lab, MR 5572, F-31400 Toulouse, France. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Max Planck Inst Extraterr Phys, Giessenbachstr, D-85748 Garching, Germany. EM yyzhang@mpe.mpg.de NR 78 TC 35 Z9 35 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JAN PY 2005 VL 429 IS 1 BP 85 EP 99 DI 10.1051/0004-6361:20041296 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 879QQ UT WOS:000225732700014 ER PT J AU Nagamine, K Cen, RY Hernquist, L Ostriker, JP Springel, V AF Nagamine, K Cen, RY Hernquist, L Ostriker, JP Springel, V TI Massive galaxies in cosmological simulations: Ultraviolet-selected sample at redshift z=2 SO ASTROPHYSICAL JOURNAL LA English DT Review DE cosmology : theory; galaxies : evolution; galaxies : formation; methods : numerical; stars : formation ID SMOOTHED PARTICLE HYDRODYNAMICS; LYMAN-BREAK GALAXIES; STAR-FORMING GALAXIES; DARK-MATTER UNIVERSE; HUBBLE DEEP FIELD; LY-ALPHA EMITTERS; LUMINOSITY FUNCTION; PHOTOMETRIC REDSHIFTS; INTERGALACTIC MEDIUM; COMMISSIONING DATA AB We study the properties of galaxies at redshift z = 2 in a Lambda cold dark matter (LambdaCDM) universe, using two different types of hydrodynamic simulation methods-Eulerian total variation diminishing (TVD) and smoothed particle hydrodynamics (SPH)-and a spectrophotometric analysis in the U-n, G, R filter set. The simulated galaxies at z = 2 satisfy the color-selection criteria proposed by Adelberger et al. and Steidel et al. when we assume Calzetti extinction with E(B-V) = 0.15. We find that the number density of simulated galaxies brighter than R < 25.5 at z = 2 is about 2 x 10(-2) h(3) Mpc(-3) for E(B-V) = 0.15 in our most representative run, roughly 1 order of magnitude larger than that of Lyman break galaxies at z = 3. The most massive galaxies at z = 2 have stellar masses of greater than or similar to 10(11) M-circle dot, and their observed-frame G-R colors lie in the range 0.0 < G-R < 1.0. They typically have been continuously forming stars at a rate exceeding 30 M-circle dot yr(-1) over a few gigayears from z = 10 to z = 2, although the TVD simulation indicates a more sporadic star formation history than the SPH simulations. On the order of half of their stellar mass was already assembled by z similar to 4. The bluest galaxies with colors -0.2 < G-R < 0.0 at z = 2 are somewhat less massive, with M-star < 10(11) h(-1) M-circle dot, and lack a prominent old stellar population. On the other hand, the reddest massive galaxies at z = 2 with G-R greater than or equal to 1.0 and M-star > 10(10) h(-1) M-circle dot completed the build-up of their stellar mass by z similar to 3. Interestingly, our study indicates that the majority of the most massive galaxies at z = 2 should be detectable at rest-frame ultraviolet wavelengths, contrary to some recent claims made on the basis of near-infrared studies of galaxies at the same epoch, provided the median extinction is less than E(B-V) < 0.3 as indicated by surveys of Lyman break galaxies at z = 3. However, our results also suggest that the fraction of stellar mass contained in galaxies that pass the color-selection criteria used by Steidel et al. (2004) could be as low as 50% of the total stellar mass in the universe at z = 2. Our simulations imply that the missing stellar mass is contained in fainter ( R > 25.5) and intrinsically redder galaxies. The bright end of the rest-frame V-band luminosity function of z 2 galaxies can be characterized by a Schechter function with parameters (Phi*, M*(V), alpha) = (1.8 x 10(-3), -23.4, -1.85), while the TVD simulation suggests a flatter faint-end slope of alpha similar to -1.2. A comparison with z = 3 shows that the rest-frame V-band luminosity function has brightened by about 0.5 mag from z = 3 to z = 2, without a significant change in the shape. Our results do not imply that hierarchical galaxy formation fails to account for the massive galaxies at zgreater than or similar to1. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Princeton Univ Observ, Princeton, NJ 08544 USA. Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. Max Planck Inst Astrophys, D-85740 Garching, Germany. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM knagamin@cfa.harvard.edu NR 102 TC 48 Z9 49 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JAN 1 PY 2005 VL 618 IS 1 BP 23 EP 37 DI 10.1086/425958 PN 1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 883XK UT WOS:000226048800003 ER PT J AU Silverman, JD Green, PJ Barkhouse, WA Kim, DW Aldcroft, TL Cameron, RA Wilkes, BJ Mossman, A Ghosh, H Tananbaum, H AF Silverman, JD Green, PJ Barkhouse, WA Kim, DW Aldcroft, TL Cameron, RA Wilkes, BJ Mossman, A Ghosh, H Tananbaum, H TI Hard X-ray-emitting active galactic nuclei selected by the Chandra multiwavelength project SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; quasars : general; surveys; X-rays : galaxies ID SURVEY PHOTOMETRIC SYSTEM; MEDIUM-SENSITIVITY SURVEY; XMM-NEWTON; OPTICAL IDENTIFICATIONS; SEYFERT-2 GALAXIES; HELLAS2XMM SURVEY; HOST GALAXIES; QUASARS; FIELD; SKY AB We present X-ray and optical analysis of 188 active galactic nuclei (AGN) identified from 497 hard X-ray f(2.0-8.0) keV > 2.7 x 10(-15) ergs cm(-2) s(-1)) sources in 20 Chandra fields (1.5 deg(2)) forming part of the Chandra Multiwavelength Project. These medium depth X-ray observations enable us to detect a representative subset of those sources responsible for the bulk of the 2-8 keV cosmic X-ray background. Brighter than our optical spectroscopic limit, we achieve a reasonable degree of completeness (77% of X-ray sources with counterparts r' < 22.5 have been classified): broad emission-line AGNs (62%), narrow emission-line galaxies (24%), absorption line galaxies (7%), stars (5%), or clusters (2%). We find that most X-ray unabsorbed AGNs (N-H < 10(22) cm(-2)) have optical properties characterized by broad emission lines and blue colors, similar to optically selected quasars from the Sloan Digital Sky Survey but with a slightly broader color distribution. However, we also find a significant population of redder (g' - i' > 1.0) AGNs with broad optical emission lines. Most of the X-ray-absorbed AGNs (10(22) cm(-2) < N-H < 10(24) cm(-2)) are associated with narrow emission- line galaxies, with red optical colors characteristically dominated by luminous, early-type galaxy hosts rather than from dust reddening of an AGN. We also find a number of atypical AGNs; for instance, several luminous AGNs show both strong X-ray absorption (N-H > 10(22) cm(-2)) and broad emission lines. Overall, we find that 81% of X-ray-selected AGNs can be easily interpreted in the context of current AGN unification models. Most of the deviations seem to be due to an optical contribution from the host galaxies of the low-luminosity AGNs. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Natl Opt Astron Observ, Cerro Tololo Inter Amer Observ, La Serena, Chile. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Natl Sci Fdn, Arlington, VA 22230 USA. Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA. Natl Opt Astron Observ, Tucson, AZ 85726 USA. RP Silverman, JD (reprint author), Univ Virginia, Dept Astron, POB 3818, Charlottesville, VA 22903 USA. EM jsilverman@cfa.harvard.edu; pgreen@cfa.harvard.edu OI Wilkes, Belinda/0000-0003-1809-2364 NR 58 TC 72 Z9 72 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 1 PY 2005 VL 618 IS 1 BP 123 EP 138 DI 10.1086/425895 PN 1 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 883XK UT WOS:000226048800009 ER PT J AU Granot, J Ramirez-Ruiz, E Loeb, A AF Granot, J Ramirez-Ruiz, E Loeb, A TI Implications of the measured image size for the radio afterglow of GRB 030329 SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma rays : bursts; ISM : jets and outflows; polarization; radiation mechanisms : nonthermal; relativity; shock waves ID GAMMA-RAY-BURST; LIGHT CURVES; LINEAR-POLARIZATION; RELATIVISTIC JET; MAGNETIC-FIELD; PROPER MOTION; ANGULAR SIZE; EMISSION; FIREBALL; SHOCKS AB We use data on the image size of the radio afterglow of GRB 030329 to constrain the physical parameters of this explosion. Together with the observed broadband spectrum, this data overconstrains the physical parameters, thus enabling us to test different GRB jet models for consistency. We consider two extreme models for the lateral spreading of the jet: model 1, with relativistic expansion in the local rest frame, and model 2, with little lateral expansion as long as the jet is highly relativistic. We find that both models are consistent with the data for a uniform external medium, while for a stellar wind environment model 1 is consistent with the data but model 2 is disfavored by the data. Our derivations can be used to place tighter constraints on the dynamics and structure of GRB jets in future afterglows, following a denser monitoring campaign for the temporal evolution of their image size. C1 Inst Adv Study, Princeton, NJ 08540 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Inst Adv Study, Einstein Dr, Princeton, NJ 08540 USA. NR 50 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 JAN 1 PY 2005 VL 618 IS 1 BP 413 EP 425 DI 10.1086/425899 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 883XK UT WOS:000226048800029 ER PT J AU Heyl, JS Hernquist, L AF Heyl, JS Hernquist, L TI A QED model for the origin of bursts from soft gamma repeaters and anomalous X-ray pulsars SO ASTROPHYSICAL JOURNAL LA English DT Article DE elementary particles; gamma rays : theory; pulsars : general; X-rays : bursts; X-rays : stars ID NEAR-INFRARED COUNTERPART; MAGNETIZED NEUTRON-STARS; NONLINEAR ELECTRODYNAMICS; CYCLOTRON-RESONANCE; PAIR PRODUCTION; FALLBACK DISKS; 1E 2259+586; SGR 1806-20; FIELD; EMISSION AB We propose a model to account for the bursts from soft gamma repeaters (SGRs) and anomalous X- ray pulsars (AXPs) in which quantum electrodynamics plays a vital role. In our theory, which we term "fast-mode breakdown,'' magnetohydrodynamic (MHD) waves that are generated near the surface of a neutron star and propagate outward through the magnetosphere will be modified by the polarization of the vacuum. For neutron star magnetic fields B-NS greater than or similar to B-QED approximate to 4.4 x 10(13) G, the interaction of the wave fields with the vacuum produces nonlinearities in fast MHD waves that can steepen in a manner akin to the growth of hydrodynamic shocks. Under certain conditions, fast modes can develop field discontinuities on scales comparable to an electron Compton wavelength, at which point the wave energy will be dissipated through electron-positron pair production. We show that this process operates if the magnetic field of the neutron star is sufficiently strong and the ratio of the wavelength of the fast mode to its amplitude is sufficiently small, in which case the wave energy will be efficiently converted into an extended pair plasma fireball. The radiative output from this fireball will consist of hard X- rays and soft gamma-rays, with a spectrum similar to those seen in bursts from SGRs and AXPs. In addition, the mostly thermal radiation will be accompanied by a high-energy tail of synchrotron emission, whose existence can be used to test this theory. Our model also predicts that for disturbances with a given wavelength and amplitude, only stars with magnetic fields above a critical threshold will experience fast-mode breakdown in their magnetospheres. In principle, this distinction provides an explanation for why SGRs and AXPs exhibit burst activity while high-field radio pulsars apparently do not. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM heyl@physics.ubc.ca; lars@cfa.harvard.edu NR 84 TC 34 Z9 34 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JAN 1 PY 2005 VL 618 IS 1 BP 463 EP 473 DI 10.1086/425974 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 883XK UT WOS:000226048800034 ER PT J AU Egami, E Kneib, JP Rieke, GH Ellis, RS Richard, J Rigby, J Papovich, C Stark, D Santos, MR Huang, JS Dole, H Le Floc'h, E Perez-Gonzalez, PG AF Egami, E Kneib, JP Rieke, GH Ellis, RS Richard, J Rigby, J Papovich, C Stark, D Santos, MR Huang, JS Dole, H Le Floc'h, E Perez-Gonzalez, PG TI Spitzer and Hubble Space Telescope constraints on the physical properties of the z similar to 7 galaxy strongly lensed by A2218 SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : observations; galaxies : evolution; galaxies : formation; galaxies : high-redshift; gravitational lensing ID LYMAN BREAK GALAXIES; HIGH-REDSHIFT AB We report the detection of a z similar to 7 galaxy strongly lensed by the massive galaxy cluster A2218 (z = 0.175) at 3.6 and 4.5 mum using the Spitzer Space Telescope and at 1.1 mum using the Hubble Space Telescope. The new data indicate a refined photometric redshift in the range of 6.6-6.8 depending on the presence of Lyalpha emission. The spectral energy distribution is consistent with having a significant Balmer break, suggesting that the galaxy is in the poststarburst stage with an age of at least similar to50 Myr and quite possibly a few hundred million years. This suggests the possibility that a mature stellar population is already in place at such a high redshift. Compared with typical Lyman break galaxies at, the stellar mass is an order of magnitude smaller (similar to10(9) M-circle dot), but the specific star formation rate (star formation rate/M-star) is similarly large (>10(-9) yr(-1)), indicating equally vigorous star-forming activity. C1 Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Observ Midi Pyrenees, F-31000 Toulouse, France. CALTECH, Dept Astron, Pasadena, CA 91125 USA. Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Egami, E (reprint author), Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA. EM eegami@as.arizona.edu; kneib@astro.caltech.edu; grieke@as.arizona.edu; rse@astro.caltech.edu; jrichard@ast.obs-mip.fr; jrigby@as.arizona.edu; papovich@as.arizona.edu; dps@astro.caltech.edu; mrs@ast.cam.ac.uk; jhuang@cfa.harvard.edu; hdole@as.arizona.edu; elefloch@as.arizona.edu; pgperez@as.arizona.edu RI Rigby, Jane/D-4588-2012; Kneib, Jean-Paul/A-7919-2015; Perez-Gonzalez, Pablo/J-2871-2016 OI Rigby, Jane/0000-0002-7627-6551; Kneib, Jean-Paul/0000-0002-4616-4989; Perez-Gonzalez, Pablo/0000-0003-4528-5639 NR 19 TC 87 Z9 87 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 1 PY 2005 VL 618 IS 1 BP L5 EP L8 DI 10.1086/427550 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 883XL UT WOS:000226048900002 ER PT J AU Park, SQ Miller, JM McClintock, JE Murray, SS AF Park, SQ Miller, JM McClintock, JE Murray, SS TI A Chandra observation of the diffuse emission centered on the low-mass X-ray binary 4U 1755-33 SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : close; stars : individual (V4134 Sagittarii, 4U 1755-33); X-rays : stars ID BLACK-HOLE CANDIDATE; 4U 1755-33; X1755-338; SPECTRUM; QUIESCENCE; UHURU AB We present an analysis of a Chandra observation of the field surrounding the low-mass X-ray binary 4U 1755-33, which has been in quiescence since 1996. In 2003, Angelini & White reported the appearance of a narrow 7'-long jetlike feature centered on the position of 4U 1755-33 using the XMM-Newton telescope. Although the source and jet are not visibly apparent in our Chandra ACIS-S image, there is a significant excess (4-6 sigma) of counts in a region that encloses the jet when compared to adjacent regions. We examined a knot of emission in the jet that was detected by XMM-Newton but not by Chandra and calculated that if the knot flux observed by XMM-Newton was concentrated in a point source, Chandra would have easily detected it; we therefore conclude that this knot of emission is diffuse. In summary, we suggest that the jetlike feature found previously in the XMM-Newton data is quite diffuse and likely a true jet and that it is not due to a chance alignment of discrete point sources or pointlike regions of emission associated with internal shocks. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Park, SQ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM spark@cfa.harvard.edu; jmmiller@cfa.harvard.edu; jmcclintock@cfa.harvard.edu; smurray@cfa.harvard.edu NR 20 TC 6 Z9 6 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 1 PY 2005 VL 618 IS 1 BP L45 EP L48 DI 10.1086/427626 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 883XL UT WOS:000226048900012 ER PT J AU Rasia, E Mazzotta, P Borgani, S Moscardini, L Dolag, K Tormen, G Diaferio, A Murante, G AF Rasia, E Mazzotta, P Borgani, S Moscardini, L Dolag, K Tormen, G Diaferio, A Murante, G TI Mismatch between X-ray and emission-weighted temperatures in galaxy clusters: Cosmological implications SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmological parameters; cosmology : theory; dark matter; galaxies : clusters : general; X-rays : galaxies ID T RELATION; MASS; SIMULATIONS; CHANDRA; NORMALIZATION; PROFILES; MODEL; ROSAT; STATE; GAS AB The thermal properties of hydrodynamical simulations of galaxy clusters are usually compared to observations by relying on the emission-weighted temperature T-ew instead of on the spectroscopic X-ray temperature T-spec, which is obtained by actual observational data. In a recent paper, Mazzotta et al. show that if the intracluster medium is thermally complex, T-ew fails at reproducing T-spec. They propose a new formula, the spectroscopic-like temperature, T-sl, which approximates T-spec better than a few percent. By analyzing a set of hydrodynamical simulations of galaxy clusters, we find that T-sl is lower than T-ew by 20%-30%. as a consequence, the normalization of the M-T-sl relation from the simulations is larger than the observed one by about 50%. If masses in simulated clusters are estimated by following the same assumptions of hydrostatic equilibrium and beta-model gas density profile, as is often done for observed clusters, then the M-T relation decreases by about 40% and significantly amplitude of the power spectrum from the X-ray temperature function could bias low sigma(s) by 10%-20%. This may alleviate the tension between the value of sigma(s) inferred from the cluster number density and those from the cosmic microwave background and large-scale structure. C1 Univ Padua, Dipartimento Astron, I-35122 Padua, Italy. Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Trieste, Dipartimento Astron, I-34131 Trieste, Italy. Ist Nazl Fis Nucl, I-34127 Trieste, Italy. Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. Univ Turin, Dipartimento Fis Gen Amedeo Avogadro, I-10125 Turin, Italy. Osservatorio Astron Pino Torinese, INAF, I-10025 Pino Torinese, Italy. RP Rasia, E (reprint author), Univ Padua, Dipartimento Astron, Vicolo Osservatorio 2, I-35122 Padua, Italy. EM rasia@pd.astro.it; pasquale.mazzotta@roma2.infn.it; borgani@ts.astro.it; lauro.moscardini@unibo.it; kdolag@pd.astro.it; tormen@pd.astro.it; diaferio@ph.unito.it; murante@to.astro.it RI Mazzotta, Pasquale/B-1225-2016; OI Mazzotta, Pasquale/0000-0002-5411-1748; rasia, elena/0000-0003-4175-002X NR 31 TC 73 Z9 73 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 1 PY 2005 VL 618 IS 1 BP L1 EP L4 DI 10.1086/427554 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 883XL UT WOS:000226048900001 ER PT J AU Marshall, HL Schwartz, DA Lovell, JEJ Murphy, DW Worrall, DM Birkinshaw, M Gelbord, JM Perlman, ES Jauncey, DL AF Marshall, HL Schwartz, DA Lovell, JEJ Murphy, DW Worrall, DM Birkinshaw, M Gelbord, JM Perlman, ES Jauncey, DL TI A Chandra survey of quasar jets: First results SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE galaxies : active; quasars : general ID X-RAY JET; ACTIVE GALACTIC NUCLEI; SPECTRAL ENERGY-DISTRIBUTIONS; HUBBLE-SPACE-TELESCOPE; EXTENDED RADIO JETS; VLBA OBSERVATIONS; H-I; EMISSION; SAMPLE; CENTAURUS AB We present results from Chandra X-ray imaging and spectroscopy of a flux-limited sample of flat-spectrum radio-emitting quasars with jetlike extended structure. Twelve of 20 quasar jets are detected in 5 ks ACIS-S exposures. The quasars without X-ray jets are not significantly different from those in the sample with detected jets except that the extended radio emission is generally fainter. New radio maps are combined with the X-ray images in order to elucidate the relation between radio and X-ray emission in spatially resolved structures. We find a variety of morphologies, including long straight jets and bends up to 90degrees. All X-ray jets are one-sided although the radio images used for source selection often show lobes opposite the X-ray jets. The FR II X-ray jets can all be interpreted as inverse Compton scattering of cosmic microwave background photons by electrons in large-scale relativistic jets although deeper observations are required to test this interpretation in detail. Applying this interpretation to the jets as a population, we find that the jets would be aligned to within 30degrees of the line of sight generally, assuming that the bulk Lorentz factor of the jets is 10. C1 MIT, Ctr Space Res, Cambridge, MA 02139 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CSIRO, Australia Telescope Natl Facil, Epping, NSW 2121, Australia. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ Bristol, Dept Phys, Bristol BS8 1TL, Avon, England. Univ Maryland Baltimore Cty, Joint Ctr Astrophys, Baltimore, MD USA. Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD USA. RP Marshall, HL (reprint author), MIT, Ctr Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA. EM hermanm@space.mit.edu; das@head-cfa.harvard.edu; jim.lovell@csiro.au; dwm@sgra.jpl.nasa.gov; d.worrall@bristol.ac.uk; mark.birkinshaw@bristol.ac.uk; jonathan@space.mit.edu; perlman@jca.umbc.edu; david.jauncey@csiro.au NR 38 TC 98 Z9 98 U1 1 U2 4 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD JAN PY 2005 VL 156 IS 1 BP 13 EP 33 DI 10.1086/425578 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 882VQ UT WOS:000225967800002 ER PT J AU Lang, MJ Carter-Lewis, DA Fegan, DJ Fegan, SJ Hillas, AM Lamb, RC Punch, M Reynolds, PT Weekes, TC AF Lang, MJ Carter-Lewis, DA Fegan, DJ Fegan, SJ Hillas, AM Lamb, RC Punch, M Reynolds, PT Weekes, TC TI A new TeV source confirmed in whipple archival data: TeV J2032+41 SO ASTROPHYSICS AND SPACE SCIENCE LA English DT Article; Proceedings Paper CT Conference on Multiwavelength Approach to Unidentified Gamma-Ray Sources CY JUN 01-04, 2004 CL Univ Hong Kong, Hong Kong, PEOPLES R CHINA HO Univ Hong Kong DE gamma rays; observations; unidentified sources ID GAMMA-RAY SOURCES; ENERGIES; EMISSION; SEARCH; CYGNUS AB A re-analysis of data near Cygnus X-3 in 1989 - 1990 using the Whipple Observatory atmospheric Cherenkov imaging telescope confirms the existence of the TeV J2032 + 4130 source first reported at a conference by the Crimean Astrophysical Observatory and confirmed independently by the HEGRA Collaboration in a referred publication. The significance of the Whipple observations at the a priori HEGRA position is 3.3 sigma. The peak signal was found at RA = 20 h 32m, Dec = + 41 degrees 33'. This is 0.6 degrees north of Cygnus X-3. The flux level (12% of the level of the Crab Nebula) is intermediate between that reported by the Crimean (100%) and HEGRA (3%) groups. C1 Natl Univ Ireland, Dept Phys, Galway, Ireland. Iowa State Univ, Dept Phys & Astron, Ames, IA USA. Univ Coll, Dept Expt Phys, Dublin, Ireland. Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ USA. Univ Leeds, Dept Phys & Astron, Leeds, W Yorkshire, England. CALTECH, Space Radiat Lab, Pasadena, CA 91125 USA. Coll France, F-75231 Paris, France. Cork Inst Technol, Dept Appl Phys & Instrumentat, Cork, Ireland. RP Lang, MJ (reprint author), Natl Univ Ireland, Dept Phys, Galway, Ireland. EM tweekes@cfa.harvard.edu OI Punch, Michael/0000-0002-4710-2165; Lang, Mark/0000-0003-4641-4201 NR 19 TC 0 Z9 0 U1 0 U2 1 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0004-640X J9 ASTROPHYS SPACE SCI JI Astrophys. Space Sci. PD JAN PY 2005 VL 297 IS 1-4 BP 345 EP 351 DI 10.1007/s10509-005-7674-y PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 918ME UT WOS:000228545100036 ER PT J AU Torres, DF Dame, TM Romero, GE AF Torres, DF Dame, TM Romero, GE TI Status of the connection between unidentified EGRET sources and supernova remnants: The case of CTA 1 SO ASTROPHYSICS AND SPACE SCIENCE LA English DT Article; Proceedings Paper CT Conference on Multiwavelength Approach to Unidentified Gamma-Ray Sources CY JUN 01-04, 2004 CL Univ Hong Kong, Hong Kong, PEOPLES R CHINA HO Univ Hong Kong DE supernova remnants; gamma rays : observations; interstellar medium ID GAMMA-RAY SOURCES; RX-J1713.7-3946; VARIABILITY; EMISSION; PULSAR AB In this paper we briefly comment on the observational status of the possible physical association between unidentified EGRET sources and supernova remnants (SNRs) in our Galaxy. We draw upon recent results presented in the review by Torres et al. (2003), concerning molecular gas in the vicinity of all 19 SNRs found to be positionally coincident with EGRET sources at low Galactic latitudes. In addition, we present new results regarding the supernova remnant CTA 1. Our findings disfavor the possibility of a physical connection with the nearby (in projection) EGRET source. There remains possible, however, that the compact object produced in the supernova explosion be related with the observed gamma-ray flux. C1 Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Inst Argentino Radioastron, Buenos Aires, DF, Argentina. RP Torres, DF (reprint author), Lawrence Livermore Natl Lab, 7000 E Ave L-413, Livermore, CA 94550 USA. EM dtorres@igpp.ucllnl.org NR 23 TC 2 Z9 2 U1 0 U2 1 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0004-640X J9 ASTROPHYS SPACE SCI JI Astrophys. Space Sci. PD JAN PY 2005 VL 297 IS 1-4 BP 393 EP 398 DI 10.1007/s10509-005-7698-3 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 918ME UT WOS:000228545100042 ER PT J AU Fegan, SJ Weekes, TC AF Fegan, SJ Weekes, TC CA VERITAS Collaboration TI A survey of unidentified EGRET sources at TeV energies SO ASTROPHYSICS AND SPACE SCIENCE LA English DT Article; Proceedings Paper CT Conference on Multiwavelength Approach to Unidentified Gamma-Ray Sources CY JUN 01-04, 2004 CL Univ Hong Kong, Hong Kong, PEOPLES R CHINA HO Univ Hong Kong DE gamma rays : observations; sources : unidentified ID GAMMA-RAY SOURCES; MARKARIAN-421; VARIABILITY; DISCOVERY; TELESCOPE; CATALOG AB The Whipple Observatory 10 m gamma-ray telescope has been used to survey the error boxes of 24 EGRET unidentified sources in an attempt to find counterparts at energies of 350 GeV and above. In no case is a statistically significant signal found in the EGRET error box which implies that, at least for this sample, the gamma-ray spectra of these sources steepen between 100 MeV and 350 GeV. C1 Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. RP Fegan, SJ (reprint author), Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. EM tweekes@cfa.harvard.edu NR 22 TC 3 Z9 3 U1 0 U2 1 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0004-640X J9 ASTROPHYS SPACE SCI JI Astrophys. Space Sci. PD JAN PY 2005 VL 297 IS 1-4 BP 431 EP 438 DI 10.1007/s10509-005-7703-x PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 918ME UT WOS:000228545100047 ER PT J AU Henkel, C Braatz, JA Tarchi, A Peck, AB Nagar, NM Greenhill, LJ Wang, M Hagiwara, Y AF Henkel, C Braatz, JA Tarchi, A Peck, AB Nagar, NM Greenhill, LJ Wang, M Hagiwara, Y TI H2O megamasers: Accretion disks, jet interaction, outflows or massive star formation? SO ASTROPHYSICS AND SPACE SCIENCE LA English DT Article; Proceedings Paper CT European Workshop on Astronomical Molecules CY FEB 18-20, 2004 CL Zwolle, NETHERLANDS DE masers ID ACTIVE GALACTIC NUCLEI; WATER MASER EMISSION; CIRCINUS GALAXY; VAPOR MASERS; BLACK-HOLE; NGC-4258; DISCOVERY; SEARCH; PARSEC; TORUS AB The 25 years following the serendipitous discovery of megamasers have seen tremendous progress in the study of luminous extragalactic H2O emission. Single-dish monitoring and high-resolution interferometry have been used to identify sites of massive star formation, to study the interaction of nuclear jets with dense molecular gas and to investigate the circumnuclear environment of active galactic nuclei (AGN). Accretion disks with radii of 0.1-3 pc were mapped and masses of nuclear engines of order 10(6)-10(8) MD were determined. So far, similar to 50 extragalactic H2O maser sources have been detected, but few have been studied in detail. C1 Max Planck Inst Radioastron, Hugel 69, Bonn, Germany. NRAO, Green Bank, WV USA. CNR, Ist Radioastron, I-40126 Bologna, Italy. Osservatorio Astron Cagliari, INAF, Capoterra, CA, Italy. Harvard Smithsonian Ctr Astrophys, SAO SMA Project, Hilo, HI USA. Kapteyn Inst AV, Groningen, Netherlands. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Chinese Acad Sci, Purple Mt Observ, Nanjing, Peoples R China. ASTRON Westerbork Radio Observ, NL-7990 AA Dwingeloo, Netherlands. RP Henkel, C (reprint author), Max Planck Inst Radioastron, Hugel 69, Bonn, Germany. EM chenkel@mpifr-bonn.mpg.de NR 52 TC 11 Z9 11 U1 0 U2 2 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0004-640X J9 ASTROPHYS SPACE SCI JI Astrophys. Space Sci. PY 2005 VL 295 IS 1-2 BP 107 EP 116 DI 10.1007/s10509-005-3668-z PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 916MG UT WOS:000228389200014 ER PT J AU Humphreys, EML Argon, AL Greenhill, LJ Reid, MJ Moran, JM AF Humphreys, EML Argon, AL Greenhill, LJ Reid, MJ Moran, JM TI The sub-PC scale accretion disk of NGC 4258 SO ASTROPHYSICS AND SPACE SCIENCE LA English DT Article; Proceedings Paper CT European Workshop on Astronomical Molecules CY FEB 18-20, 2004 CL Zwolle, NETHERLANDS DE NGC 4258; water masers; accretion disks; AGN ID BLACK-HOLES; NGC4258; GALAXY; PARSEC AB Water megamasers have been found to trace parsec/sub-parsec, circumnuclear accretion disks in several AGN (e.g., Circinus, NGC 1068 W NGC 4258). High-spatial (0.5 mas) and velocity resolution (0.2 km s(-1)) VLBA imaging of the disks reveals thin, warped 'pannekoeken(pancake)'-style structures as opposed to thick tori in the inner regions of the central engines (40 000 R-sch). In this contribution, I will describe some current investigations into the dynamical and physical attributes of the water maser disk in NGC 4258, as revealed by VLBA, VLA and Effelsberg monitoring over 8 years. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Humphreys, EML (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM ehumphreys@cfa.harvard.edu NR 11 TC 1 Z9 1 U1 0 U2 1 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0004-640X J9 ASTROPHYS SPACE SCI JI Astrophys. Space Sci. PY 2005 VL 295 IS 1-2 BP 285 EP 289 DI 10.1007/s10509-005-3728-4 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 916MG UT WOS:000228389200034 ER PT J AU Couper, PJ Wilmer, JW Roberts, L Amey, AP Zug, GR AF Couper, PJ Wilmer, JW Roberts, L Amey, AP Zug, GR TI Skinks currently assigned to Carlia aerata (Scincidae : Lygosominae) of north-eastern Queensland: a preliminary study of cryptic diversity and two new species SO AUSTRALIAN JOURNAL OF ZOOLOGY LA English DT Article ID AUSTRALIAN LIZARDS; RAIN-FORESTS; LACERTILIA; PHYLOGENY; TAXONOMY; ECOLOGY; HISTORY; EGERNIA; DNA AB A preliminary investigation of genetic diversity in Carlia aerata, by sequencing the mitochondrial ND4 gene, revealed the presence of two cryptic species, described herein. The sequence data was added to an existing phylogeny to discern molecular relationships. Interestingly, genetic affinities lie not with C. aerata, the species to which they key. Instead, one has affinities with C. tanneri, the other with C. foliorum. This casts doubt on the validity of morphological characters alone to infer relationships within this genus. Despite low levels of genetic divergence from sister taxa, the new species can be diagnosed from these by morphological characters that exhibit little or no intraspecific variation. The addition of these new species to the gene tree did not enhance resolution of the phylogenetic relationships at the deeper nodes of the Carlia tree. The discovery of these two new cryptic species provides further support for a previously suggested rapid mid- Miocene diversification of Carlia that may have resulted from the successful expansion of a rainforest- dwelling ancestor into the expanding woodlands associated with Miocene climate fluctuations. C1 Queensland Museum, Brisbane, Qld 4101, Australia. Smithsonian Inst, Washington, DC 20013 USA. RP Couper, PJ (reprint author), Queensland Museum, POB 3300,S Bank, Brisbane, Qld 4101, Australia. EM patrickc@qm.qld.gov.au NR 44 TC 15 Z9 16 U1 1 U2 3 PU CSIRO PUBLISHING PI COLLINGWOOD PA 150 OXFORD ST, PO BOX 1139, COLLINGWOOD, VICTORIA 3066, AUSTRALIA SN 0004-959X J9 AUST J ZOOL JI Aust. J. Zool. PY 2005 VL 53 IS 1 BP 35 EP 49 DI 10.1071/ZO04010 PG 15 WC Zoology SC Zoology GA 900ND UT WOS:000227220700005 ER PT S AU Dierking, LD AF Dierking, Lynn D. BE Alsop, S TI MUSEUMS, AFFECT, AND COGNITION: THE VIEW FROM ANOTHER WINDOW SO BEYOND CARTESIAN DUALISM: ENCOUNTERING AFFECT IN THE TEACHING AND LEARNING OF SCIENCE SE Science & Technology Education Library LA English DT Article; Book Chapter ID INTRINSIC MOTIVATION; COMPETENCE C1 [Dierking, Lynn D.] Univ Florida, Gainesville, FL 32611 USA. [Dierking, Lynn D.] Univ Maryland, Coll Educ, Smithsonian Off Educ Res, College Pk, MD 20742 USA. RP Dierking, LD (reprint author), Univ Florida, Gainesville, FL 32611 USA. NR 38 TC 1 Z9 1 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 1572-5987 BN 978-1-4020-3808-2 J9 SCI TECHNOL EDUC LIB PY 2005 VL 29 BP 111 EP 122 D2 10.1007/1-4020-3808-9 PG 12 WC Education & Educational Research; Multidisciplinary Sciences SC Education & Educational Research; Science & Technology - Other Topics GA BLA66 UT WOS:000269777300009 ER PT J AU Wildt, DE Pukazhenthi, BS Ballou, JD Pelican, KM Howard, J AF Wildt, DE Pukazhenthi, BS Ballou, JD Pelican, KM Howard, J TI Genes versus environment, and reproductive success in endangered species. SO BIOLOGY OF REPRODUCTION LA English DT Meeting Abstract CT 38th Annual Meeting of the Society-for-the-Study-of-Reproduction CY JUL 24-27, 2005 CL Ctr Rech Biol Reproduct, Quebec City, CANADA HO Ctr Rech Biol Reproduct C1 Smithsonians Natl Zool Pk, Conservat & Res Ctr, Front Royal, VA USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SOC STUDY REPRODUCTION PI MADISON PA 1603 MONROE ST, MADISON, WI 53711-2021 USA SN 0006-3363 J9 BIOL REPROD JI Biol. Reprod. PY 2005 SI SI BP 70 EP 70 PG 1 WC Reproductive Biology SC Reproductive Biology GA 946EX UT WOS:000230556300016 ER PT J AU Songsasen, N Spindler, RE Wildt, DE AF Songsasen, N Spindler, RE Wildt, DE TI Impact of nuclear status and maturation period on energy substrate use by in vitro-cultured dog oocytes. SO BIOLOGY OF REPRODUCTION LA English DT Meeting Abstract CT 38th Annual Meeting of the Society-for-the-Study-of-Reproduction CY JUL 24-27, 2005 CL Ctr Rech Biol Reproduct, Quebec City, CANADA HO Ctr Rech Biol Reproduct C1 Smithsonians Natl Zool Pk, Front Royal, VA USA. Toronto Zoo, Scarborough, ON, Canada. 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 2005 SI SI BP 221 EP 221 PG 1 WC Reproductive Biology SC Reproductive Biology GA 946EX UT WOS:000230556301217 ER PT J AU Bauer, RA Pelican, KM Wildt, DE Ottinger, MA Howard, J AF Bauer, RA Pelican, KM Wildt, DE Ottinger, MA Howard, J TI Oral progestogen, altrenogest, provides short-term inhibition of ovarian activity in the domestic cat. SO BIOLOGY OF REPRODUCTION LA English DT Meeting Abstract CT 38th Annual Meeting of the Society-for-the-Study-of-Reproduction CY JUL 24-27, 2005 CL Ctr Rech Biol Reproduct, Quebec City, CANADA HO Ctr Rech Biol Reproduct C1 Smithsonians Natl Zool Pk, Front Royal, VA USA. Univ Maryland, College Pk, MD 20742 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 2005 SI SI BP 238 EP 238 PG 1 WC Reproductive Biology SC Reproductive Biology GA 946EX UT WOS:000230556301294 ER PT J AU Schwartz, B Fukuoka, K Takita-Ishii, S AF Schwartz, Barry Fukuoka, Kazuya Takita-Ishii, Sachiko BE Jacobs, MD Hanrahan, NW TI Collective Memory: Why Culture Matters SO BLACKWELL COMPANION TO THE SOCIOLOGY OF CULTURE SE Blackwell Companions to Sociology LA English DT Article; Book Chapter C1 [Schwartz, Barry] Univ Georgia, Humanities Ctr, Athens, GA 30602 USA. [Schwartz, Barry] Smithsonian Inst, Washington, DC 20560 USA. [Schwartz, Barry] Hebrew Univ Jerusalem, Jerusalem, Israel. [Fukuoka, Kazuya] Univ Georgia, Ctr Study Global Issues GLOBIS, Athens, GA 30602 USA. [Takita-Ishii, Sachiko] Yokohama City Univ, Dept Int Relat, Yokohama, Kanagawa, Japan. NR 77 TC 10 Z9 10 U1 0 U2 4 PU BLACKWELL SCIENCE PUBL PI OXFORD PA OSNEY MEAD, OXFORD OX2 0EL, ENGLAND BN 978-0-47099-674-4 J9 BLACKW COMPAN SOCIO PY 2005 BP 253 EP 271 DI 10.1002/9780470996744.ch17 D2 10.1002/9780470996744 PG 19 WC Cultural Studies; Sociology SC Cultural Studies; Sociology GA BYD60 UT WOS:000298107300017 ER PT J AU Fu, XH Nobuyoshi, O Vencl, FV Lei, CL AF Fu, XH Nobuyoshi, O Vencl, FV Lei, CL TI Structure, behavior, and the life cycle of an aquatic firefly, Luciola substriata, in China SO CANADIAN ENTOMOLOGIST LA English DT Article ID LAMPYRIDAE; COLEOPTERA AB The aquatic firefly Luciola substriata Gorham, 1880 (Coleoptera: Lampyridae) was first discovered in mainland China in 2000. The larvae of L. substriata inhabit ponds and lakes rich in aquatic vegetation. We recorded L. substriata feeding on two species of aquatic snails, Lymnaea stagnalis (L., 1758) (Basommatophora: Lymnaeidae) and Gyraulus convexiusculus (Hutton, 1849) (Basommatophora: Planorbidae). Three predators of fireflies were also recorded for the first time: the red swamp crayfish, Procambarus clarkii (Girard, 1852) (Decapoda: Cambaridae), the crab Eriocheir sinensis H. Milne-Edwards, 1853 (Decapoda: Varunidae), and the grass carp, Ctenopharyngodon idellus (Valenciennes in Cuvier et Valenciennes, 1844) (Cypriniformes: Cyprinidae). Egg incubation averaged 11 days at an ambient temperature of 2025 degrees C. The prepupal stage of L. substriata lasted 6.2 days, and the pupal stage lasted 4.4 days. The imaginal period lasted from May to September. Courtship light-flashing activity peaked 1 h after sunset. The light spectrum of responsiveness of L. substriata was 425-603 nm, with a peak responsive emission at 504 nm. In addition, we have described and illustrated the morphology of L. substriata. C1 Huanzhong Agr Univ, Inst Insect Resources, Wuhan 430070, Peoples R China. Yokosuka City Univ, Yokosuka, Kanagawa 238, Japan. SUNY Stony Brook, Dept Ecol & Evolut, Stony Brook, NY 11794 USA. Smithsonian Trop Res Inst, Balboa, Panama. RP Lei, CL (reprint author), Huanzhong Agr Univ, Inst Insect Resources, Wuhan 430070, Peoples R China. EM ioir@mail.hzau.edu.cn NR 20 TC 16 Z9 21 U1 2 U2 7 PU ENTOMOL SOC CANADA PI OTTAWA PA 393 WINSTON AVE, OTTAWA, ONTARIO K2A 1Y8, CANADA SN 0008-347X J9 CAN ENTOMOL JI Can. Entomol. PD JAN-FEB PY 2005 VL 137 IS 1 BP 83 EP 90 PG 8 WC Entomology SC Entomology GA 910KK UT WOS:000227929900006 ER PT J AU Davis, JLD Young-Williams, AC Hines, AH Zohar, Y AF Davis, JLD Young-Williams, AC Hines, AH Zohar, Y TI Assessing the potential for stock enhancement in the case of the Chesapeake Bay blue crab (Callinectes sapidus) SO CANADIAN JOURNAL OF FISHERIES AND AQUATIC SCIENCES LA English DT Article ID POPULATION-DYNAMICS; COD ENHANCEMENT; JUVENILE; SURVIVAL; SIZE; PROGRAMS; WILD; RESTORATION; RECRUITMENT; AUSTRALIA AB In certain cases of severely depleted fishery stocks, combining stock enhancement with traditional management techniques may be a useful way of returning stocks to an exploitable size. The Chesapeake Bay stock of blue crabs (Callinectes sapidus) has declined over the past decade and appears to be recruitment-limited, making it an appropriate candidate for enhancement efforts. This study serves as a first step in determining whether large-scale enhancement of blue crab stocks is feasible. Four hatchery-raised cohorts of 4000 - 10 000 (25 000 in total) juvenile (6-30 mm carapace width, 58-70 days old) crabs were released in upper Chesapeake Bay coves. Sixty days after release, these crabs constituted 22%-79% of all crabs in the hatchery-crab size range (corresponding to an enhancement level of 28%-366%). Crabs released earlier in the summer reached maturity at the age of 6 months, younger than their wild counterparts. Estimated survivorship to maturity was 16%-20% for early-released crabs and 5-15% for late-released crabs. Late-released crabs, like wild crabs, had to overwinter before becoming mature. Our study suggests ways to improve success of hatchery-raised individuals that can be broadly applied across taxa. The results also contribute specifically to determining whether large-scale stock enhancement is possible in the case of the Chesapeake Bay blue crab. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Univ Maryland, Ctr Marine Biotechnol, Inst Biotechnol, Baltimore, MD 21202 USA. RP Davis, JLD (reprint author), Smithsonian Environm Res Ctr, 647 Contess Wharf Rd, Edgewater, MD 21037 USA. EM janalddavis@yahoo.com NR 50 TC 21 Z9 21 U1 0 U2 7 PU NATL RESEARCH COUNCIL CANADA PI OTTAWA PA RESEARCH JOURNALS, MONTREAL RD, OTTAWA, ONTARIO K1A 0R6, CANADA SN 0706-652X J9 CAN J FISH AQUAT SCI JI Can. J. Fish. Aquat. Sci. PD JAN PY 2005 VL 62 IS 1 BP 109 EP 122 DI 10.1139/F04-150 PG 14 WC Fisheries; Marine & Freshwater Biology SC Fisheries; Marine & Freshwater Biology GA 906AY UT WOS:000227614100011 ER PT J AU Collin, R AF Collin, R TI Crepidula badisparsa sp nov (Gastropoda : Calyptraeidae) from Bocas Del Toro Province, Panama SO CARIBBEAN JOURNAL OF SCIENCE LA English DT Article DE Calyptraeidae; Crepidula riisei; Crepidula convexa; Crepidula navicula ID CAENOGASTROPODA; PROSOBRANCHIA; PHYLOGENY; PATTERNS; MODE AB The taxonomy of calyptraeid gastropods is made difficult by their morphologically simple, plastic shells and the numerous instances of morphological convergence within the family. The small speckled species of Crepidula from the West Atlantic have all previously been referred to as C. conveva Say, 1822. Recent developmental and genetic work has shown that there are two species along the coast of North America, C. convexa and C. ustidatidina, and that there are at least two other species in the southern Caribbean. Here I describe, Crepidula badisparsa sp. nov., the small speckled species from the Caribbean coast of Panama and augment the original description of C. navicula from Venezeula and the Lesser Antillies. These species are easily distinguished from the more northern C. convexa and C. ustidatidina by the absence of the right muscle scar, and from each other by genetic, conchological, and anatomical characters. C1 Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Collin, R (reprint author), Smithsonian Trop Res Inst, Apartado Postal 0843-03092, Balboa, Ancon, Panama. EM collinr@naos.si.edu RI Collin, Rachel/G-2001-2010 NR 22 TC 2 Z9 2 U1 0 U2 0 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 2005 VL 41 IS 2 BP 269 EP 276 PG 8 WC Biodiversity Conservation SC Biodiversity & Conservation GA 956UO UT WOS:000231325600008 ER PT J AU Olson, SL AF Olson, SL TI Refutation of the historical evidence for a Hispaniolan macaw (Aves : Psittacidae : Ara) SO CARIBBEAN JOURNAL OF SCIENCE LA English DT Article DE extinct birds; Hispaniola; Oviedo; parrots AB Historical accounts from Hispaniola in the 16(th) century have been misinterpreted since the late 19(th) century as indicating that three species of parrots once occurred on the island, one of which was thought to be a macaw (Ara). Careful rereading and analysis of these accounts show that only two parrots were described, which correspond exactly with the existing species Amazona ventralis and Aratinga chloroptera. There is now no credible evidence for the existence of a macaw on Hispaniola in historic times. C1 Smithsonian Inst, Natl Museum Nat Hist, Div Birds, Washington, DC 20560 USA. RP Olson, SL (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Div Birds, Washington, DC 20560 USA. EM olsons@si.edu NR 22 TC 1 Z9 2 U1 0 U2 1 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 2005 VL 41 IS 2 BP 319 EP 323 PG 5 WC Biodiversity Conservation SC Biodiversity & Conservation GA 956UO UT WOS:000231325600013 ER PT J AU Collin, R AF Collin, R TI Ecological monitoring and biodiversity surveys at the Smithsonian Tropical Research Institute's Bocas del Toro Research Station SO CARIBBEAN JOURNAL OF SCIENCE LA English DT Article ID STRAWBERRY POISON FROG; CORAL-REEFS; DENDROBATES-PUMILIO; CONSERVATION STATUS; CONTINENTAL REEFS; CARIBBEAN COAST; ANNOTATED LIST; PANAMA; BIOGEOGRAPHY; ARCHIPELAGO AB The Bocas del Toro Archipelago, site of the Smithsonian Tropical Research Institute's new Bocas Research Station, is a complex area of islands, mangrove cays, peninsulas, fringing reefs and seagrass beds on the Caribbean coast of Panama. The state-of-the-art research station runs long-term monitoring of physical and biological aspects of the local environments, that includes water and air temperature, precipitation, and tidal height. Biological monitoring includes annual or biannual surveys of seagrass productivity, mangrove forests and coral cover at reef sites. In 2003 and 2004 the station hosted workshops focused on taxonomic surveys of the marine fauna in the vicinity of the station. Collections of most major phyla resulted in the discovery of several new species and produced numerous new records for the country and region. This peer-reviewed special issue of the Caribbean journal of Science presents results of the ongoing monitoring and faunal surveys with the goal of providing a solid foundation and context for future research in the area. C1 Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Collin, R (reprint author), Smithsonian Trop Res Inst, Apartado Postal 0843-03092, Balboa, Ancon, Panama. EM collinr@naos.si.edu RI Collin, Rachel/G-2001-2010 NR 15 TC 7 Z9 8 U1 3 U2 9 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 2005 VL 41 IS 3 BP 367 EP 373 PG 7 WC Biodiversity Conservation SC Biodiversity & Conservation GA 000KD UT WOS:000234459600001 ER PT J AU Coates, AG McNeill, DF Aubry, MP Berggren, WA Collins, LS AF Coates, AG McNeill, DF Aubry, MP Berggren, WA Collins, LS TI An introduction to the geology of the Bocas del Toro archipelago, Panama SO CARIBBEAN JOURNAL OF SCIENCE LA English DT Article DE neogene; Bocas del Toro; Central American isthmus ID COSTA-RICA; WESTERN PANAMA; SOUTH-AMERICA; COCOS-RIDGE; ISTHMUS; STRATIGRAPHY; EMERGENCE; CLOSURE; LIMON; ARC AB We review the stratigraphy of the Neogene rocks of the Bocas del Toro archipelago, western Caribbean coast of Panama, and provide new geological maps and a preliminary description of new Neogene formations on the islands of Bastimentos and Colon. The Punta Alegre and Valiente formations range in age from 19 to 12 Ma. After a hiatus from 12 to 8 Ma, a transgressive/regressive sedimentary cycle is recorded by the Tobobe, Nancy Point, Shark Hole, Cayo Agua, and Escudo de Veraguas formations (=the Bocas del Toro Group), that range in age from 7.2-5.3 to 1.8 Ma. In contrast, in the northern region, the Old Bank, La Gruta, and Ground Creek units and the Swan Cay Formation only range in age from about 3.5 to 0.78 Ma. The hiatus represented by the unconformity is from 12 to 3.5 Ma. We integrate the geology of the Bocas del Toro archipelago into a brief history of the Neogene of the lower Central American isthmus. C1 Smithsonian Trop Res Inst, Balboa, Panama. Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, Div Marine Geol & Geophys, Miami, FL 33149 USA. Rutgers State Univ, Dept Geol Sci, Piscataway, NJ 08854 USA. Woods Hole Oceanog Inst, Dept Geol & Geophys, Woods Hole, MA 02543 USA. Florida Int Univ, Dept Earth Sci, Miami, FL 33199 USA. RP Coates, AG (reprint author), Smithsonian Trop Res Inst, Apartado 2072, Balboa, Panama. EM coatesj@hardynet.com NR 34 TC 43 Z9 50 U1 1 U2 8 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 2005 VL 41 IS 3 BP 374 EP 391 PG 18 WC Biodiversity Conservation SC Biodiversity & Conservation GA 000KD UT WOS:000234459600002 ER PT J AU Kaufmann, KW Thompson, RC AF Kaufmann, KW Thompson, RC TI Water temperature variation and the meteorological and hydrographic environment of Bocas del Toro, Panama SO CARIBBEAN JOURNAL OF SCIENCE LA English DT Article DE rainfall; water temperature; solar radiation; wind speed; Central America; temperature stress; coral bleaching ID NORTHWESTERN SOUTH-AMERICA; DIURNAL PATTERNS; RAINFALL AB Bahia Almirante is a shallow lagoon on the Caribbean coast of western Panama almost entirely surrounded by land. Rainfall is most intense during the night and least intense in the late afternoon, a pattern common in tropical coastal areas. Water temperatures are often elevated in the inshore waters relative to surface temperatures immediately offshore, at times exceeding 30 degrees C. Analysis of solar radiation, wind speed, humidity and air temperature indicate that variations in solar radiation and wind speed were responsible for much of the observed excursions from the offshore temperatures. Environmentally stressful temperatures can result from a month or two of clear skies, and an equal period of cloudy skies can bring the temperatures down again rapidly. Shallow water has the most extreme daily and annual ranges in temperature, but water up to 20 m shows a similar range in temperatures over periods of several years. Salinity at the surface is usually 30 to 34 ppt, but can drop to as low as 20 ppt after heavy rain. Historical records of monthly rainfall explain only 9.6% of the variation in monthly water temperature changes. There appears to be a thermal gradient in the bay and adjacent areas across three sites with for which we have 4 to 6 years of hourly temperature data. The innermost site, closest to the mainland, had the highest mean temperature and the highest range in temperature. The two sites on the seaward side of the bay had less extreme temperatures. C1 Smithsonian Trop Res Inst, Balboa, Panama. RP Kaufmann, KW (reprint author), Smithsonian Trop Res Inst, POB 2072, Balboa, Panama. EM kaufmank@si.edu NR 17 TC 24 Z9 28 U1 0 U2 1 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 2005 VL 41 IS 3 BP 392 EP 413 PG 22 WC Biodiversity Conservation SC Biodiversity & Conservation GA 000KD UT WOS:000234459600003 ER PT J AU D'Croz, L Del Rosario, JB Gondola, P AF D'Croz, L Del Rosario, JB Gondola, P TI The effect of fresh water runoff on the distribution of dissolved inorganic nutrients and plankton in the Bocas del Toro archipelago, Caribbean Panama SO CARIBBEAN JOURNAL OF SCIENCE LA English DT Article DE Central America; eutrophication; chlorophyll a; zooplankton; coral reefs ID CORAL-REEFS; TROPHIC GRADIENTS; PHYTOPLANKTON; BAY; EUTROPHICATION; GROWTH; SEA; ENVIRONMENT; PHOSPHORUS; LIMITATION AB The distribution of dissolved inorganic nutrients (nitrate + nitrite, phosphate, and silicate) and plankton (chlorophyll a and zooplankton biomass) was investigated in the Bocas del Toro Archipelago, western Caribbean coast of Panama. The archipelago is naturally divided in two large semi-enclosed lagoons: the Chiriqui Lagoon which is a turbid environment under high influence from runoff, and Almirante Bay that is less affected by runoff. Three surveys were carried out covering both wet and dry months. Hydrological measures varied spatially between regions and temporally on a seasonal basis. High concentrations of nutrients, chlorophyll a, and zooplankton biomass coincided with heavy rainfalls. Significant inverse correlations between dissolved inorganic nutrients and salinity during the rainy months confirmed the nutrient contribution from runoff. When compared to the ocean exposed environments high concentrations of chlorophyll and zooplankton biomass were observed in the semi-enclosed lagoons. The episodes of natural eutrophication due to high levels of fresh water runoff in the Bocas del Toro Archipelago contrast to the nutrient and plankton poor waters in coral reef environments along the eastern Caribbean coast of the Isthmus of Panama. C1 Smithsonian Trop Res Inst, Balboa, Panama. Univ Panama, Dept Biol Marina & Limnol, Panama City, Panama. RP D'Croz, L (reprint author), Smithsonian Trop Res Inst, Box 2072, Balboa, Panama. EM dcrozl@naos.si.edu NR 50 TC 36 Z9 40 U1 0 U2 13 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 2005 VL 41 IS 3 BP 414 EP 429 PG 16 WC Biodiversity Conservation SC Biodiversity & Conservation GA 000KD UT WOS:000234459600004 ER PT J AU Guzman, HM Barnes, PAG Lovelock, CE Feller, IC AF Guzman, HM Barnes, PAG Lovelock, CE Feller, IC TI A site description of the CARICOMP mangrove, seagrass and coral reef sites in Bocas del Toro, Panama SO CARIBBEAN JOURNAL OF SCIENCE LA English DT Article DE environmental monitoring; CARICOMP; Bocas del Toro; Panama ID VS. PHOSPHORUS LIMITATION; POPULATION CHARACTERISTICS; NUTRIENT ENRICHMENT; CONSERVATION STATUS; CONTINENTAL REEFS; CARIBBEAN COAST; CENTRAL-AMERICA; FOREST; GROWTH; PHOTOSYNTHESIS AB Bocas del Toro is located in the western region of the Republic of Panama. It is part of a province of approximately 8917 km(2) with an estimated 68% of its area covered by tropical rainforest. The area receives 2870 mm/year of rainfall. The dry and rainy seasons are not clearly defined. There are two periods each of low and high rainfall, March and September-October, and July and December, respectively. Mangrove forests, seagrass meadows and coral reefs are vast, covering large areas in the shallow waters surrounding the islands of the archipelago and along the mainland coast. The CARICOMP sites were established in 1998-99 and are periodically monitored following Level I protocol. Herein we describe the sites in a regional context and present the baseline data for each site. This paper fulfills the requirements of the formal site description for CARICOMP monitoring sites. C1 Smithsonian Trop Res Inst, Balboa, Panama. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Guzman, HM (reprint author), Smithsonian Trop Res Inst, Box 2072, Balboa, Panama. EM guzmanh@naos.si.edu RI Lovelock, Catherine/G-7370-2012; OI Lovelock, Catherine/0000-0002-2219-6855; Feller, Ilka/0000-0002-6391-1608 NR 51 TC 22 Z9 25 U1 0 U2 4 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 2005 VL 41 IS 3 BP 430 EP 440 PG 11 WC Biodiversity Conservation SC Biodiversity & Conservation GA 000KD UT WOS:000234459600005 ER PT J AU Carruthers, TJB Barnes, PAG Jacome, GE Fourqurean, JW AF Carruthers, TJB Barnes, PAG Jacome, GE Fourqurean, JW TI Lagoon scale processes in a coastally influenced Caribbean system: Implications for the seagrass Thalassia testudinum SO CARIBBEAN JOURNAL OF SCIENCE LA English DT Article DE nitrogen; phosphorus; sediment; nutrient processes; Bocas del Toro; Panama ID BOCAS DEL TORO; N-P RATIOS; FLORIDA BAY; PHOSPHORUS LIMITATION; NUTRIENT AVAILABILITY; CARBONATE SEDIMENTS; CORAL-REEFS; PANAMA; PATTERNS; NITROGEN AB The Bocas del Toro archipelago in the Caribbean sea on the northwest coast of Panama has high annual rainfall (> 3000 mm) and a mountainous watershed, resulting in high inflow of fresh water. The two main lagoons have different geologic structure and different inputs; while Bahia Almirante has carbonate sediment and a relatively small watershed, Laguna de Chiriqui has predominantly siliclastic sediment and a very large watershed. The region also has a long history of clearing and agriculture. The purpose of this research was to use the seagrass Thalassia testudinum as a bio-indicator of nutrient status of these lagoons, particularly to assess the extent and influence of mainland inputs of freshwater, nutrients and sediments. Leaf tissue nitrogen and phosphorus, as well as surface water quality and porewater nutrients, were measured from 32 sites throughout the archipelago. The Bocas del Toro archipelago showed clear but relatively small differences in these parameters between the carbonate, moderate freshwater input Bahia Almirante and the siliclastic, high freshwater input Laguna de Chiriqui. No evidence of a mainland to offshore (Cayos Zapatillos) gradient in nutrient status was observed in T. testudinum meadows. Leaf tissue nitrogen (ca. 2.4%) and phosphorus (ca. 0.25%) as well as chlorophyll a concentrations were high throughout the archipelago and higher than many tropical seagrass dominated ecosystems of the Caribbean. It is likely that this is partly a result of the mountainous, volcanic watershed and high rainfall, but the influence of extensive agriculture and land clearing has yet to be explicitly determined. C1 Smithsonian Trop Res Inst, Balboa, Panama. Florida Int Univ, Dept Biol Sci, Miami, FL 33199 USA. Florida Int Univ, SE Environm Res Ctr, Miami, FL 33199 USA. RP Carruthers, TJB (reprint author), Univ Maryland, Ctr Environm Sci, Integrat & Applicat Network, 2020 Horns Point Rd, Cambridge, MD 21613 USA. EM tcarruth@umces.edu RI Fourqurean, James/B-4606-2008 OI Fourqurean, James/0000-0002-0811-8500 NR 43 TC 9 Z9 12 U1 0 U2 10 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 2005 VL 41 IS 3 BP 441 EP 455 PG 15 WC Biodiversity Conservation SC Biodiversity & Conservation GA 000KD UT WOS:000234459600006 ER PT J AU Lovelock, CE Feller, IC McKee, KL Thompson, R AF Lovelock, CE Feller, IC McKee, KL Thompson, R TI Variation in mangrove forest structure and sediment characteristics in Bocas del Toro, Panama SO CARIBBEAN JOURNAL OF SCIENCE LA English DT Article DE Rhizophora mangle; dwarf forests; biomass ID VS. PHOSPHORUS LIMITATION; CORAL-REEFS; ABOVEGROUND BIOMASS; RHIZOPHORA-MANGLE; GROWTH; ISLANDS; ECOSYSTEMS; DYNAMICS; SEEDLINGS; GRADIENT AB Mangrove forest structure and sediment characteristics were examined in the extensive mangroves of Bocas del Toro, Republic of Panama. Forest structure was characterized to determine if spatial vegetation patterns were repeated over the Bocas del Toro landscape. Using a series of permanent plots and transects we found that the forests of Bocas del Toro were dominated by Rhizophora maugle with very few individuals of Avicennia germinans and Laguncularia racemosa. Despite this low species diversity, there was large variation in forest structure and in edaphic conditions (salinity, concentration of available phosphorus, Eh and sulphide concentration). Aboveground biomass varied 20-fold, from 6.8 Mg ha(-1) in dwarf forests to 194.3 Mg ha(-1) in the forests fringing the land. But variation in forest structure was predictable across the intertidal zone. There was a strong tree height gradient from seaward fringe (mean tree height 3.9 m), decreasing in stature in the interior dwarf forests (mean tree height 0.7 m), and increasing in stature in forests adjacent to the terrestrial forest (mean tree height 4.1 m). The predictable variation in forest structure emerges due to the complex interactions among edaphic and plant factors. Identifying predictable patterns in forest structure will aid in scaling up the ecosystem services provided by mangrove forests in coastal landscapes. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Univ Queensland, Ctr Marine Studies, St Lucia, Qld 4072, Australia. Univ Queensland, Sch Life Sci, St Lucia, Qld 4072, Australia. US Geol Survey, Natl Wetlands Res Ctr, Lafayette, LA 70506 USA. Smithsonian Trop Res Inst, Balboa, Panama. RP Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM c.lovelock@uq.edu.au RI Lovelock, Catherine/G-7370-2012; McKee, Karen/D-1365-2014; OI Lovelock, Catherine/0000-0002-2219-6855; McKee, Karen/0000-0001-7042-670X; Feller, Ilka/0000-0002-6391-1608 NR 45 TC 46 Z9 50 U1 3 U2 21 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 2005 VL 41 IS 3 BP 456 EP 464 PG 9 WC Biodiversity Conservation SC Biodiversity & Conservation GA 000KD UT WOS:000234459600007 ER PT J AU Diaz, MC AF Diaz, MC TI Common sponges from shallow marine habitats from Bocas del Toro region, Panama SO CARIBBEAN JOURNAL OF SCIENCE LA English DT Article DE sponges; biodiversity; mangrove; reefs; field guide ID CORAL-REEFS; TWIN-CAYS; COMMUNITIES; BELIZE; ABUNDANCE; PORIFERA; ISLANDS AB A survey of Porifera biodiversity and distribution was done in three islands of the Bocas del Toro region, Panama. Fourteen sites were explored using mask and snorkel, and occasionally scuba equipment, during ten days. Forty-one species are added to the species known for the region. Our current estimate of sponge diversity in shallow exposed marine habitats of Bocas del Toro is 120 species. Twenty-three species are added to the Panamanian sponge fauna, four of which are new species currently being described. A patchy distribution was observed for most of the sponge species, while few species were present at all sites visited. Approximately 23% (30 species) of the diversity encountered was widely distributed. The species composition of the most typical or common sponges from reef, seagrass beds, or mangrove habitats, agrees with that of other Caribbean sites. An appendix with a field guide to the species encountered in this study is presented. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Zool, Washington, DC 20560 USA. Museo Marino Margarita, Nueva Esparta, Venezuela. RP Diaz, MC (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Zool, Washington, DC 20560 USA. EM crisdiaz@ix.netcom.com NR 33 TC 30 Z9 39 U1 3 U2 12 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 2005 VL 41 IS 3 BP 465 EP 475 PG 11 WC Biodiversity Conservation SC Biodiversity & Conservation GA 000KD UT WOS:000234459600008 ER PT J AU Schulze, A AF Schulze, A TI Sipuncula (Peanut worms) from Bocas del Toro, Panama SO CARIBBEAN JOURNAL OF SCIENCE LA English DT Article DE peanut worms; invertebrate; Caribbean; larvae; pelagosphera; diversity AB In a survey of sipunculan diversity in the Bocas del Toro (Panama) region, sipunculans were collected from 10 stations, ranging in depth from intertidal to 37 m. Nineteen species of adult sipunculans were collected. In addition, two types of pelagic sipunculan larvae were retrieved from plankton tows. Thirteen of the adult sipunculan species were inhabitants of hard substrate, either in crevices or burrowing into rocks. These included representatives of the genera Antillesoma, Aspidosiphon, Golfingia, Nephasoma, Phascolosoma, Phascolion and Themiste. An unidentified Phascolion, an unidentified Aspidosiphon and Antillesoma antillarum (the latter usually an inhabitant of rock crevices) were retrieved from gastropod shells. Sipunculidae sp., Sipunculus sp., Phascolion sp. and Nephasoma cf. eremita were recovered by trawling in soft mud. While the hard-substrate sipunculans are all well-known and widely distributed species, three of the four soft-substrate inhabitants were morphologically unusual and/or unexpected in tropical waters. C1 Smithsonian Marine Stn, Ft Pierce, FL 34949 USA. RP Schulze, A (reprint author), Smithsonian Marine Stn, 701 Seaway Dr, Ft Pierce, FL 34949 USA. EM schulze@sms.si.edu RI Schulze, Anja/I-4215-2012 NR 13 TC 6 Z9 8 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 2005 VL 41 IS 3 BP 523 EP 527 PG 5 WC Biodiversity Conservation SC Biodiversity & Conservation GA 000KD UT WOS:000234459600012 ER PT J AU Schwartz, ML Norenburg, JL AF Schwartz, ML Norenburg, JL TI Three new species of Micrura (Nemertea : Heteronemertea) and a new type of heteronemertean larva from the Caribbean sea SO CARIBBEAN JOURNAL OF SCIENCE LA English DT Article DE Nemertea; taxonomy; pilidium; direct development ID PHYLOGENY AB Three new species of Micrura are described from shallow water of the Belize barrier reef and Bahia Almirante, Panama. Specimens were found at 0-30 m depth in association with a variety of rubble and its encrusting epibiota. The three species are morphologically very similar to each other, and are distinguished here primarily by color and by substantial differences in nucleotide sequence data for 16S rDNA and 28S rDNA. As many Micrura, they are slightly compressed dorso-ventrally, possess a caudal cirrus, and the cephalic lobe is bluntly rounded anteriorly and is the same width as the body. At least one species has distinct oblique musculature between the body-wall circular and inner longitudinal musculatures. One of the three species possesses a new morphotype larva rather than the expected typical pilidium larva. C1 George Washington Univ, Dept Biol, Washington, DC 20052 USA. Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Schwartz, ML (reprint author), George Washington Univ, Dept Biol, Washington, DC 20052 USA. EM schwartzm@seattleu.edu RI Norenburg, Jon/K-3481-2015 OI Norenburg, Jon/0000-0001-7776-1527 NR 21 TC 19 Z9 21 U1 0 U2 0 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 2005 VL 41 IS 3 BP 528 EP 543 PG 16 WC Biodiversity Conservation SC Biodiversity & Conservation GA 000KD UT WOS:000234459600013 ER PT J AU Collin, R Diaz, MC Norenburg, J Rocha, RM Sanchez, JA Schulze, A Schwartz, M Valdes, A AF Collin, R Diaz, MC Norenburg, J Rocha, RM Sanchez, JA Schulze, A Schwartz, M Valdes, A TI Photographic identification guide to some common marine invertebrates of Bocas del Toro, Panama SO CARIBBEAN JOURNAL OF SCIENCE LA English DT Article C1 Smithsonian Trop Res Inst, Balboa, Panama. Museo Marino Margarita, Nueva Esparta, Venezuela. Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. Univ Fed Parana, Dept Zool, BR-81531980 Curitiba, Parana, Brazil. Univ Los Andes, Dept Ciencias Biol, Bogota, Colombia. Smithsonian Marine Stn, Ft Pierce, FL 34949 USA. Natl Hist Museum Los Angeles Cty, Los Angeles, CA 90007 USA. RP Collin, R (reprint author), Smithsonian Trop Res Inst, Apartado Postal 0843-03092, Balboa, Panama. RI Collin, Rachel/G-2001-2010; Valdes, Angel/K-3051-2012; Schulze, Anja/I-4215-2012; Norenburg, Jon/K-3481-2015 OI Valdes, Angel/0000-0002-2347-4896; Norenburg, Jon/0000-0001-7776-1527 NR 0 TC 31 Z9 39 U1 0 U2 1 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 2005 VL 41 IS 3 BP 638 EP 707 PG 70 WC Biodiversity Conservation SC Biodiversity & Conservation GA 000KD UT WOS:000234459600018 ER PT S AU Sorensen, SS Sisson, VB Lallemant, HGA AF Sorensen, Sorena S. Sisson, Virginia B. Lallemant, Hans G. Ave BE AveLallemant, HG Sisson, VB TI Geochemical evidence for possible trench provenance and fluid-rock histories, Cordillera de la Costa eclogite belt, Venezuela SO CARIBBEAN-SOUTH AMERICAN PLATE INTERACTIONS, VENEZUELA SE Geological Society of America Special Papers LA English DT Article; Book Chapter DE Venezuela; trace elements; eclogite; garnet amphibolite; Cordillera de la Costa ID MEXICAN VOLCANIC BELT; MOTAGUA FAULT ZONE; SUBDUCTION ZONE; CATALINA-SCHIST; SOUTHERN-CALIFORNIA; ISLA-MARGARITA; EXTENSIONAL TECTONICS; GARNET AMPHIBOLITES; CALC-ALKALINE; METASOMATISM AB The Cordillera de la Costa eclogite belt, exposed along the Caribbean coastline of Venezuela near Puerto Cabello, consists of lensoid bodies and boudins of high pressure-temperature (P-T) metabasite in a heterogeneous matrix of mica schist and metacarbonate rocks. The metabasite bodies consist of eclogite and its retrogression products. Data for less mobile elements indicate that protoliths ranged from normal mid-oceanic-ridge basalt (N-MORB), to enriched (E)-MORB, to cumulate gabbro. Some eclogites and their retrogression products are enriched in large ion lithophile elements (LILE). The covariations of K and Ba are evidence that these elements were most likely incorporated into phengite, which has textures that suggest it crystallized from retrograde fluids. A similar style of LILE enrichment is also documented for eclogites of the Samana Peninsula, Dominican Republic, but not in eclogites from Isla de Margarita, Venezuela. Low-T, K-metasomatized basalts from the Bermuda Rise display different K-Ba systematics than the eclogite suites, which suggests that LILE enrichment of the latter rocks was not merely inherited from altered protoliths. In contrast to the LILE-enriched eclogites, some Cordillera de la Costa belt eclogite bodies have apparently been stripped of K, Rb, Ba, and U. Some metasedimentary rocks, in an outcrop that also contains LILE- poor metabasite, also show extreme LILE depletion relative to counterparts elsewhere in the Cordillera de la Costa. In this outcrop, LILE are most conspicuously depleted in a lens of kyanite + glaucophane schist that formed at P > 20 kb, T similar to 600 degrees C. Although the rock has Al/Si ratios, rare earth element, and high field strength element abundances comparable to shale, it contains <0.3 wt% K2O. Some rocks of the Cordillera de la Costa eclogite belt thus appear to record LILE expulsion, probably at the "peak" P-T conditions of P > 20 kb at T similar to 600 degrees C, whereas others chronicle LILE enrichment during retrogression at lower P-T conditions. Some outcrops show both effects. In a few outcrops, eclogitic blocks that appear to be LILE-depleted occur in metasedimentary host rocks that are not. C1 [Sorensen, Sorena S.] Smithsonian Inst, Dept Mineral Sci, Natl Museum Nat Hist, Washington, DC 20560 USA. [Sisson, Virginia B.; Lallemant, Hans G. Ave] Rice Univ, Dept Earth Sci, Houston, TX 77005 USA. RP Sorensen, SS (reprint author), Smithsonian Inst, Dept Mineral Sci, Natl Museum Nat Hist, NHB-119, Washington, DC 20560 USA. EM sorena@volcano.si.edu; j_sisson@netzero.com; ave@rice.edu NR 68 TC 4 Z9 4 U1 0 U2 0 PU GEOLOGICAL SOC AMER INC PI BOULDER PA 3300 PENROSE PL, PO BOX 9140, BOULDER, CO 80301 USA SN 0072-1077 BN 978-0-8137-2394-5 J9 GEOL SOC AM SPEC PAP PY 2005 VL 394 BP 173 EP 192 DI 10.1130/2005.SPE394(06) PG 20 WC Geochemistry & Geophysics; Geology SC Geochemistry & Geophysics; Geology GA BLY12 UT WOS:000271394900007 ER PT S AU Jones, C Forman, W Kraft, R Markevitch, M Nulsen, P Vikhlinin, A Churazov, E Heinz, S AF Jones, C Forman, W Kraft, R Markevitch, M Nulsen, P Vikhlinin, A Churazov, E Heinz, S BE Kaastra, JS TI Outbursts from the supermassive black hole in M87 and the impact on the hot gas SO CLUSTERS OF GALAXIES: NEW INSIGHTS FROM XMM-NEWTON, CHANDRA AND INTEGRAL SE ADVANCES IN SPACE RESEARCH-SERIES LA English DT Article; Proceedings Paper CT 35th COSPAR Scientific Assembly CY JUL 18-25, 2004 CL Paris, FRANCE SP Comm Space Res DE AGN outbursts; cooling flows; elliptical galaxies; shocks; ICM ID EARLY-TYPE GALAXIES; RAY-EMITTING GAS; COOLING FLOWS; THERMAL CONDUCTION; CHANDRA OBSERVATION; INTRACLUSTER MEDIUM; BUOYANT BUBBLES; VIRGO CLUSTER; RADIO LOBES; MODELS AB Deep Chandra, XMM-Newton and ROSAT observations show the impact of AGN outbursts on M87's hot gaseous atmosphere. Many X-ray features, including X-ray cavities around the jet and counterjet and rings of enhanced emission appear to be the direct result of repetitive AGN outbursts. The rings of emission Lit 14 and 17 kpc are likely shock fronts. The energetics of the M87 outbursts show that shocks may be the most significant channel for AGN input into its cooling flow atmosphere. The X-ray, as well as the radio observations, show not only the current state of the AGN, but by looking at the reflections of those outbursts in the surrounding gas, we can learn the history of AGN outbursts. (c) 2005 Published by Elsevier Ltd on behalf of COSPAR. C1 Harvard Smithsonian Ctr Astrophys, High Energy Astrophys Div, Cambridge, MA 02138 USA. Max Planck Inst Astrophys, D-85741 Garching, Germany. Russian Acad Sci, Inst Space Res, Moscow V71, Russia. MIT, Cambridge, MA 02139 USA. RP Jones, C (reprint author), Harvard Smithsonian Ctr Astrophys, High Energy Astrophys Div, 60 Garden St, Cambridge, MA 02138 USA. EM cjf@cfa.harvard.edu RI Churazov, Eugene/A-7783-2013; OI Heinz, Sebastian/0000-0002-8433-8652; Forman, William/0000-0002-9478-1682 NR 41 TC 1 Z9 1 U1 0 U2 0 PU ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD 0X5 1GB, OXON, ENGLAND SN 0273-1177 J9 ADV SPACE RES-SERIES PY 2005 VL 36 IS 4 SI 2005 BP 597 EP 600 DI 10.1016/j.asr.2004.12.063 PG 4 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BDR55 UT WOS:000235098100001 ER PT S AU Durret, F Neto, GBL Forman, W AF Durret, F Neto, GBL Forman, W BE Kaastra, JS TI The merging cluster Abell 85 caught between meals by XMM-Newton SO CLUSTERS OF GALAXIES: NEW INSIGHTS FROM XMM-NEWTON, CHANDRA AND INTEGRAL SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT 35th COSPAR Scientific Assembly CY JUL 18-25, 2004 CL Paris, FRANCE SP Comm Space Res DE clusters of galaxies; Abell 85; X-rays ID RICH CLUSTER; GALAXIES ABELL-85; TEMPERATURE; ENTROPY; CATALOG AB Our XMM-Newton observations of Abell 85 confirm the extended 4 Mpc filament first detected with ROSAT, which has an Xray temperature of about similar to 2 keV and is probably made of groups failing on to the cluster. A comparison of the temperature map with numerical simulations show that Abell 85 had intense merging activity in the past and is not fully relaxed, even in the central region. Finally, a deprojected temperature profile has been calculated and used, together with the surface brightness, to estimate the entropy and pressure profiles. Abell 85 only presents a mild flattening of the entropy profile in the center, showing no evidence of an "entropy floor". (c) 2005 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 Inst Astrophys Paris, F-75014 Paris, France. USP, IAG, BR-05508090 Sao Paulo, Brazil. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Durret, F (reprint author), Inst Astrophys Paris, 98Bis Bd Arago, F-75014 Paris, France. EM durret@iap.fr RI Lima Neto, Gastao/J-6117-2014; OI Forman, William/0000-0002-9478-1682 NR 17 TC 3 Z9 3 U1 0 U2 0 PU ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD 0X5 1GB, OXON, ENGLAND SN 0273-1177 J9 ADV SPACE RES PY 2005 VL 36 IS 4 SI 2005 BP 618 EP 621 DI 10.1016/j.asr.2005.01.035 PG 4 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BDR55 UT WOS:000235098100005 ER PT S AU Nicastro, F Elvis, M Fiore, F Mathur, S AF Nicastro, F Elvis, M Fiore, F Mathur, S BE Kaastra, JS TI Measured cosmological mass density in the WHIM: The solution to the 'Missing Baryons' problem SO CLUSTERS OF GALAXIES: NEW INSIGHTS FROM XMM-NEWTON, CHANDRA AND INTEGRAL SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT 35th COSPAR Scientific Assembly CY JUL 18-25, 2004 CL Paris, FRANCE SP Comm Space Res DE IGM; WHIM; cosmological mass density ID X-RAY FOREST; LY-ALPHA FOREST; INTERGALACTIC MEDIUM; SPACE-TELESCOPE; WMAP OBSERVATIONS; ABSORPTION; EMISSION; SPECTRA; SYSTEMS AB We review the current high-significance X-ray detections of Warm-Hot Intergalactic Medium (WHIM) filaments at z > 0 along the lines of sight to the two blazars Mrk 421 (z = 0.03) and 1ES 1028 + 511 (z = 0.361). For these WHIM filaments, we derive ionization corrections and, when possible, metallicity estimates. This allows LIS to obtain refined estimates of the number density of O VII WHIM systems down to the 0 VII Column density sensitivity of our observations, and most importantly, a measurement of the cosmological mass density Omega(b)(WHIM) in the WHIM, Lit redshift z < 0.361. These estimates agree well with model predictions and with the total estimated amount of missing baryons in the local Universe, although errors are large, due to the still limited number of systems. We conclude discussing future observational strategies and mission designs for WHIM studies. (c) 2005 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. Osserv Astron Roma, Monte Porzio Catone, Italy. RP Nicastro, F (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-83, Cambridge, MA 02138 USA. EM fnicastro@cfa.harvard.edu OI Nicastro, Fabrizio/0000-0002-6896-1364; Fiore, Fabrizio/0000-0002-4031-4157 NR 23 TC 5 Z9 5 U1 0 U2 0 PU ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD 0X5 1GB, OXON, ENGLAND SN 0273-1177 J9 ADV SPACE RES PY 2005 VL 36 IS 4 SI 2005 BP 721 EP 726 DI 10.1016/j.asr.2005.01.053 PG 6 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BDR55 UT WOS:000235098100025 ER PT J AU Moser, WE Van Devender, RW Klemm, DJ AF Moser, WE Van Devender, RW Klemm, DJ TI Life history and distribution of the leech Oligobdella biannulata (Moore, 1900) (Euhirudinea : Glossiphoniidae) SO COMPARATIVE PARASITOLOGY LA English DT Article DE Hirudinea; Euhirudinea; rhynchobdellida; Glossiphonidae; Oligobdella biannulata; salamanders; desmognathinae; Desmognathus quadramaculatus; Desmognathus marmoratus AB Oligobdella biannulata is a rare, endemic leech species originally described from a mountain stream near Blowing Rock, North Carolina, U.S.A. Specimens of O. biannulata were collected seasonally (fall 1999-summer 2002), documenting new county records from North Carolina and South Carolina and new state records from Georgia and Tennessee, U.S.A. Fifty-one percent of Desmognathus quadramaculatus and 50% of Desmognathus marmoratus were parasitized with O. biannulata. Between late May and early July, O. biannulata leaves its salamander host to lay 15-30 bright yellow, yolky eggs and brood them on its ventral surface. Eggs hatch in 10-20 d, and in about 50 d both hatchlings and adult search for a blood meal. Oligobdella biannulata reattaches to its host between late August and early October. When a desmognathine salamander host is found the adult leech attaches and hatchlings leave the adult, attaching singly or in clusters on the limbs or axillary and inguinal regions of the salamander, blood feeding, and overwintering on the host. C1 Natl Museum Nat Hist, Smithsonian Inst, Dept Zool, Washington, DC 20013 USA. Appalachian State Univ, Dept Biol, Boone, NC 28608 USA. US EPA, Natl Exposure Res Lab, Ecol Exposure Res Div, Ecosyst Res Branch, Cincinnati, OH 45268 USA. RP Moser, WE (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Dept Zool, MRC-163,POB 37012, Washington, DC 20013 USA. EM moser.william@nmnh.si.edu; vandevenderr@appstate.edu; klemm.donald@epa.gov NR 12 TC 7 Z9 7 U1 0 U2 3 PU HELMINTHOLOGICAL SOC WASHINGTON PI LAWRENCE PA C/O ALLEN PRESS INC, 1041 NEW HAMPSHIRE ST, LAWRENCE, KS 66044 USA SN 1525-2647 J9 COMP PARASITOL JI Comp. Parasitol. PD JAN PY 2005 VL 72 IS 1 BP 17 EP 21 DI 10.1654/4160 PG 5 WC Parasitology; Zoology SC Parasitology; Zoology GA 894PJ UT WOS:000226803800004 ER PT J AU Ernst, CH AF Ernst, CH TI The type host of Neoechinorhynchus schmidti (Acanthocephala : Neoechinorhynchidae): A correction SO COMPARATIVE PARASITOLOGY LA English DT Article DE Acanthocephala; Neoechinorhynchidae; Neoechinorhynchus schmidti; type host; turtle host; Tabasco slider; Trachemys venusta; Tabasco; Mexico ID TRACHEMYS AB The type host of the acanthocephalan Neoechinorhynchus schmidti from Tabasco, Mexico, was erroneously reported to be the red-eared slider, Trachemys scripta elegans, which does not occur in Tabasco. Examination of specimens from the turtle host series determined that the correct type host is the Tabasco slider, Trachemys venusta. C1 Smithsonian Inst, Div Amphibians & Reptiles, Washington, DC 20013 USA. RP Ernst, CH (reprint author), Smithsonian Inst, Div Amphibians & Reptiles, MRC 162,POB 37012, Washington, DC 20013 USA. EM motherbox2@aol.com NR 6 TC 1 Z9 2 U1 0 U2 2 PU HELMINTHOLOGICAL SOC WASHINGTON PI LAWRENCE PA C/O ALLEN PRESS INC, 1041 NEW HAMPSHIRE ST, LAWRENCE, KS 66044 USA SN 1525-2647 J9 COMP PARASITOL JI Comp. Parasitol. PD JAN PY 2005 VL 72 IS 1 BP 118 EP 118 DI 10.1654/4163 PG 1 WC Parasitology; Zoology SC Parasitology; Zoology GA 894PJ UT WOS:000226803800016 ER PT S AU Babb, JF AF Babb, JF BE Weiner, J Feenstra, L Schmiedmayer, J TI Long-range atom-surface interactions for cold atoms SO CONFERENCE ON ATOMS AND MOLECULES NEAR SURFACES SE Journal of Physics Conference Series LA English DT Proceedings Paper CT International Conference on Atoms and Molecules Near Surfaces CY APR 04-08, 2005 CL Int Wissenschaft Forum Ruprech-Karls Univ, Heidelberg, GERMANY HO Int Wissenschaft Forum Ruprech-Karls Univ ID VAN-DER-WAALS; ZERO-POINT RADIATION; ALKALI-METAL ATOMS; CASIMIR INTERACTIONS; VANDERWAALS FORCES; CLASSICAL ELECTRODYNAMICS; DISPERSION COEFFICIENTS; POTENTIALS; INTERFACE; MOLECULES AB Studies of the long-range interactions between cold atoms and surfaces are now of vital interest. The interest is partly driven by nanotechnology applications, partly by the exploding interest in the encompassing superfield of Casimir effects, and partly by the burgeoning overlap between atomic and molecular physics, condensed matter, and quantum optics. This tutorial lecture will address long-range atom-surface interactions for cold atoms, including an overview of Casimir-Polder interactions and their various manifestations. Some previous theoretical studies that are of particular relevance will be reviewed. In addition some different approaches to the problem and corresponding results, especially concerning the effects of substrate composition, geometry, and finite temperature, will be discussed. C1 Harvard Smithsonian Ctr Astrophys, Ins Theoret Atom Mol & Opt Phys, Cambridge, MA 02138 USA. RP Babb, JF (reprint author), Harvard Smithsonian Ctr Astrophys, Ins Theoret Atom Mol & Opt Phys, MS 14,60 Garden St, Cambridge, MA 02138 USA. EM jbabb@cfa.harvard.edu OI Babb, James/0000-0002-3883-9501 NR 50 TC 4 Z9 4 U1 1 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 1742-6588 J9 J PHYS CONF SER PY 2005 VL 19 BP 1 EP 9 DI 10.1088/1742-6596/19/1/001 PG 9 WC Physics, Atomic, Molecular & Chemical SC Physics GA BDE29 UT WOS:000233011800001 ER PT J AU Schwartz, MK Ralls, K Williams, DF Cypher, BL Pilgrim, KL Fleischer, RC AF Schwartz, MK Ralls, K Williams, DF Cypher, BL Pilgrim, KL Fleischer, RC TI Gene flow among San Joaquin kit fox populations in a severely changed ecosystem SO CONSERVATION GENETICS LA English DT Article DE gene flow; kit fox; microsatellite; population genetics; Vulpes macrotis mutica ID MULTILOCUS GENOTYPES; ONE-MIGRANT; DISPERSAL; INDIVIDUALS; EXTINCTION; MIGRATION; TESTS; SIZE; DIFFERENTIATION; CONSERVATION AB The San Joaquin kit fox (Vulpes macrotis mutica) was once ubiquitous throughout California's San Joaquin Valley and its surrounds. However, most of its habitat has been lost to irrigated agriculture, urban development, and oil fields. The remaining foxes are concentrated in six areas, although there are several small pockets of foxes throughout the Valley. To help conserve kit foxes, we sought an ecological understanding of the level of genetic variation remaining in these locations and the extent of gene flow among them. We collected tissue from 317 kit foxes from 8 sites and estimated genetic variability in and gene flow among sites using data from 8 polymorphic, microsatellite markers. We found no differences in both observed and expected heterozygosity between locations using Bonferonni corrected paired t-tests. We found differences in mean number of alleles per locus, even after we used Monte Carlo simulations to adjust for sample size differences. Population subdivision was low among sites (F-st=0.043), yet a matrix of pairwise F-st values was correlated with a matrix of pairwise geographic distances. An assignment test classified only 45% of the individuals to the site where they were captured. Overall, these data suggest that kit fox dispersal between locations may still maintain genetic variation throughout most of the areas we sampled. C1 Univ Montana, Wildlife Biol Program, Missoula, MT 59812 USA. USDA, USFS, Rocky Mt Res Stn, Missoula, MT 59801 USA. Smithsonian Inst, Natl Zool Pk, Washington, DC 20008 USA. Calif State Univ Stanislaus, Dept Biol Sci, Turlock, CA 95382 USA. Calif State Univ Stanislaus, Endangered Species Recovery Program, Turlock, CA 95382 USA. Calif State Univ, Endangered Species Recovery Program, Bakersfield, CA 93389 USA. RP Schwartz, MK (reprint author), Univ Montana, Wildlife Biol Program, Missoula, MT 59812 USA. EM mkschwartz@fs.fed.us RI Schwartz, Michael/C-3184-2014 OI Schwartz, Michael/0000-0003-3521-3367 NR 68 TC 15 Z9 16 U1 1 U2 24 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 1566-0621 J9 CONSERV GENET JI Conserv. Genet. PD JAN PY 2005 VL 6 IS 1 BP 25 EP 37 DI 10.1007/s10592-004-7719-8 PG 13 WC Biodiversity Conservation; Genetics & Heredity SC Biodiversity & Conservation; Genetics & Heredity GA 910ND UT WOS:000227937300003 ER PT J AU Flores, J AF Flores, Juan BE Knight, FW MartinezVergne, T TI Creolite in the Hood: Diaspora as Source and Challenge SO CONTEMPORARY CARIBBEAN CULTURES AND SOCIETIES IN A GLOBAL CONTEXT LA English DT Article; Book Chapter C1 [Flores, Juan] CUNY Hunter Coll, Dept Black & Puerto Rican Studies, New York, NY 10021 USA. [Flores, Juan] CUNY Grad Ctr, Sociol Program, New York, NY USA. [Flores, Juan] New York Council Humanities, New York, NY USA. [Flores, Juan] Smithsonian Inst, Latin Jazz Project, Washington, DC 20560 USA. [Flores, Juan] Smithsonian Inst, Hispan Literary Heritage Project, Washington, DC 20560 USA. NR 0 TC 2 Z9 2 U1 0 U2 0 PU UNIV NORTH CAROLINA PRESS PI CHAPEL HILL PA BOX 2288, CHAPEL HILL, NC 27514 USA BN 978-0-8078-7690-9 PY 2005 BP 117 EP 129 PG 13 WC History; Sociology SC History; Sociology GA BWR72 UT WOS:000294675500006 ER PT B AU Ho, PTP AF Ho, PTP BE Lidman, C Alloin, D TI Emission processes in the interstellar medium SO Cool Universe: Observing Cosmic Dawn SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Workshop of the International-Astronomical-Observatories-in-Chile (IAOC) CY OCT 04-08, 2004 CL Univ Tecn Santa Maria, Valparaiso, CHILE SP Int Astron Observ Chile, ESO, NOAO, LCO, GEMINI, NRAO, NAOJ HO Univ Tecn Santa Maria ID SUBMILLIMETER ARRAY; DEBRIS AB The bulk of the universe is in fact quite cool. The typical temperature which characterizes most of the interstellar medium is about 10 K. The peak of its spectral energy distribution lies at far-infrared and sub-millimeter wavelengths. The construction of ALMA in the Atacama desert will bring on line a very powerful instrument for studying the dust continuum emission as well as the many molecular lines which become detectable at millimeter and sub-millimeter wavelengths. Moreover, ALMA will provide sub-arcsecond angular resolution which will resolve a wide range of astrophysical phenomena, from solar system bodies to the most distant high redshift systems. Sub-millimeter interferometry is already underway with the completion of the Sub-millimeter Array (SMA) on Mauna Kea. The initial science results offer some hints of what. might be achievable in the next decade. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Ho, PTP (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. NR 6 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-211-3 J9 ASTR SOC P PY 2005 VL 344 BP 126 EP 139 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BDW56 UT WOS:000235843600016 ER PT B AU Beuther, H Shepherd, D AF Beuther, H Shepherd, D BE Kumar, MSN Tafalla, M Caselli, P TI Precursors of UCHII regions and the evolution of massive outflows SO Cores to Clusters: STAR FORMATION WITH NEXT GENERATION TELESCOPES SE ASTROPHYSICS AND SPACE SCIENCE LIBRARY LA English DT Proceedings Paper CT Workshop on Cores to Clusters CY OCT 07-09, 2004 CL Univ Porto, Ctr Astrofis, Oporto, PORTUGAL SP FCT, Fundacao Calouste Gulbenkian HO Univ Porto, Ctr Astrofis ID YOUNG STELLAR OBJECTS; STAR-FORMING REGIONS; BIPOLAR MOLECULAR OUTFLOWS; ULTRACOMPACT HII-REGIONS; LUMINOUS IRAS SOURCES; H-II REGIONS; METHANOL MASERS; PROTOSTELLAR CANDIDATES; SUBMILLIMETER CONTINUUM; MULTIPLE OUTFLOWS AB This paper covers two subjects in the field of massive star formation which in its details can be discussed separately. Therefore, we present first characteristics of precursors of UCHII regions and their likely evolutionary properties. The second section discusses massive molecular outflows, their implications for high-mass star formation, and a possible evolutionary sequence for massive outflows. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Beuther, H (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 82 TC 64 Z9 64 U1 0 U2 0 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013, UNITED STATES BN 0-387-26322-5 J9 ASTROPHYS SPACE SC L PY 2005 VL 324 BP 105 EP 119 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BDE55 UT WOS:000233083000008 ER PT B AU Keto, E AF Keto, E BE Kumar, MSN Tafalla, M Caselli, P TI Observations of accretion onto high mass stars SO Cores to Clusters: STAR FORMATION WITH NEXT GENERATION TELESCOPES SE ASTROPHYSICS AND SPACE SCIENCE LIBRARY LA English DT Proceedings Paper CT Workshop on Cores to Clusters CY OCT 07-09, 2004 CL Univ Porto, Ctr Astrofis, Oporto, PORTUGAL SP FCT, Fundacao Calouste Gulbenkian HO Univ Porto, Ctr Astrofis ID H-II REGIONS; MAIN-SEQUENCE; HII-REGIONS; EVOLUTION; G10.6-0.4; PHOTOEVAPORATION; COLLAPSE; CLOUDS; ORION; DISKS AB Observations of the H66 alpha recombination line from the ionized gas in the cluster of newly formed massive stars, G106-0.4, show that most of the continuum emission derives from the dense gas in an ionized accretion flow that forms an ionized disk or torus around a group of stars in the center of the cluster. The inward motion observed in the accretion flow suggests that despite the equivalent luminosity and ionizing radiation of several O stars, neither radiation pressure nor thermal pressure has reversed the accretion flow. The observations indicate why the radiation pressure of the stars and the thermal pressure of the HII region are not effective in reversing the accretion flow. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Keto, E (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 28 TC 0 Z9 0 U1 0 U2 1 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013, UNITED STATES BN 0-387-26322-5 J9 ASTROPHYS SPACE SC L PY 2005 VL 324 BP 121 EP 130 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BDE55 UT WOS:000233083000009 ER PT B AU Teixeira, PS Lada, CJ Alves, J AF Teixeira, PS Lada, CJ Alves, J BE Kumar, MSN Tafalla, M Caselli, P TI Revealing the structure of lupine darkness: From cores to clusters SO Cores to Clusters: STAR FORMATION WITH NEXT GENERATION TELESCOPES SE ASTROPHYSICS AND SPACE SCIENCE LIBRARY LA English DT Proceedings Paper CT Workshop on Cores to Clusters CY OCT 07-09, 2004 CL Univ Porto, Ctr Astrofis, Oporto, PORTUGAL SP FCT, Fundacao Calouste Gulbenkian HO Univ Porto, Ctr Astrofis ID DENSE CLOUD CORES; MOLECULAR CLOUDS; CORONA-AUSTRALIS; STAR-FORMATION; EXTINCTION; LUPUS; (CO)-O-18; COUNTS; LAW AB We report in this paper results obtained from the analysis of deep near-infrared (NIR) observations of the densest region of the Lupus 3 cloud acquired from the European Southern Observatory's (ESO) New technology Telescope (NTT) and Very Large Telescope (VLT). By constructing a dust extinction map (using the near-infrared color excess method) and examining the detailed internal structure of this prime example of a filamentary dark cloud, we have isolated 5 prominent embedded cores, a dense filament and a dense ring structure in this cloud. The cores have distinctive profiles, sizes, masses, some of them have on-going star formation while others are apparently starless. Building azimuthal density profiles and using Bormor-Ebert and Jeans analysis, we are able to place these cores in an evolutionary sequence. We discuss the relation between the dense ring structure and the emerging cluster in the cloud. Assuming that the ring is the remnant of the disrupted core from which the small cluster originated, we calculate a corresponding star formation efficiency of approximate to 30% for the original core. Lupus 3 is a very interesting cloud for having so many different structures within - where we identify both starless, stellar cores as well as a cluster emerging from a disrupted core. A correlation between the density structures of the cores and its stability and star formation status is evident. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Teixeira, PS (reprint author), Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. NR 17 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013, UNITED STATES BN 0-387-26322-5 J9 ASTROPHYS SPACE SC L PY 2005 VL 324 BP 191 EP 196 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BDE55 UT WOS:000233083000015 ER PT S AU Suleiman, RM Crooker, NU Raymond, JC van Ballegooijen, A AF Suleiman, RM Crooker, NU Raymond, JC van Ballegooijen, A BE Dere, K Wang, J Yan, Y TI UVCS observations of a helical CME structure SO CORONAL AND STELLAR MASS EJECTIONS SE IAU Symposium Proceedings Series LA English DT Proceedings Paper CT 226th Symposium of the International-Astronomical-Union CY SEP 13-17, 2004 CL Beijing, PEOPLES R CHINA SP Int Astron Union, Div II, Chinese Acad Sci, Natl Astron Observat, Local Org Comm, Int Astron Union, Minist Sci & Technol, Natl Nat Sci Fdn China, Natl Sci Fdn, NASA, SOHO Project, SOHO/LASCO Project DE Sun : corona; Sun : coronal mass ejections (CMEs); Sun : filaments; Sun : UV radiation ID CORONAL MASS EJECTION; SOLAR AB A helical structure in the coronal mass ejection (CME) of 12 September 2000 was observed by the Ultraviolet Coronagraph Spectrometer (UVCS) aboard the Solar and Heliospheric Observatory (SOHO) at heliocentric distances of 3.5 and 6 R(circle dot). A difference of 300 km sec(-1) in line-of-sight velocities for two segments of the helix obtained from Doppler measurements implies expansion and allows one to distinguish which segment was closest to the observer. The tilt of the segment then determines the handedness. Observed Ly alpha and C III line emissions indicate that the helix was threaded with filament plasma of varying density. While the helix constituted the bright core of filament plasma, the helix itself was most likely not the pre-existing filament structure. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Suleiman, RM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI van Ballegooijen, Adriaan/0000-0002-5622-3540 NR 8 TC 1 Z9 1 U1 0 U2 0 PU CAMBRIDGE UNIV PRESS PI CAMBRIDGE PA THE PITT BUILDING, TRUMPINGTON ST, CAMBRIDGE CB2 1RP, CAMBS, ENGLAND SN 1743-9213 BN 0-521-85197-1 J9 IAU SYMP P SERIES JI IAU Symposium Proc. Series PY 2005 IS 226 BP 71 EP 75 DI 10.1017/S1743921305000165 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BDF01 UT WOS:000233166700010 ER PT S AU Lin, J van Ballegooijen, AA AF Lin, J van Ballegooijen, AA BE Dere, K Wang, J Yan, Y TI Magnetic structure equilibria and evolutions due to active region interactions SO CORONAL AND STELLAR MASS EJECTIONS SE IAU Symposium Proceedings Series LA English DT Proceedings Paper CT 226th Symposium of the International-Astronomical-Union CY SEP 13-17, 2004 CL Beijing, PEOPLES R CHINA SP Int Astron Union, Div II, Chinese Acad Sci, Natl Astron Observat, Local Org Comm, Int Astron Union, Minist Sci & Technol, Natl Nat Sci Fdn China, Natl Sci Fdn, NASA, SOHO Project, SOHO/LASCO Project DE Sun : coronal mass ejections (CMEs); evolution; filaments; MHD ID CORONAL MASS EJECTIONS; MODEL; FIELDS; FLARES AB Equilibria and evolutions in the coronal magnetic configurations due to the interactions among active regions are investigated. The magnetic structure includes a current-carrying flux rope that is used to model the prominence or filament. We use either two dipoles or four monopoles on the boundary surface to model active regions, and the change in the boundary conditions corresponds to either the horizontal motion of magnetic sources or decaying of the active regions. Both cases show the catastrophic behavior in the system's evolutions. The results have important observational consequences: most eruptive prominences that give rise to CMEs are driven by the interactions between two or more active regions. Such eruptions may not necessarily take place in the growing phase of the active regions, instead they usually occur at the decay phase. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Lin, J (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jlin@cfa.harvard.edu; vanballe@cfa.harvard.edu RI LIN, JUN/B-9890-2017 NR 13 TC 0 Z9 0 U1 0 U2 0 PU CAMBRIDGE UNIV PRESS PI CAMBRIDGE PA THE PITT BUILDING, TRUMPINGTON ST, CAMBRIDGE CB2 1RP, CAMBS, ENGLAND SN 1743-9213 BN 0-521-85197-1 J9 IAU SYMP P SERIES JI IAU Symposium Proc. Series PY 2005 IS 226 BP 257 EP 262 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BDF01 UT WOS:000233166700061 ER PT S AU Lin, J Ko, YK Sui, L Raymond, JC Stenborg, GA Jiang, Y Zhao, S Mancuso, S AF Lin, J Ko, YK Sui, L Raymond, JC Stenborg, GA Jiang, Y Zhao, S Mancuso, S BE Dere, K Wang, J Yan, Y TI Magnetic reconnection inflow near the CME/flare current sheet SO CORONAL AND STELLAR MASS EJECTIONS SE IAU Symposium Proceedings Series LA English DT Proceedings Paper CT 226th Symposium of the International-Astronomical-Union CY SEP 13-17, 2004 CL Beijing, PEOPLES R CHINA SP Int Astron Union, Div II, Chinese Acad Sci, Natl Astron Observat, Local Org Comm, Int Astron Union, Minist Sci & Technol, Natl Nat Sci Fdn China, Natl Sci Fdn, NASA, SOHO Project, SOHO/LASCO Project DE sun : coronal mass ejections; flares; MHD ID CORONAL MASS EJECTIONS; SOLAR ERUPTIONS; FLARES; RHESSI AB This work reports direct observations of the magnetic reconnection site during an eruptive process occurring on November 18, 2003. The event started with a rapid expansion of a few magnetic arcades located over the east limb of the Sun and developed an energetic partial halo coronal mass ejection (CME), a long current sheet and a group of bright flare loops in the wake of the CME. It was observed by several instruments both in space and on ground, including the EUV Imaging Telescope, the Ultraviolet Coronagraph Spectrometer, and the Large Angle and Spectrometric Coronagraph experiment on board the Solar and Heliosphenc Observatory, the Reuven Ramaty High Energy Solar Spectroscopic Imager, as well as the Mauna Loa Solar Observatory Mark IV K-coronameter. We combine the data from these instruments to investigate various properties of the eruptive process, including those around the current sheet. The composite of images from different instruments and the corresponding results specify explicitly how the different objects developed by a single eruptive process are related to one another. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Lin, J (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jlin@cfa.harvard.edu RI LIN, JUN/B-9890-2017 NR 14 TC 0 Z9 0 U1 0 U2 0 PU CAMBRIDGE UNIV PRESS PI CAMBRIDGE PA THE PITT BUILDING, TRUMPINGTON ST, CAMBRIDGE CB2 1RP, CAMBS, ENGLAND SN 1743-9213 BN 0-521-85197-1 J9 IAU SYMP P SERIES JI IAU Symposium Proc. Series PY 2005 IS 226 BP 311 EP 313 DI 10.1017/S1743921305000785 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BDF01 UT WOS:000233166700072 ER PT S AU Matheson, T AF Matheson, T BE Marcaide, JM Weiler, KW TI Optical spectroscopy of Type Ia supernovae SO COSMIC EXPLOSIONS SE SPRINGER PROCEEDINGS IN PHYSICS LA English DT Proceedings Paper CT IAU Colloquium 192 on Supernovae CY APR 22-26, 2003 CL Valencia, SPAIN SP IAU ID LIGHT-CURVE SHAPES; SPECTRA AB The supernova, (SN) group at the Harvard-Smithsonian Center for Astrophysics has been using the facilities of the F. L. Whipple Observatory to gather optical photometric and spectroscopic data on nearby supernovae for several years. The collection of spectra of Type Ia SNe is now large enough to allow a comprehensive analysis. I will present preliminary results from a study of a subsample of the CfA Type la spectroscopic database, with over 200 spectra of 31 Type la SNe. The SNe selected all have well-calibrated light curves and cover a, wide scope of luminosity classes. The epochs of observation range from fourteen days before maximum to fifty days past maximum. All of the spectra were obtained with the same instrument on the same telescope, and were reduced using the same techniques. With such a large, homogeneous data set, the spectroscopic similarities and differences among Type Ia SNe become readily apparent. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Matheson, T (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 15 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY SN 0930-8989 BN 3-540-23039-4 J9 SPRINGER PROC PHYS PY 2005 VL 99 BP 161 EP 165 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BBQ08 UT WOS:000227012100021 ER PT S AU Bloom, JS AF Bloom, JS BE Marcaide, JM Weiler, KW TI Optical bumps in cosmological GRBs as supernovae SO COSMIC EXPLOSIONS SE SPRINGER PROCEEDINGS IN PHYSICS LA English DT Proceedings Paper CT IAU Colloquium 192 on Supernovae CY APR 22-26, 2003 CL Valencia, SPAIN SP IAU ID GAMMA-RAY BURST; 25 APRIL 1998; GRB-011121; GRB-030329 AB From both photometric and broadband spectral monitoring of gamma-ray burst (GRB) lightcurve "bumps," particularly in GRB011121, a strong case grew for a supernova (SN) origin. The GRB-SN connection was finally solidified beyond a reasonable doubt with the discovery that the bump in GRB 030329 was spectroscopically similar to a bright Type Ic SN. In light of this result, I re-assess the previous SN bump claims and conclude that: 1) the distribution of GRB-SN bump peak magnitudes is consistent with the local Type Ib/c SNe peak distribution and 2) the late-time bumps in all long-duration GRBs are likely supernovae. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Bloom, JS (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MC 20, Cambridge, MA 02138 USA. NR 24 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY SN 0930-8989 BN 3-540-23039-4 J9 SPRINGER PROC PHYS PY 2005 VL 99 BP 411 EP 415 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BBQ08 UT WOS:000227012100056 ER PT J AU von Sternberg, R Shapiro, JA AF von Sternberg, R Shapiro, JA TI How repeated retroelements format genome function SO CYTOGENETIC AND GENOME RESEARCH LA English DT Review ID X-CHROMOSOME INACTIVATION; TRANSPOSABLE ELEMENTS; REPETITIVE ELEMENTS; L1 RETROTRANSPOSON; EPIGENETIC INHERITANCE; ARABIDOPSIS-THALIANA; CHROMATIN-STRUCTURE; ANTISENSE PROMOTER; MAMMALIAN GENOME; GYPSY INSULATOR AB Genomes operate as sophisticated information storage systems. Generic repeated signals in the DNA format expression of coding sequence files and organize additional functions essential for genome replication and accurate transmission to progeny cells. Retroelements comprise a major fraction of many genomes and contain a surprising diversity of functional signals. In this article, we summarize some features of the taxonomic distribution of retroelements, especially mammalian SINEs, tabulate functional roles documented for different classes of retroelements, and discuss their potential roles as genome organizers. In particular, the fact that certain retroelements serve as boundaries for heterochromatin domains and provide a significant fraction of scaffolding/matrix attachment regions (S/MARs) suggests that the reversed transcribed component of the genome plays a major architectonic role in higher order physical structuring. Employing an information science model, the "functionalist" perspective on repetitive DNA leads to new ways of thinking about the systemic organization of cellular genomes and provides several novel possibilities involving retroelements in evolutionarily significant genome reorganization. Copyright (c) 2005 S. Karger AG, Basel. C1 Univ Chicago, Dept Biochem & Mol Biol, Chicago, IL 60637 USA. Natl Ctr Biotechnol Informat, NIH, Bethesda, MD USA. Natl Museum Nat Hist, Smithsonian Inst, Dept Systemat Biol, Washington, DC USA. RP Shapiro, JA (reprint author), Univ Chicago, Dept Biochem & Mol Biol, 920 E,58th St, Chicago, IL 60637 USA. EM jsha@uchicago.edu NR 102 TC 14 Z9 15 U1 1 U2 4 PU KARGER PI BASEL PA ALLSCHWILERSTRASSE 10, CH-4009 BASEL, SWITZERLAND SN 1424-8581 EI 1424-859X J9 CYTOGENET GENOME RES JI Cytogenet. Genome Res. PY 2005 VL 110 IS 1-4 BP 108 EP 116 DI 10.1159/000084942 PG 9 WC Cell Biology; Genetics & Heredity SC Cell Biology; Genetics & Heredity GA 953GM UT WOS:000231064600010 PM 16093662 ER PT J AU Saini, MS Vasu, V Smith, DR AF Saini, Malkiat S. Vasu, V. Smith, David R. TI Review of the genus Eutomostethus Enslin (Hymenoptera, Tenthredinidae, Blennocampinae) from India, with new species and a key to species SO DEUTSCHE ENTOMOLOGISCHE ZEITSCHRIFT LA English DT Review DE revised generic limits; Eutomostethus; Blennocampinae; new species; India AB Ten new species of Eutomostethus from India are described: E. sulcatus, E. unciformis, E. clypeiambus, E. sinuatus, E. circularis, E. canaliculus, E. bifidus, E. emarginatus, E. protrudus, and E. flagellaris. Several generic characters are reevaluated because of variation in some of the additional species. A key is provided for the 45 species now known in India including a summary of the previous literature on the genus. Eutomostethus wed is proposed as a new name for E. distinctus Wei 1997, preoccupied by E. distinctus Saini and Vasu 1996, and Eutomostethus vasui is proposed as a new name for E. sikkimensis Saini and Vasu 1997, preoccupied by E. sikkimensis (Forsius 1931). (C) 2005 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim. C1 [Saini, Malkiat S.; Vasu, V.] Punjabi Univ, Dept Zool, Patiala 147002, Punjab, India. [Smith, David R.] Smithsonian Inst, Natl Museum Nat Hist, USDA, PSI,Agr Res Serv,Systemat Entomol Lab, Washington, DC 20013 USA. RP Smith, DR (reprint author), Smithsonian Inst, Natl Museum Nat Hist, USDA, PSI,Agr Res Serv,Systemat Entomol Lab, POB 37012,CE-523,MRC-168, Washington, DC 20013 USA. NR 37 TC 1 Z9 2 U1 0 U2 0 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA PO BOX 10 11 61, D-69451 WEINHEIM, GERMANY SN 0012-0073 J9 DEUT ENTOMOL Z JI Dtsch. Entomol. Z. PY 2005 VL 52 IS 1 BP 139 EP 153 DI 10.1002/mmnd.200210007 PG 15 WC Entomology SC Entomology GA V44OW UT WOS:000203013000007 ER PT S AU Dalgarno, A AF Dalgarno, A BE Wolf, A Lammich, L Schmelcher, P TI Molecular processes in the early Universe SO DR2004: Sixth International Conference on Dissociative Recombination: Theory, Experiments and Applications SE JOURNAL OF PHYSICS CONFERENCE SERIES LA English DT Proceedings Paper CT 6th International Conference on Dissociative Recombination CY JUL 12-16, 2004 CL Mosbach, GERMANY ID STIMULATED RADIATIVE ASSOCIATION; HYDROGEN; CHEMISTRY; H+; LI AB Molecular processes first took place in the Universe in the recombination era as the expanding Universe cooled adiabatically and recombined when the cooling radiation field ran out of photons energetic enough to cause photoionization. The formation of neutral helium heralded the dawn of chemistry as the neutral atoms participated in processes of radiative association to form molecular ions. Dissociative recombination of the molecular ions produced neutral atoms and accelerated the conversion of the ionized plasma into a neutral gas. The subsequent chemistry involved hydrogen, deuterium, helium and lithium created earlier in a brief period of nucleosynthesis. With the continued expansion the Universe became cold and dark and chemistry came to a temporary end until the formation and gravitational collapse of the first distinct cosmological objects. Heavy elements were made, a new source of radiation - starlight appeared and a richer chemistry was initiated. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Dalgarno, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 21 TC 20 Z9 20 U1 1 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 2005 VL 4 BP 10 EP 16 DI 10.1088/1742-6596/4/1/002 PG 7 WC Physics, Atomic, Molecular & Chemical SC Physics GA BCE13 UT WOS:000228817000002 ER PT S AU Frisch, PC Slavin, JD AF Frisch, PC Slavin, JD BE Fichtner, H TI Heliospheric implications of structure in the interstellar medium SO DYNAMIC HELIOSPHERE SE ADVANCES IN SPACE RESEARCH-SERIES LA English DT Article; Proceedings Paper CT 35th COSPAR Scientific Assembly CY JUL 18-25, 2004 CL Paris, FRANCE SP Comm Space Res DE interplanetary Ly alpha; heliosphere; interstellar ID LYMAN-ALPHA OBSERVATIONS; SOLAR-WIND; CHARGE-EXCHANGE; GAS; EMISSION; MATTER; CONSEQUENCES; COPERNICUS; IONIZATION; PARAMETERS AB Equilibrium models of diffuse interstellar material (ISM) near the Sun show a range of cloud densities, ionization, and temperatures which are consistent with data, although the local ISM must be inhomogeneous over similar to 2 pc scales. The ISM close to the Sun has properties that are consistent with the sheetlike warm neutral (and partially ionized) gas detected in the Arecibo Millennium Survey. Local interstellar magnetic fields are poorly understood, but data showing weak polarization for nearby stars indicate dust may be trapped in fields or currents in the heliosheath nose region. Implications of this dust capture are widespread, and may impact the interpretation of the cosmic microwave background data. Observations of interstellar Ho inside of the solar system between 1975 and 2000 do not suggest any variation in the properties or structure of local interstellar Ho over distance scales of similar to 750 AU to within the uncertainties. (c) 2005 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 Univ Chicago, Dept Astron, Chicago, IL 60637 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Frisch, PC (reprint author), Univ Chicago, Dept Astron, 5640 S Ellis Ave, Chicago, IL 60637 USA. EM frisch@oddjob.uchicago.edu; jslavin@cfa.harvard.edu OI Slavin, Jonathan/0000-0002-7597-6935 NR 40 TC 3 Z9 3 U1 0 U2 1 PU ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD 0X5 1GB, OXON, ENGLAND SN 0273-1177 J9 ADV SPACE RES-SERIES PY 2005 VL 35 IS 12 SI 2005 BP 2048 EP 2054 DI 10.1016/j.asr.2005.03.010 PG 7 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BDT00 UT WOS:000235191000001 ER PT B AU Heyer, WR de Sa, RO Muller, S AF Heyer, WR de Sa, RO Muller, S BE Donnelly, MA Crother, BI Guyer, C Wake, MH White, ME TI On the enigmatic distribution of the Honduran endemic Leptodactylus silvanimbus (Amphibia : Anura : Leptodactylidae) SO Ecology & Evolution in the Tropics: A Herpetological Perspective LA English DT Proceedings Paper CT 80th Annual Meeting of the American-Society-of-Ichthyologists-and-Herpetologists/Society-for-the-St udy-of-Amphibians-and-Reptiles and Herpetologists-League CY JUN 14-20, 2000 CL Univ Autonoma Baja Calif Sur, La Paz, MEXICO SP Amer Soc Ichthyologists & Herpetologists, Soc Study Amphibians & Reptiles, Herpetologists League HO Univ Autonoma Baja Calif Sur C1 Smithsonian Inst, Washington, DC 20013 USA. RP Heyer, WR (reprint author), Smithsonian Inst, MRC 162,NHB W-201,POB 37012, Washington, DC 20013 USA. NR 0 TC 2 Z9 6 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60 ST, CHICAGO, IL 60637 USA BN 0-226-15658-3 PY 2005 BP 81 EP 101 PG 21 WC Ecology; Evolutionary Biology; Zoology SC Environmental Sciences & Ecology; Evolutionary Biology; Zoology GA BCN05 UT WOS:000230111100004 ER PT B AU McDiarmid, RW Savage, JM AF McDiarmid, RW Savage, JM BE Donnelly, MA Crother, BI Guyer, C Wake, MH White, ME TI The herpetofauna of the Rincon area, Peninsula de Osa, Costa Rica, a central American lowland evergreen forest site SO Ecology & Evolution in the Tropics: A Herpetological Perspective LA English DT Proceedings Paper CT 80th Annual Meeting of the American-Society-of-Ichthyologists-and-Herpetologists/Society-for-the-St udy-of-Amphibians-and-Reptiles and Herpetologists-League CY JUN 14-20, 2000 CL Univ Autonoma Baja Calif Sur, La Paz, MEXICO SP Amer Soc Ichthyologists & Herpetologists, Soc Study Amphibians & Reptiles, Herpetologists League HO Univ Autonoma Baja Calif Sur C1 Natl Museum Nat Hist, Smithsonian Inst, USGS Patuxent Wildlife Res Ctr, Washington, DC 20013 USA. RP McDiarmid, RW (reprint author), Natl Museum Nat Hist, Smithsonian Inst, USGS Patuxent Wildlife Res Ctr, POB 37012,Room 378,MRC III, Washington, DC 20013 USA. NR 0 TC 9 Z9 12 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60 ST, CHICAGO, IL 60637 USA BN 0-226-15658-3 PY 2005 BP 366 EP 427 PG 62 WC Ecology; Evolutionary Biology; Zoology SC Environmental Sciences & Ecology; Evolutionary Biology; Zoology GA BCN05 UT WOS:000230111100016 ER PT B AU McDiarmid, RW Donnelly, MA AF McDiarmid, RW Donnelly, MA BE Donnelly, MA Crother, BI Guyer, C Wake, MH White, ME TI The herpetofauna of the Guayana highlands: Amphibians and reptiles of the lost world SO Ecology & Evolution in the Tropics: A Herpetological Perspective LA English DT Proceedings Paper CT 80th Annual Meeting of the American-Society-of-Ichthyologists-and-Herpetologists/Society-for-the-St udy-of-Amphibians-and-Reptiles and Herpetologists-League CY JUN 14-20, 2000 CL Univ Autonoma Baja Calif Sur, La Paz, MEXICO SP Amer Soc Ichthyologists & Herpetologists, Soc Study Amphibians & Reptiles, Herpetologists League HO Univ Autonoma Baja Calif Sur C1 Museo Nacl Hist Nat, USGS Patuxent Wildlife Res Ctr, Smithsonian Inst, Washington, DC 20013 USA. RP McDiarmid, RW (reprint author), Museo Nacl Hist Nat, USGS Patuxent Wildlife Res Ctr, Smithsonian Inst, POB 37012,Room 378,MRC III, Washington, DC 20013 USA. NR 0 TC 44 Z9 50 U1 0 U2 4 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60 ST, CHICAGO, IL 60637 USA BN 0-226-15658-3 PY 2005 BP 461 EP 560 PG 100 WC Ecology; Evolutionary Biology; Zoology SC Environmental Sciences & Ecology; Evolutionary Biology; Zoology GA BCN05 UT WOS:000230111100018 ER PT S AU Slane, P AF Slane, P BE Baykal, A Yerli, SK Inam, SC Grebenev, S TI Young neutron stars and their wind nebulae SO ELECTROMAGNETIC SPECTRUM OF NEUTRON STARS SE NATO Science Series II-Mathematics Physics and Chemistry LA English DT Proceedings Paper CT 6th NATO-Advanced-Study-Institute on Electromagnetic Spectrum of Neutron Stars CY JUN 07-18, 2004 CL Marmaris, TURKEY DE stars : neutron; stars : pulsar; stars : circumstellar matter ID SUPERNOVA REMNANT G292.0+1.8; X-RAY OBSERVATIONS; CRAB-NEBULA; PULSAR WIND; MAGNETOHYDRODYNAMIC MODEL; SYNCHROTRON NEBULA; MAGNETIC-FIELD; VELA PULSAR; 3C 58; DISCOVERY AB With Tera gauss magnetic fields, surface gravity sufficiently strong to significantly modify light paths, central densities higher than that of a standard nucleus, and rotation periods of only hundredths of a second, young neutron stars are sites of some of the most extreme physical conditions known in the Universe. They generate magnetic winds with particles that are accelerated to energies in excess of a TeV These winds form synchrotron-emitting bubbles as the particle stream is eventually decelerated to match the general expansion caused by the explosion that formed the neutron stars. The structure of these pulsar wind nebulae allow us to infer properties of the winds and the pulsating neutron stars themselves. The surfaces of the the stars radiate energy from the rapidly cooling interiors where the physical structure is basically unknown because of our imprecise knowledge of the strong interaction at ultrahigh densities. Here I present a summary of recent measurements that allow us to infer the birth properties of neutron stars and to probe the nature of their winds, the physics of their atmospheres, and the structure of their interiors. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Slane, P (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. EM slane@cfa.harvard.edu NR 47 TC 1 Z9 1 U1 0 U2 0 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013, UNITED STATES SN 1568-2609 BN 1-4020-3859-3 J9 NATO SCI SER II-MATH PY 2005 VL 210 BP 15 EP 30 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BDS01 UT WOS:000235158900002 ER PT J AU Ertl, A Pertlik, F Prem, M Post, JE Kim, SJ Brandstatter, F Schuster, R AF Ertl, A Pertlik, F Prem, M Post, JE Kim, SJ Brandstatter, F Schuster, R TI Rancieite crystals from Friesach, Carinthia, Austria SO EUROPEAN JOURNAL OF MINERALOGY LA English DT Article DE rancieite; birnessite-group; phyllomanganate; X-ray powder data; structure proposal ID MANGANESE OXIDE MINERALS; POTASSIUM BIRNESSITE; EASTERN ALPS; SPECTROSCOPY; TAKANELITE; BEHAVIOR; VARNISH AB Rancieite from Friesach, Carinthia, Austria, is described from an oxidation zone of a small (Mn-bearing) siderite deposit. This mineral is associated with "buserite-(Ca)", hollandite, braunite, romanechite, todorokite, cryptomelane, pyrolusite, manganite, nsutite, goethite, lepidocrocite, and calcite. Rancieite rarely forms small purple-silver grey crystals with a bright metallic luster. Single crystals are up to 200 mu m in length and similar to 0.1 mu m in thickness and exhibit well-formed crystal faces in some cases. The foliated habit of these crystals may be due to rapid growth on the plane of fissure. For the first time a relatively large number of X-ray powder diffraction lines (19 lines) of rancieite are described. Structure modeling, by the Rietveld method and with difference-Fourier summations shows, that rancieite is most probably trigonal in structure, in contrast to the monoclinic structure of bimessite. The layers of the (Mn4+,Mn3+)O-6 octahedra, arranged parallel to (00.1), are intercalated predominantly by Ca atoms and water molecules, which are in a statistic and disordered arrangement. The powder pattern of this rancieite was indexed on a trigonal cell, space group P3 [147], with a = 2.845(1) and c = 7.485(1) angstrom, a:c = 1 : 2.632, Z = 1. The unit formula can be written as (Ca0.85Mn0.062+K0.05Mg0.02Fe0.013+Ba0.01) (Mn3.604+Mn0.403+)O-9. similar to 2.8 H2O (calculated on the basis of 0 = 9; water and the valence states of Mn were calculated), or as Ca0.19Mn0.012+K0.01(Mn(0.80)(4+)Mn(0.09)(3+)square(0.11))O-2. similar to 0.6 H2O (calculated on the basis of O = 2). C1 Univ Vienna, Inst Mineral & Kristallog, Geozentrum, A-1090 Vienna, Austria. Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. Seoul Natl Univ, Sch Earth & Environm Sci, Seoul 151742, South Korea. Museum Nat Hist, Mineral Petrog Abt, A-1014 Vienna, Austria. Geol Bundesanstalt, A-1030 Vienna, Austria. RP Ertl, A (reprint author), Univ Vienna, Inst Mineral & Kristallog, Geozentrum, Althanstr 14, A-1090 Vienna, Austria. EM andreas.ertl@a1.net NR 72 TC 5 Z9 6 U1 1 U2 9 PU E SCHWEIZERBARTSCHE VERLAGS PI STUTTGART PA NAEGELE U OBERMILLER JOHANNESSTRASSE 3A, D 70176 STUTTGART, GERMANY SN 0935-1221 J9 EUR J MINERAL JI Eur. J. Mineral. PD JAN-FEB PY 2005 VL 17 IS 1 BP 163 EP 172 DI 10.1127/0935-1221/2005/0017-0163 PG 10 WC Mineralogy SC Mineralogy GA 912UJ UT WOS:000228105100016 ER PT B AU Matthews, LD AF Matthews, LD BE Braun, R TI Extra-planar HI in low surface brightness galaxies SO Extra-Planar Gas SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Meeting on Extra-Planar Gas CY JUN 07-11, 2004 CL Dwingeloo, NETHERLANDS ID HIGH-LATITUDE HI; SUPERTHIN GALAXIES; SPIRAL GALAXIES; I HALO; CORRUGATIONS; ENVIRONMENT; NGC-2403; UGC-7321; DISK AB Sensitive HI imaging observations of two isolated, edge-on, low surface brightness (LSB) spiral galaxies have revealed a vertically-extended neutral hydrogen component in both systems, extending to vertical bar z vertical bar similar to 2.3-2.9 kpc. These represent the first reported detections of extra-planar Hi emission in galaxies with such low current star formation rate (similar to 0.01 - 0.02 M-circle dot yr(-1)). Three-dimensional modeling of one of these galaxies (UGC 7321) shows that neither warping nor flaring of the gas layer alone can account for the observations, implying the existence of an additional H I "halo" component. This "halo" appears to lag in rotation relative to the material in the midplane. In the second galaxy, IC 2233, the high-latitude HI is more extensive and shows more complex kinematics, including possible evidence for a component that is orbiting inclined similar to 45 degrees to the disk. I briefly discuss possible origins for the high-latitude gas in these two LSB galaxies. C1 Harvard Univ, Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Matthews, LD (reprint author), Harvard Univ, Smithsonian Ctr Astrophys, 60 Garden St,MS-42, Cambridge, MA 02138 USA. NR 20 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 1-58381-194-X J9 ASTR SOC P PY 2005 VL 331 BP 253 EP 259 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BCO45 UT WOS:000230412000033 ER PT J AU Jaegle, L Steinberger, L Martin, RV Chance, K AF Jaegle, L Steinberger, L Martin, RV Chance, K TI Global partitioning of NOx sources using satellite observations: Relative roles of fossil fuel combustion, biomass burning and soil emissions SO FARADAY DISCUSSIONS LA English DT Article ID NITRIC-OXIDE EMISSIONS; NITROUS-OXIDE; VEGETATION FIRE; SAVANNA SOILS; SEASON; AFRICA; IMPACT; MODEL; GOME; ATMOSPHERE AB We use space-based observations of NO2 columns from the Global Ozone Monitoring Experiment (GOME) to derive monthly top-down NOx emissions for 2000 via inverse modeling with the GEOS-CHEM chemical transport model. Top-down NOx sources are partitioned among fuel combustion (fossil fuel and biofuel), biomass burning and soils by exploiting the spatio-temporal distribution of remotely sensed fires and a priori information on the location of regions dominated by fuel combustion. The top-down inventory is combined with an a priori inventory to obtain an optimized a posteriori estimate of the relative roles of NOx sources. The resulting a posteriori fuel combustion inventory (25.6 TgN year(-1)) agrees closely with the a priori (25.4 TgN year(-1)), and errors are reduced by a factor of 2, from 80% to 40%. Regionally, the largest differences are found over Japan and South Africa, where a posteriori estimates are 25% larger than a priori. A posteriori fuel combustion emissions are aseasonal, with the exception of East Asia and Europe where winter emissions are 30-40% larger relative to summer emissions, consistent with increased energy use during winter for heating. Global a posteriori biomass burning emissions in 2000 resulted in 5.8 TgN (compared to 5.9 TgN year(-1) in the a priori), with Africa accounting for half of this total. A posteriori biomass burning emissions over Southeast Asia/India are decreased by 46% relative to a priori; but over North equatorial Africa they are increased by 50%. A posteriori estimates of soil emissions (8.9 TgN year(-1)) are 68% larger than a priori (5.3 TgN year(-1)). The a posteriori inventory displays the largest soil emissions over tropical savanna/woodland ecosystems (Africa), as well as over agricultural regions in the western U.S. (Great Plains), southern Europe (Spain, Greece, Turkey), and Asia (North China Plain and North India), consistent with field measurements. Emissions over these regions are highest during summer at mid-latitudes and during the rainy season in the Tropics. We estimate that 2.5-4.5 TgN year(-1) are emitted from N-fertilized soils, at the upper end of previous estimates. Soil and biomass burning emissions account for 22% and 14% of global surface NOx emissions, respectively. We infer a significant role for soil NOx emissions at northern mid-latitudes during summer, where they account for nearly half that of the fuel combustion source, a doubling relative to the a priori. The contribution of soil emissions to background ozone is thus likely to be underestimated by the current generation of chemical transport models. C1 Univ Washington, Dept Atmospher Sci, Seattle, WA 98195 USA. Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS, Canada. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Jaegle, L (reprint author), Univ Washington, Dept Atmospher Sci, Seattle, WA 98195 USA. EM jaegle@atmos.washington.edu RI Martin, Randall/A-2051-2008; Martin, Randall/C-1205-2014; Chem, GEOS/C-5595-2014; OI Martin, Randall/0000-0003-2632-8402; Chance, Kelly/0000-0002-7339-7577 NR 68 TC 188 Z9 193 U1 5 U2 65 PU ROYAL SOC CHEMISTRY PI CAMBRIDGE PA THOMAS GRAHAM HOUSE, SCIENCE PARK, MILTON RD, CAMBRIDGE CB4 0WF, CAMBS, ENGLAND SN 1364-5498 J9 FARADAY DISCUSS JI Faraday Discuss. PY 2005 VL 130 BP 407 EP 423 DI 10.1039/b502128f PG 17 WC Chemistry, Physical SC Chemistry GA 963KV UT WOS:000231804100024 PM 16161795 ER PT B AU Matheson, T AF Matheson, T BE Humphreys, RM Stanek, KZ TI Supernova impostors in the center for astrophysics SN database SO Fate of the Most Massive Stars, Proceedings SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Meeting on Fate of the Most Massive Stars CY MAY 23-28, 2004 CL Grand Teton Natl Pk, WY SP Natl Sci Fdn, Astron Div ID TELESCOPE AB Outbursts of luminous blue variables can be mistaken for supernovae (SNe) in nearby galaxies. Spectroscopy alone is often not enough to identify the true nature of the object as some SNe have very similar spectra. Knowledge of the luminosity and spectroscopic evolution of the object is often necessary to be certain in distinguishing SNe from the impostors. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Matheson, T (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 7 TC 1 Z9 1 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-195-8 J9 ASTR SOC P PY 2005 VL 332 BP 86 EP 89 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BDG86 UT WOS:000233430500009 ER PT B AU Bonanos, AZ Stanek, KZ AF Bonanos, AZ Stanek, KZ BE Humphreys, RM Stanek, KZ TI The most massive stars in the local group: Measuring accurate masses of stars in eclipsing binaries SO Fate of the Most Massive Stars, Proceedings SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Meeting on Fate of the Most Massive Stars CY MAY 23-28, 2004 CL Grand Teton Natl Pk, WY SP Natl Sci Fdn, Astron Div ID DIRECT DISTANCES; VARIABLES; CEPHEIDS; CURVES; LIGHT AB Accurate masses and, in general, all fundamental parameters of distant stars can only be measured in eclipsing binaries. Several massive star candidates with masses near 200M(circle dot) exist, however they have large uncertainties associated with them. The most massive binary ever measured accurately is WR 20a, for which we present the light curve. Measuring the period and inclination, we derive masses greater than 80M(circle dot) for each component. Massive binaries are bound to exist in Local Group galaxies, such as M31 and M33. These can be selected from their light curves, obtained by variability studies, such as the DIRECT project. We present photometry and spectroscopy of the detached system M33A, for which we are obtaining a direct distance determination. The DIRECT project has detected several candidate massive binaries which are brighter but nondetached systems, perhaps similar to WR 20a. We plan to obtain spectra for them and measure their masses. C1 Harvard Smithsonian Ctr Astrophys, Ctr Astrophys, Cambridge, MA 02138 USA. RP Bonanos, AZ (reprint author), Harvard Smithsonian Ctr Astrophys, Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 13 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 1-58381-195-8 J9 ASTR SOC P PY 2005 VL 332 BP 253 EP 256 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BDG86 UT WOS:000233430500041 ER PT B AU Matheson, T AF Matheson, T BE Humphreys, RM Stanek, KZ TI The supernovae associated with gamma-ray bursts SO FATE OF THE MOST MASSIVE STARS, PROCEEDINGS SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT Meeting on Fate of the Most Massive Stars CY MAY 23-28, 2004 CL Grand Teton Natl Pk, WY SP Natl Sci Fdn, Astron Div ID 25 APRIL 1998; OPTICAL AFTERGLOW; SPECTROSCOPY; GRB-030329; HYPERNOVA; GRB-011121; PHOTOMETRY; DISCOVERY; SPECTRUM; 2003DH AB Supernovae (SNe) were long suspected as possible mechanisms to produce gamma-ray bursts (GRBs). The arguments relied on circumstantial evidence. Several recent GRBs, notably GRB 030329, have provided direct, spectroscopic evidence that SNe and GRBs are related. The SNe associated with GRBs are all of Type Ic, implying a compact progenitor, which has implications for GRB models. Other peculiar Type Ic SNe may help to elucidate the mechanisms involved. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Matheson, T (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM tmatheson@cfa.harvard.edu NR 24 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 1-58381-195-8 J9 ASTR SOC P PY 2005 VL 332 BP 403 EP 406 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BDG86 UT WOS:000233430500062 ER PT J AU Vila, R Tomi, M Mundina, M Santana, AI Solis, PN Arce, JBL Iclina, JLB Iglesias, J Gupta, MP Casanova, J Canigueral, S AF Vila, R Tomi, M Mundina, M Santana, AI Solis, PN Arce, JBL Iclina, JLB Iglesias, J Gupta, MP Casanova, J Canigueral, S TI Unusual composition of the essential oils from the leaves of Piper aduncum SO FLAVOUR AND FRAGRANCE JOURNAL LA English DT Article DE Piper aduncum; Piperaceae; essential oil; 1,8-cineole; beta-caryophyllene; aromadendrene; sarisan; GC-MS; C-13-NMR ID C-13 NMR; CONSTITUENTS; COMPONENTS; SARISAN; PEPPER AB The chemical compositions of the essential oils from the leaves of Piper aduncum from Panama and Bolivia were investigated by GC-FID, GC-MS and C-13-NMR. In total, 55 components were identified representing 99.3 and 80.3% of each sample, respectively. The oil from Panama was characterized by a high percentage of sesquiterpene hydrocarbons (38.9%), the main ones being beta-caryophyllene (17.4%) and aromadendrene (13.4%). In contrast, the oil from Bolivia showed a high content of monoterpenes (76%), the major constituent being 1,8-cineole (40.5%). Phenylpropanoids, mainly sarisan (1-allyl-2-methoxy-4,5-methylenedioxybenzene; 12.9%), were only detected in the latter. Copyright (C) 2004 John Wiley Sons, Ltd. C1 Univ Barcelona, Fac Farm, Unitat Farmacol & Farmacognosia, E-08028 Barcelona, Spain. Univ Corse, Equipe Chim & Biomasse, CNRS, UMR 6134, F-20000 Ajaccio, France. Univ Panama, Fac Farm, CIFLORPAN, Panama City, Panama. Univ Mayor San Simon, Fac Ciencias & Tecnol, Ctr Tecnol Agroind, Cochabamba, Bolivia. Smithsonian Trop Res Inst, Panama City, Panama. RP Canigueral, S (reprint author), Univ Barcelona, Fac Farm, Unitat Farmacol & Farmacognosia, Avda Diagonal,643, E-08028 Barcelona, Spain. EM s.canigueral@ub.edu RI Canigueral, Salvador/O-2767-2013; OI Canigueral, Salvador/0000-0001-5056-489X; Gupta, Mahabir/0000-0002-9302-7864 NR 28 TC 16 Z9 17 U1 1 U2 4 PU JOHN WILEY & SONS LTD PI CHICHESTER PA THE ATRIUM, SOUTHERN GATE, CHICHESTER PO19 8SQ, W SUSSEX, ENGLAND SN 0882-5734 J9 FLAVOUR FRAG J JI Flavour Frag. J. PD JAN-FEB PY 2005 VL 20 IS 1 BP 67 EP 69 DI 10.1002/ffj.1369 PG 3 WC Chemistry, Applied; Food Science & Technology SC Chemistry; Food Science & Technology GA 883UD UT WOS:000226040300016 ER PT B AU Forman, W AF Forman, W BE Blanchard, A Signore, M TI The X-ray view of galaxy clusters SO Frontiers of Cosmology SE NATO SCIENCE SERIES, SERIES II: MATHEMATICS, PHYSICS AND CHEMISTRY LA English DT Proceedings Paper CT Conference of the NATO-Advanced-Study-Institute on Frontiers of Cosmology CY SEP 08-20, 2003 CL Cargese, FRANCE SP NATO Adv Study Inst ID COOLING FLOWS; THERMAL CONDUCTION; COSMOLOGICAL CONSTRAINTS; CHANDRA OBSERVATION; BUOYANT BUBBLES; HOT PLASMA; COLD-FRONT; GAS; M87; EVOLUTION C1 Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Forman, W (reprint author), Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. OI Forman, William/0000-0002-9478-1682 NR 54 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS BN 1-4020-3055-X J9 NATO SCI SER II MATH PY 2005 VL 187 BP 23 EP 42 PG 20 WC Astronomy & Astrophysics; Physics, Multidisciplinary SC Astronomy & Astrophysics; Physics GA BCY21 UT WOS:000231849200002 ER PT J AU Kral, P Segal, D Shapiro, M Thanopulos, I Granger, BE Sadeghpour, HR AF Kral, P Segal, D Shapiro, M Thanopulos, I Granger, BE Sadeghpour, HR TI Bands of image states in nanowire lattices and infrared-control of proteins on nanotube ropes SO FULLERENES NANOTUBES AND CARBON NANOSTRUCTURES LA English DT Article; Proceedings Paper CT Symposium on Advanced Multifunctional Nanocarbon Materials and Nanosystems held at the E-MRS Spring Meeting CY MAY 24-28, 2004 CL Strasbourg, FRANCE SP E-MRS DE nanotube; image state; band structure ID WALL CARBON NANOTUBES; MOTIONS AB We show. that suspended arrarys of parallel nanowires support bound electron image states with rich band structures. These states could be controlled by electric and magnetic fields and used in building of waveguides, mirrors, and storage places for Rydberg-like electrons. We also exploit the possibility of controlling proteins attached to hybrid nanotube ropes. Near infrared excitation of such ropes causes their depolarization, leading to the change of protein's conformation. C1 Weizmann Inst Sci, Dept Chem Phys, IL-76100 Rehovot, Israel. Univ British Columbia, Dept Chem Phys, Vancouver, BC V5Z 1M9, Canada. Santa Clara Univ, Dept Phys, Santa Clara, CA 95053 USA. Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. RP Kral, P (reprint author), Weizmann Inst Sci, Dept Chem Phys, IL-76100 Rehovot, Israel. EM pkral@uic.edu NR 24 TC 0 Z9 0 U1 1 U2 3 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 325 CHESTNUT ST, SUITE 800, PHILADELPHIA, PA 19106 USA SN 1536-383X J9 FULLER NANOTUB CAR N JI Fuller. Nanotub. Carbon Nanostruct. PY 2005 VL 13 SU 1 BP 267 EP 274 DI 10.1081/FST-200039302 PG 8 WC Chemistry, Physical; Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Physics, Atomic, Molecular & Chemical SC Chemistry; Science & Technology - Other Topics; Materials Science; Physics GA 920VL UT WOS:000228718200033 ER PT J AU Winter, K Aranda, J Holtum, JAM AF Winter, K Aranda, J Holtum, JAM TI Carbon isotope composition and water-use efficiency in plants with crassulacean acid metabolism SO FUNCTIONAL PLANT BIOLOGY LA English DT Article DE C(3) photosynthesis; C(4) photosynthesis; carbon-isotope ratio; crassulacean acid metabolism; transpiration ratio; water-use efficiency ID TROPICAL PIONEER TREE; FICUS-INSIPIDA WILLD; CLUSIA-UVITANA; TRANSPIRATION EFFICIENCY; VASCULAR EPIPHYTES; DELTA-C-13 VALUES; CO2 ASSIMILATION; ELEVATED CO2; CAM; DISCRIMINATION AB The relationship between water-use efficiency, measured as the transpiration ratio ( g H(2)O transpired g(-1) above-plus below-ground dry mass accumulated), and (13)C /(12)C ratio ( expressed as delta(13)C value) of bulk biomass carbon was compared in 15 plant species growing under tropical conditions at two field sites in the Republic of Panama. The species included five constitutive crassulacean acid metabolism ( CAM) species [ Aloe vera ( L.) Webb & Berth., Ananas comosus ( L.) Merr., Euphorbia tirucalli L., Kalanchoe daigremontiana Hamet et Perr., Kalanchoe pinnata ( Lam.) Pers.], two species of tropical C(3) trees ( Tectona grandis Linn. f. and Swietenia macrophylla King), one C(4) species (Zea mays L.), and seven arborescent species of the neotropical genus Clusia, of which two exhibited pronounced CAM. The transpiration ratios of the C(3) and CAM species, which ranged between 496 g H(2)O g(-1) dry mass in the C(3) - CAM species Clusia pratensis Seeman to 54 g H(2)O g(-1) dry mass in the constitutive CAM species Aloe vera, correlated strongly with delta(13)C values and nocturnal CO(2) gain suggesting that delta(13)C value can be used to estimate both water-use efficiency and the proportion of CO(2) gained by CAM species during the light and the dark integrated over the lifetime of the tissues. C1 Smithsonian Trop Res Inst, Balboa, Ancon, Panama. James Cook Univ N Queensland, Sch Trop Biol, Townsville, Qld 4811, Australia. RP Winter, K (reprint author), Smithsonian Trop Res Inst, POB 2072, Balboa, Ancon, Panama. EM winterk@tivoli.si.edu RI Holtum, Joseph/B-3063-2012 OI Holtum, Joseph/0000-0001-6568-8019 NR 55 TC 53 Z9 60 U1 5 U2 36 PU CSIRO PUBLISHING PI COLLINGWOOD PA 150 OXFORD ST, PO BOX 1139, COLLINGWOOD, VICTORIA 3066, AUSTRALIA SN 1445-4408 J9 FUNCT PLANT BIOL JI Funct. Plant Biol. PY 2005 VL 32 IS 5 BP 381 EP 388 DI 10.1071/FP04123 PG 8 WC Plant Sciences SC Plant Sciences GA 929VE UT WOS:000229373900002 ER PT J AU Silvera, K Santiago, LS Winter, K AF Silvera, K Santiago, LS Winter, K TI Distribution of crassulacean acid metabolism in orchids of Panama: evidence of selection for weak and strong modes SO FUNCTIONAL PLANT BIOLOGY LA English DT Article DE carbon stable isotope; crassulacean acid metabolism; evolution; Orchidaceae; photosynthesis ID CARBON-ISOTOPE DISCRIMINATION; VASCULAR EPIPHYTES; DELTA-C-13 VALUES; PLANTS; CLUSIA; CAM; PHOTOSYNTHESIS; BROMELIACEAE; INTEGRATION; MADAGASCAR AB Crassulacean acid metabolism (CAM) is one of three metabolic pathways found in vascular plants for the assimilation of carbon dioxide. In this study, we investigate the occurrence of CAM photosynthesis in 200 native orchid species from Panama and 14 non-native species by carbon isotopic composition (delta(13)C) and compare these values with nocturnal acid accumulation measured by titration in 173 species. Foliar delta(13)C showed a bimodal distribution with the majority of species exhibiting values of approximately - 28 parts per thousand ( typically associated with the C(3) pathway), or - 15 parts per thousand ( strong CAM). Although thick leaves were related to delta(13)C values in the CAM range, some thin-leaved orchids were capable of CAM photosynthesis, as demonstrated by acid titration. We also found species with C(3) isotopic values and significant acid accumulation at night. Of 128 species with delta(13)C more negative than - 22 parts per thousand, 42 species showed nocturnal acid accumulation per unit fresh mass characteristic of weakly expressed CAM. These data suggest that among CAM orchids, there may be preferential selection for species to exhibit strong CAM or weak CAM, rather than intermediate metabolism. C1 Smithsonian Trop Res Inst, Balboa, Ancon, Panama. Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. Univ Calif Berkeley, Ctr Stable Isotope Biogeochem, Berkeley, CA 94720 USA. RP Silvera, K (reprint author), Smithsonian Trop Res Inst, POB 2072, Balboa, Ancon, Panama. EM katiasilvera@yahoo.com RI Santiago, Louis/E-3185-2016 OI Santiago, Louis/0000-0001-5994-6122 NR 40 TC 58 Z9 59 U1 4 U2 25 PU CSIRO PUBLISHING PI COLLINGWOOD PA 150 OXFORD ST, PO BOX 1139, COLLINGWOOD, VICTORIA 3066, AUSTRALIA SN 1445-4408 J9 FUNCT PLANT BIOL JI Funct. Plant Biol. PY 2005 VL 32 IS 5 BP 397 EP 407 DI 10.1071/FP04179 PG 11 WC Plant Sciences SC Plant Sciences GA 929VE UT WOS:000229373900004 ER PT J AU Gehrig, HH Wood, JA Cushman, MA Virgo, A Cushman, JC Winter, K AF Gehrig, HH Wood, JA Cushman, MA Virgo, A Cushman, JC Winter, K TI Large gene family of phosphoenolpyruvate carboxylase in the crassulacean acid metabolism plant Kalanchoe pinnata (Crassulaceae) characterised by partial cDNA sequence analysis SO FUNCTIONAL PLANT BIOLOGY LA English DT Article DE crassulacean acid metabolism; evolution; gene family; isogenes; Kalanchoe pinnata; phosphoenolpyruvate carboxylase ID CAM PLANT; FLAVERIA-TRINERVIA; C4 PHOTOSYNTHESIS; DELTA-C-13 VALUES; LEAF AGE; EXPRESSION; CO2; IDENTIFICATION; EVOLUTION; FIXATION AB Clones coding for a 1100-bp cDNA sequence of phosphoenolpyruvate carboxylase ( PEPC) of the constitutive crassulacean acid metabolism (CAM) plant Kalanchoe pinnata ( Lam.) Pers., were isolated by reverse transcription-polymerase chain reaction (RT - PCR) and characterised by restriction fragment length polymorphism analysis and DNA sequencing. Seven distinct PEPC isogenes were recovered, four in leaves and three in roots ( EMBL accession numbers: AJ344052 - AJ344058). Sequence similarity comparisons and distance neighbour-joining calculations separate the seven PEPC isoforms into two clades, one of which contains the three PEPCs found in roots. The second clade contains the four isoforms found in leaves and is divided into two branches, one of which contains two PEPCs most similar with described previously CAM isoforms. Of these two isoforms, however, only one exhibited abundant expression in CAM-performing leaves, but not in very young leaves, which do not exhibit CAM, suggesting this isoform encodes a CAM-specific PEPC. Protein sequence calculations suggest that all isogenes are likely derived from a common ancestor gene, presumably by serial gene duplication events. To our knowledge, this is the most comprehensive identification of a PEPC gene family from a CAM plant, and the greatest number of PEPC isogenes reported for any vascular plant to date. C1 Univ Nevada, Dept Biochem & Mol Biol, Reno, NV 89557 USA. Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Cushman, JC (reprint author), Univ Nevada, Dept Biochem & Mol Biol, Reno, NV 89557 USA. EM jcushman@unr.edu NR 38 TC 13 Z9 13 U1 2 U2 14 PU C S I R O PUBLISHING PI COLLINGWOOD PA 150 OXFORD ST, PO BOX 1139, COLLINGWOOD, VICTORIA 3066, AUSTRALIA SN 1445-4408 J9 FUNCT PLANT BIOL JI Funct. Plant Biol. PY 2005 VL 32 IS 5 BP 467 EP 472 DI 10.1071/FP05079 PG 6 WC Plant Sciences SC Plant Sciences GA 929VE UT WOS:000229373900009 ER PT B AU Modjaz, M Moran, JM Greenhill, LJ Kondratko, PT AF Modjaz, M Moran, JM Greenhill, LJ Kondratko, PT BE Romney, JD Reid, MJ TI Magnetic fields in accretion disks of AGN: The case of NGC 4258 SO Future Directions in High Resolution Astronomy: The 10th Anniversary of the VLBA SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 10th Anniversary of the VLBA CY JUN 08-12, 2003 CL Socorro, NM SP NRAO, NMT ID WATER MASERS; NGC 4258; NGC4258 AB We have improved the upper limit estimate on the toroidal component of the magnetic field in NGC 4258 at a radius of 0.2 pc from 300 mG (the former limit) to 50 mG. Assuming thermal and magnetic pressure balance, we estimate the accretion rate to be M/alpha <= 10(-3.5)cos theta(-2) M(circle dot)yr(-1) (where alpha is the viscosity parameter and theta the angle between our line-of-sight and the B field), which is much less than the predicted value of the standard ADAF model. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Modjaz, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 9 TC 1 Z9 1 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-207-5 J9 ASTR SOC P PY 2005 VL 340 BP 192 EP 194 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BDV12 UT WOS:000235590900047 ER PT B AU Greenhill, LJ AF Greenhill, LJ BE Romney, JD Reid, MJ TI Water masers and accretion disks in galactic nuclei SO Future Directions in High Resolution Astronomy: The 10th Anniversary of the VLBA SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 10th Anniversary of the VLBA CY JUN 08-12, 2003 CL Socorro, NM SP NRAO, NMT ID H2O MASER; CIRCINUS GALAXY; VAPOR MEGAMASER; EMISSION; DISCOVERY; SEARCH; NGC-4258; PARSEC AB There are over 50 sources of H2O maser emission in type-2 active galactic nuclei, a large fraction discovered in the last two years. Interferometer maps of water masers are presently the only means by which structures 1 pc from massive black holes can be mapped directly, which is particularly important for type-2 systems because edge-on orientation and obscuration complicate study by other means. Investigations of several sources have demonstrated convincingly that the maser emission traces warped accretion disks 0.1 to 1 pc from central engines of order 10(6)-10(8) M-circle dot. The same may be true for almost half the known (but unmapped) sources, based on spectral characteristics consistent with emission from edge-on accretion disks. Mapping these sources is a high priority. Study of most recently discovered masers requires long baseline arrays that include 100-m class apertures and would benefit from aggregate bit rates on the order of 1 gigabit per second. The Square Kilometer Array should provide an order of magnitude boost in mapping sensitivity, but outrigger antennas will be needed to achieve necesssary angular resolutions; as may be space-borne antennas. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Greenhill, LJ (reprint author), Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. NR 30 TC 4 Z9 4 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-207-5 J9 ASTR SOC P PY 2005 VL 340 BP 203 EP 209 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BDV12 UT WOS:000235590900050 ER PT B AU Peck, AB AF Peck, AB BE Romney, JD Reid, MJ TI The atomic and molecular environments of AGN SO FUTURE DIRECTIONS IN HIGH RESOLUTION ASTRONOMY: THE 10TH ANNIVERSARY OF THE VLBA SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 10th Anniversary of the VLBA CY JUN 08-12, 2003 CL Socorro, NM SP NRAO, NMT ID MASSIVE BLACK-HOLE; PARSEC-SCALE JETS; MERLIN OBSERVATIONS; CIRCUMNUCLEAR DISK; ACCRETION; MEGAMASER; NGC-4261; NGC4258; REGION; GAS AB The unified scheme of AGN requires an obscuring region of atomic or molecular gas surrounding the central engine which effectively shields the inner few parsecs of the source from view if the radio axis lies close to the plane of the sky. There are three methods by which it is possible to detect this circumnuclear structure; atomic gas seen in absorption, molecular gas seen either masing or in absorption, and ionized gas in absorption or emission. I will attempt to summarize some of the recent observations using all 3 of these methods. C1 Harvard Smithsonian Ctr Astrophys, SMA Project, Hilo, HI 96721 USA. RP Peck, AB (reprint author), Harvard Smithsonian Ctr Astrophys, SMA Project, POB 824, Hilo, HI 96721 USA. EM apeck@cfa.harvard.edu NR 23 TC 1 Z9 1 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-207-5 J9 ASTR SOC P PY 2005 VL 340 BP 210 EP 215 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BDV12 UT WOS:000235590900051 ER PT B AU Ball, GH Greenhill, LJ Moran, JM Zaw, I Henkel, C AF Ball, GH Greenhill, LJ Moran, JM Zaw, I Henkel, C BE Romney, JD Reid, MJ TI Parsec-scale water maser structure in TXS 2226-184 SO Future Directions in High Resolution Astronomy: The 10th Anniversary of the VLBA SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 10th Anniversary of the VLBA CY JUN 08-12, 2003 CL Socorro, NM SP NRAO, NMT ID EMISSION; GALAXY; DISK; H2O AB We report the first VLBI images of the water vapor maser emission in TXS 2226-184, one of the most distant known maser galaxies, at 102 Mpc. The emission is spread over a range of 350 km s(-1) in velocity and over a projected distance of almost 5 pc, oriented at approximate to 60 degrees with respect to a kpc-scale jet. The distribution of emission is consistent with a parsec-scale structure rotating around a central mass of similar to 10(7) M-circle dot. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Ball, GH (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 9 TC 1 Z9 1 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-207-5 J9 ASTR SOC P PY 2005 VL 340 BP 235 EP 237 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BDV12 UT WOS:000235590900056 ER PT B AU Reid, MJ Brunthaler, A AF Reid, MJ Brunthaler, A BE Romney, JD Reid, MJ TI The proper motion of Sgr A SO Future Directions in High Resolution Astronomy: The 10th Anniversary of the VLBA SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 10th Anniversary of the VLBA CY JUN 08-12, 2003 CL Socorro, NM SP NRAO, NMT ID GALACTIC-CENTER; BLACK-HOLE; ASTERISK; DYNAMICS; POSITION; RADIO AB We have now been measuring the position of Sgr A*, the candidate super-massive black hole at the center of the Galaxy, with the VLBA for about 8 years. Sgr A* appears to move almost entirely along the Galactic Plane at a rate of 6.37 +/- 0.02 mas yr(-1). For a distance to the Galactic Center of 8.0 +/- 0.5 kpc, this translates to 241 +/- 15 km s(-1) consistent with that expected for a stationary object observed from the Sun as it orbits the Galactic Center. The motion of Sgr A* out of the plane of the Galaxy, after removing the 7 km s-1 motion of the Sun in that direction, is less than about 2 km s(-1). Combining stellar orbital information (measured in the infrared) with the upper limit Of 2 kill s-1 for the intrinsic proper motion of Sgr A* (perpendicular to the Galactic plane), places a lower limit on the mass of Sgr A* of 2 x 10(6) M-circle dot. Thus, most of the mass sensed by stellar orbits is tied to the compact radio source Sgr A*, whose size is less than 1 AU, yielding the strongest case ever for a SMBH. This also argues against "exotic" forms of mass, postulated to explain the extreme mass concentration at the Galactic Center. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Reid, MJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 12 TC 7 Z9 7 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-207-5 J9 ASTR SOC P PY 2005 VL 340 BP 253 EP 257 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BDV12 UT WOS:000235590900060 ER PT B AU Fish, VL Reid, MJ Argon, AL Menten, KM AF Fish, VL Reid, MJ Argon, AL Menten, KM BE Romney, JD Reid, MJ TI VLBA full-polarization observations of interstellar hydroxyl masers: Preliminary results SO Future Directions in High Resolution Astronomy: The 10th Anniversary of the VLBA SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 10th Anniversary of the VLBA CY JUN 08-12, 2003 CL Socorro, NM SP NRAO, NMT ID YOUNG STELLAR OBJECTS; METHANOL MASERS; OH MASERS; W3(OH); REGION AB We present full-polarization VLBA images of 1665 and 1667 MHz OH masers toward massive star-forming regions. We discuss the significance of circular and linear polarization fractions as well as the alignment of linear polarization relative to source features. Magnetic fields deduced from Zeeman splitting suggest organized field structures with at most one line-of-sight field direction reversal. The magnetic field in a subregion of W75N appears to be aligned along the collinear arrangement of maser spots. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Fish, VL (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 13 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-207-5 J9 ASTR SOC P PY 2005 VL 340 BP 329 EP 333 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BDV12 UT WOS:000235590900075 ER PT B AU Humphreys, EML Argon, AL Greenhill, LJ Moran, JM Reid, MJ AF Humphreys, EML Argon, AL Greenhill, LJ Moran, JM Reid, MJ BE Romney, JD Reid, MJ TI Recent progress on a new distance to NGC 4258 SO Future Directions in High Resolution Astronomy: The 10th Anniversary of the VLBA SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 10th Anniversary of the VLBA CY JUN 08-12, 2003 CL Socorro, NM SP NRAO, NMT ID H2O MASER EMISSION; GALAXY NGC4258; DISK; NUCLEUS AB We report on our ongoing, high-resolution study of H2O masers in the innermost parsec of NGC 4258. Over thirty epochs of VLBA and VLA data, taken over six years, are being used to monitor the velocities, accelerations, positions and proper motions of water masers rotating in a warped, Keplerian disk about a supermassive central object. Our extensive monitoring results in an improved accuracy in the distance determination to this galaxy (i) via a reduction in experimental random errors due to a longer time-baseline than in previous work; and (ii) via a better modeling of sources of systematic error, such as disk eccentricity. These data can therefore yield an extremely accurate geometric distance to NGC 4258. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Humphreys, EML (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 10 TC 12 Z9 12 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-207-5 J9 ASTR SOC P PY 2005 VL 340 BP 466 EP 470 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BDV12 UT WOS:000235590900103 ER PT B AU Grimm, HJ Gilfanov, M Sunyaev, R AF Grimm, HJ Gilfanov, M Sunyaev, R BE Merloni, A Nayakshin, S Sunyaev, RA TI X-ray variability of the Milky Way SO Growing Black Holes: Accretion in a Cosmological Context SE ESO ASTROPHYSICS SYMPOSIA LA English DT Proceedings Paper CT MPA/ESO/MPE/USM Joint Astronomy Conference on Growing Black Holes CY JUN 21-25, 2004 CL Garching, GERMANY SP MPA, ESO, MPE, USM AB By constructing the power density spectrum of the Milky Way due to Galactic X-ray binaries (XRB) we investigate the prospect of disentangling the X-ray emission of galaxies due to SMBHs and X-ray binary populations for future X-ray missions. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Max Planck Inst Astrophys, D-85741 Garching, Germany. RP Grimm, HJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 2 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY BN 3-540-25275-4 J9 ESO ASTROPHY SYMP PY 2005 BP 181 EP 182 DI 10.1007/11403913_33 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BCP80 UT WOS:000230621000033 ER PT B AU Modjaz, M Moran, JM Greenhill, LJ Kondratko, PT AF Modjaz, M Moran, JM Greenhill, LJ Kondratko, PT BE Merloni, A Nayakshin, S Sunyaev, RA TI Probing the magnetic field at sub-Parsec radii in the accretion disk of NGC 4258 SO Growing Black Holes: Accretion in a Cosmological Context SE ESO ASTROPHYSICS SYMPOSIA LA English DT Proceedings Paper CT MPA/ESO/MPE/USM Joint Astronomy Conference on Growing Black Holes CY JUN 21-25, 2004 CL Garching, GERMANY SP MPA, ESO, MPE, USM ID ACTIVE GALACTIC NUCLEI; NGC 4258; BLACK-HOLES; JETS; NGC4258; REGION; MASERS; FLOWS AB We present an analysis of polarimetric observations of the water vapor masers in NGC 4258 obtained with the GBT at 22 GHz. We do not detect any circular polarization in the spectrum indicative of Zeeman-induced splitting of the maser lines of water. We have improved the 1-sigma upper limit estimate on the toroidal component of the magnetic field in the circumnuclear disk of NGC 4258 at a radius of 0.2 pc from 300 mG to 90 mG. We have developed a new method for the analysis of spectra with blended features and derive a 1-sigma upper limit of 30 mG on the radial component of the magnetic field at a radius of 0.14 pc. Assuming thermal and magnetic pressure balance, we estimate an upper limit on the mass accretion rate of similar to 10(-3.7) M(circle dot)yr(-1). We discuss the ramifications of our results on current accretion theories that have been used to explain low luminosity active galactic nuclei. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Modjaz, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 23 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY BN 3-540-25275-4 J9 ESO ASTROPHY SYMP PY 2005 BP 296 EP 301 DI 10.1007/11403913_53 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BCP80 UT WOS:000230621000053 ER PT B AU Forman, W Jones, C Churazov, E Heinz, S Kraft, R Markevitch, M Nulsen, P Vikhlinin, A AF Forman, W Jones, C Churazov, E Heinz, S Kraft, R Markevitch, M Nulsen, P Vikhlinin, A BE Merloni, A Nayakshin, S Sunyaev, RA TI Outbursts from supermassive black holes and their impacts on the hot gas in elliptical galaxies SO Growing Black Holes: Accretion in a Cosmological Context SE ESO ASTROPHYSICS SYMPOSIA LA English DT Proceedings Paper CT MPA/ESO/MPE/USM Joint Astronomy Conference on Growing Black Holes CY JUN 21-25, 2004 CL Garching, GERMANY SP MPA, ESO, MPE, USM ID COOLING FLOWS; THERMAL CONDUCTION; CENTAURUS-A; BUOYANT BUBBLES; RADIO LOBES; CLUSTERS; M87; EVOLUTION; MODELS; HALO C1 Smithsonian Astrophys Observ, CFA, Cambridge, MA 02138 USA. RP Forman, W (reprint author), Smithsonian Astrophys Observ, CFA, Cambridge, MA 02138 USA. RI Churazov, Eugene/A-7783-2013 NR 47 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY BN 3-540-25275-4 J9 ESO ASTROPHY SYMP PY 2005 BP 363 EP 370 DI 10.1007/11403913_70 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BCP80 UT WOS:000230621000070 ER PT S AU Horan, D Badran, HM Blaylock, G Bond, IH Boyle, PJ Bradbury, SM Buckley, JH Byrum, K Carter-Lewis, DA Celik, O Cogan, P Cui, W Daniel, MK Perez, ID Duke, C Falcone, A Fegan, DJ Fegan, SJ Finley, JP Fortson, LF Gammell, S Gibbs, K Gillanders, GH Grube, J Guiterrez, KJ Hall, J Hanna, D Holder, J Hughes, S Humensky, TB Jung, I Kenny, GE Kertzman, M Kieda, D Kildea, J Knapp, J Kosack, K Krawczynski, H Krennrich, F Lang, MJ Le Bohec, S Linton, E Lloyd-Evans, J Mendoza, D Merriman, A Milovanovic, A Moriarty, P Nagai, T Ong, RA Pallassini, R Perkins, J Petry, D Pohl, M Power-Mooney, B Quinn, J Quinn, M Ragan, K Rebillot, P Reynolds, PT Rose, HJ Schroedter, M Sembroski, GH Swordy, SP Syson, A Valcarcel, L Vassiliev, VV Wagner, R Wakely, SP Walker, G Weekes, TC White, RJ Zweerink, J AF Horan, D Badran, HM Blaylock, G Bond, IH Boyle, PJ Bradbury, SM Buckley, JH Byrum, K Carter-Lewis, DA Celik, O Cogan, P Cui, W Daniel, MK Perez, ID Duke, C Falcone, A Fegan, DJ Fegan, SJ Finley, JP Fortson, LF Gammell, S Gibbs, K Gillanders, GH Grube, J Guiterrez, KJ Hall, J Hanna, D Holder, J Hughes, S Humensky, TB Jung, I Kenny, GE Kertzman, M Kieda, D Kildea, J Knapp, J Kosack, K Krawczynski, H Krennrich, F Lang, MJ Le Bohec, S Linton, E Lloyd-Evans, J Mendoza, D Merriman, A Milovanovic, A Moriarty, P Nagai, T Ong, RA Pallassini, R Perkins, J Petry, D Pohl, M Power-Mooney, B Quinn, J Quinn, M Ragan, K Rebillot, P Reynolds, PT Rose, HJ Schroedter, M Sembroski, GH Swordy, SP Syson, A Valcarcel, L Vassiliev, VV Wagner, R Wakely, SP Walker, G Weekes, TC White, RJ Zweerink, J BE Aharonian, FA Volk, HJ Horns, D TI Very high energy observations of gamma ray bursts with the Whipple/VERITAS telescopes SO High Energy Gamma-Ray Astronomy SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT 2nd International Symposium on High Energy Gamma-Ray Astronomy CY JUL 26-30, 2004 CL Heidelberg, GERMANY SP Max-Planck Soc, German Fed Minist Educ Res, Deutsch Forsch Gemeinsch ID TEV; SEARCH; SUPERNOVA; ORIGIN; ARRAY AB Gamma-ray Burst (GRB) observations at Very High Energies (VHE, E > 100 GeV) can impose light constraints on some GRB emission models. Many GRB after-low models predict a VHE component similar to that seen in blazars and supernova remnants, in which the GRB spectral energy distribution has a double-peaked shape extending into the VHE regime. Consistent with this afterglow scenario. EGRET detected delayed high energy emission from all five bright BATSE GRBs that occurred within its field of view. GRB observations have had high priority in the observing program at the Whipple 10m Telescope and will continue to be high priority targets when the next generation observatory VERITAS comes online. Upper limits on the VHE emission from ten GRBs observed with the Whipple Telescope are reported here. C1 Harvard Smithsonian Ctr Astrophys, Amado, AZ 85645 USA. RP Horan, D (reprint author), Harvard Smithsonian Ctr Astrophys, POB 97, Amado, AZ 85645 USA. RI Daniel, Michael/A-2903-2010; OI Daniel, Michael/0000-0002-8053-7910; Cui, Wei/0000-0002-6324-5772; Knapp, Johannes/0000-0003-1519-1383; Lang, Mark/0000-0003-4641-4201 NR 22 TC 3 Z9 3 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 0-7354-0229-9 J9 AIP CONF PROC PY 2005 VL 745 BP 591 EP 596 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BCA30 UT WOS:000228449000077 ER PT S AU Butt, YM AF Butt, Yousaf Mahmood BE Engvold, O TI Some aspects of galactic cosmic ray acceleration SO HIGHLIGHTS OF ASTRONOMY, VOL 13 SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 25th General Assembly of the International-Astronomical-Union CY JUL 13-26, 2003 CL Sydney, AUSTRALIA SP Int Astronom Union ID SUPERNOVA REMNANT RCW-86; SINGLE-SOURCE; GAMMA-RAYS; EMISSION; REGIONS; ORIGIN AB I give a synopsis of two aspects of the Galactic Cosmic Ray (GCR) acceleration problem: the importance of the medium energy gamma-ray window, and several specific astrophysical sources which merit further investigation. NOTE: figures may be found in the on-line version only: astro-ph/0309758. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Butt, YM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 39 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA SN 0074-1809 BN 1-58381-189-3 J9 IAU SYMP PY 2005 VL 13 BP 24 EP 29 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BFB49 UT WOS:000240768700005 ER PT S AU Schneider, G Pasachoff, JM Golub, L AF Schneider, Glenn Pasachoff, Jay M. Golub, Leon BE Engvold, O TI Space studies of the black-drop effect at a mercury transit SO HIGHLIGHTS OF ASTRONOMY, VOL 13 SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 25th General Assembly of the International-Astronomical-Union CY JUL 13-26, 2003 CL Sydney, AUSTRALIA SP Int Astronom Union AB Transits of Mercury and Venus across the face of the Sun are rare. The 20th century had 15 transits of Mercury and the 21st century will have 14, the two most recent occurring on 15 November 1999 and 7 May 2003. We report on our observations and analysis of a black-drop effect at the 1999 and 2003 transits of Mercury seen in high spatial resolution optical imaging with NASA's Transition Region and Coronal Explorer (TRACE) spacecraft. We have separated the primary contributors to this effect, solar limb darkening and broadening due to the instrumental point spread function, for the 1999 event. The observations are important for understanding historical observations of transits of Venus, which in the 18th and 19th centuries were basic for the determination of the scale of the solar system. Our observations are in preparation for the 8 June 2004 transit of Venus, the first to occur since 1882. Only five transits of Venus have ever been seen - in 1639, 1761, 1769, 1874, and 1882. These events occur in pairs, whose members are separated by 8 years, with an interval between pairs of 105 or 122 years. Nobody alive has ever seen a transit of Venus. C1 Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Williams Coll, Hopkins Observ, Williamstown, MA 01267 USA. Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Schneider, G (reprint author), Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA. NR 3 TC 1 Z9 1 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA SN 0074-1809 BN 1-58381-189-3 J9 IAU SYMP PY 2005 VL 13 BP 70 EP 72 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BFB49 UT WOS:000240768700017 ER PT S AU Nulsen, PEJ McNamara, BR David, LP Wise, MW AF Nulsen, Paul E. J. McNamara, Brian R. David, Laurence P. Wise, Michael W. BE Engvold, O TI X-ray cavities and cooling flows SO HIGHLIGHTS OF ASTRONOMY, VOL 13 SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 25th General Assembly of the International-Astronomical-Union CY JUL 13-26, 2003 CL Sydney, AUSTRALIA SP Int Astronom Union ID THERMAL CONDUCTION; GALAXY CLUSTERS; HIGH-RESOLUTION; RADIO LOBES; HYDRA-A; CHANDRA; GAS; SAMPLE; ROSAT; CONSTRAINTS AB Recent data have radically altered the X-ray perspective on cooling flow clusters. X-ray spectra show that very little of the hot intra-cluster medium is cooler than about 1 keV, despite having short cooling times. In an increasing number of cooling flow clusters, the lobes of a central radio source are found to have created cavities in the hot gas. Generally, the cavities are not overpressured relative to the intra-cluster gas, but act as buoyant bubbles of radio emitting plasma that drive circulation as they rise, mixing and heating the intra-cluster gas. All this points to the radio source, i.e., an active galactic nucleus, as the heat source that prevents gas from cooling to low temperatures. However, heating due to bubbles alone seems to be insufficient, so the energetics of cooling flows remain obscure. We briefly review the data and theory supporting this view and discuss the energetics of cooling flows. C1 Univ Wollongong, Sch Engn Phys, Wollongong, NSW 2522, Australia. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Ohio Univ, Dept Phys & Astron, Athens, OH 45701 USA. MIT, Ctr Space Res, Cambridge, MA 02139 USA. RP Nulsen, PEJ (reprint author), Univ Wollongong, Sch Engn Phys, Wollongong, NSW 2522, Australia. NR 31 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA SN 0074-1809 BN 1-58381-189-3 J9 IAU SYMP PY 2005 VL 13 BP 307 EP 311 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BFB49 UT WOS:000240768700092 ER PT S AU Pradhan, AK Nahar, SN Smith, PL AF Pradhan, Anil K. Nahar, Sultana N. Smith, Peter L. BE Engvold, O TI IAU XXV JD17: Atomic data for X-ray astronomy SO HIGHLIGHTS OF ASTRONOMY, VOL 13 SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 25th General Assembly of the International-Astronomical-Union CY JUL 13-26, 2003 CL Sydney, AUSTRALIA SP Int Astronom Union C1 Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Pradhan, AK (reprint author), Ohio State Univ, Dept Astron, 174 W 18Th Ave, Columbus, OH 43210 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA SN 0074-1809 BN 1-58381-189-3 J9 IAU SYMP PY 2005 VL 13 BP 617 EP 617 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BFB49 UT WOS:000240768700171 ER PT S AU Beiersdorfer, P Chen, H Boyce, KR Brown, GV Kelley, RL Porter, FS Stahle, CK Lepson, JK Jernigan, JG Wargelin, BJ Kahn, SM AF Beiersdorfer, P. Chen, H. Boyce, K. R. Brown, G. V. Kelley, R. L. Porter, F. S. Stahle, C. K. Lepson, J. K. Jernigan, J. G. Wargelin, B. J. Kahn, S. M. BE Engvold, O TI New results in laboratory X-ray astrophysics SO HIGHLIGHTS OF ASTRONOMY, VOL 13 SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 25th General Assembly of the International-Astronomical-Union CY JUL 13-26, 2003 CL Sydney, AUSTRALIA SP Int Astronom Union ID HIGH-RESOLUTION MEASUREMENTS; BEAM ION-TRAP; FE-XXV; HELIUM-LIKE; CROSS-SECTIONS; LINE EMISSION; ELECTRON-BEAM; RELATIVE INTENSITY; TRANSITIONS; SPECTRUM AB A multi-faceted, multi-institutional laboratory astrophysics program is carried out at the Livermore electron beam ion trap facility, which is a mature spectroscopic source with unsurpassed controls and capabilities, and an unparalleled assortment of spectroscopic equipment, including a full complement of grating and crystal spectrometers and a 6x6 micro-calorimeter array. Recent results range from the calibration of x-ray diagnostics, including the Fe XVII and Fe XXV emission lines, extensive lists of L-shell ions, the first laboratory simulation and fit of a cometary x-ray emission spectrum, and the discovery of new spectral diagnostics for measuring magnetic field strengths. C1 Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Stanford Univ, Dept Phys, Stanford, CA 94305 USA. RP Beiersdorfer, P (reprint author), Lawrence Livermore Natl Lab, POB 5508, Livermore, CA 94550 USA. RI Porter, Frederick/D-3501-2012; Kelley, Richard/K-4474-2012 OI Porter, Frederick/0000-0002-6374-1119; NR 35 TC 2 Z9 2 U1 0 U2 1 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA SN 0074-1809 BN 1-58381-189-3 J9 IAU SYMP PY 2005 VL 13 BP 633 EP 639 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BFB49 UT WOS:000240768700177 ER PT S AU Smith, RK Brickhouse, NS Liedahl, DA AF Smith, Randall K. Brickhouse, Nancy S. Liedahl, Duane A. BE Engvold, O TI The astrophysical plasma emission database: Progress and plans SO HIGHLIGHTS OF ASTRONOMY, VOL 13 SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 25th General Assembly of the International-Astronomical-Union CY JUL 13-26, 2003 CL Sydney, AUSTRALIA SP Int Astronom Union ID SPECTRA; IONS AB The Astrophysical Plasma Emission Database (APED) contains atomic data for the 14 most abundant astrophysical elements, collected from the literature. Although APED was originally designed for use in calculating a collisional-equilibrium X-ray spectrum suitable for analysis of high-resolution data, it is in a general format which can be efficiently used to calculate absorption spectra, photoionization models, and non-equilibrium collisional models. We emphasize original sources; each transition, rate, and energy level in APED contains a bibliographic reference. The APED can be downloaded from http://cxc.harvard.edu/atomdb/ ,or our website WebGUIDE (http://obsvis.harvard.edu/WebGUIDE/) can be used to search for individual lines or transitions. We are continually working to expand APED (current version 1.3.1) and regularly issue updated collections. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Lawrence Livermore Natl Lab, Dept Phys & Adv Technol, Livermore, CA 94550 USA. RP Smith, RK (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Brickhouse, Nancy/0000-0002-8704-4473 NR 5 TC 0 Z9 0 U1 1 U2 1 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA SN 0074-1809 BN 1-58381-189-3 J9 IAU SYMP PY 2005 VL 13 BP 666 EP 667 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BFB49 UT WOS:000240768700185 ER PT S AU Brickhouse, NS AF Brickhouse, Nancy S. BE Engvold, O TI Astrophysics at X-ray spectral resolution 1000 SO HIGHLIGHTS OF ASTRONOMY, VOL 13 SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 25th General Assembly of the International-Astronomical-Union CY JUL 13-26, 2003 CL Sydney, AUSTRALIA SP Int Astronom Union AB The Chandra gratings exceed a resolving power R = 1000, but only at the longest wavelengths and with relatively low effective areas. Recent X-ray observations of cool stars illustrate the problem of line blending at different resolutions and give a good sense of what we will routinely be able to measure with Constellation-X, provided it has high enough spectral resolution. We also expect new diagnostics from weak lines and line profiles. Support for this work is provided by NASA NAS8-39083 to SAO for the CXC and LTSA NAG5-3559. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Brickhouse, NS (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Brickhouse, Nancy/0000-0002-8704-4473 NR 5 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA SN 0074-1809 BN 1-58381-189-3 J9 IAU SYMP PY 2005 VL 13 BP 787 EP 789 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BFB49 UT WOS:000240768700219 ER PT S AU Mohanty, S Basri, G Jayawardhana, R AF Mohanty, Subhanjoy Basri, Gibor Jayawardhana, Ray BE Engvold, O TI Surface gravities and masses in substellar objects SO HIGHLIGHTS OF ASTRONOMY, VOL 13 SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 25th General Assembly of the International-Astronomical-Union CY JUL 13-26, 2003 CL Sydney, AUSTRALIA SP Int Astronom Union ID ATMOSPHERES AB Using high-resolution optical spectra, we determine effective temperatures and gravities for a sample of very low-mass stellar and substellar PMS cluster objects. Masses and radii are then derived using known cluster distance and photometry; two of our targets seem to have planetary masses. Our results are independent of theoretical evolutionary tracks. While our results agree with the track predictions for hotter, higher mass objects, discrepancies appear for the coolest, lowest mass ones. This may be due to track uncertainties related to formation effects, and/or internal conditions, in these very young, ultra-low-mass objects. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. RP Mohanty, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 3 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA SN 0074-1809 BN 1-58381-189-3 J9 IAU SYMP PY 2005 VL 13 BP 813 EP 815 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BFB49 UT WOS:000240768700228 ER PT S AU Peck, AB Tarchi, A Henkel, C Nagar, NM Braatz, J Moscadelli, L AF Peck, A. B. Tarchi, A. Henkel, C. Nagar, N. M. Braatz, J. Moscadelli, L. BE Engvold, O TI Newly detected H(2)O masers in Seyfert and starburst galaxies SO HIGHLIGHTS OF ASTRONOMY, VOL 13 SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 25th General Assembly of the International-Astronomical-Union CY JUL 13-26, 2003 CL Sydney, AUSTRALIA SP Int Astronom Union AB We report new detections of three H(2)O Inegamasers and one kilomaser using the Effelsberg 100-m telescope. Isotropic luminosities are similar to 50, 300, 1, and 230 L(circle dot) for Mrk 1066, Mrk 34, NGC 3556, and Arp 299, respectively. Mrk 34 contains the most distant H(2)O megamaser ever detected in a Seyfert. Our targets in this survey were chosen to fit one of the following criteria: 1) to have a high probability of interaction between the radio jet and the ISM within the central few parsecs of the radio galaxy, yielding masers which arise in local molecular clouds, or 2) to have very bright IRAS sources in which massive star forming regions might yield powerful masers. The 'jet maser' sources can provide detailed information about the conditions in the ISM in the central 1-10 pc of AGN. The extra-galactic 'star formation masers' can be used to pinpoint and characterize locations of high mass star formation in nearby galaxies. In addition, these sources will help to provide a better understanding of the chemical properties of molecular clouds in extra-galactic systems. C1 Harvard Smithsonian Ctr Astrophys, SMA Project, Hilo, HI 96721 USA. CNR, Ist Radioastron, I-40129 Bologna, Italy. Osservat Astron Cagliari, I-09012 Capoterra, Italy. MPIfR, D-53121 Bonn, Germany. Univ Groningen, Kapteyn Inst, NL-9747 AD Groningen, Netherlands. NRAO, Green Bank, WV USA. RP Peck, AB (reprint author), Harvard Smithsonian Ctr Astrophys, SMA Project, POB 824, Hilo, HI 96721 USA. NR 8 TC 0 Z9 0 U1 2 U2 2 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA SN 0074-1809 BN 1-58381-189-3 J9 IAU SYMP PY 2005 VL 13 BP 851 EP 853 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BFB49 UT WOS:000240768700238 ER PT S AU Kim, S Walsh, W Xiao, KC Lane, AP Stark, AA AF Kim, Sungeun Walsh, Wilfred Xiao, Kecheng Lane, Adair P. Stark, Antony A. BE Engvold, O TI CO J=7 -> 6 emission in the Large Magellanic Cloud SO HIGHLIGHTS OF ASTRONOMY, VOL 13 SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 25th General Assembly of the International-Astronomical-Union CY JUL 13-26, 2003 CL Sydney, AUSTRALIA SP Int Astronom Union ID SEST KEY PROGRAM; APERTURE SYNTHESIS AB We present the first detection of (12)CO (J = 7 -> 6) emission in the Magellanic Clouds toward the 30 Doradus region using the Antarctic Sub-millimeter Telescope and Remote Observatory (AST/RO). C1 Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kim, S (reprint author), Univ Massachusetts, Dept Astron, 710 N Pleasant St, Amherst, MA 01003 USA. NR 8 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA SN 0074-1809 BN 1-58381-189-3 J9 IAU SYMP PY 2005 VL 13 BP 860 EP 863 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BFB49 UT WOS:000240768700240 ER PT S AU Stark, AA AF Stark, Antony A. BE Engvold, O TI The AST/RO survey of the Galactic Center Region SO HIGHLIGHTS OF ASTRONOMY, VOL 13 SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 25th General Assembly of the International-Astronomical-Union CY JUL 13-26, 2003 CL Sydney, AUSTRALIA SP Int Astronom Union ID ANTARCTIC-SUBMILLIMETER-TELESCOPE; KINEMATICS AB AST/RO is a 1.7m diameter submillimeter-wave telescope at the geographic South Pole. A key AST/RO project is the mapping of CI and CO J = 4 -> 3 and J = 7 -> 6 emission from the inner Milky Way (Martin et al. 2003). These data are released for general use. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Stark, AA (reprint author), Smithsonian Astrophys Observ, 60 Garden St MS 12, Cambridge, MA 02138 USA. NR 7 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA SN 0074-1809 BN 1-58381-189-3 J9 IAU SYMP PY 2005 VL 13 BP 945 EP 946 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BFB49 UT WOS:000240768700277 ER PT S AU Stark, AA AF Stark, Antony A. BE Engvold, O TI The case for a 30m diameter submillimeter telescope on the Antarctic plateau SO HIGHLIGHTS OF ASTRONOMY, VOL 13 SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 25th General Assembly of the International-Astronomical-Union CY JUL 13-26, 2003 CL Sydney, AUSTRALIA SP Int Astronom Union ID GALAXY FORMATION; SOUTH-POLE AB A large single-dish submillimeter-wave telescope equipped with a focal plane array containing similar to 10(4) bolometers and costing about $120M could locate most protogalaxies in the southern sky within a year of operation. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Stark, AA (reprint author), Smithsonian Astrophys Observ, 60 Garden St MS 12, Cambridge, MA 02138 USA. NR 6 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA SN 0074-1809 BN 1-58381-189-3 J9 IAU SYMP PY 2005 VL 13 BP 954 EP 955 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BFB49 UT WOS:000240768700282 ER PT S AU Walsh, W Xiao, KC AF Walsh, Wilfred Xiao, Kecheng BE Engvold, O TI An AST/RO survey of the coalsack SO HIGHLIGHTS OF ASTRONOMY, VOL 13 SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 25th General Assembly of the International-Astronomical-Union CY JUL 13-26, 2003 CL Sydney, AUSTRALIA SP Int Astronom Union AB Selected regions of the southern molecular cloud complex, the Coalsack are being imaged at sub-millimeter wavelengths using the Antarctic Sub-millimeter Telescope and Remote Observatory (AST/RO) located at the South Pole. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Walsh, W (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS12, Cambridge, MA 02138 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA SN 0074-1809 BN 1-58381-189-3 J9 IAU SYMP PY 2005 VL 13 BP 965 EP 965 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BFB49 UT WOS:000240768700288 ER PT S AU Tothill, NFH Marston, AP Martin, CL Leppik, K AF Tothill, N. F. H. Marston, A. P. Martin, C. L. Leppik, K. BE Engvold, O TI CO 2-1 mapping of WR16 with AST/RO SO HIGHLIGHTS OF ASTRONOMY, VOL 13 SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 25th General Assembly of the International-Astronomical-Union CY JUL 13-26, 2003 CL Sydney, AUSTRALIA SP Int Astronom Union AB Massive stars have profound effects on their surroundings, influencing them by their energetic stellar winds, and finally by supernova explosions. We present a CO 2-1 map of the surroundings of the Wolf-Rayet star WR16, taken with AST/RO at the South Pole, which shows some of these effects. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CALTECH, SIRTF Sci Ctr, IPAC, Pasadena, CA 91125 USA. RP Tothill, NFH (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA SN 0074-1809 BN 1-58381-189-3 J9 IAU SYMP PY 2005 VL 13 BP 967 EP 967 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BFB49 UT WOS:000240768700290 ER PT S AU Traub, WA Stark, AA Jucks, KW Kilston, S Turner, EL Seager, S AF Traub, Wesley A. Stark, Antony A. Jucks, Kenneth W. Kilston, Steven Turner, Edwin L. Seager, Sara BE Engvold, O TI Earth as an extrasolar planet: South Pole advantages SO HIGHLIGHTS OF ASTRONOMY, VOL 13 SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 25th General Assembly of the International-Astronomical-Union CY JUL 13-26, 2003 CL Sydney, AUSTRALIA SP Int Astronom Union AB We could observe the Earth as an extra-solar planet, viewing Earthshine on the dark side of the Moon, at the Pole, in winter. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Ball Aerosp, Boulder, CO USA. Princeton Univ, Princeton, NJ 08544 USA. Carnegie Inst, Washington, DC USA. RP Traub, WA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Turner, Edwin/A-4295-2011 NR 0 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA SN 0074-1809 BN 1-58381-189-3 J9 IAU SYMP PY 2005 VL 13 BP 970 EP 970 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BFB49 UT WOS:000240768700293 ER PT S AU Winter, FH AF Winter, FH BE Elder, DC James, GS TI Rocketdyne - A giant pioneer in rocket technology: The earliest years, 1945-1955 SO History of Rocketry and Astronautics SE AAS HISTORY SERIES LA English DT Proceedings Paper CT 31st History Symposium of the International-Academy-of-Astronautics CY OCT 06-10, 1997 CL Turin, ITALY SP Int Acad Astronaut C1 Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA. NR 79 TC 1 Z9 1 U1 0 U2 0 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 0730-3564 BN 0-87703-518-0 J9 AAS HIST S PY 2005 VL 26 BP 65 EP 93 PG 29 WC History & Philosophy Of Science SC History & Philosophy of Science GA BCO84 UT WOS:000230451700006 ER PT J AU Ishtiaq, F Rahmani, AR AF Ishtiaq, F Rahmani, AR TI The Forest Owlet Heteroglaux blewitti: vocalization, breeding biology and conservation SO IBIS LA English DT Article AB The little-known, endemic Forest Owlet Heteroglaux blewitti was studied from June 1998 to June 1999 in Maharashtra, India. Vocalizations associated with contact, courtship feeding and food solicitation were recorded and sonagrams are presented for the first time. The nesting period started in October 1998 and continued until May 1999. Four nests were located and three were monitored for intensive studies on the breeding biology. Thirty days were spent on incubation (n = 2), mainly performed by the female while the male supplied food to the female and chicks. The observed brood size was two. The chicks fledged at 40 days but were dependent on their parents for food and protection for a further 45 days. The very low population density of the species could be due to degraded and fragmented habitat, scarcity of nest-sites or cronism observed in the species. C1 Bombay Nat Hist Soc, Bombay 400023, Maharashtra, India. RP Ishtiaq, F (reprint author), Smithsonian Inst, Genet Program, 3001 Connecticut Ave NW, Washington, DC 20008 USA. EM farahishtiaq@yahoo.com NR 15 TC 4 Z9 8 U1 3 U2 7 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0019-1019 J9 IBIS JI Ibis PD JAN PY 2005 VL 147 IS 1 BP 197 EP 205 DI 10.1111/j.1474-919x.2004.00389 PG 9 WC Ornithology SC Zoology GA 889XT UT WOS:000226476900018 ER PT J AU Ogunjemiyo, S Parker, G Roberts, D AF Ogunjemiyo, S Parker, G Roberts, D TI Reflections in bumpy terrain: Implications of canopy surface variations for the radiation balance of vegetation SO IEEE GEOSCIENCE AND REMOTE SENSING LETTERS LA English DT Article DE Airborne Visible Infrared/Imaging Spectrometer (AVIRIS); albedo; reflectance; rugosity; small-footprint lidar ID FOREST; ALBEDO; LANDSCAPE; CLIMATE; MODELS; AVIRIS; AVHRR; MODIS AB Data from an optical imaging sensor and a small-footprint lidar were used to examine the relation between canopy reflectance and outer surface complexity in forest stands in the southern Cascades of Washington state. Albedo was estimated from the Airborne Visible Infrared/Imaging Spectrometer; canopy surface variation (termed "rugosity") was estimated from small-footprint lidar; and stand ages were obtained through U.S. Forest Service records and global information system coverages. Results showed that albedo from Douglas-fir/western hemlock stands decreased, and variation in the outer surface of the canopy increased with age. Estimates of rugosity increased most rapidly in young stands and then more slowly after about 150 years. Albedo declined by 10% across the age sequence, suggesting that older stands of this forest type enjoy a substantial advantage in energy input. The results highlight the impacts of land-cover change on local energy balance and climate. C1 Univ Calif Santa Barbara, Dept Geog, Santa Barbara, CA 93106 USA. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Ogunjemiyo, S (reprint author), Univ Calif Santa Barbara, Dept Geog, Santa Barbara, CA 93106 USA. OI Parker, Geoffrey/0000-0001-7055-6491 NR 23 TC 13 Z9 13 U1 0 U2 4 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 1545-598X J9 IEEE GEOSCI REMOTE S JI IEEE Geosci. Remote Sens. Lett. PD JAN PY 2005 VL 2 IS 1 BP 90 EP 93 DI 10.1109/LGRS.2004.841418 PG 4 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 949NP UT WOS:000230795700020 ER PT J AU Battat, J Blundell, R Hunter, TR Kimberk, R Leiker, PS Tong, CYE AF Battat, J Blundell, R Hunter, TR Kimberk, R Leiker, PS Tong, CYE TI Gain stabilization of a submillimeter SIS heterodyne receiver SO IEEE TRANSACTIONS ON MICROWAVE THEORY AND TECHNIQUES LA English DT Article DE gain control; servosystems; stability; submillimeter-wave radiometry; submillimeter-wave receivers ID ARRAY AB We have designed a system to stabilize the gain of a submillimeter heterodyne receiver against thermal fluctuations of the mixing element. In the most sensitive heterodyne receivers, the mixer is usually cooled to 4 K using a closed-cycle cryocooler, which can introduce similar to1% fluctuations in the physical temperature of the receiver components. We compensate for the resulting mixer conversion gain fluctuations by monitoring the physical temperature of the mixer and adjusting the gain of the IF amplifier that immediately follows the mixer. This IF power stabilization scheme; developed for use at the Submillimeter Array, a submillimeter interferometer telescope located on Mauna Kea, HI, routinely achieves a receiver gain stability of one part in 6000 (rms to mean). This is an order of magnitude improvement over the typical uncorrected stability of one part in a few hundred. Our gain stabilization scheme is a useful addition to superconductor-insulator-superconductor heterodyne receivers that are cooled using closed-cycle cryocoolers in which the 4-K temperature fluctuations tend to be the leading cause of IF power fluctuations. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Battat, J (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jbattat@cfa.harvard.edu OI Tong, Edward/0000-0002-7736-4203; Hunter, Todd/0000-0001-6492-0090 NR 11 TC 4 Z9 4 U1 0 U2 1 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0018-9480 J9 IEEE T MICROW THEORY JI IEEE Trans. Microw. Theory Tech. PD JAN PY 2005 VL 53 IS 1 BP 389 EP 395 DI 10.1109/TMTT.2004.839942 PG 7 WC Engineering, Electrical & Electronic SC Engineering GA 887ZI UT WOS:000226343600045 ER PT S AU Melnick, GJ Bergin, EA AF Melnick, GJ Bergin, EA BE Wesselius, PR Encrenaz, T TI The legacy of SWAS: Water and molecular oxygen in the interstellar medium SO INFRARED/SUBMM ASTRONOMY FROM SPACE SE ADVANCES IN SPACE RESEARCH-SERIES LA English DT Article; Proceedings Paper CT 35th COSPAR Scientific Assembly CY JUL 18-25, 2004 CL Paris, FRANCE SP Comm Space Res DE ISM; astrochemistry; molecular clouds; water; molecular oxygen ID WAVE-ASTRONOMY-SATELLITE; CLOUDS; ABSORPTION; ABUNDANCE; CHEMISTRY; EMISSION; REGIONS AB The Submillimeter Wave Astronomy Satellite has recently completed 5.5 years of successful operation. Among the legacies of the mission has been a greater understanding of the abundance and spatial distribution of H2O and O-2 within molecular clouds. The model summarized here provides an explanation for the relatively low gaseous H2O abundance and the high H2O-ice abundance in cold dense clouds, the higher H2O abundance toward diffuse clouds, the low O-2 abundance toward all clouds observed. (c) 2005 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Univ Michigan, Dept Astron, 825 Dennison,501 E Univ Ave, Ann Arbor, MI 48109 USA. EM ebergin@umich.edu NR 15 TC 27 Z9 27 U1 0 U2 1 PU ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD 0X5 1GB, OXON, ENGLAND SN 0273-1177 J9 ADV SPACE RES-SERIES PY 2005 VL 36 IS 6 SI 2005 BP 1027 EP 1030 DI 10.1016/j.asr.2005.05.110 PG 4 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BDT08 UT WOS:000235191800001 ER PT B AU Lada, CJ AF Lada, CJ BE Corbelli, E Palla, F Zinnecker, H TI Embedded clusters and the IMF SO Initial Mass Function 50 years Later SE ASTROPHYSICS AND SPACE SCIENCE LIBRARY LA English DT Proceedings Paper CT International Conference on Initial Mass Function 50 Years Later CY MAY 16-20, 2004 CL Siena, ITALY SP Osservator Astrofis Arcetri ID ORION NEBULA CLUSTER; INITIAL MASS FUNCTION; BROWN DWARFS; STARS; LUMINOSITY; POPULATION; PLANETS AB Despite valiant efforts over nearly five decades, attempts to determine the IMF over a complete mass range for galactic field stars and in open clusters have proved difficult. Infrared imaging observations of extremely young embedded clusters coupled with Monte Carlo modeling of their luminosity functions are improving this situation and providing important new contributions to our fundamental knowledge of the IMF and its universality in both space and time. C1 Smithsonian Astrophys Observ, Cambridge, MA USA. RP Lada, CJ (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA USA. NR 14 TC 1 Z9 1 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS BN 1-4020-3406-7 J9 ASTROPHYS SPACE SC L PY 2005 VL 327 BP 109 EP 114 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BDD78 UT WOS:000232952300016 ER PT B AU Luhman, KL AF Luhman, KL BE Corbelli, E Palla, F Zinnecker, H TI The IMF of stars and brown dwarfs in star forming regions SO Initial Mass Function 50 years Later SE ASTROPHYSICS AND SPACE SCIENCE LIBRARY LA English DT Proceedings Paper CT International Conference on Initial Mass Function 50 Years Later CY MAY 16-20, 2004 CL Siena, ITALY SP Osservator Astrofis Arcetri ID ORION NEBULA CLUSTER; PLANETARY-MASS OBJECTS; LUMINOSITY; IC-348 AB I present recent measurements of the initial mass function and spatial distribution of stars and brown dwarfs in nearby star-forming regions. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Luhman, KL (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 18 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS BN 1-4020-3406-7 J9 ASTROPHYS SPACE SC L PY 2005 VL 327 BP 115 EP 120 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BDD78 UT WOS:000232952300017 ER PT B AU Beuther, H AF Beuther, H BE Corbelli, E Palla, F Zinnecker, H TI Fragmentation of a high-mass star forming core SO Initial Mass Function 50 years Later SE ASTROPHYSICS AND SPACE SCIENCE LIBRARY LA English DT Proceedings Paper CT International Conference on Initial Mass Function 50 Years Later CY MAY 16-20, 2004 CL Siena, ITALY SP Osservator Astrofis Arcetri ID PROTOSTELLAR CANDIDATES; EMISSION; CONTINUUM; OUTFLOWS; CLOUD AB At the earliest evolutionary stages, massive star forming regions are deeply embedded within their natal cores and not observable at optical and near-infrared wavelengths. Interferometric high-spatial resolution mm dust continuum observations of one very young high-mass star forming region disentangle its cluster-like nature already at the very beginning of the star formation process. The derived protocluster mass function is consistent with the stellar IMF Hence, fragmentation of the initial massive cores may determine the IMF and the masses of the final stars. This implies that stars of all masses can form via accretion. and coalescence of protostars appears not to be necessary. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Beuther, H (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 14 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS BN 1-4020-3406-7 J9 ASTROPHYS SPACE SC L PY 2005 VL 327 BP 323 EP 326 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BDD78 UT WOS:000232952300062 ER PT B AU Hartmann, L AF Hartmann, L BE Corbelli, E Palla, F Zinnecker, H TI Flows, filaments and fragmentation SO Initial Mass Function 50 years Later SE ASTROPHYSICS AND SPACE SCIENCE LIBRARY LA English DT Proceedings Paper CT International Conference on Initial Mass Function 50 Years Later CY MAY 16-20, 2004 CL Siena, ITALY SP Osservator Astrofis Arcetri ID INITIAL MASS FUNCTION; STAR-FORMING REGION; CLOUD FRAGMENTATION; CYLINDRICAL CLOUDS; MOLECULAR CLOUDS; TAURUS AB The location and extension of protostellar cloud cores in Taurus suggests that gravitational fragmentation in filaments is responsible for making those cores. To understand the basic mechanisms of this kind of fragmentation, we conducted simple simulations of finite self-gravitating sheets, envisioning these sheets as an approximation to molecular clouds formed by large scale flows. These simulations show that overall equilibrium is difficult if not impossible to maintain; that filaments are a general result of gravitational collapse in non-circular sheets; and that the structure of cloud edges are amplified by gravity to make focal points which can be the trigger for low-mass core fragmentation on small scales as well as likely sites for large mass concentrations needed to make high-mass stars and clusters. The effects of gravity suggest a possible link between cloud edges and mass spectra. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Hartmann, L (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. NR 18 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS BN 1-4020-3406-7 J9 ASTROPHYS SPACE SC L PY 2005 VL 327 BP 341 EP 346 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BDD78 UT WOS:000232952300064 ER PT B AU Melnick, GJ AF Melnick, GJ BE Corbelli, E Palla, F Zinnecker, H TI Future observational opportunities SO Initial Mass Function 50 years Later SE ASTROPHYSICS AND SPACE SCIENCE LIBRARY LA English DT Proceedings Paper CT International Conference on Initial Mass Function 50 Years Later CY MAY 16-20, 2004 CL Siena, ITALY SP Osservator Astrofis Arcetri AB The opportunities available to infrared, submillimeter, and millimeter wave astronomers are on the threshold of a revolution. Within the next 20 years, the number of new facilities coupled with their size, superb locations, and increased sensitivities will allow for markedly greater capabilities. This contribution will summarize the advances expected from those new telescopes operating between 30 mu m and I cm. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Melnick, GJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS BN 1-4020-3406-7 J9 ASTROPHYS SPACE SC L PY 2005 VL 327 BP 533 EP 538 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BDD78 UT WOS:000232952300098 ER PT S AU Margarita, K AF Margarita, K BE Burderi, L Antonelli, LA DAntona, F Israel, GL DiSalvo, T Piersanti, L Tornambe, A Straniero, O TI High-angular resolution imaging of interacting binaries SO Interacting Binaries: Accretion, Evolution, and Outcomes SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT Conference on Interacting Binaries CY JUL 04-10, 2004 CL Cefalu, ITALY SP Astron Observ Rome, Astron Observ Teramo, Univ Palermo, Dept Phys & Astron DE interacting binaries; symbiotics; accretion ID HUBBLE-SPACE-TELESCOPE; MIRA-B; ULTRAVIOLET-SPECTRA; H-2 EMISSION; CH CYGNI; SYSTEM AB I describe examples of long-term studies of interacting binary systems which have detected dramatic changes in the spatial and spectral distribution of the emission related to changes in accretion processes. These studies demonstrate that there are many aspects of accretion processes in general, and of wind accretion processes in particular, that are not yet understood. The key to further accretion studies is resolving a wide range of interacting binaries and studying their components and mass flows. A sub-milliarcsecond resolution is required to carry out detailed studies of nearby interacting binaries. I discuss future prospects for resolving accreting binary systems using the Stellar Imager - a many-element interferometer in space. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Margarita, K (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 14 TC 0 Z9 0 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0286-8 J9 AIP CONF PROC PY 2005 VL 797 BP 265 EP 270 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BDJ83 UT WOS:000233934400034 ER PT J AU Hochberg, R AF Hochberg, R TI First record of Polymerurus (Gastrotricha, Chaetonotida) from Australia with the description of a new species from Queensland and of cuticular ultrastructure in P-nodicaudus SO INVERTEBRATE BIOLOGY LA English DT Article DE gastrotrich; meiofauna; Paucitubulatina; electron microscopy ID MACRODASYIDA; MORPHOLOGY; BEACHES AB Identification of specimens in the genus Polymerurus (Gastrotricha, Chactonotida) is reported for the first time from Australia. The genus includes 3 species from a freshwater lake in southern Queensland. Two species, Polymerurus rhomboides and P. nodicaudus, are well-known cosmopolitans: P. rhomboides is now known from every continent except Antarctica, and P. nodicaudus from all continents except Africa and Antarctica. An ultrastructural description of the cuticle in P. nodicaudus is provided and confirms earlier observations on the structure of spined scales in other species of Chaetonotida, suborder Paucitubulatina. The utility of cuticle ultrastructure is discussed in reference to the search for characters defining higher-level taxa, in the Paucitubulatina. A new species, P. andreae, also cohabits the Queensland lake and is distinguished by the following combination of characters: wide mouth ring; pharynx with terminal bulb; simple spineless scales on the dorsal, lateral, and ventrolateral body surfaces; and a column of ventral interciliary scales in rectangular, ovoid, and intermediate shapes. C1 Smithsonian Marine Stn, Ft Pierce, FL 34949 USA. RP Hochberg, R (reprint author), Smithsonian Marine Stn, Ft Pierce, FL 34949 USA. EM Hochberg_Rick@yahoo.com NR 26 TC 4 Z9 4 U1 0 U2 1 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 1077-8306 J9 INVERTEBR BIOL JI Invertebr. Biol. PY 2005 VL 124 IS 2 BP 119 EP 130 PG 12 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA 942JI UT WOS:000230278300004 ER PT J AU Kuntner, M AF Kuntner, M TI A revision of Herennia (Araneae : Nephilidae : Nephilinae), the Australasian 'coin spiders' SO INVERTEBRATE SYSTEMATICS LA English DT Article ID WEB-BUILDING SPIDERS; ORB-WEAVING SPIDERS; ARANEIDAE; PHYLOGENY; BEHAVIOR; ORBICULARIAE; LIMITS; GENUS AB The nephilid 'coin spiders' (Herennia Thorell) are known for their arboricolous ladder webs, extreme sexual size dimorphism and peculiar sexual biology. This paper revises Herennia taxonomy, systematics, biology and biogeography. The widespread Asian Herennia multipuncta (Doleschall) ( = H. sampitana Karsch, new synonymy; = H. mollis Thorell, new synonymy) is synanthropic and invasive, whereas the other 10 species are narrowly distributed Australasian island endemics: H. agnarssoni, sp. nov. is known from Solomon Islands; H. deelemanae, sp. nov. from northern Borneo; H. etruscilla, sp. nov. from Java; H. gagamba, sp. nov. from the Philippines; H. jernej, sp. nov. from Sumatra; H. milleri, sp. nov. from New Britain; H. oz, sp. nov. from Australia; H. papuana Thorell from New Guinea; H. sonja, sp. nov. from Kalimantan and Sulawesi; and H. tone, sp. nov. from the Philippines. A phylogenetic analysis of seven species of Herennia, six nephilid species and 15 outgroup taxa scored for 190 morphological and behavioural characters resulted in 10 equally parsimonious trees supporting the monophyly of Nephilidae, Herennia, Nephila, Nephilengys and Clitaetra, but the sister-clade to the nephilids is ambiguous. Coin spiders do not fit well established biogeographic lines (Wallace, Huxley) dividing Asian and Australian biotas, but the newly drawn 'Herennia line' suggests an all-Australasian speciation in Herennia. To explain the peculiar male sexual behaviour (palpal mutilation and severance) known in Herennia and Nephilengys, three specific hypotheses based on morphological and behavioural data are proposed: (1) broken embolic conductors function as mating plugs; (2) bulb severance following mutilation is advantageous for the male to avoid hemolymph leakage; and (3) the eunuch protects his parental investment by fighting off rival males. C1 Slovenian Acad Sci & Arts, Inst Biol, Ctr Sci Res, SI-1001 Ljubljana, Slovenia. George Washington Univ, Dept Biol Sci, Washington, DC 20052 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20013 USA. 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 NR 58 TC 55 Z9 62 U1 1 U2 8 PU CSIRO PUBLISHING PI CLAYTON PA UNIPARK, BLDG 1, LEVEL 1, 195 WELLINGTON RD, LOCKED BAG 10, CLAYTON, VIC 3168, AUSTRALIA SN 1445-5226 EI 1447-2600 J9 INVERTEBR SYST JI Invertebr. Syst. PY 2005 VL 19 IS 5 BP 391 EP 436 DI 10.1071/IS05024 PG 46 WC Evolutionary Biology; Zoology SC Evolutionary Biology; Zoology GA 991PL UT WOS:000233825800003 ER PT J AU Zibrov, AS Novikova, I AF Zibrov, AS Novikova, I TI Observation of quantum noise in the polarization of laser light in a rubidium-vapor cell SO JETP LETTERS LA English DT Article ID SPECTROSCOPY; MEDIA AB Experimental observation of quantum noise in the polarization of laser light that has passed through a dense Rb-87 atomic vapor is reported. The step-like noise spectrum is observed. Factors responsible for the form of the observed spectrum and the absence of noise "squeezing" predicted by Matsko et al. [Phys. Rev. A 63, 043814 (2001)] are discussed. (C) 2005 Pleiades Publishing, Inc. C1 Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. Russian Acad Sci, PN Lebedev Phys Inst, Moscow 117924, Russia. RP Zibrov, AS (reprint author), Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. EM inovikova@cfa.harvard.edu RI Novikova, Irina/B-9041-2008; Zibrov, Alexander/G-7419-2014 NR 28 TC 5 Z9 5 U1 0 U2 2 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0021-3640 J9 JETP LETT+ JI Jetp Lett. PY 2005 VL 82 IS 3 BP 110 EP 114 DI 10.1134/1.2086125 PG 5 WC Physics, Multidisciplinary SC Physics GA 970CS UT WOS:000232283400003 ER PT J AU Zibrov, SA Velichansky, VL Zibrov, AS Taichenachev, AV Yudin, VI AF Zibrov, SA Velichansky, VL Zibrov, AS Taichenachev, AV Yudin, VI TI Experimental investigation of the dark pseudoresonance on the D1 line of the Rb-87 atom excited by a linearly polarized field SO JETP LETTERS LA English DT Article ID RESONANCES; CONTRAST AB The measurements of the metrological characteristics (amplitude, width, and shift in the magnetic field) of the dark pseudoresonance, which was proposed by Kazakov et al. [quant-ph/0506167] as the reference resonance for an atomic frequency standard, are reported. It has been shown that the characteristics of the pseudoresonance are worse than those of the unsplit electromagnetically induced transparency resonance for the excitation scheme with the lin parallel to lin polarization on the D1 line of the Rb-87 atom. (C) 2005 Pleiades Publishing, Inc. C1 Russian Acad Sci, PN Lebedev Phys Inst, Moscow 117924, Russia. State Univ, Moscow Phys Engn Inst, Moscow 115409, Russia. Russian Acad Sci, Inst Laser Phys, Siberian Div, Novosibirsk 630090, Russia. Novosibirsk State Univ, Novosibirsk 630090, Russia. Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Zibrov, SA (reprint author), Russian Acad Sci, PN Lebedev Phys Inst, Leninskii Pr 53, Moscow 117924, Russia. EM szibrov@yandex.ru RI Taichenachev, Aleksei/K-7065-2015; Velichansky, Vladimir/M-4861-2015; Zibrov, Sergei/M-6400-2015; Zibrov, Alexander/G-7419-2014 OI Taichenachev, Aleksei/0000-0003-2273-0066; NR 18 TC 17 Z9 18 U1 2 U2 3 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0021-3640 J9 JETP LETT+ JI Jetp Lett. PY 2005 VL 82 IS 8 BP 477 EP 481 DI 10.1134/1.2150865 PG 5 WC Physics, Multidisciplinary SC Physics GA 996JX UT WOS:000234171300004 ER PT J AU Miller, JA AF Miller, JA TI A redescription of Porrhomma cavernicola Keyserling (Araneae, Linyphiidae) with notes on Appalachian troglobites SO JOURNAL OF ARACHNOLOGY LA English DT Article DE dispersal; phylogeny; stridulatory organ; Nesticus; Nesticidae ID SPIDERS ARANEAE; ERIGONINE SPIDERS; CAVE SPIDERS; NESTICIDAE; CLADE AB The Appalachian troglobite Porrhomma cavernicola (Keyserling 1886) is redescribed. Porrhomma emertoni Roewer 1942 is a junior synonym (new synonymy). An unusual stridulatory organ with the plectrum on trochanter Pi and the striac on coxa I is found in both sexes of this species. Porrhomina catertnicola is widespread in Appalachian eaves. By contrast, Appalachian Nesticus (Nesticidae) troglobites tend to be highly endemic. This despite the fact that both groups of spiders are web-builders that may be found in the same caves. Porrhomma cavernicola is added to a previous phylogenetic analysis of linyphiid spiders. Implications of this analysis for the phylogenetic structure of linyphiid spiders is discussed. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20013 USA. RP Miller, JA (reprint author), Calif Acad Sci, Dept Entomol, 875 Howart St, San Francisco, CA 94103 USA. EM jmiller@Calacademy.org NR 64 TC 7 Z9 7 U1 0 U2 0 PU AMER ARACHNOLOGICAL SOC PI NEW YORK PA C/O NORMAN I PLATNICK, AMER MUSEUM NATURAL HISTORY, CENTRAL PK WEST AT 79TH ST, NEW YORK, NY 10024 USA SN 0161-8202 J9 J ARACHNOL JI J. Arachnol. PY 2005 VL 33 IS 2 BP 426 EP 438 DI 10.1636/04-51.1 PG 13 WC Entomology SC Entomology GA 994EK UT WOS:000234013200025 ER PT J AU Miller, J Agnarsson, I AF Miller, J Agnarsson, I TI A redescription of Chrysso nigriceps (Araneae, Theridiidae) with evidence for maternal care SO JOURNAL OF ARACHNOLOGY LA English DT Article DE Chrysso; evolution of sociality; maternal care; taxonomy; South America ID SPIDERS ARANEAE AB Chrysso nigriceps is redescribed and the male is described for the first time based on material from Colombia. Evidence for maternal care of juveniles in Chrysso is presented. This evidence is consistent with predictions based on phylogenetic analysis that maternal care is primitively present in the lost colulus clade, the lineage containing all social theridiids. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20013 USA. George Washington Univ, Dept Biol Sci, Washington, DC 20052 USA. RP Miller, J (reprint author), Calif Acad Sci, Dept Entomol, 875 Howard St, San Francisco, CA 94103 USA. EM jmiller@Calacademy.org NR 12 TC 7 Z9 8 U1 0 U2 12 PU AMER ARACHNOLOGICAL SOC PI NEW YORK PA C/O NORMAN I PLATNICK, AMER MUSEUM NATURAL HISTORY, CENTRAL PK WEST AT 79TH ST, NEW YORK, NY 10024 USA SN 0161-8202 J9 J ARACHNOL JI J. Arachnol. PY 2005 VL 33 IS 3 BP 711 EP 714 DI 10.1636/H04-10.1 PG 4 WC Entomology SC Entomology GA 000WL UT WOS:000234493000006 ER PT J AU Cavigellil, SA Monfort, SL Whitney, TK Mechref, YS Novotny, M McClintock, MK AF Cavigellil, SA Monfort, SL Whitney, TK Mechref, YS Novotny, M McClintock, MK TI Frequent serial fecal corticoid measures from rats reflect circadian and ovarian corticosterone rhythms SO JOURNAL OF ENDOCRINOLOGY LA English DT Article ID AFRICAN WILD DOGS; FEMALE RATS; PLASMA-CORTICOSTERONE; ADRENAL ACTIVITY; INDIVIDUAL-DIFFERENCES; NONINVASIVE METHOD; SPOTTED HYENAS; CORTISOL; EXCRETION; METABOLITES AB The circadian glucocorticoid rhythm provides important information on the functioning of the hypothalamic-pituitary-adrenal axis in individuals. Frequent repeated blood sampling can limit the kinds of studies conducted on this rhythm, particularly in small laboratory rodents that have limited blood volumes and are easily stressed by handling. We developed an extraction and assay protocol to measure fecal corticosterone metabolites in repeated samples collected from undisturbed male and female adult Sprague-Dawley rats. This fecal measure provides a non-invasive method to assess changes in corticosterone within a single animal over time, with sufficient temporal acuity to quantify several characteristics of the circadian rhythm: e.g. the nadir, acrophase, and asymmetry (saw-tooth) of the rhythm. Males excreted more immunoreactive fecal corticoids than did females. Across the estrous cycle, females produced more fecal corticoids on proestrus (the day of the preovulatory luteinizing hormone surge) than during estrus or metestrus. These results establish a baseline from which to study environmental, psychological, and physiological disturbances of the circadian corticosterone rhythm within individual rats. C1 Penn State Univ, Dept Biobehav Hlth, State Coll, PA 16802 USA. Smithsonian Inst, Natl Zoo, Conservat & Res Ctr, Front Royal, VA 22630 USA. Univ Wisconsin, Dept Psychol, Madison, WI 53706 USA. Indiana Univ, Dept Chem, Bloomington, IN 47405 USA. Univ Chicago, Dept Psychol, Chicago, IL 60637 USA. Univ Chicago, Inst Mind & Biol, Chicago, IL 60637 USA. RP Cavigellil, SA (reprint author), Penn State Univ, Dept Biobehav Hlth, State Coll, PA 16802 USA. EM s-cavigclli@psu.edu OI Mechref, Yehia/0000-0002-6661-6073 FU NIA NIH HHS [P01 AG018911]; NICHD NIH HHS [F32 HD08693]; NIMH NIH HHS [R37 MH41788] NR 44 TC 75 Z9 80 U1 1 U2 6 PU SOC ENDOCRINOLOGY PI BRISTOL PA 22 APEX COURT, WOODLANDS, BRADLEY STOKE, BRISTOL BS32 4JT, ENGLAND SN 0022-0795 J9 J ENDOCRINOL JI J. Endocrinol. PD JAN PY 2005 VL 184 IS 1 BP 153 EP 163 DI 10.1677/joe.1.05935 PG 11 WC Endocrinology & Metabolism SC Endocrinology & Metabolism GA 890LY UT WOS:000226513900016 PM 15642792 ER PT J AU Seddeek, MK Sharshar, T Ragab, HS Badran, HM AF Seddeek, MK Sharshar, T Ragab, HS Badran, HM TI Radioactivities related to coal mining SO JOURNAL OF ENVIRONMENTAL MONITORING LA English DT Article ID NATURAL RADIOACTIVITY; BUILDING-MATERIALS; RADON CONCENTRATIONS; POWER-PLANTS; BY-PRODUCTS; MINES; RADIONUCLIDES; CALIBRATION; PAKISTAN AB Natural radioactivity concentrations due to the coal mining in Gabal El-Maghara, North Sinai, Egypt, were determined using gamma-ray spectroscopy. Coal, water and soil samples were investigated in this study. The Ra-226, Th-232 and K-40 activity concentrations in coal before extraction were 18.5 +/- 0.5, 29.5 +/- 1.2 and 149.0 +/- 8.4 Bq kg(-1), respectively. These concentrations were reduced to 18-22% after extraction due to the clay removal of the coal ore. The activity contents of the water and soil samples collected from the surrounding area did not show any evidence of enhancement due to the mining activities. Absorbed dose rate and effective dose equivalent in the mine environment were 29.4 nGy h(-1) and 128.0 mu Sv a(-1), respectively. The measured activity concentrations in the mine environment and the surrounding areas (5 km away from the mine) are similar to that found in other regions in North and South Sinai. Based on the measurements of gamma-ray emitting radionuclides, the mine activity does not lead to any enhancement in the local area nor represents any human risk. C1 Tanta Univ, Fac Sci, Dept Phys, Tanta 31527, Egypt. Suez Canal Univ, Fac Educ, Dept Phys, Al Arish, Egypt. Tanta Univ, Fac Educ, Dept Chem & Phys, Kafr El Shaikh, Egypt. Harvard Smithsonian Ctr Astrophys, Whipple Observ, Amado, AZ 85645 USA. RP Badran, HM (reprint author), Tanta Univ, Fac Sci, Dept Phys, Tanta 31527, Egypt. EM badran@egret.sao.arizona.edu NR 25 TC 6 Z9 6 U1 0 U2 6 PU ROYAL SOC CHEMISTRY PI CAMBRIDGE PA THOMAS GRAHAM HOUSE, SCIENCE PARK, MILTON RD, CAMBRIDGE CB4 0WF, CAMBS, ENGLAND SN 1464-0325 J9 J ENVIRON MONITOR JI J. Environ. Monit. PY 2005 VL 7 IS 8 BP 767 EP 770 DI 10.1039/b502133b PG 4 WC Chemistry, Analytical; Environmental Sciences SC Chemistry; Environmental Sciences & Ecology GA 955SA UT WOS:000231246700004 PM 16049576 ER PT J AU Seddeek, MK Badran, HM Sharshar, T Elnimr, T AF Seddeek, MK Badran, HM Sharshar, T Elnimr, T TI Characteristics, spatial distribution and vertical profile of gamma-ray emitting radionuclides in the coastal environment of North Sinai SO JOURNAL OF ENVIRONMENTAL RADIOACTIVITY LA English DT Article DE black sand; profile distribution; Sinai; Egypt; Cs-137; Ra-226; Th-232; K-40 ID RADON EXHALATION RATES; BUILDING-MATERIALS; NATURAL RADIOACTIVITY; BEACH SAND; EGYPTIAN MONAZITE; HEAVY MINERALS; BY-PRODUCTS; DOSE-RATES; NILE DELTA; HONG-KONG AB Radionuclide concentrations of beach and dune sand from various sites in Al-Arish city and surrounding area, North Sinai, Egypt, were measured. The sampling sites included locations in the local harbor, Al-Arish valley and Zaranik protected area. The results indicate that the activities of the products of Th-232 and Ra-226 series in samples from the harbor and along the beach were higher than those from non-coastal sites. The activity concentrations of Th-232 for beach sand ranged from 2.3 to 506.5 Bq/kg with an average of 83.4 Bq/kg, while that for dune sand ranged from 2.2 to 15.1 Bq/kg with an average of 6.4 Bq/kg. The average activity concentration of Ra-226 for beach sand was 56.0 Bq/kg (2.9-261.5 Bq/kg), while that for dune sand was 6.5 Bq/kg (3.0-14.7 Bq/kg). The average activity concentrations of K-40 for beach and dune sand were 88.1 Bq/kg and 178.4 Bq/kg, respectively. Six depth profiles in the harbor area were measured up to a depth of 1 m within more than two years. These sets of measurements allowed the determination of the migration rate of black sand to be 0.094 cm/day. Samples with the smallest grain size (< 0.2 mm) were found to have the highest level of activities, which were attributed to their high content of black sand. No risk exists for public health based on the calculated effective dose equivalent and the recommended limit of 5 mSv/y. On the other hand, local children and adults may receive doses higher than this recommended limit in two locations in the Zaranik protected area according to a model developed in this study. (c) 2005 Elsevier Ltd. All rights reserved. C1 Suez Canal Univ, Fac Educ, Dept Phys, Al Arish, Egypt. Tanta Univ, Fac Sci, Dept Phys, Tanta 31527, Egypt. Harvard Smithsonian Ctr Astrophys, Whipple Observat, Amado, AZ 85645 USA. Tanta Univ, Fac Educ, Dept Phys & Chem, El Shaikh, Egypt. RP Badran, HM (reprint author), Suez Canal Univ, Fac Educ, Dept Phys, Al Arish, Egypt. EM badran@egret.sao.arizona.edu RI huang, hongqi/N-1473-2014 NR 65 TC 41 Z9 41 U1 2 U2 10 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0265-931X J9 J ENVIRON RADIOACTIV JI J. Environ. Radioact. PY 2005 VL 84 IS 1 BP 21 EP 50 DI 10.1016/j.jenvrad.2005.03.005 PG 30 WC Environmental Sciences SC Environmental Sciences & Ecology GA 968ON UT WOS:000232171900002 PM 15923069 ER PT J AU Jett, JA AF Jett, JA TI Recent literature on Foraminifera SO JOURNAL OF FORAMINIFERAL RESEARCH LA English DT Bibliography C1 Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA. RP Jett, JA (reprint author), Smithsonian Inst, Dept Paleobiol, MRC-121, Washington, DC 20560 USA. NR 0 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 JAN PY 2005 VL 35 IS 1 BP 84 EP 85 DI 10.2113/35.1.84 PG 2 WC Paleontology SC Paleontology GA 897GC UT WOS:000226991000008 ER PT J AU Langley, HD AF Langley, HD TI Union Jacks: Yankee sailors in the Civil War. SO JOURNAL OF MILITARY HISTORY LA English DT Book Review C1 Smithsonian Inst, Washington, DC 20560 USA. RP Langley, HD (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU SOC MILITARY HISTORY PI LEXINGTON PA C/O VIRGINIA MILITARY INST, GEORGE C MARSHALL LIBRARY, LEXINGTON, VA 24450-1600 USA SN 0899-3718 J9 J MILITARY HIST JI J. Mil. Hist. PD JAN PY 2005 VL 69 IS 1 BP 239 EP 239 DI 10.1353/jmh.2005.0030 PG 1 WC History SC History GA 883IO UT WOS:000226005000028 ER PT J AU Markhaseva, EL Ferrari, FD AF Markhaseva, EL Ferrari, FD TI New species of Lucicutia and taxonomic status of L-grandis (Copepoda, Calanoida, Lucicutiidae) SO JOURNAL OF NATURAL HISTORY LA English DT Article DE Calanoida; distribution; Lucicutia; new species; taxonomy ID OXYGEN MINIMUM ZONE; ARABIAN-SEA; LOWER INTERFACE; ECOLOGY AB Calanoid copepod specimens attributable to Lucicutia grandis (Giesbrecht, 1895), L. bradyana Cleve, 1904, L. wolfendeni Sewell, 1932, and L. rara Hulsemann, 1966 were studied from antarctic and subantarctic waters collected during RV Eltanin crusies 4-11 and 23, and RV Ob cruises 1 and 3. In addition, identified specimens from the Pacific and Indian Oceans deposited in the systematic collections of the National Museum of Natural History, Smithsonian Institution (Washington, DC, USA) and the Zoological Institute, Russian Academy of Sciences (St Petersburg) were also examined. Both sexes of a new species are described from the eastern tropical Pacific Ocean, L. hulsemannae. Lucicutia hulsemannae is distinguished from L. grandis, L. bradyana and L. wolfendeni by the morphology of the rostrum, genital complex, including plug, and leg 5 of both sexes. Lucicutia bradyana is not found outside the Southern Hemisphere but L. grandis is recorded from the Arabian Sea, the Bay of Bengal, tropical Indian Ocean, as well as its type locality in the eastern tropical Pacific Ocean. Lucicutia wolfendeni is found in all oceans except the Arctic Ocean. The status of L. bradyana, previously rejected as a separate species by Hulsemarm (1966), is restored. Lucitutia rara is considered a junior synonym of L. bradyana. C1 Russian Acad Sci, Inst Zool, St Petersburg 199034, Russia. Smithsonian Inst, Museum Hist Nat, Dept Sysemat Biol, Washington, DC 20560 USA. RP Markhaseva, EL (reprint author), Russian Acad Sci, Inst Zool, Universitetskaya Nab 1, St Petersburg 199034, Russia. EM copepoda@zin.ru NR 26 TC 1 Z9 2 U1 1 U2 1 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 0022-2933 J9 J NAT HIST JI J. Nat. Hist. PY 2005 VL 39 IS 15 BP 1077 EP 1100 DI 10.1080/00222930400005740 PG 24 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 897CY UT WOS:000226982800001 ER PT J AU Schotte, M Brian, K AF Schotte, M Brian, K TI New species and records of flabellifera from the Indian ocean (Crustacea : Peracarida : Isopoda) SO JOURNAL OF NATURAL HISTORY LA English DT Article DE Crustacea; Flabellifera; Indian ocean; Isopoda; Peracarida ID SPHAEROMATID ISOPOD; FAMILY CIROLANIDAE; CORAL-REEFS; SEA ISOPODA; GENUS; SYSTEMATICS; AUSTRALIA; ECOLOGY; GENERA; KENYA AB In this study of flabelliferan Isopoda from the Indian Ocean, 19 species are described as new, in 11 genera and two families: family Cirolanidae, Baharitana koloura, B. lira, Cirolana aldabrensis, C. mimulus, C. somalia, C. undata, Eurydice paxilli, and Metacirolana chemola; family Sphaeromatidae, Cassidinidea clarkae, Cymodoce fuscina, C. lirella, Dynamenella alveolata, D. remex, Heterodina (new genus), H. mccaini, Oxinasphaera brucei, O. furcata, O. tetrodon, Paracilicaea stauros, and Sphaeromopsis sulcifera. Diagnoses of the genera and species are provided, and keys to the Indian Ocean species of most of the genera are provided. The material comes primarily from Aldabra Atoll, the granitic Seychelles islands, Zanzibar Island, and Phuket in Thailand. A few miscellaneous samples from the South African Museum collections, and from the International Indian Ocean Expedition carried out in the mid-1960s are included. C1 Smithsonian Inst, Dept Zool, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Schotte, M (reprint author), Smithsonian Inst, Dept Zool, Natl Museum Nat Hist, Washington, DC 20013 USA. EM schotte.marilyn@nmnh.si.edu NR 78 TC 15 Z9 17 U1 0 U2 3 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 0022-2933 J9 J NAT HIST JI J. Nat. Hist. PY 2005 VL 39 IS 16 BP 1211 EP 1282 DI 10.1080/0022293040005757 PG 72 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 899XT UT WOS:000227179800002 ER PT J AU Fernandez-Marin, H Zimmerman, JK Wcislo, WT Rehner, SA AF Fernandez-Marin, H Zimmerman, JK Wcislo, WT Rehner, SA TI Colony foundation, nest architecture and demography of a basal fungus-growing ant, Mycocepurus smithii (Hymenoptera, Formicidae) SO JOURNAL OF NATURAL HISTORY LA English DT Article DE Attini; fungiculture; haplometrosis; hygiene; polygyny ID ATTINI; BIOLOGY; ORIGIN AB The genus Mycocepurus is a phylogenetically basal attine ant, so studies of its biology may provide insight into the evolution of behaviours associated with fungus-growing that characterize the tribe Attini. Mycocepurus smithii from Puerto Rico produces sexual females from July to September, but no males were observed in 2 years of observations, confirming previous observations elsewhere. Colonies were founded between July and August and most nests were haplometrotic (85% of 74 nests). After excavating a tunnel and small chamber, a foundress queen inserted her fore wings into the ceiling and used the wing surfaces as a platform on which the incipient fungal garden was grown. Foundresses foraged for substrate to grow the fungus garden. Growth of incipient colonies was slow: the first workers emerged 2-5 months after colony founding and, after 8 months, colonies contained on average only a single worker. C1 Univ Puerto Rico, Dept Biol, San Juan, PR USA. Inst Trop Ecosyst Studies, San Juan, PR USA. Smithsonian Trop Res Inst, Ancon, Panama. RP Wcislo, WT (reprint author), Smithsonian Trop Res Inst, Unit 0948, APO AA, Miami, FL 34002 USA. EM WcisloW@tivoli.si.edu NR 26 TC 30 Z9 31 U1 1 U2 13 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 0022-2933 J9 J NAT HIST JI J. Nat. Hist. PY 2005 VL 39 IS 20 BP 1735 EP 1743 DI 10.1080/00222930400027462 PG 9 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 920CG UT WOS:000228665900004 ER PT J AU Jenkins, PD Carleton, MD AF Jenkins, PD Carleton, MD TI Charles Immanuel Forsyth Major's expedition to Madagascar, 1894 to 1896: beginnings of modern systematic study of the island's mammalian fauna SO JOURNAL OF NATURAL HISTORY LA English DT Article DE History of collection; Madagascar; mammals; specimen localities; type specimens AB Charles Immanuel Forsyth Major (1843-1923) made the first synoptic systematic collection of mammals from Madagascar in the last decade of the 19th century. To reconstruct Major's obscurely known itinerary, we located 994 specimens that originated from his 1894-1896 expedition and determined their identification, dates and locality of collection, and current institutional repository. Fifty species were recovered from 26 localities centred in the Central Highlands and Eastern Humid Forest of east-central Madagascar. The geographic position of several type localities is refined and their coordinates estimated, and the type locality of one taxon (Microgale pusilla Major, 1896) is accordingly amended. Biographical details of the man, the biodiversity significance of his collections and the historical context of his discoveries are discussed. C1 Nat Hist Museum, Dept Zool, London SW7 5BD, England. Natl Museum Nat Hist, Smithsonian Inst, Dept Zool, Washington, DC USA. RP Jenkins, PD (reprint author), Nat Hist Museum, Dept Zool, Cromwell Rd, London SW7 5BD, England. EM pdj@nhm.ac.uk NR 73 TC 13 Z9 14 U1 0 U2 3 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 0022-2933 J9 J NAT HIST JI J. Nat. Hist. PY 2005 VL 39 IS 20 BP 1779 EP 1818 DI 10.1080/00222930400023719 PG 40 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 920CG UT WOS:000228665900007 ER PT J AU Litulo, C Tudge, C AF Litulo, C Tudge, C TI Population structure and breeding season of the hermit crab Diogenes brevirostris Stimpson, 1858 (Decapoda, Anomura, Diogenidae) from southern Mozambique SO JOURNAL OF NATURAL HISTORY LA English DT Article DE Diogenes brevirostris; hermit crabs; population structure; reproduction ID SHELL UTILIZATION; LIFE-HISTORY; QUIRIMBA ISLAND; NITIDIMANUS TERAO; UBATUBA REGION; SAO-PAULO; BRAZIL; ECOLOGY; PATTERNS; BIOLOGY AB In this study the population dynamics of the diogenid hermit crab Diogenes brevirostris is evaluated focusing on size structure, sex ratio and breeding season. Crabs were randomly taken on a monthly basis from January to December 2003 at Costa do Sol, Maputo Bay, southern Mozambique. A total of 622 crabs was obtained of which 290 were males (46.6%), 170 were non-ovigerous females (27.3%) and 162 were ovigerous females (26.1%). The overall size frequency distribution was unimodal for males, non-ovigerous females and ovigerous females. The overall sex ratio (1:1.15) differed from the expected 1: 1 ratio. Sexual dimorphism was evidenced by the larger size attained by males in relation to both ovigerous and non-ovigerous females. Breeding took place year-round with three peaks of spawning (March, August and December). Despite the high reproductive activity, young recruits were scarce in the population. The present results suggest that the study area is suitable for reproduction and growth whereas recruitment may take place in different areas from that occupied by the adults. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20013 USA. Amer Univ, Dept Biol, Washington, DC 20016 USA. Univ Eduardo Mondlane, Fac Ciencias, Dept Ciencias Biol, Maputo, Mozambique. RP Tudge, C (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20013 USA. EM tudgec@si.edu NR 57 TC 2 Z9 2 U1 0 U2 2 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 0022-2933 J9 J NAT HIST JI J. Nat. Hist. PY 2005 VL 39 IS 31 BP 2887 EP 2899 DI 10.1080/00222930500206107 PG 13 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 970AA UT WOS:000232276400002 ER PT J AU Percy, DM Day, MF AF Percy, DM Day, MF TI Observations of unusual acoustic behaviour in two Australian leafhoppers (Hemiptera; Cicadellidae) SO JOURNAL OF NATURAL HISTORY LA English DT Article DE acoustic communication; female interaction; leafhopper; substrate transmission ID TREEHOPPER HEMIPTERA; CALLING SIGNALS; COMMUNICATION; PLANTHOPPER; HOMOPTERA; VARIABILITY; DELPHACIDAE; MEMBRACIDAE AB Acoustic substrate-borne communication between hoppers has been well studied with certain patterns of acoustic behaviour considered typical. We report observations of acoustic behaviour in two Australian leafhoppers, Stenocotis depressa (Walker) and Austrolopa brnnensis Evans, that are markedly atypical. Two types of unusual acoustic behaviour were observed: female-female interactions, and the transmission of an elaborate male call through direct physical contact with the female. We discuss the evolution of these acoustic displays based on our observations of these hoppers and their environments, including the potential roles of intra-sexual competition and the carrying capacity of the plant substrate. The discovery of these unusual behaviour patterns emphasizes the need for broader surveys of the diversity of acoustic behaviour in the Hemiptera. C1 CSIRO Entomol, Canberra, ACT, Australia. RP Percy, DM (reprint author), Smithsonian Inst, Natl Zool Pk, 3001 Connecticut Ave NW, Washington, DC 20008 USA. EM percyd@si.edu NR 20 TC 3 Z9 3 U1 1 U2 3 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 0022-2933 J9 J NAT HIST JI J. Nat. Hist. PY 2005 VL 39 IS 38 BP 3407 EP 3417 DI 10.1080/00222930500393087 PG 11 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 001NJ UT WOS:000234543300003 ER PT J AU Renner, SC AF Renner, SC TI The Resplendent Quetzal (Pharomachrus mocinno) in the Sierra Yalijux, Alta Verapaz, Guatemala SO JOURNAL OF ORNITHOLOGY LA English DT Article DE conservation; Guatemala; Pharomachrus mocinno; Resplendent Quetzal; tropical montane cloud forest ID FOREST AB The Resplendent Quetzal Pharomachrus mocinno is a restricted-range species occurring from Chiapas ( Mexico) to Panama, generally at elevations above 1,400 m. P. mocinno is a frugivore that feeds on a variety of fruits. Listed as "Lower Risk/Near Threatened Species'' and in CITES Appendix I, P. mocinno is dependent on standing dead and mature trees for breeding holes, which are only formed in primary cloud forest, even if tree stumps occur temporally in secondary growth as remnants of primary cloud forest. A population of P. mocinno in the northernmost Guatemalan mountain range (Chelemha Plot, Sierra Yalijux, Alta Verapaz) was studied in 2002 and compared with a census at the same location in 1988. Between 1988 and 2002, the number of males did not change significantly: a small increase took place from 15 to 18 individuals per 100 ha. The species' breeding behaviour is linked to the long-term existence of primary forests such as the few remaining in highland Guatemala. Breeding success was proven and at least three juveniles from two breeding pairs were observed until the end of September 2002. C1 Smithsonian Inst, Conservat & Res Ctr, Front Royal, VA 22630 USA. RP Renner, SC (reprint author), Smithsonian Inst, Conservat & Res Ctr, 1500 Remount Rd, Front Royal, VA 22630 USA. EM renners@crc.si.edu RI Renner, Swen/J-3502-2014 OI Renner, Swen/0000-0002-6893-4219 NR 29 TC 5 Z9 6 U1 17 U2 42 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013 USA SN 1439-0361 J9 J ORNITHOL JI J. Ornithol. PD JAN PY 2005 VL 146 IS 1 BP 79 EP 84 DI 10.1007/s10336-004-0060-7 PG 6 WC Ornithology SC Zoology GA 889TG UT WOS:000226464900010 ER PT J AU Niro, F von Clarmann, T Jucks, K Hartmann, JM AF Niro, F von Clarmann, T Jucks, K Hartmann, JM TI Spectra bands calculations in central and wing regions of CO2IR between 10 and 20 mu m. III: atmospheric emission spectra SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE CO2; infrared; absorption; shape; model; atmospheric; emission ID INFRARED Q BRANCHES; MODEL; MIPAS; COMPUTATION; ISOTOPOMERS; SOFTWARE; DATABASE; SPACE; BASE AB A theoretical model for the prediction of CO2 absorption in both central and wing regions of infrared absorption bands was presented in the companion paper I. It correctly accounts for line-mixing effects and was validated by comparisons with laboratory spectra in the 600-1000 cm(-1) region. This quality was confirmed using atmospheric transmissions measured by solar occultation experiments in the second paper. The present work completes these studies by now considering atmospheric emission in the 10-20 mum range. Comparisons are made between computed atmospheric radiances and measurements obtained using four different Fourier transform experiments collecting spectra for nadir, up-looking, as well as limb (from balloon and satellite) geometries. Our results confirm that using a Voigt model can lead to very large errors that affect the spectrum more than 300 cm(-1) away from the center of the CO2 nu(2) band. They also demonstrate the capability of our model to represent accurately the radiances in the entire region for a variety of atmospheric paths. This success opens interesting perspectives for the sounding of pressure and temperature profiles, particularly at low altitudes. Another benefit of the quality of the model should be an increased accuracy in the retrieval of atmospheric state parameters from broad features in the measured spectra (clouds, aerosols, heavy trace gases). (C) 2004 Elsevier Ltd. All rights reserved. C1 CNRS, UPR 3361, Photophys Mol Lab, F-91405 Orsay, France. Univ Paris 11, F-91405 Orsay, France. Forschungszentrum Karlsruhe, Inst Meteorol & Climate Res, IMK, D-76021 Karlsruhe, Germany. Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Hartmann, JM (reprint author), CNRS, UPR 3361, Photophys Mol Lab, Bat 350, F-91405 Orsay, France. EM jean-michel.hartmann@ppm.u-psud.fr RI von Clarmann, Thomas/A-7287-2013 OI von Clarmann, Thomas/0000-0003-2219-3379 NR 17 TC 25 Z9 26 U1 0 U2 2 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD JAN 1 PY 2005 VL 90 IS 1 BP 61 EP 76 DI 10.1016/j.jqsrt.2004.04.005 PG 16 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 856HQ UT WOS:000224036700004 ER PT J AU Cochran, JB Bonnell, R AF Cochran, JB Bonnell, R TI Patterns of sustainable agriculture adoption/non-adoption in Panama SO JOURNAL OF SUSTAINABLE AGRICULTURE LA English DT Article DE sustainable agriculture; slash and burn agriculture; agroforestry; promoters; adoption; non-adoption; Panama ID AGROFORESTRY AB The promoter model for implementing Sustainable agriculture has been successfully applied ill numerous Countries across the developing world. In Panama it is being used by several development agencies to train local farmers in the manner Of Sustainable agriculture. In this paper the effectiveness of the promoter model was assessed. Starting with the trained promoter, the number Of Sustainable farmers who were influenced by the promoter was determined. The number of first generation adopters was low compared to rates typically presented in the literature. Reasons for these low rates are discussed. Non-adopters were interviewed to determine reasons for non-adoption of sustainable agriculture and why use of slash and burn continues. These reasons for adoption or non-adoption are discussed. C1 McGill Univ, Dept Bioresource Engn, Brace Ctr Water Resources Management, Ste Anne De Bellevue, PQ H9X 3V9, Canada. Smithsonian Inst, Washington, DC 20560 USA. Peace Corps, Sustainable Agr Syst Program, Paitilla, Panama. RP Cochran, JB (reprint author), McGill Univ, Dept Bioresource Engn, Brace Ctr Water Resources Management, Eng 21,111 Lakeshore Rd,Macdonald Campus, Ste Anne De Bellevue, PQ H9X 3V9, Canada. EM cochranjason2000@hotmail.com NR 20 TC 1 Z9 1 U1 1 U2 7 PU HAWORTH PRESS INC PI BINGHAMTON PA 10 ALICE ST, BINGHAMTON, NY 13904-1580 USA SN 1044-0046 J9 J SUSTAIN AGR JI J. Sustain. Agric. PY 2005 VL 27 IS 3 BP 147 EP 162 DI 10.1300/J064v27n03_10 PG 16 WC Agriculture, Multidisciplinary SC Agriculture GA 025KV UT WOS:000236265800009 ER PT J AU Kurtz, MJ Eichhorn, G Accomazzi, A Grant, C Demleitner, M Murray, SS AF Kurtz, MJ Eichhorn, G Accomazzi, A Grant, C Demleitner, M Murray, SS TI Worldwide use and impact of the NASA astrophysics data system digital library SO JOURNAL OF THE AMERICAN SOCIETY FOR INFORMATION SCIENCE AND TECHNOLOGY LA English DT Article ID ASTRONOMY; RETRIEVAL; NATIONS; URANIA AB The NASA Astrophysics Data System (ADS), along with astronomy's journals and data centers (a collaboration dubbed URANIA), has developed a distributed online digital library which has become the dominant means by which astronomers search, access, and read their technical literature. Digital libraries permit the easy accumulation of a new type of bibliometric measure: the number of electronic accesses ("reads") of individual articles. By combining data from the text, citation, and reference databases with data from the ADS readership logs we have been able to create second-order bibliometric operators, a customizable class of collaborative filters that permits substantially improved accuracy in literature queries. Using the ADS usage logs along with membership statistics from the International Astronomical Union and data on the population and gross domestic product (GDP), we have developed an accurate model for worldwide basic research where the number of scientists in a country is proportional to the GDP of that country, and the amount of basic research done by a country is proportional to the number of scientists in that country times that country's per capita GDP. We introduce the concept of utility time to measure the impact of the ADS/URANIA and the electronic astronomical library on astronomical research. We find that in 2002 it amounted to the equivalent of 736 full-time researchers, or $250 million, or the astronomical research done in France. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Eichhorn, Guenther/C-9480-2009; KURTZ, Michael /B-3890-2009; OI Eichhorn, Guenther/0000-0002-3032-1978; Grant, Carolyn/0000-0003-4424-7366; Kurtz, Michael/0000-0002-6949-0090; Accomazzi, Alberto/0000-0002-4110-3511 NR 37 TC 46 Z9 47 U1 2 U2 10 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1532-2882 EI 1532-2890 J9 J AM SOC INF SCI TEC JI J. Am. Soc. Inf. Sci. Technol. PD JAN 1 PY 2005 VL 56 IS 1 BP 36 EP 45 DI 10.1002/asi.20095 PG 10 WC Computer Science, Information Systems; Information Science & Library Science SC Computer Science; Information Science & Library Science GA 880OO UT WOS:000225799300005 ER PT J AU Novikova, I Matsko, AB Welch, GR AF Novikova, I Matsko, AB Welch, GR TI Influence of a buffer gas on nonlinear magneto-optical polarization rotation SO JOURNAL OF THE OPTICAL SOCIETY OF AMERICA B-OPTICAL PHYSICS LA English DT Article ID ELECTROMAGNETICALLY INDUCED TRANSPARENCY; RAMSEY FRINGES; RELAXATION; SODIUM; COLLISIONS; COHERENCE AB We show experimentally that the presence of a buffer gas in a rubidium vapor cell modifies significantly the nonlinear magneto-optical rotation of polarization of near-resonant light propagating through the cell. We observe not only the well-known narrowing of the nonlinear magneto-optical resonances, but also changes in their shape and visibility. We explain these effects in terms of coherence-preserving, velocity-changing collisions between rubidium and buffer gas atoms. (C) 2005 Optical Society of America. C1 Texas A&M Univ, Dept Phys, College Stn, TX 77843 USA. Texas A&M Univ, Inst Quantum Studies, College Stn, TX 77843 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Novikova, I (reprint author), Texas A&M Univ, Dept Phys, College Stn, TX 77843 USA. RI Matsko, Andrey/A-1272-2007; Novikova, Irina/B-9041-2008 NR 36 TC 19 Z9 19 U1 0 U2 6 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 0740-3224 J9 J OPT SOC AM B JI J. Opt. Soc. Am. B-Opt. Phys. PD JAN PY 2005 VL 22 IS 1 BP 44 EP 56 DI 10.1364/JOSAB.22.000044 PG 13 WC Optics SC Optics GA 886JP UT WOS:000226223600006 ER PT J AU Greenberg, R Bichier, P AF Greenberg, R Bichier, P TI Determinants of tree species preference of birds in oak-acacia woodlands of Central America SO JOURNAL OF TROPICAL ECOLOGY LA English DT Article DE ant-herbivory defences; breeding currency hypothesis; foliage palatability hypothesis; insectivorous birds; migratory birds; tree preference; tropical savannas ID SOUTH-AFRICAN SAVANNA; INSECTIVOROUS BIRDS; HERBIVOROUS INSECTS; BROWSING RUMINANTS; FOOD AVAILABILITY; MIGRATORY BIRDS; FOREST BIRDS; WOODY-PLANTS; HARDWOODS; DEFENSES AB In mid-elevation areas of Mesoamerica, Acacia pennatula commonly occurs in mixed woods with various species of oak. During a 1-y study in Nicaragua, we found the abundance of birds in acacia was far higher than the representation of this species in the mix of trees, whether this is estimated by number of individual trees, canopy cover or foliage cover. This higher abundance was probably related to the fact that acacias supported approximately three to four times the abundance of arthropods that were found in oaks and twice the biomass. Although oak foliage supported fewer arthropods, relatively more of them were large (> 1 cm). The greater preponderance of small arthropods in acacias versus oaks was probably related to the small leaflet size of acacias. However, it is likely that the higher abundance of arthropods in acacias, particularly herbivorous species, was related to the higher nutritional content of the acacia foliage (crude protein, minerals. non-structural carbohydrates) and lower content of digestion-inhibiting compounds (structural carbohydrates, total phenolics, condensed tannins). The major defensive mechanisms of acacia are mechanical (thorns) or qualitative-defence chemicals (cyanogenic glucosides) that are apparently more effective against vertebrate than invertebrate herbivores. These observations support the hypothesis that the anti-herbivore defences of acacia are primarily directed against large mammalian herbivores, rendering the foliage highly palatable to arthropods. C1 Natl Zool Pk, Smithsonian Migratory Bird Ctr, Washington, DC 20008 USA. RP Greenberg, R (reprint author), Natl Zool Pk, Smithsonian Migratory Bird Ctr, Washington, DC 20008 USA. EM antbird@erols.com NR 42 TC 10 Z9 10 U1 0 U2 13 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 40 WEST 20TH ST, NEW YORK, NY 10011-4211 USA SN 0266-4674 J9 J TROP ECOL JI J. Trop. Ecol. PD JAN PY 2005 VL 21 BP 57 EP 66 DI 10.1017/S0266467404001762 PN 1 PG 10 WC Ecology SC Environmental Sciences & Ecology GA 898NL UT WOS:000227083400006 ER PT S AU Castro, JM Dingwell, DB Nichols, ARL Gardner, JE AF Castro, Jonathan M. Dingwell, Donald B. Nichols, Alexander R. L. Gardner, James E. BE Manga, M Ventura, G TI New insights on the origin of flow bands in obsidian SO KINEMATICS AND DYNAMICS OF LAVA FLOWS SE Geological Society of America Special Papers LA English DT Article; Book Chapter DE obsidian; flow banding; welding; deformation ID CRYSTAL-SIZE DISTRIBUTIONS; MOUNT-ST-HELENS; EASTERN CALIFORNIA; SILICATE MELTS; MAGMA ASCENT; ERUPTIONS; RELAXATION; DYNAMICS; GLASSES; WATER AB We examined the textures, volatile contents, and cooling histories of microlite-defined flow bands in several rhyolitic obsidians in order to test whether textural variations between bands could be ascribed to different degassing and cooling histories, and to assess the timing and location of band formation. Flow bands are defined by variations in microlite number density (N(V)) and size. For each mineral phase examined, smaller average crystal sizes characterize the microlite-rich bands in contrast to microlite-poor bands, which contain relatively larger crystals of lower N(V). Magmatic H(2)O concentrations of microlite-rich and microlite-poor bands show no statistical difference between the textures. Calorimetric measurements yield similar glass transition temperatures and cooling rates for adjacent bands. These observations suggest that microlite heterogeneities could not have developed during late stage cooling and degassing during flow emplacement, as such textural variations imply distinct cooling and/or degassing histories. Rather, textural heterogeneities must have formed during flow in the conduit. Hydrothermal annealing experiments were conducted on natural fragmented rhyolite in order to simulate the welding process in silicate melt and to provide first-order estimates of the time scales and deformation required to produce flow bands. Flow bands formed in experiments conducted at H(2)O-vapor pressures of 50 and 100 MPa, and for temperatures ranging from 800 to 850 degrees C. In each case, bands formed as a result of redistribution of oxide-rich domains and grain boundary coatings in annealed glass powders that underwent viscous deformation. Experiments suggest that bands may form on relatively short time scales (similar to 7 d) and for small bulk strains (similar to 1). Band formation may be promoted by high melt-H(2)O concentrations, shear stress, and viscous and frictional heating. C1 [Castro, Jonathan M.] Smithsonian Inst, Dept Mineral Sci, Washington, DC 20013 USA. [Dingwell, Donald B.; Nichols, Alexander R. L.] Univ Munich, Dept Geo & Umweltwissenshaften, D-80333 Munich, Germany. [Gardner, James E.] Univ Texas Austin, Dept Geol Sci, Austin, TX 78712 USA. RP Castro, JM (reprint author), Smithsonian Inst, Dept Mineral Sci, POB 37012,NMNH MRC 119, Washington, DC 20013 USA. EM castro@volcano.si.edu RI Dingwell, Donald/A-4724-2011; OI Dingwell, Donald/0000-0002-3332-789X; Nichols, Alexander/0000-0002-8298-2882 NR 26 TC 7 Z9 7 U1 0 U2 0 PU GEOLOGICAL SOC AMER INC PI BOULDER PA 3300 PENROSE PL, PO BOX 9140, BOULDER, CO 80301 USA SN 0072-1077 BN 978-0-8137-2396-9 J9 GEOL SOC AM SPEC PAP PY 2005 VL 396 BP 55 EP 65 DI 10.1130/0-8137-2396-5.55 PG 11 WC Geochemistry & Geophysics; Geology; Geosciences, Multidisciplinary SC Geochemistry & Geophysics; Geology GA BLX26 UT WOS:000271268500006 ER PT B AU Lin, J AF Lin, J BE Sankarasubramanian, K Penn, M Pevtsov, A TI Large-scale organizations related to eruptive phenomena on the solar surface SO LARGE-SCALE STRUCTURES AND THEIR ROLE IN SOLAR ACTIVITY SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 22nd Sacramento Peak Workshop on Large-Scale Structures and Their Role in Solar Activity CY OCT 18-22, 2004 CL Natl Solar Observ, Sunspot, NM HO Natl Solar Observ ID CORONAL MASS EJECTIONS; MAGNETIC-FIELD CONFIGURATIONS; 2002 JULY 23; CURRENT SHEET; OBSERVATIONAL EVIDENCE; RECONNECTION INFLOW; ACTIVE REGIONS; FLUX ROPE; FLARE; LOOPS AB This review highlights recent, progress made in the research on eruptive phenomena related to the large-scale organizations near the solar surface. Usually, these organizations are manifested by solar flares and eruptive prominences during the eruptions. We start by briefly overviewing the properties of the prominences and the related magnetic configurations prior to the eruptions. Then, we discuss the correlations among various manifestations displayed by a typical eruptive process. Our main focus is on the works related to the observations kind studies of the current sheet and other important features related to the magnetic reconnection process during the eruptions. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Lin, J (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jlin@cfa.harvard.edu RI LIN, JUN/B-9890-2017 NR 93 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 1-58381-214-8 J9 ASTR SOC P PY 2005 VL 346 BP 289 EP 304 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BDY93 UT WOS:000236273500030 ER PT S AU Luhman, KL Fazio, G Megeath, T Hartmann, L Calvet, N AF Luhman, KL Fazio, G Megeath, T Hartmann, L Calvet, N TI Young brown dwarfs: IMF, disks, spatial distribution, and binarity SO Low-Mass Stars and Brown Dwarfs - IMF Accretion and Activity SE MEMOIRE DELLA SOCIETA ASTRONOMICA ITALIANA - SERIES LA English DT Proceedings Paper CT Workshop on Low-Mass Stars and Brown Dwarfs - IMF Accretion and Activity CY OCT 17-20, 2004 CL Volterra, ITALY DE infrared : stars; stars : evolution; stars : formation; stars : low-mass; brown dwarfs; stars : pre-main sequence ID LOW-MASS STARS; ORION NEBULA CLUSTER; FORMING REGION; EVOLUTIONARY MODELS; TAURUS; OBJECTS; SPECTROSCOPY; CENSUS AB We present new results regarding the initial mass function, circumstellar disks, spatial distribution, and binarity of young brown dwarfs. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Luhman, KL (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. NR 28 TC 2 Z9 2 U1 0 U2 0 PU SOC ASTRONOMICA ITALIANA PI FLORENCE PA LARGO ENRICO FERMI 5, FLORENCE, 50125, ITALY SN 0037-8720 J9 MEM SOC ASTRON ITAL PY 2005 VL 76 IS 2 BP 285 EP 290 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BCY34 UT WOS:000231852200017 ER PT S AU Mohanty, S Jayawardhana, R Basri, G AF Mohanty, S Jayawardhana, R Basri, G TI Accretion, jets and disk-locking in the brown dwarf domain SO Low-Mass Stars and Brown Dwarfs - IMF Accretion and Activity SE MEMOIRE DELLA SOCIETA ASTRONOMICA ITALIANA - SERIES LA English DT Proceedings Paper CT Workshop on Low-Mass Stars and Brown Dwarfs - IMF Accretion and Activity CY OCT 17-20, 2004 CL Volterra, ITALY DE low-mass stars and brown dwarfs; accretion and jets; disk-locking AB We demonstrate that in accreting ultra-low mass stars and brown dwarfs, the Call lambda 8662 emission line flux yields a robust quantitative estimate of the mass accretion rate (1 1), providing an easier 4 determination technique than detailed Ha line-profile modeling. With optical high-resolution spectra, we derive M from Call fluxes for young ultralow mass objects down to nearly the deuterium-burning (planetary-mass) limit. Our results, combined with prior studies of higher-mass classical T Taurii stars (CTTs), show that M decreases steeply with (sub-)stellar mass, roughly as M proportional to M-*(2) (albeit with considerable scatter). A similar relationship has been suggested by previous studies; we extend it to nearly the planetary regime, We also find forbidden [011 lambda 6300 emission in the similar to 10 Myr-old, M8 accreting brown dwarf 2MASS 1207-3932, making this the oldest and one of the lowest-mass brown dwarfs with a mass outflow. Finally, in CTTs, accretion and jets are often linked to disk-locking. Using vsin i derived from our high-resolution spectra, we show that the same phenomenon arises in the ultra-low mass regime as well: accretors near and below the sub-stellar boundary appear to be preferentially slow rotators compared to non-accretors. These results suggests that ultra-low mass stellar and sub-stellar objects pass, in their youth, through a T Tauri phase completely analogous to that observed in higher-mass stars, bolstering the idea of a common formation mechanism in the two mass regimes. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Mohanty, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 42, Cambridge, MA 02138 USA. NR 8 TC 5 Z9 5 U1 0 U2 0 PU SOC ASTRONOMICA ITALIANA PI FLORENCE PA LARGO ENRICO FERMI 5, FLORENCE, 50125, ITALY SN 0037-8720 J9 MEM SOC ASTRON ITAL PY 2005 VL 76 IS 2 BP 303 EP 308 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BCY34 UT WOS:000231852200020 ER PT S AU Haverkorn, M AF Haverkorn, M BE DeGouveiaDal Pino, EM Lugones, G Lazarian, A TI Galactic turbulence and magnetic fields through radiopolarimetry of the Galactic synchrotron background SO MAGNETIC FIELDS IN THE UNIVERSE: FROM LABORATORY AND STARS TO PRIMORDIAL STRUCTURES SE AIP Conference Proceedings LA English DT Proceedings Paper CT Conference on Magnetic Fields in the Universe - From Laboratory and Stars to Primordial Structures CY NOV 28-DEC 03, 2004 CL Angra dos Reis, BRAZIL SP Univ Sao Paulo, Univ Pisa, Univ Wisconsin Madison DE polarimetry; ISM; magnetic fields; HII regions; turbulence; flux tubes; spiral arms; Galactic magnetism ID INTERSTELLAR-MEDIUM; MULTIFREQUENCY POLARIMETRY; INNER GALAXY; PLANE SURVEY; IONIZED-GAS; 350 MHZ; REGION; SCALE; DENSITY; POLARIZATION AB Multi-frequency radiopolarimetry of diffuse Galactic synchrotron emission and polarized extragalactic sources can yield estimates of Galactic magnetic field strength, of maximum scales of fluctuations in the magneto-ionized medium, or enable discovery of magnetic objects which are difficult or impossible to observe otherwise. I will discuss these methods and present the continuum part of the large, arcminute resolution Southern Galactic Plane Survey. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mhaverkon@cfa.harvard.edu NR 28 TC 3 Z9 3 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 0-7354-0273-6 J9 AIP CONF PROC PY 2005 VL 784 BP 308 EP 317 PG 10 WC Astronomy & Astrophysics; Physics, Fluids & Plasmas SC Astronomy & Astrophysics; Physics GA BDI28 UT WOS:000233597400028 ER PT J AU Shapley, RL Wilson, DE Warren, AN Barnett, AA AF Shapley, RL Wilson, DE Warren, AN Barnett, AA TI Bats of the Potaro Plateau region, western Guyana SO MAMMALIA LA English DT Article DE Chiroptera; Guyana potato; Platyrrhinus; Carollia castanea; ecology; distribution ID FRENCH-GUIANA; SOUTH-AMERICA; MIST-NETS; CHIROPTERA; DIVERSITY; FOREST; PHYLLOSTOMIDAE; CONSERVATION; COMMUNITIES; SPECIMEN AB This paper present species records and inferable habitat preferences of a total of 35 bat species in 25 genera that were captured during three separate studies on the Potato Plateau, western Guyana. One, Carollia castanea, is a new country record. Reproductive data is presented for seven species. Measurements and habitat data given for Platyrrhinus aurarius, a little-known species. The composition of the Potato Plateau bat community is contextualized by comparison with 13 other sites in the north-east South America. A map shows all known bat collection localites in Guyana, for which a gazetteer provides supporting information. C1 Akodon Ecol Consulting, Concord, CA 94518 USA. Smithsonian Inst, Div Mammals, Nat Hist Museum, Washington, DC 20560 USA. Last Refuge Ltd, Batch Farm, Panborough BA5 1PN, Somerset, England. Roehampton Univ, Ctr Res Evolutionary Anthropol, Sch Human & Life Sci, London SW15 4JD, England. RP Shapley, RL (reprint author), Akodon Ecol Consulting, 951 Bancroft Rd, Concord, CA 94518 USA. EM Rebecca@Akodon.com NR 76 TC 2 Z9 3 U1 2 U2 8 PU MUSEUM NAT HIST NATURELLE PI PARIS PA SERVICE PUBLICATIONS SCIENTIFIQUES, 57 RUE CUVIER, 75005 PARIS, FRANCE SN 0025-1461 J9 MAMMALIA JI Mammalia PY 2005 VL 69 IS 3-4 BP 375 EP 394 DI 10.1515/mamm.2005.030 PG 20 WC Zoology SC Zoology GA 004PH UT WOS:000234764200006 ER PT J AU Dubost, G Henry, O Comizzoli, P AF Dubost, G Henry, O Comizzoli, P TI Seasonality of reproduction in the three largest terrestrial rodents of French Guiana forest SO MAMMALIAN BIOLOGY LA English DT Article DE large rodents; reproduction; seasonality; French Guiana ID ORANGE-RUMPED AGOUTI; FEMALE GREEN ACOUCHI; DASYPROCTA-LEPORINA; MYOPROCTA-PRATTI; COMPARATIVE DIET; ECOLOGY AB We investigated the main Life history of the three Largest terrestrial rodents of French Guiana forest: the acouchy (Myoprocto exilis), the agouti (Dasyprocto leporina) and the paca (Agouti paca), using data collected during several years. There were noticeable differences among the species in sexual maturation and degree of seasonality in reproduction. Percentage of pregnant females, births and juveniles, and body weight of juveniles decreased progressively from the acouchy, through the agouti to tFe paca. The acouchy was by far the most seasonal: no births occur in the period August-October, 56% of births were encountered in November-January; consequently, young form an unique cohort in the population. The agouti was also seasonal, but to a Lesser degree. Newborns appeared in every period of the year in paca, without any formation of cohort of young. These differences tended to be linked to the seasonal importance of fruits in diets, the most aseasonal species having the most diversified diet during the poor fruit season. (c) 2005 Elsevier GmbH. All rights reserved. C1 Museum Natl Hist Nat, CNRS, UMR 5173, F-75231 Paris, France. Smithsonian Inst, Natl Zool Pk, Dept Reprod Sci, Conservat & Res Ctr, Washington, DC 20008 USA. RP Dubost, G (reprint author), Museum Natl Hist Nat, CNRS, UMR 5173, 57 Rue Cuvier, F-75231 Paris, France. EM gdubost@mnhn.fr NR 34 TC 11 Z9 12 U1 0 U2 7 PU URBAN & FISCHER VERLAG PI JENA PA BRANCH OFFICE JENA, P O BOX 100537, D-07705 JENA, GERMANY SN 1616-5047 J9 MAMM BIOL JI Mamm. Biol. PY 2005 VL 70 IS 2 BP 93 EP 109 DI 10.1016/j.mambio.2004.09.001 PG 17 WC Zoology SC Zoology GA 921ZG UT WOS:000228804100003 ER PT S AU Nagamine, K Springel, V Hernquist, L AF Nagamine, K Springel, V Hernquist, L BE Colless, M StaveleySmith, L Stathakis, R TI Damped Lyman-alpha absorbers in cosmological SPH simulations: the "metallicity problem" SO MAPS OF THE COSMOS SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 216th Symposium of the International-Astronomical-Union CY JUL 14-17, 2003 CL Sydney, AUSTRALIA SP Int Astron Union ID PARTICLE HYDRODYNAMICS SIMULATIONS; II-ASTERISK ABSORPTION; STAR-FORMATION; SYSTEMS; UNIVERSE; GALAXIES; HISTORY; GAS; ABUNDANCE; EVOLUTION AB We study the distribution of star formation rate (SFR) and metallicity of damped Lyman-alpha absorbers (DLAs) using cosmological smoothed particle hydrodynamics (SPH) simulations of the A cold dark matter (CDM) model. Our simulations include a phenomenological model for feedback by galactic winds which allows us to examine the effect of galactic outflows on the distribution of SFR and metallicity of DLAs. For models with strong galactic winds, we obtain good agreement with recent observations with respect to total neutral hydrogen mass density, N-HI column-density distribution, abundance of DLAs, and for the distribution of SFR in DLAs. However, we also find that the median metallicity of simulated DLAs is higher than the values typically observed by nearly an order of magnitude. This discrepancy with observations could be due to shortcomings in the treatment of the supernova feedback or the multiphase structure of the gas in our current simulations. Recent observations by Wolfe et al. (2003a,b) seem to point to the same problem; i.e. the observed DLA metallicities are much lower than those expected from the (either observed or simulated) DLA star formation rates, a puzzle that has been known as the "missing metals" -problem for the globally averaged quantities. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Nagamine, K (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 22 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA SN 0074-1809 BN 1-58381-202-4 J9 IAU SYMP PY 2005 IS 216 BP 266 EP 273 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BDE52 UT WOS:000233081400027 ER PT S AU Nicastro, F AF Nicastro, F BE Colless, M StaveleySmith, L Stathakis, R TI Chandra and FUSE view of the WHIM: the local group and beyond SO MAPS OF THE COSMOS SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 216th Symposium of the International-Astronomical-Union CY JUL 14-17, 2003 CL Sydney, AUSTRALIA SP Int Astron Union ID X-RAY FOREST; SPECTROSCOPIC-EXPLORER OBSERVATIONS; HOT INTERGALACTIC MEDIUM; ABSORPTION-LINE SYSTEMS; HIGH-VELOCITY CLOUDS; GALACTIC HALO; O-VI; LOW-REDSHIFT; OVI ABSORPTION; IONIZED-GAS AB In this contribution, I review the current observational evidence for the existence of filaments of Warm-Hot Intergalactic Medium (WHIM). In particular, I first focus on the controversial issue of the identification of the z similar to 0 highly ionized far-ultraviolet (i.e. OVI) and X-ray (i.e. OVII, OVIII and NeIX) absorbers with either a very tenuous and diffuse WHIM filament, or with much denser condensations of material at large distances in the Galactic halo. I then present our recent detection (confidence level > 3 sigma) of the OVII WHIM at z > 0 and derive an estimate of the total number of baryons contained in this hard-to-detect phase of the IGM. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Nicastro, F (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 30 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA SN 0074-1809 BN 1-58381-202-4 J9 IAU SYMP PY 2005 IS 216 BP 297 EP 305 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BDE52 UT WOS:000233081400030 ER PT J AU Hochberg, R AF Hochberg, R TI Musculature of the primitive gastrotrich Neodasys (Chaetonotida): functional adaptations to the interstitial environment and phylogenetic significance SO MARINE BIOLOGY LA English DT Article ID MORPHOLOGY; EVOLUTION; ULTRASTRUCTURE; ASCHELMINTHES; MUSCLES; SYSTEM AB Gastrotrichs are acoelomate micrometazoans common to marine interstitial environments of sublittoral sediments and exposed sandy beaches. The genus Neodasys (Chaetonotida) contains three marine species known from oceans and seas worldwide, and figures prominently in discussions of gastrotrich origins. To gain insight into the phylogenetic position of Neodasys and to understand the adaptive significance of muscle anatomy in marine interstitial gastrotrichs, a fluorescent phalloidin-linked marker was used to view the organization of muscles in two species from North America and Australia. Muscular topography of Neodasys cirritus from Florida, USA, and Neodasys cf. uchidai from Queensland, Australia, was found to be similar between species and to basal species of Macrodasyida; muscles were present in circular, longitudinal and helicoidal patterns. Musculature of the midgut region was partially reduced relative to basal macrodasyidan gastrotrichs, but well developed relative to most other chaetonotidan gastrotrichs. In general, muscle patterns in species of Neodasys closely correspond with those of other gastrotrichs of similar size and body type, and may therefore reflect a common adaptive solution to the physical demands of the interstitial environment. Results also suggest that reductions in midgut musculature may be functionally related to oviposition and, as such, are probably not homologous with similar reductions of circular muscles in other species of Chaetonotida. C1 Smithsonian Marine Stn, Ft Pierce, FL 34949 USA. RP Hochberg, R (reprint author), Smithsonian Marine Stn, 701 Seaway Dr, Ft Pierce, FL 34949 USA. EM Hochberg_Rick@yahoo.com NR 27 TC 13 Z9 14 U1 0 U2 0 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013 USA SN 0025-3162 J9 MAR BIOL JI Mar. Biol. PD JAN PY 2005 VL 146 IS 2 BP 315 EP 323 DI 10.1007/s00227-004-1437-0 PG 9 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 881YP UT WOS:000225905700010 ER PT J AU Jewett, EB Hines, AH Ruiz, GM AF Jewett, EB Hines, AH Ruiz, GM TI Epifaunal disturbance by periodic low levels of dissolved oxygen: native vs. invasive species response SO MARINE ECOLOGY PROGRESS SERIES LA English DT Article DE periodic hypoxia; invasive species; Chesapeake Bay; disturbance; epifauna ID ESTUARINE FOULING COMMUNITY; CHESAPEAKE-BAY; BALTIC SEA; SUBTIDAL ZONE; WATER-QUALITY; HYPOXIA; DIVERSITY; PREDATION; EUTROPHICATION; RECRUITMENT AB Hypoxia is increasing in marine and estuarine systems worldwide, primarily due to anthropogenic causes. Periodic hypoxia represents a pulse disturbance, with the potential to restructure estuarine biotic communities. We chose the shallow, epifaunal community in the lower Chesapeake Bay, Virginia, USA, to test the hypothesis that low dissolved oxygen (DO) (< 4 mg l(-1)) affects community dynamics by reducing the cover of spatial dominants, creating space both for less dominant native species and for invasive species, Settling panels were deployed at shallow depths in spring 2000 and 2001. at Gloucester Point, Virginia, and were manipulated every 2 wk from late June to mid-August. Manipulation involved exposing epifaunal communities to varying levels of DO for up to 24 h followed by redeployment in the York River. Exposure to low DO affected both species composition (presence or absence) and the abundance of the organisms present. Community dominance shifted away from barnacles as level of hypoxia increased. Barnacles were important spatial dominants which reduced species diversity when locally abundant. The cover of Hydroides dianthus, a native serpulid polychaete, doubled when exposed to periodic hypoxia. Increased H. dianthus cover may indicate whether a local region has experienced periodic, local DO depletion and thus provide an indicator of poor water-quality conditions. In 2001, the combined cover of the invasive and cryptogenic species in this community, Botryllus schlosseri (tunicate), Molgula manhattensis (tunicate), Ficopomatus enigmaticus (polychaete) and Diadumene lineata (anemone), was highest on the plates exposed to moderately low DO (2 mg l(-1) < DO < 4 mg l(-1)). All 4 of these species are now found worldwide and exhibit life histories well adapted for establishment in foreign habitats. Low DO events may enhance success of invasive species, which further stress marine and estuarine ecosystems. C1 Univ Maryland, Dept Biol, College Pk, MD 20742 USA. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Jewett, EB (reprint author), Univ Maryland, Dept Biol, College Pk, MD 20742 USA. EM jewette@si.edu OI Ruiz, Gregory/0000-0003-2499-441X NR 72 TC 30 Z9 32 U1 3 U2 27 PU INTER-RESEARCH PI OLDENDORF LUHE PA NORDBUNTE 23, D-21385 OLDENDORF LUHE, GERMANY SN 0171-8630 J9 MAR ECOL PROG SER JI Mar. Ecol.-Prog. Ser. PY 2005 VL 304 BP 31 EP 44 DI 10.3354/meps304031 PG 14 WC Ecology; Marine & Freshwater Biology; Oceanography SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Oceanography GA 004JW UT WOS:000234750100004 ER PT J AU Litchman, E Neale, PJ AF Litchman, E Neale, PJ TI UV effects on photosynthesis, growth and acclimation of an estuarine diatom and cryptomonad SO MARINE ECOLOGY PROGRESS SERIES LA English DT Article DE estuarine phytoplankton; UV radiation; photosynthesis; photoinhibition; biological weighting functions; acclimation; Thalassiosira pseudonana; Cryptomonas sp. ID SOLAR ULTRAVIOLET-RADIATION; B RADIATION; PHYTOPLANKTON PHOTOSYNTHESIS; SENSITIVITY; INHIBITION; VOLUME; LAKES; PHOTOPROTECTION; EXPOSURE AB Ultraviolet (UV) radiation is a significant stressor in aquatic environments and can inhibit primary productivity of phytoplankton. The effects of UV depend on many factors, including phytoplankton community composition and acclimation status. Using spectrally resolved biological weighting functions (BWFs), we determined sensitivity of photosynthesis and acclimation to UV in a common estuarine diatom, Thalassiosira pseudonana (Hustedt) Hasle et Heimdal, and cryptomonad, Cryptomonas sp. Cryptomonas sp. grown under high PAR (photosynthetically active radiation) (250 mu mol quanta m(-2) s(-1)) was significantly more sensitive to photoinhibition in the UV-B part of the spectrum (280 to 320 nm) than T pseudonana under high PAR. Growth under low irradiance (25 mu mol quanta m(-2) s(-1)) increased sensitivity of T pseudonana. After a week-long exposure to moderate UV radiation, sensitivity of Cryptomonas sp. declined, while sensitivity of T pseudonana did not change. Growth rates and chlorophyll a-specific absorption decreased in both species. Based on the BWFs obtained in this study, we predict 11 to 26% UV inhibition of depth-integrated primary production by these species under summer conditions in a shallow, turbid temperate estuary. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Georgia Inst Technol, Sch Biol, Atlanta, GA 30332 USA. RP Litchman, E (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM litchman@msu.edu RI Neale, Patrick/A-3683-2012 NR 36 TC 29 Z9 31 U1 3 U2 10 PU INTER-RESEARCH PI OLDENDORF LUHE PA NORDBUNTE 23, D-21385 OLDENDORF LUHE, GERMANY SN 0171-8630 J9 MAR ECOL PROG SER JI Mar. Ecol.-Prog. Ser. PY 2005 VL 300 BP 53 EP 62 DI 10.3354/meps300053 PG 10 WC Ecology; Marine & Freshwater Biology; Oceanography SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Oceanography GA 976EF UT WOS:000232714900006 ER PT J AU Eisert, R Oftedal, OT Lever, M Ramdohr, S Breier, BH Barrell, GK AF Eisert, R Oftedal, OT Lever, M Ramdohr, S Breier, BH Barrell, GK TI Detection of food intake in a marine mammal using marine osmolytes and their analogues as dietary biomarkers SO MARINE ECOLOGY PROGRESS SERIES LA English DT Review DE foraging; dietary biomarker; arsenobetaine; trimethylamine N-oxide; osmolytes; lactation; Weddell seal; marine mammal ID SEALS LEPTONYCHOTES-WEDDELLII; TRIMETHYLAMINE-N-OXIDE; ATOMIC-ABSORPTION-SPECTROMETRY; 3-DIMENSIONAL DIVE PROFILES; SOUTHERN ELEPHANT SEALS; GROWTH FACTOR-I; HPLC-ICP-MS; ARSENIC COMPOUNDS; DIVING BEHAVIOR; GLYCINE BETAINE AB We report a novel method of investigating foraging in marine mammals based on detecting biomarkers of strictly dietary origin in blood. Arsenobetaine (AsB), the arsenic analogue of the osmolyte glycine betaine, and trimethylamine N-oxide (TMAO), an osmolyte used by marine fish and invertebrates, were measured in plasma of lactating Weddell seals Leptonychotes weddellii during the postpartum fast and at different stages of lactation. Plasma dietary biomarker concentrations were low in early lactation (<14 d postpartum [d p.p.]; AsB: 5.5 +/- 2 ppb As, TMAO: 66 +/- 20 mu mol l(-1)) and increased 10-fold in late lactation ( >= 27 d p.p.; AsB: 57 17 ppb As, TMAO: 685 +/- 199 mu mol l(-1)). In lactating females (n = 6) monitored longitudinally, plasma TMAO remained low for the first 3 wk p.p. Increases in AsB concentrations observed in late lactation were closely correlated (Pearson correlation r = 0.96, p < 0.01, n = 6) with increases in plasma insulin-like growth factor I (IGF1), a growth factor known to reflect nutritional status in other mammals. Two seals outfitted with time-depth recorders began regular deep diving at different times p.p. and showed corresponding differences in biomarker concentrations. Our results indicate that (1) most lactating Weddell seals at the study site (70 % of 20 seals studied) feed after 3 to 4 wk p.p., (2) individual lactating Weddell seals may forage as early as 9 d p.p., and (3) some Weddell seals may consume little or no food throughout lactation. Dietary biomarkers provide a simple method for distinguishing feeding and fasting in free-living marine mammals. C1 Dept Conservat Biol, Washington, DC 20008 USA. Canterbury Hlth Labs, Christchurch, New Zealand. Alfred Wegener Inst Polar & Marine Res, D-27570 Bremerhaven, Germany. Univ Auckland, Liggins Inst, Fac Med & Hlth Sci, Auckland 1, New Zealand. Lincoln Univ, Anim & Food Sci Div, Canterbury, New Zealand. RP Eisert, R (reprint author), Dept Conservat Biol, Smithsonian Natl Zool Pk,3001 Connecticut Ave NW, Washington, DC 20008 USA. EM eisertr@si.edu RI Breier, Bernhard/D-1176-2009 NR 140 TC 23 Z9 23 U1 0 U2 8 PU INTER-RESEARCH PI OLDENDORF LUHE PA NORDBUNTE 23, D-21385 OLDENDORF LUHE, GERMANY SN 0171-8630 J9 MAR ECOL PROG SER JI Mar. Ecol.-Prog. Ser. PY 2005 VL 300 BP 213 EP 228 DI 10.3354/meps300213 PG 16 WC Ecology; Marine & Freshwater Biology; Oceanography SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Oceanography GA 976EF UT WOS:000232714900019 ER PT J AU Kuhlmann, ML Hines, AH AF Kuhlmann, ML Hines, AH TI Density-dependent predation by blue crabs Callinectes sapidus on natural prey populations of infaunal bivalves SO MARINE ECOLOGY PROGRESS SERIES LA English DT Article DE predator-prey interactions; foraging behavior; density dependence; functional response; experimental scale; agonism; Callinectes sapidus; Macoma balthica ID CENTRAL CHESAPEAKE BAY; MACOMA-BALTHICA L; FUNCTIONAL-RESPONSE; FORAGING BEHAVIOR; PATCH SIZE; MUTUAL INTERFERENCE; ESTUARINE PREDATOR; MARINE PREDATOR; SHALLOW-WATER; PATTERNS AB We used field and laboratory mesocosm experiments to examine the effects of the functional response of the blue crab Callinectes sapidus foraging on Balthic clams Macoma balthica in the upper Chesapeake Bay. Field experiments measured the density-dependent effect of blue crabs on clam patches in both mud and sand substrates at multiple sites spanning the natural range of clam densities, allowing us to examine the effects of larger-scale variation in prey abundance on prey mortality patterns. We compared the results of our field experiments to mesocosm experiments with 1 and 2 blue crabs to determine differences in the effects of single and multiple predators on the density-dependence of clam mortality. We observed predator behavior to identify mechanisms responsible for differences in prey mortality patterns. In the field, M balthica mortality was not significantly density dependent, but the natural density of prey surrounding experimental patches had a negative density-dependent effect on clam mortality in mud. In the mesocosms, 1 or 2 blue crabs caused density-dependent mortality. Density dependence was weaker in mesocosms with 2 crabs. Agonistic behaviors were not significantly affected by clam density, but the presence of a conspecific increased a crab's foraging time at the lowest clam density. Changes in behavior when multiple crabs forage together may partly account for the reduction in density dependence of clam mortality. Predator responses such as the effects of conspecifics on foraging and patch choice that were lacking in the laboratory appear to be key in determining prey mortality patterns in the field. Larger-scale patterns of prey density variation were more important in determining prey mortality rates than the small-scale variation represented by the experimentally manipulated patches. C1 Hartwick Coll, Dept Biol, Oneonta, NY 13820 USA. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Kuhlmann, ML (reprint author), Hartwick Coll, Dept Biol, Oneonta, NY 13820 USA. EM kuhlmannm@hartwick.edu NR 52 TC 14 Z9 14 U1 1 U2 5 PU INTER-RESEARCH PI OLDENDORF LUHE PA NORDBUNTE 23, D-21385 OLDENDORF LUHE, GERMANY SN 0171-8630 J9 MAR ECOL PROG SER JI Mar. Ecol.-Prog. Ser. PY 2005 VL 295 BP 215 EP 228 DI 10.3354/meps295215 PG 14 WC Ecology; Marine & Freshwater Biology; Oceanography SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Oceanography GA 947UC UT WOS:000230671800019 ER PT J AU Robertson, DR Ackerman, JL Choat, JH Posada, JM Pitt, J AF Robertson, DR Ackerman, JL Choat, JH Posada, JM Pitt, J TI Ocean surgeonfish Acanthurus bahianus. I. The geography of demography SO MARINE ECOLOGY PROGRESS SERIES LA English DT Article DE Acanthuridae; Acanthurus bahianus; tropical west Atlantic; otolith; longevity; growth; size; temperature ID GREAT-BARRIER-REEF; CORAL-REEF; MENIDIA-MENIDIA; LIFE-HISTORY; COUNTERGRADIENT VARIATION; POPULATION-STRUCTURE; ATLANTIC SILVERSIDE; DIFFERENT LATITUDES; EARLY RECRUITMENT; PUERTO-RICO AB The ocean. surgeonfish Acanthurus bahianus is a common inhabitant of reefs throughout the west and central Atlantic. We examined geographic variation in its demography among 10 locations spanning 56 degrees of latitude. These populations exhibit a great diversity of growth trajectories, as well as 3-fold variation in terminal size and maximum longevity. There are strongly contrasting patterns of habitat variation in demography at 2 sites: at Bermuda, fish settle inshore, grow to about asymptotic size and then, when 2 to 6 yr old, relocate permanently to outer reefs, where they can reach 32 yr. At Belize, fish settle and attain 10 yr on both inner and outer reefs, but grow faster and reach a similar to 50% greater asymptotic weight on inner reefs. Habitat differences in growth at Belize largely span the range of variation among NW Atlantic locations, A. bahianus exhibits the fastest growth known for an acanthurid, and the strongest spatial variation in demography known for a tropical reef-fish. Maximum age, adult survivorship, terminal size and absolute growth rate are inversely related to temperature. However, relative growth rate is not: in all populations a similar percentage of mean asymptotic standard length (L-infinity) is achieved at 1, 2 and 3 yr, and then growth effectively ceases. Variation in longevity is related to temperature, and is largely independent of size. Variation in growth and size is related strongly to both habitat and temperature effects, and the rate of growth appears to set terminal size. High longevity at 3 isolated oceanic islands seems to reflect a temperature effect, rather than an island effect. C1 Smithsonian Trop Res Inst Panama, STRI, Unit 0948, APO, AA 34002 USA. James Cook Univ N Queensland, Sch Marine Biol & Aquaculture, Townsville, Qld 4811, Australia. Univ Simon Bolivar, Dept Biol Organismos, Caracas 1080A, Venezuela. Bermuda Biol Stn Res, Benth Ecol Lab, Ferry Reach, Bermuda. RP Robertson, DR (reprint author), Smithsonian Trop Res Inst Panama, STRI, Unit 0948, APO, AA 34002 USA. EM drr@stri.org NR 61 TC 43 Z9 44 U1 1 U2 10 PU INTER-RESEARCH PI OLDENDORF LUHE PA NORDBUNTE 23, D-21385 OLDENDORF LUHE, GERMANY SN 0171-8630 J9 MAR ECOL PROG SER JI Mar. Ecol.-Prog. Ser. PY 2005 VL 295 BP 229 EP 244 DI 10.3354/meps295229 PG 16 WC Ecology; Marine & Freshwater Biology; Oceanography SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Oceanography GA 947UC UT WOS:000230671800020 ER PT J AU Robertson, DR Choat, JH Posada, JM Pitt, J Ackerman, JL AF Robertson, DR Choat, JH Posada, JM Pitt, J Ackerman, JL TI Ocean surgeonfish Acanthurus bahianus. II. Fishing effects on longevity, size and abundance? SO MARINE ECOLOGY PROGRESS SERIES LA English DT Article DE surgeonfish; Acanthurus bahianus; tropical west Atlantic; demography; density; fishing effects ID GREAT-BARRIER-REEF; US VIRGIN-ISLANDS; MARINE RESERVES; EARLY RECRUITMENT; CARIBBEAN PANAMA; PROTECTED AREAS; PATCH-REEFS; FISHES; BIOMASS; COMMUNITIES AB The ocean surgeonfish Acanthurus bahianus, an abundant small herbivore on reefs throughout the tropical west and central Atlantic, is a significant component of Caribbean trap-fishery catches. To assess effects of fishing on this species we compared its longevity, survivorship, size and abundance at localities throughout its range that have differing intensities and targets of fishing. Temperature explains nearly all of the geographic variation in maximum longevity of A. bahianus, and most of the variation in adult survivorship, with no indications of consistent fishing effects on either. Variation in maximum and median length (1.6-fold) and in abundance (16-fold) also are not consistently related to fishing. A. bahianus has similar demographic characteristics at 2 neighbouring (50 km apart) offshore Venezuelan reefs, one a well protected reserve, the other with intense fishing for predators. At Panama, the abundance of adult A. bahianus showed no trend of change from 1979 to 1997, as the local density of subsistence fishers increased by similar to 70%. The lack of consistent fishing-effects on this species found in this and some other studies may reflect a combination of (1) resilience to fishing mortality arising from rapid growth to asymptotic size, early maturity, small size and abundance, and (2) strong, natural, large- and small-scale spatial variation in demography and abundance obscuring any such effects. Effects of non-catastrophic fishing on sedentary reef-fishes with similar demographic characteristics probably will be revealed only through comparisons of subpopulations in adjacent fished and no-take areas involving careful consideration of small-scale habitat effects. C1 Smithsonian Trop Res Inst Panama, STRI, Unit 0948, APO, AA 34002 USA. James Cook Univ N Queensland, Sch Marine Biol & Aquaculture, Townsville, Qld 4811, Australia. Univ Simon Bolivar, Dept Biol Organismos, Caracas 1080A, Venezuela. Bermuda Biol Stn Res, Benth Ecol Lab, Ferry Reach, Bermuda. RP Robertson, DR (reprint author), Smithsonian Trop Res Inst Panama, STRI, Unit 0948, APO, AA 34002 USA. EM drr@stri.org NR 53 TC 13 Z9 13 U1 1 U2 13 PU INTER-RESEARCH PI OLDENDORF LUHE PA NORDBUNTE 23, D-21385 OLDENDORF LUHE, GERMANY SN 0171-8630 J9 MAR ECOL PROG SER JI Mar. Ecol.-Prog. Ser. PY 2005 VL 295 BP 245 EP 256 DI 10.3354/meps295245 PG 12 WC Ecology; Marine & Freshwater Biology; Oceanography SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Oceanography GA 947UC UT WOS:000230671800021 ER PT J AU Kuntz, NM Kline, DI Sandin, SA Rohwer, F AF Kuntz, NM Kline, DI Sandin, SA Rohwer, F TI Pathologies and mortality rates caused by organic carbon and nutrient stressors in three Caribbean coral species SO MARINE ECOLOGY PROGRESS SERIES LA English DT Article DE coral; disease; symptoms; chronic stress; ecotoxicology ID REEF; COMMUNITY; ECOLOGY; DISEASE; DIVERSITY; IMPACTS; SCALE; ECOSYSTEMS; ANNULARIS; FAVEOLATA AB Anthropogenic inputs, including organic carbon and nutrient loading, are increasingly changing the water quality on coral reefs. Herein we show that treating Montastraea annularis, Agaricia tenuifolia and Porites furcata with various organic carbon sources (starch, lactose, arabinose and mannose) results in different species-specific and carbon-specific pathologies and rates of mortality. The variation in the pathological characteristics caused by stressors showed that visual cues for determining coral health and disease may be misleading. The probability of mortality increased significantly over time with continual exposure to several of the stressors, suggesting that chronic stressors may be more harmful than acute stressors. In contrast to the organic carbon sources, high concentrations of nutrients (phosphate, ammonium and nitrate) did not directly kill corals. The variation in coral responses to anthropogenic stressors means that changes on disturbed coral reefs will depend on the type of and duration of exposure to the stressor, as well as on the species of coral. C1 San Diego State Univ, Dept Biol, San Diego, CA 92182 USA. Univ Calif San Diego, Scripps Inst Oceanog, Ctr Marine Biodivers & Conservat, La Jolla, CA 92093 USA. Smithsonian Trop Res Inst, Balboa, Panama. San Diego State Univ, Ctr Microbial Sci, San Diego, CA 92182 USA. RP Rohwer, F (reprint author), San Diego State Univ, Dept Biol, LS301,5500 Campanile Dr, San Diego, CA 92182 USA. EM forest@sunstroke.sdsu.edu NR 50 TC 81 Z9 85 U1 1 U2 21 PU INTER-RESEARCH PI OLDENDORF LUHE PA NORDBUNTE 23, D-21385 OLDENDORF LUHE, GERMANY SN 0171-8630 J9 MAR ECOL PROG SER JI Mar. Ecol.-Prog. Ser. PY 2005 VL 294 BP 173 EP 180 DI 10.3354/meps294173 PG 8 WC Ecology; Marine & Freshwater Biology; Oceanography SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Oceanography GA 943XA UT WOS:000230387600014 ER PT J AU Sobrino, C Montero, I Lubian, LM AF Sobrino, C Montero, I Lubian, LM TI Effect of UV-A and UV-B on diel patterns of growth and metabolic activity in Nannochloris atomus cultures assessed by flow cytometry SO MARINE ECOLOGY PROGRESS SERIES LA English DT Article DE UV radiation; Diel cycles; flow cytometry; Nannochloris atomus ID ULTRAVIOLET-RADIATION; CELL-CYCLE; MARINE PICOPLANKTON; CHLOROPHYLL-A; PHOTOSYNTHESIS; PHYTOPLANKTON; CYANOBACTERIA; INHIBITION; MICROALGAE; RESPONSES AB The aim of this study was to assess the effect of UV-A (320 to 400 nm) and UV-B (280 to 320 nm) radiation on diel patterns of growth and metabolic activity of the marine picoplankter Nannochloris atomus using flow cytometry. N, atomus cells exposed to PAR (400 to 700 nm), PAR+UV-A and PAR+UV-A+UV-B showed clear diel patterns in cell size, chlorophyll fluorescence and metabolic activity, the latter being measured by a fluorescein diacetate-based cell esterase activity assay. For all spectral treatments, patterns increased during the day and decreased during the night, with minima near dawn and maxima near dusk. In addition, cell division was tightly phased to the light dark (L:D) cycle, occurring soon after dark. Exposure to UVR did not alter the synchrony of the parameters measured, but the extent of variation between dawn and dusk was dependent on the spectral conditions. Chlorophyll autofluorescence and metabolic activity decreased to a larger extent when cells were exposed to UV-B than in treatments where UV-B was excluded. In contrast, the cell size was larger under the treatment including UV-A+UV-B than under the treatment including only UV-A. These results show that UV-B damage can decrease growth and metabolic activity in N. atomus without altering the synchronization of the diel patterns, and contribute to a better understanding of phytoplankton behavior under UVR exposures. C1 CSIC, Inst Ciencias Marinas Andalucia, Cadiz 11510, Spain. RP Sobrino, C (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM sobrinoc@si.edu RI Sobrino, Cristina/J-3534-2012; LUBIAN, LUIS/L-7241-2014; OI Sobrino, Cristina/0000-0003-0431-1220; Montero, Olimpio/0000-0002-0241-8756 NR 21 TC 7 Z9 8 U1 0 U2 9 PU INTER-RESEARCH PI OLDENDORF LUHE PA NORDBUNTE 23, D-21385 OLDENDORF LUHE, GERMANY SN 0171-8630 J9 MAR ECOL PROG SER JI Mar. Ecol.-Prog. Ser. PY 2005 VL 293 BP 29 EP 35 DI 10.3354/meps293029 PG 7 WC Ecology; Marine & Freshwater Biology; Oceanography SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Oceanography GA 943WY UT WOS:000230387400003 ER PT J AU Collin, R McLellan, M Gruber, K Bailey-Jourdain, C AF Collin, R McLellan, M Gruber, K Bailey-Jourdain, C TI Effects of conspecific associations on size at sex change in three species of calyptraeid gastropods SO MARINE ECOLOGY PROGRESS SERIES LA English DT Article DE protandry; Crepidula spp; size advantage; Bostrycapulus calyptreaformis ID CORAL-INHABITING SNAIL; SOCIAL-CONTROL; THALASSOMA-BIFASCIATUM; BLUEHEAD WRASSE; BODY-SIZE; CREPIDULA; HERMAPHRODITE; REPRODUCTION; ALLOCATION; EVOLUTION AB In marine molluscs, sex change is often labile and is thought to be largely influenced by interactions with conspecifics. Previous studies of calyptraeid gastropods concluded that their social environment influences the timing of protandrous sex change. We conducted field surveys and laboratory experiments to examine the effects of conspecifics on size at sex change in 3 Panamanian calyptraeids. Crepidula cf. onyx, C. incurva Broderip, 1834 and Bostrycapulus calyptraeformis (Des-hayes, 1830) vary in densities, sex ratio and mode of development, which suggests that they might respond to associations with conspecifics in different ways. However, our laboratory experiments showed that the response to interactions with conspecifics is generally similar. In all 3 species, individuals raised in isolation pass through a male phase and males raised alone change sex at the same size as males raised with another male. Both C. cf. onyx and C. incurva change sex at a larger size when kept with a female than when kept alone or with another male. The differences in size at sex change between the treatments is small and the treatment effect explains more of the variation in size at sex change in C. cf. onyx, the more solitary species, than in C. incurva, a species that is usually found in pairs. In all species, individuals with high initial growth rates change sex sooner and at a smaller size than those with slower initial growth rates. Growth rates increase significantly during sex change in C. cf. onyx and C. incurva but not in B. calyptraeformis. C1 Smithsonian Trop Res Inst, Balboa, Panama. Univ Minnesota, Bell Museum Nat Hist, St Paul, MN 55108 USA. Univ Minnesota, Dept Ecol Evolut & Behav, St Paul, MN 55108 USA. RP Collin, R (reprint author), Smithsonian Trop Res Inst, Apartado Postal 0843-03092, Balboa, Panama. EM collinr@naos.si.edu RI Collin, Rachel/G-2001-2010 NR 35 TC 28 Z9 29 U1 0 U2 2 PU INTER-RESEARCH PI OLDENDORF LUHE PA NORDBUNTE 23, D-21385 OLDENDORF LUHE, GERMANY SN 0171-8630 J9 MAR ECOL PROG SER JI Mar. Ecol.-Prog. Ser. PY 2005 VL 293 BP 89 EP 97 DI 10.3354/meps293089 PG 9 WC Ecology; Marine & Freshwater Biology; Oceanography SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Oceanography GA 943WY UT WOS:000230387400009 ER PT J AU Rohde, K MacKenzie, K Hayward, C Torchin, ME Kuris, AM Bray, RA AF Rohde, Klaus MacKenzie, Ken Hayward, Craig Torchin, Mark E. Kuris, Armand M. Bray, Rodney A. BE Rohde, K TI Zoogeography SO MARINE PARASITOLOGY LA English DT Article; Book Chapter AB The geographical distribution of marine parasites has not been well studied and is largely, although not entirely, limited to some aspects of the zoogeography of parasites of marine fishes. Some effort has gone into studying latitudinal, longitudinal and depth gradients of fish parasites. Interestingly, ectoparasites and endoparasites of marine fishes show different latitudinal patterns. Whereas the relative species richness (number of parasite species per host species) increases markedly from high to low latitudes for ectoparasites, this is not the case for endoparasites. The latter also show greatest diversity in the tropics, but this is entirely due to an increased diversity of host species at low latitudes. Thorson's rule, which states that benthic marine invertebrates tend to produce large numbers of small pelagic larvae in warm waters, but small numbers of large offspring by various mechanisms at high latitudes, applies to monogenean gill parasites of marine fishes. Furthermore, host ranges (but not host specificity) are greater for digeneans at high than at low latitudes, whereas monogeneans do not show differences between latitudes. Concerning longitudinal gradients, a study of scombrid ectoparasites has shown that there is a primary centre of diversity in South-East Asian waters, and a secondary one in the Caribbean, with diversity decreasing with distance from these centres. Concerning gradients with depth, relative species diversity of monogeneans is several times greater in surface than in deep waters off eastern Australia. Parasites can be used to study host populations and their migration, not only of marine fish but also of various invertebrates. Such parasite tags are much cheaper than other methods, such as comparative genetic studies, as discussed (on pages 351-355). The section discusses general methodology, selection criteria for tag parasites and application of the method to different host groups. Parasites also are useful for making inferences about long-term historical dispersal. The relevant section describes the only two examples studied (i.e. that of scombrid dispersal with emphasis on the role of oceanic barriers, and that on the historical migrations of Indo-Pacific whiting, Sillaginidae). The section on introduced marine parasites addresses a very important problem (i.e. that of the many parasites introduced into new regions, where they have become important pests). It also discusses the use of deliberately introduced parasites to control introduced free-living pest species, such as crabs or echinoderms. The Chapter concludes with a concise discussion of deep-sea parasites. Very little is known about the diversity and distribution of free-living deep-sea organisms (probably more than 99% of invertebrates have not yet been described), and deep-sea parasites have been studied even less. They are of great importance, considering the huge spaces of the deep-seas, and the many species of fish and invertebrates found there. C1 [Rohde, Klaus] Univ New England, Sch Environm Sci & Resources Management, Armidale, NSW 2351, Australia. [MacKenzie, Ken] Univ Aberdeen, Dept Zool, Sch Biol Sci, Aberdeen AB24 2TZ, Scotland. [Hayward, Craig] Univ Tasmania, Sch Aquaculture & Aquafin CRC, Port Lincoln, SA 5606, Australia. [Torchin, Mark E.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Kuris, Armand M.] Univ Calif Santa Barbara, Dept Ecol Evolut & Marine Biol, Santa Barbara, CA 93106 USA. [Kuris, Armand M.] Univ Calif Santa Barbara, Coll Creat Studies, Santa Barbara, CA 93106 USA. [Bray, Rodney A.] Nat Hist Museum, Dept Zool, London SW7 5BD, England. RP Rohde, K (reprint author), Univ New England, Sch Environm Sci & Resources Management, Armidale, NSW 2351, Australia. EM krohde@metz.une.edu.au; k.mackenzie@abdn.ac.uk; craig.hayward@utas.edu.au; torchinm@si.edu; kuris@lifesci.ucsb.edu; rab@nhm.ac.uk; krohde@metz.une.edu.au NR 0 TC 5 Z9 5 U1 2 U2 4 PU CSIRO PUBLISHING PI COLLINGWOOD PA 150 OXFORD STREET, PO BOX 1139, COLLINGWOOD, VIC 3066, AUSTRALIA BN 978-0-643-09307-2 PY 2005 BP 347 EP 369 PG 23 WC Marine & Freshwater Biology; Parasitology SC Marine & Freshwater Biology; Parasitology GA BVM07 UT WOS:000291853200010 ER PT S AU Mecklenburg, MF Tumosa, CS Erhardt, D AF Mecklenburg, MF Tumosa, CS Erhardt, D BE Vandiver, PB Mass, JL Murray, A TI The changing mechanical properties of aging oil paints SO MATERIALS ISSUES IN ART AND ARCHAEOLOGY VII SE Materials Research Society Symposium Proceedings LA English DT Proceedings Paper CT 7th Symposium on Materials Issues in Art and Archaeology, held at the 2004 MRS Fall Meeting CY NOV 30-DEC 03, 2004 CL Boston, MA SP Mat Res Soc ID DRYING OILS; LIPIDS AB The stiffening and embrittlement of oil paints over time has been a real concern for those responsible for the long term care and preservation of paintings. This paper examines the effects of time, pigments, relative humidity (RH), temperature and solvents on the mechanical properties of traditional oil paints. In this way it is possible to determine the role of each factor in causing the paints to become brittle. Even after 14 years the oil paints show little evidence that the long term "maturing" processes have begun to slow down. It is shown that there seems to be little correlation between the time paint requires to "dry-to-the-touch" and the longer term mechanical properties. Both low and high temperature levels can increase the stiffness of the paints though the mechanisms are quite different. Considerable hydrolysis of the paints occurs early in their history and the ones that hydrolyze most quickly are the ones that remain the most flexible. C1 Smithsonian Ctr Mat Res & Educ, Suitland, MD 20746 USA. NR 14 TC 7 Z9 7 U1 1 U2 6 PU MATERIALS RESEARCH SOC PI WARRENDALE PA 506 KEYSTONE DRIVE, WARRENDALE, PA 15088-7563 USA SN 0272-9172 BN 1-55899-800-4 J9 MATER RES SOC SYMP P PY 2005 VL 852 BP 13 EP 24 PG 12 WC Archaeology; Art; Chemistry, Applied; Materials Science, Multidisciplinary; Physics, Applied SC Archaeology; Art; Chemistry; Materials Science; Physics GA BDH94 UT WOS:000233592800002 ER PT S AU Tumosa, CS Erhardt, D Mecklenburg, MF Su, XF AF Tumosa, CS Erhardt, D Mecklenburg, MF Su, XF BE Vandiver, PB Mass, JL Murray, A TI Linseed oil paint as ionomer: Synthesis and characterization SO Materials Issues in Art and Archaeology VII SE MATERIALS RESEARCH SOCIETY SYMPOSIUM PROCEEDINGS LA English DT Proceedings Paper CT 7th Symposium on Materials Issues in Art and Archaeology, held at the 2004 MRS Fall Meeting CY NOV 30-DEC 03, 2004 CL Boston, MA SP Mat Res Soc ID LIPIDS AB As linseed oil ages, hydrolysis and oxidation produce acid groups on the polymer chain that may lead to ionomeric behavior. The effect of these changes is difficult to determine in old paints because of the lack of records of environmental and treatment histories that can alter the physical properties significantly. A series of paints were made that have chemical properties similar to those of aged paints and that mimic old paints. Their properties seem to show flexibility as well as coherency but low strength and a high susceptibility to solvents. C1 Smithsonian Ctr Mat Res & Educ, Suitland, MD 20746 USA. NR 18 TC 3 Z9 3 U1 0 U2 1 PU MATERIALS RESEARCH SOCIETY PI WARRENDALE PA 506 KEYSTONE DRIVE, WARRENDALE, PA 15088-7563 USA SN 0272-9172 BN 1-55899-800-4 J9 MATER RES SOC SYMP P PY 2005 VL 852 BP 25 EP 31 PG 7 WC Archaeology; Art; Chemistry, Applied; Materials Science, Multidisciplinary; Physics, Applied SC Archaeology; Art; Chemistry; Materials Science; Physics GA BDH94 UT WOS:000233592800003 ER PT S AU Dussubieux, L AF Dussubieux, L BE Vandiver, PB Mass, JL Murray, A TI Using ICP-MS to detect inorganic elements in organic materials: A new tool to identify mordants or dyes on ancient textiles SO Materials Issues in Art and Archaeology VII SE MATERIALS RESEARCH SOCIETY SYMPOSIUM PROCEEDINGS LA English DT Proceedings Paper CT 7th Symposium on Materials Issues in Art and Archaeology, held at the 2004 MRS Fall Meeting CY NOV 30-DEC 03, 2004 CL Boston, MA SP Mat Res Soc AB The feasibility of determining metallic elements used as mordants or dyes with inorganic constituents was tested using inductively coupled plasma - mass spectrometry (ICP-MS). For this purpose, modern, historic and archaeological samples were investigated. Mordants containing copper, iron, tin, aluminium or uranium were successfully identified as well as an organic dye with a substitutional bromine. C1 Smithsonian Ctr Mat Res & Educ, Museum Support Ctr, Suitland, MD 20746 USA. NR 3 TC 2 Z9 2 U1 0 U2 1 PU MATERIALS RESEARCH SOCIETY PI WARRENDALE PA 506 KEYSTONE DRIVE, WARRENDALE, PA 15088-7563 USA SN 0272-9172 BN 1-55899-800-4 J9 MATER RES SOC SYMP P PY 2005 VL 852 BP 291 EP 296 PG 6 WC Archaeology; Art; Chemistry, Applied; Materials Science, Multidisciplinary; Physics, Applied SC Archaeology; Art; Chemistry; Materials Science; Physics GA BDH94 UT WOS:000233592800032 ER PT J AU French, BM AF French, BM TI William L. Quaide, 1927-2004 - Memorial SO METEORITICS & PLANETARY SCIENCE LA English DT Biographical-Item C1 Natl Museum Nat Hist, Smithsonian Inst, Dept Paleobiol, Washington, DC 20013 USA. RP French, BM (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Dept Paleobiol, POB 37012,Room E-210,MRC 01321, Washington, DC 20013 USA. NR 1 TC 0 Z9 0 U1 1 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 JAN PY 2005 VL 40 IS 1 BP 139 EP 141 PG 3 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 913XW UT WOS:000228189900008 ER PT S AU Aranda-Gomez, JJ Housh, TB Luhr, JF Henry, CD Becker, T Chavez-Cabello, G AF Jorge Aranda-Gomez, Jose Housh, Todd B. Luhr, James F. Henry, Christopher D. Becker, Tim Chavez-Cabello, Gabriel BE Anderson, TH Nourse, JA McKee, JW Steiner, MB TI Reactivation of the San Marcos fault during mid-to-late Tertiary extension, Chihuahua, Mexico SO MOJAVE-SONORA MEGASHEAR HYPOTHESIS: DEVELOPMENT, ASSESSMENT, AND ALTERNATIVES SE Geological Society of America Special Papers LA English DT Article; Book Chapter DE Basin and Range; transtension; transpression; intraplate volcanism ID NORTHEASTERN MEXICO; RANGE PROVINCE; BASIN; EVOLUTION; COAHUILA; HISTORY; STRESS; FOLDS AB The San Marcos fault is a >300-km-long, WNW- to NW-trending structure that has been repeatedly reactivated during Mesozoic and Tertiary pulses of deformation. The San Marcos fault has previously been demonstrated to extend across Coahuila in a trend roughly parallel to the proposed Mojave-Sonora megashear. Exposures in this broad region are dominated by Mesozoic marine sedimentary rocks. Northwest of the border between Coahuila and Chihuahua a thick cover of Tertiary volcanic rocks masks the fault trace. We believe that the San Marcos fault trace projects across the eastern branch of the Bolson de Mapim, a major Basin and Range structure, into the northern portion of the Sierra del Diablo and into the central part of the Pliocene-Quaternary Camargo volcanic field ((40)Ar/(39)Ar ages are 4.7-0.09 Ma). In the same area, upper Tertiary normal faults that bound both branches of the Bolson de Mapim show a marked change in orientation. South of the projected San Marcos fault the extensional structures strike similar to north-south. Northwest of the San Marcos fault, a conspicuous northwest-trending graben ( ca. 4.7-2.1 Ma) crosses the Camargo volcanic field. A lineament identified in digital elevation models suggests that the San Marcos fault extends beneath the Camargo volcanic field, passes west of Sierra Aguachile, and can be traced at least an additional 300 km to the northwest, which effectively doubles the known or inferred length of the San Marcos fault. Mid-Tertiary volcanic rocks (ca. 32-14 Ma) are folded into NNW-trending, SSE-plunging synclines in areas immediately northwest and southeast of the Camargo volcanic field. A short distance (similar to 5 km) west of Sierra El Morrion in central Chihuahua another NNW-trending syncline, observable in satellite images and in regional geologic and topographic maps, is developed in mid-Tertiary volcanic rocks. Miocene folding in the volcanic sequence at Pena Blanca has been reported in the literature near the NNW projection of the San Marcos fault. The central graben of the Camargo volcanic field, the upper Tertiary synclines, and the abrupt change in trend of the Tertiary normal faults are all closely associated with a distinct bend in the San Marcos fault, marking a change in trend from WNW to NW. The Camargo volcanic field central graben and the adjacent synclines were developed in the same northwest-trending segment of the fault. We interpret the central graben of the Camargo volcanic field as a pull-apart basin, whereas the synclines were formed in areas where a small left-lateral component in the fault movement produced shortening. We believe this deformation was accomplished in at least two pulses of late Tertiary extension. An older event that occurred between ca. 14 Ma and 5 Ma produced the left-lateral movement and associated folding. This pulse corresponds to a short episode of regional northwestern extension documented in northern Mexico and the southern United States. The younger event (<= 5 Ma) was in part synchronous with the activity in the Camargo volcanic field and was caused by NE to ENE extension. C1 [Jorge Aranda-Gomez, Jose] Inst Potosino Invest Cient & Tecnol AC, Dept Geol Econ, San Luis Potosi 78216, Mexico. [Housh, Todd B.] Univ Texas Austin, Dept Geol Sci, Austin, TX 78712 USA. [Luhr, James F.] Smithsonian Inst, Dept Mineral Sci, Washington, DC 20013 USA. [Henry, Christopher D.] Univ Nevada, Nevada Bur Mines & Geol, Reno, NV 89557 USA. [Becker, Tim] Berkeley Geochronol Ctr, Berkeley, CA 94709 USA. [Chavez-Cabello, Gabriel] Univ Nacl Autonoma Mexico, Ctr Geociencias, Queretaro 76001, Mexico. RP Aranda-Gomez, JJ (reprint author), Inst Potosino Invest Cient & Tecnol AC, Dept Geol Econ, POB 3-74, San Luis Potosi 78216, Mexico. EM jaranda@ipicyt.edu.mx NR 40 TC 9 Z9 10 U1 0 U2 0 PU GEOLOGICAL SOC AMER INC PI BOULDER PA 3300 PENROSE PL, PO BOX 9140, BOULDER, CO 80301 USA SN 0072-1077 BN 978-0-8137-2393-8 J9 GEOL SOC AM SPEC PAP PY 2005 VL 393 BP 509 EP 521 DI 10.1130/2005.2393(19) PG 13 WC Geochemistry & Geophysics; Geology SC Geochemistry & Geophysics; Geology GA BLY07 UT WOS:000271390400020 ER PT J AU Leonard, JA Vila, C Wayne, RK AF Leonard, JA Vila, C Wayne, RK TI Legacy lost: genetic variability and population size of extirpated US grey wolves (Canis lupus) SO MOLECULAR ECOLOGY LA English DT Article DE ancient DNA; genetic diversity; glacial refugia; Mexican wolves; mitochondrial DNA; predator control ID COYOTE MITOCHONDRIAL-DNA; MICROSATELLITE LOCI; GRAY WOLF; QUATERNARY; HYBRIDIZATION; BOTTLENECK AB By the mid 20th century, the grey wolf (Canis lupus) was exterminated from most of the conterminous United States (cUS) and Mexico. However, because wolves disperse over long distances, extant populations in Canada and Alaska might have retained a substantial proportion of the genetic diversity once found in the cUS. We analysed mitochondrial DNA sequences of 34 pre-extermination wolves and found that they had more than twice the diversity of their modern conspecifics, implying a historic population size of several hundred thousand wolves in the western cUS and Mexico. Further, two-thirds of the haplotypes found in the historic sample are unique. Sequences from Mexican grey wolves (C. l. baileyi) and some historic grey wolves defined a unique southern clade supporting a much wider geographical mandate for the reintroduction of Mexican wolves than currently planned. Our results highlight the genetic consequences of population extinction within Ice Age refugia and imply that restoration goals for grey wolves in the western cUS include far less area and target vastly lower population sizes than existed historically. C1 Uppsala Univ, Dept Evolutionary Biol, S-75236 Uppsala, Sweden. Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA 90095 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Zool, Genet Program, Washington, DC 20008 USA. RP Leonard, JA (reprint author), Uppsala Univ, Dept Evolutionary Biol, S-75236 Uppsala, Sweden. EM Jennifer.Leonard@ebc.uu.se RI Vila, Carles/H-4893-2013; Leonard, Jennifer/A-7894-2010 OI Vila, Carles/0000-0002-4206-5246; Leonard, Jennifer/0000-0003-0291-7819 NR 42 TC 106 Z9 113 U1 20 U2 83 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0962-1083 J9 MOL ECOL JI Mol. Ecol. PD JAN PY 2005 VL 14 IS 1 BP 9 EP 17 DI 10.1111/j.1365-294X.2004.02389.x PG 9 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 889CL UT WOS:000226421000002 PM 15643947 ER PT J AU Duda, TF Rolan, E AF Duda, TF Rolan, E TI Explosive radiation of Cape Verde Conus, a marine species flock SO MOLECULAR ECOLOGY LA English DT Article DE Cape Verde; Conus; endemic; marine; phylogeny; species flock ID SUBSTITUTION; FISHES; ISLANDS; MODEL AB Nearly 50 species of the marine gastropod genus Conus are restricted to the Cape Verde archipelago. This unusual concentration of endemics within a single set of oceanic islands is extremely uncharacteristic of marine taxa. Here we used phylogenetic analyses of 90 Conus species, including 30 endemics from Cape Verde, to reveal the relationships and origins of the endemic Cape Verde Conus. Results show that these species group in two distinct clades and represent a marine species flock that is restricted to a very narrowly confined geographical area. Species' originations occurred in exceptionally limited parts of the archipelago and in some cases radiations took place solely within single islands. Finally, comparison of levels of divergence between Cape Verde endemics and other Conus species suggests that the radiation of Conus in Cape Verde occurred during the last few million years. C1 Smithsonian Trop Res Inst, Naos Marine Lab, Balboa, Panama. Univ Washington, Dept Biol, Seattle, WA 98195 USA. Museo Hist Nat, Santiago De Compostela 15782, Spain. RP Duda, TF (reprint author), Smithsonian Trop Res Inst, Naos Marine Lab, Apartado 2072, Balboa, Panama. EM tfduda@umich.edu NR 41 TC 41 Z9 42 U1 1 U2 5 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0962-1083 J9 MOL ECOL JI Mol. Ecol. PD JAN PY 2005 VL 14 IS 1 BP 267 EP 272 DI 10.1111/j.1365-294X.2004.02397.x PG 6 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 889CL UT WOS:000226421000024 PM 15643969 ER PT S AU Eggert, LS Maldonado, JE Fleischer, RC AF Eggert, LS Maldonado, JE Fleischer, RC BE Zimmer, EA Roalson, EH TI Nucleic acid isolation from ecological samples - Animal scat and other associated materials SO MOLECULAR EVOLUTION: PRODUCING THE BIOCHEMICAL DATA, PART B SE Methods in Enzymology LA English DT Review; Book Chapter ID ESTIMATING POPULATION-SIZE; POLYMERASE-CHAIN-REACTION; BEARS URSUS-ARCTOS; FECAL DNA; MITOCHONDRIAL-DNA; MOLECULAR ANALYSIS; BROWN BEARS; PRESERVATION METHODS; PCR AMPLIFICATION; HAIR CAPTURE AB Noninvasive sampling is very attractive to field biologists and has tremendous potential for studying secretive species and being a cost-effective method of increasing sample sizes in studies of large, dangerous animals. Extracting DNA from noninvasively collected samples can be challenging, and the methods have been developed mainly through modification of previously developed protocols for other sample types. We present the most commonly used methods along with modifications used by some researchers to deal with the problem of coextraction of polymerase chain reaction (PCR) inhibitors. Although it is difficult to generalize about which methods should be used on particular sample types, we discuss the success of the methods in studies to date. We close with general suggestions for dealing with potential problems associated with the analysis of DNA obtained from noninvasively collected samples. C1 Smithsonian Inst, Natl Museum Nat Hist, Genet Program, Dept Systemat Biol, Washington, DC 20008 USA. Smithsonian Inst, Natl Museum Nat Hist, Genet Program, Dept Systemat Biol, Washington, DC 20008 USA. RP Eggert, LS (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Genet Program, Dept Systemat Biol, Washington, DC 20008 USA. NR 64 TC 38 Z9 42 U1 2 U2 22 PU ELSEVIER ACADEMIC PRESS INC PI SAN DIEGO PA 525 B STREET, SUITE 1900, SAN DIEGO, CA 92101-4495 USA SN 0076-6879 BN 0-12-182800-X J9 METHOD ENZYMOL JI Methods Enzymol. PY 2005 VL 395 BP 73 EP 87 DI 10.1016/S0076-6879(05)95006-4 PG 15 WC Biochemical Research Methods; Biochemistry & Molecular Biology SC Biochemistry & Molecular Biology GA BCM61 UT WOS:000230001100006 PM 15865962 ER PT J AU Soria, R Cropper, M Pakull, M Mushotzky, R Wu, K AF Soria, R Cropper, M Pakull, M Mushotzky, R Wu, K TI The star-forming environment of an ultraluminous X-ray source in NGC 4559: an optical study SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Review DE accretion, accretion discs; black hole physics; galaxies : individual : NGC 4559; X-rays : galaxies; X-rays : stars ID ANTENNAE GALAXIES NGC-4038/4039; HUBBLE-SPACE-TELESCOPE; INITIAL MASS FUNCTION; HIGH-VELOCITY CLOUDS; BLACK-HOLE BINARIES; EQUATION-OF-STATE; H-ALPHA EMISSION; CHANDRA OBSERVATIONS; PHOTOMETRIC SYSTEMS; IRREGULAR GALAXIES AB We have studied the candidate optical counterparts and the stellar population in the star-forming complex around the bright ultraluminous X-ray source (ULX) in the western part of the spiral galaxy NGC 4559, using the HST Wide Field Planetary Camera 2 (WFPC2), XMM-Newton/Optical Monitor and ground-based data. We find that the ULX is located near a small group of OB stars, but is not associated with any massive young clusters nor with any extraordinary massive stars. The brightest point source in the Chandra error circle is consistent with a single blue supergiant (BSG) of mass approximate to20 M(circle dot) and age approximate to10 Myr. A few other stars are resolved inside the error circle: mostly BSGs and red supergiants (RSGs) with inferred masses approximate to10-15 M(circle dot) and ages approximate to20 Myr. This is consistent with the interpretation of this ULX as a black hole (BH) accreting from a high-mass donor star in its supergiant phase, with mass transfer occurring via Roche-lobe overflow. The observed optical colours and the blue-to-red supergiant ratio suggest a low metal abundance for the stellar population: 0.2 less than or similar toZ/Z(circle dot)less than or similar to 0.4 (using the Padua tracks), or 0.05 less than or similar toZ/Z(circle dot)less than or similar to 0.2 (using the Geneva tracks). The age of the star-forming complex is less than or similar to30 Myr. Halpha images show that this star-forming region has a ring-like appearance. We propose that it is an expanding wave of star formation, triggered by an initial density perturbation, in a region where the gas was only marginally stable to gravitational collapse. We also suggest that the most likely trigger was a collision with a satellite dwarf galaxy going through the gas-rich outer disc of NGC 4559 less than 30 Myr ago. The culprit could be the dwarf galaxy visible a few arcsec north-west of the complex. If this is the case, this system is a scaled-down version of the Cartwheel galaxy. The X-ray data favour a BH more massive (M > 50 M(circle dot)) than typical Milky Way BH candidates. The optical data favour a young BH originating in the recent episode of massive star formation; however, they also rule out an association with young massive star clusters (none are present in the X7 field). We speculate that other mechanisms may lead to the formation of relatively massive BHs (perhaps Msimilar to 50-100 M(circle dot)) from stellar evolution processes in low-metallicity environments, or when star formation is triggered by galactic collisions. C1 UCL, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Observ Strasbourg, F-67000 Strasbourg, France. NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. RP Soria, R (reprint author), UCL, Mullard Space Sci Lab, Holmbury St Mary, Dorking RH5 6NT, Surrey, England. EM Roberto.Soria@mssl.ucl.ac.uk RI Cropper, Mark/C-1574-2008 NR 130 TC 63 Z9 63 U1 0 U2 2 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 JAN 1 PY 2005 VL 356 IS 1 BP 12 EP 28 DI 10.1111/j.1365-2966.2004.08438.x PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 879WG UT WOS:000225749300002 ER PT J AU Weil, SE AF Weil, SE TI A success/failure matrix for museums SO MUSEUM NEWS LA English DT Article C1 Smithsonian Ctr Educ & Museum Studies, Washington, DC USA. RP Weil, SE (reprint author), Smithsonian Ctr Educ & Museum Studies, Washington, DC USA. NR 9 TC 3 Z9 3 U1 0 U2 2 PU AMER ASSOC MUSEUMS PI WASHINGTON PA 1575 EYE ST, NW, STE 400, WASHINGTON, DC 20005 USA SN 0027-4089 J9 MUSEUM NEWS JI Mus. News PD JAN-FEB PY 2005 VL 84 IS 1 BP 36 EP 40 PG 5 WC Art SC Art GA 059FN UT WOS:000238718800014 ER PT J AU DePriest, PT Sikaroodi, M Lawrey, JD Diederich, P AF DePriest, PT Sikaroodi, M Lawrey, JD Diederich, P TI Marchandiomyces lignicola sp nov shows recent and repeated transition between a lignicolous and a lichenicolous habit SO MYCOLOGICAL RESEARCH LA English DT Article ID RIBOSOMAL-RNA GENES; SACCHAROMYCES CEREVISIAE; FUNGI; SYMBIOSES; BASIDIOMYCOTA; SEQUENCE; HOBSONIA AB The anamorphic basidiomycete genus Marchandiomyces presently includes two common lichenicolous (lichen-inhabiting) species, M. corallinus and M. aurantiacus (teleomorph Marchandiobasiditan aurantiacum). We describe here a new species, M. lignicola sp. nov., that is similar to M. corallinus in the colour of its sclerotia, but differs in having a wood-inhabiting (lignicolous) habit. The phylogenetic position of this lignicolous fungus was compared with the lichenicolous species of Marchandiomyces and related species currently placed in the basidiomycetous families Corticiaceae and Ceratobasidiaceae using parsimony, likelihood, and Bayesian analyses of complete sequences of the nuclear small subunit and internal transcribed spacers ribosomal DNA, and a portion of the nuclear large subunit ribosomal DNA. These DNA sequences were obtained from isolated cultures of freshly collected specimens. Significant Bayesian posterior probabilities, as well as maximum likelihood and parsimony analyses, indicate that the new lignicolous species is closely related to M. corallinus, the type species of Marchandiomyces. In most analyses these two species are monophyletic with the lichenicolous M. aurantiacus, although this relationship is not strongly supported. Since M. lignicola is more closely related to M. corallinus than to M. aurantiacus, either a transition to the lignicolous habit occurred recently within an ancestral lichenicolous group or, more likely, transition to the lichenicolous habit arose recently and in parallel from an ancestral lignicolous habit. C1 Smithsonian Inst, Natl Museum Nat Hist, US Natl Herbarium, Bot Sect, Washington, DC 20013 USA. George Mason Univ, Dept Environm Sci & Policy, Fairfax, VA 22030 USA. George Mason Univ, Dept Environm Sci & Policy, Fairfax, VA 22030 USA. Musee Natl Hist Nat, L-2160 Luxembourg, Luxembourg. RP DePriest, PT (reprint author), Smithsonian Inst, Natl Museum Nat Hist, US Natl Herbarium, Bot Sect, POB 37012, Washington, DC 20013 USA. EM depriest.paula@nmnh.si.edu RI DePriest, Paula/K-6633-2015 NR 29 TC 6 Z9 6 U1 1 U2 2 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 40 WEST 20TH ST, NEW YORK, NY 10011-4211 USA SN 0953-7562 J9 MYCOL RES JI Mycol. Res. PD JAN PY 2005 VL 109 BP 57 EP 70 DI 10.1017/S0953756204001601 PN 1 PG 14 WC Mycology SC Mycology GA 903JE UT WOS:000227421200005 PM 15736863 ER PT B AU Hartmann, L AF Hartmann, L BE Ignace, R Gayley, KG TI Accretion disks of young stars SO Nature and Evolution of Disks Around Hot Stars SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Meeting on the Nature and Evolution of Disks Around Hot Stars CY JUL 07-09, 2004 CL Johnson City, TN ID T-TAURI STARS; HERBIG-AE/BE STARS; MAGNETOSPHERIC ACCRETION; LAYERED ACCRETION; STELLAR OBJECTS; MASSIVE STARS; AB AURIGAE; INSTABILITY; FLOWS; PHOTOEVAPORATION AB Some of the properties of disks around pre-main sequence stars are discussed, along with our (limited) theoretical understanding of the physical processes involved, and some applications to disks around higher-mass (young) stars are suggested, along with many open questions. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Hartmann, L (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 46 TC 9 Z9 9 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-203-2 J9 ASTR SOC P PY 2005 VL 337 BP 3 EP 14 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BDN82 UT WOS:000234511900001 ER PT B AU Fazio, GG AF Fazio, GG BE Shapiro, MM Stanev, T Wefel, JP TI Recent results from the Spitzer Space Telescope: A new view of the infrared universe SO Neutrinos and Explosive Events in the Universe SE NATO SCIENCE SERIES, SERIES II: MATHEMATICS, PHYSICS AND CHEMISTRY LA English DT Proceedings Paper CT Conference of the NATO-Advanced-Study-Institute on Neutrinos and Explosive Events in the Universe CY JUL 02-13, 2004 CL Erice, ITALY SP NATO Study Inst DE infrared; galaxy classification; interstellar dust; star formation; interacting galaxies; active galactic nuclei; planetary nebula ID ARRAY CAMERA IRAC; EARLY-TYPE GALAXIES; YOUNG STELLAR CLUSTER; INTERSTELLAR DUST; ELLIPTIC GALAXIES; ANTENNAE GALAXIES; STAR-FORMATION; II EMISSION; MICRON; GAS AB The Spitzer Space Telescope, NASA's Great Observatory for infrared exploration, was launched on August 25, 2003, and is returning excellent scientific data. Combining the intrinsic sensitivity obtained with a cooled telescope in space and the imaging and spectroscopic power of modern array detectors, huge gains have been achieved in exploring the infrared universe. This paper describes the Spitzer Space Mescope and its focal-plane instruments and summarizes some of the spectacular images and new scientific results that have been obtained. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Fazio, GG (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 41 TC 3 Z9 3 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS BN 1-4020-3746-5 J9 NATO SCI SER II MATH PY 2005 VL 209 BP 47 EP 71 DI 10.1007/1-4020-3748-1_3 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BDT15 UT WOS:000235192500003 ER PT B AU DeVorkin, D AF DeVorkin, D BE Orchiston, W TI SAO during the Whipple years: The origins of project celescope SO New Astronomy: Opening the Electromagnetic Window and Expanding our View of Planet Earth: A MEETING TO HONOR WOODY SULLIVAN ON HIS 60TH BIRTHDAY SE ASTROPHYSICS AND SPACE SCIENCE LIBRARY LA English DT Proceedings Paper CT Woodfest Meeting on Astrobiology, History of Astronomy and Sundials held in Honor of Woody Sullivan on his 60th Birthday CY JUN 16-18, 2004 CL Seattle, WA SP UW Kammeyer Fund DE Smithsonian Institution; Fred Whipple; NASA; Project Celescope; Smithsonian Astrophysical Observatory; Harvard College Observatory; space science AB In 1955, the moribund Astrophysical Observatory of the Smithsonian Institution closed its doors on the south lawn of the Smithsonian Castle. Vestiges of its 60-year old legacy of monitoring solar radiation were transferred to Cambridge under a new name, the Smithsonian Astrophysical Observatory, and became housed within the Harvard College Observatory complex under the direction of Fred Whipple. Whipple, restarting the SAO almost from scratch, worked within the Smithsonian's ancient tradition of maintaining a world-wide network of solar observation stations by morphing it into a similar network of satellite tracking facilities for the IGY, quickly and quietly phasing out the solar work. Under the SAO name, however, Whipple did much more, vastly expanding his interests in meteor research and hyperballistic studies, deftly orchestrated to parallel his tracking facility empire which in time included aeroballistic studies, atomic time standards, and other associated technological and scientific campaigns. He also made sure SAO played a prominent role in NASA's emerging 'observatory class' series of scientific satellites and used it to create a theoretical astrophysics unit. It is this last activity that we will introduce here, showing how Project Celescope fitted into Whipple's plan for SAO, and how it contributed to make the combined Harvard-Smithsonian Center for Astrophysics the largest astronomical organization on the planet by the 1970s. C1 Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA. NR 30 TC 1 Z9 1 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS BN 1-4020-3723-6 J9 ASTROPHYS SPACE SC L PY 2005 VL 334 BP 229 EP 250 PG 22 WC Astronomy & Astrophysics; History & Philosophy Of Science SC Astronomy & Astrophysics; History & Philosophy of Science GA BDP58 UT WOS:000234789700014 ER PT B AU Brashear, R AF Brashear, R BE Orchiston, W TI The transits of venus and new technologies: A time to reflect SO New Astronomy: Opening the Electromagnetic Window and Expanding our View of Planet Earth: A MEETING TO HONOR WOODY SULLIVAN ON HIS 60TH BIRTHDAY SE ASTROPHYSICS AND SPACE SCIENCE LIBRARY LA English DT Proceedings Paper CT Woodfest Meeting on Astrobiology, History of Astronomy and Sundials held in Honor of Woody Sullivan on his 60th Birthday CY JUN 16-18, 2004 CL Seattle, WA SP UW Kammeyer Fund DE transits of Venus; new astronomies; Kepler; Laplace; Langley; Keeler AB in the recent history of astronomy there have been occasions where 'New Astronomies' have been introduced. In the spirit of the recent excitement of the 2004 transit of Venus, I have used the periods around the historical transits to reflect on the 'New Astronomies' of those eras. Johannes Kepler's Astronomia Nova is a fine representation of the New Astronomy of the 163 11639 transit pair and Pierre Simon, Marquis de Laplace's Traite de Mecanique Celeste reflects the New Astronomy of the 1761-1769 transit pair. A combination of Samuel P. Langley's The New Astronomy and James E. Keeler's 1897 paper on astrophysics have been chosen as the exemplars of the New Astronomy of the 1874-1882 transit pair. I am open to suggestions for the works that best represent the 2004-2012 transit pairs. C1 Smithsonian Inst Libs, Dibner Lib, Washington, DC 20013 USA. NR 12 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS BN 1-4020-3723-6 J9 ASTROPHYS SPACE SC L PY 2005 VL 334 BP 251 EP 260 PG 10 WC Astronomy & Astrophysics; History & Philosophy Of Science SC Astronomy & Astrophysics; History & Philosophy of Science GA BDP58 UT WOS:000234789700015 ER PT S AU Remo, JL AF Remo, JL BE Belbruno, E TI NEO impact projections SO NEW TRENDS IN ASTRODYNAMICS AND APPLICATIONS SE ANNALS OF THE NEW YORK ACADEMY OF SCIENCES LA English DT Article; Proceedings Paper CT Conference on New Trends in Astrodynamics and Applications II CY JUN 03-05, 2005 CL Princeton Univ, Princeton, NJ SP NASA Headquarters, Aviat Week & Space Technol Magazine, Wilmer Cutler Pickering Hale Dorr LLP, Natl Space Soc, NY City Chapter HO Princeton Univ DE near-Earth object; impact projection ID HAZARD MITIGATION AB The concept of a near-Earth object (NEO) impact projection metric (PM) based on the ratio of the observation time to the impact time, p(t), for a projected NEO impact is developed. The PM can assist NEO mitigation decision-making that is based on the discontinuously changing cumulative impact probability and help mitigate false alarms of NEO impact with Earth that have undermined public perception toward the veracity of predicting NEO threats. C1 Harvard Smithsonian Ctr Astrophys, Dept Solar Stellar & Planetary Sci, Cambridge, MA 02138 USA. Harvard Univ, Cambridge, MA 02138 USA. Sandia Natl Labs, Albuquerque, NM 87185 USA. RP Remo, JL (reprint author), Harvard Smithsonian Ctr Astrophys, Dept Solar Stellar & Planetary Sci, 60 Garden St, Cambridge, MA 02138 USA. EM jremo@cfa.harvard.edu NR 10 TC 1 Z9 1 U1 0 U2 2 PU NEW YORK ACAD SCIENCES PI NEW YORK PA 2 EAST 63RD ST, NEW YORK, NY 10021 USA SN 0077-8923 BN 1-57331-630-X J9 ANN NY ACAD SCI JI Ann.NY Acad.Sci. PY 2005 VL 1065 BP 285 EP 295 DI 10.1196/annals.1370.010 PG 11 WC Engineering, Aerospace; Mechanics; Multidisciplinary Sciences SC Engineering; Mechanics; Science & Technology - Other Topics GA BEC73 UT WOS:000236816300017 PM 16510415 ER PT J AU Hosaka, N Gomez, S Kachi, N Stuefer, JF Whigham, DF AF Hosaka, N Gomez, S Kachi, N Stuefer, JF Whigham, DF TI The ecological significance of clonal growth in the understory tree, pawpaw (Asimina triloba) SO NORTHEASTERN NATURALIST LA English DT Article ID FAGUS-GRANDIFOLIA; RAMET DEMOGRAPHY; WOODY-PLANTS; FOREST; SHRUB; DYNAMICS; STANDS; REGENERATION; DISTURBANCE; ASPEN AB We evaluated three possible functions of clonal growth related to genet persistence in the root-suckering understory tree pawpaw, Asimina triloba (L.) Dunal: (1) risk spreading through multiplication of stems, (2) enhanced establishment and survival of new stems, and (3) horizontal expansion growth of patches. The number, diameter growth, and spatial distribution of annual stem recruits were examined over three years in a natural population of pawpaw. The rate of stem recruitment was consistently higher than stem mortality. We found no difference in stem turnover rate for patches of different size, indicating that stem production is more than high enough to avoid patch extinction. Although newly formed stems were considerably smaller than previously established stems, they grew and survived as well as established stems. We found no evidence for clonal growth contributing to extensive horizontal expansion of patches. Our results suggest that ensuring survivorship of new stems is the main ecological role of clonal growth in pawpaw. C1 Tokyo Metropolitan Univ, Tokyo 1920397, Japan. Radbond Univ Nijmegen, NL-6525 ED Nijmegen, Netherlands. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Hosaka, N (reprint author), Tokyo Metropolitan Univ, Minami Osawa 1-1, Tokyo 1920397, Japan. EM nhosaka@comp.metro-u.ac.jp OI Stuefer, Josef/0000-0001-8740-9762; Whigham, Dennis/0000-0003-1488-820X NR 36 TC 7 Z9 8 U1 9 U2 14 PU HUMBOLDT FIELD RESEARCH INST PI STEUBEN PA PO BOX 9, STEUBEN, ME 04680-0009 USA SN 1092-6194 J9 NORTHEAST NAT JI Northeast. Nat PY 2005 VL 12 IS 1 BP 11 EP 22 DI 10.1656/1092-6194(2005)012[0011:TESOCG]2.0.CO;2 PG 12 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 917TQ UT WOS:000228492500002 ER PT J AU Clark, JL Skog, LE Salinas, I AF Clark, JL Skog, LE Salinas, I TI Novae gesneriaceae neotroplearum XIV: Four new species of Alloplectus from South America SO NOVON LA English DT Article DE Alloplectus; Colombia; Ecuador; Gesneriaceae; Peru AB A monographic revision of Alloplectus (Gesneriaceae) has revealed four species new to science from Colombia, Ecuador. and Peru. These species are described here and include A. carpishensis from Peru, A. inflatus from Colombia., A. serpens from Colombia and Ecuador, and A. oblongical yx from Colombia and Ecuador. C1 George Washington Univ, Dept Biol Sci, Washington, DC 20052 USA. Natl Museum Nat Hist, Smithsonian Inst, Dept Bot, Washington, DC 20013 USA. Museum Nat Hist, Div Bot, Lima, Peru. RP Clark, JL (reprint author), George Washington Univ, Dept Biol Sci, 2023 G St,NW, Washington, DC 20052 USA. EM clarkjo@si.edu; skogl@sl.edu; i_sa_hi@yahoo.com NR 6 TC 0 Z9 1 U1 0 U2 0 PU MISSOURI BOTANICAL GARDEN PI ST LOUIS PA 2345 TOWER GROVE AVENUE, ST LOUIS, MO 63110 USA SN 1055-3177 J9 NOVON JI Novon PY 2005 VL 15 IS 1 BP 70 EP 79 PG 10 WC Plant Sciences SC Plant Sciences GA 923EN UT WOS:000228892100007 ER PT J AU Faden, RB Cameron, DM AF Faden, RB Cameron, DM TI Cyanoiis repens (Commelinaceae): A new species from tropical Africa SO NOVON LA English DT Article DE Commelinaceae; Cyanotis; tropical Africa AB Cyanotis repens, a mat-forming perennial, is described from Kenya in tropical Africa. It differs from related species by its prostrate habit, indeterminate flowering shoots, and fusiform swelling terminating the style. Two subspecies are recognized, diploid C. repens subsp. repens from Kenya, Tanzania, and Uganda, and polyploid C. repens subsp. robusta from Kenya. Tanzania, Uganda. Rwanda, Democratic Republic of Congo, and Gabon. Cyanotis repens belongs to the Cyanotis foecunda species group, the species of which have a basic chromosome number of x = 13 and often distinctive karyotypes. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA. Pepperdine Univ, Div Nat Sci, Malibu, CA 90263 USA. RP Faden, RB (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, MRC-166,POB 37012, Washington, DC 20013 USA. EM faden.robert@nmnh.si.edu; David.Cameron@pepperdine.edu NR 12 TC 0 Z9 0 U1 1 U2 1 PU MISSOURI BOTANICAL GARDEN PI ST LOUIS PA 2345 TOWER GROVE AVENUE, ST LOUIS, MO 63110 USA SN 1055-3177 J9 NOVON JI Novon PY 2005 VL 15 IS 1 BP 110 EP 116 PG 7 WC Plant Sciences SC Plant Sciences GA 923EN UT WOS:000228892100011 ER PT J AU Strong, MT AF Strong, MT TI Two new species of Rhynchospora sect. Tenues (Cyperaceae) from the Guianas, South America SO NOVON LA English DT Article DE Cyperaceae; French Guiana; Guianas; Rhynchospora sect. Tenues; South America; Surinam AB Two flew species are described (R. cordatachenia and R. saxisavannicola) in Rhynchospora sect. Tenues Kukenthal from northeastern South America (Guianas). A key to the species of R. sect. Tenues in the Guianas is given, and illustrations are provided for the new species. C1 Smithsonian Inst, Dept Bot, MRC 166, Washington, DC 20013 USA. RP Strong, MT (reprint author), Smithsonian Inst, Dept Bot, MRC 166, POB 37012, Washington, DC 20013 USA. EM strongm@si.edu NR 9 TC 0 Z9 0 U1 0 U2 0 PU MISSOURI BOTANICAL GARDEN PI ST LOUIS PA 2345 TOWER GROVE AVENUE, ST LOUIS, MO 63110 USA SN 1055-3177 J9 NOVON JI Novon PY 2005 VL 15 IS 3 BP 479 EP 483 PG 5 WC Plant Sciences SC Plant Sciences GA 970HD UT WOS:000232295000021 ER PT S AU Erb, AS van der Heijden, A AF Erb, Amy S. van der Heijden, Anna TI The STAR program: An innovative approach to teaching the scientific method to high school students SO OCEANS 2005, VOLS 1-3 SE OCEANS-IEEE LA English DT Proceedings Paper CT Oceans 2005 Conference CY SEP 17-23, 2005 CL Washington, DC SP IEEE C1 Smithsonian Environm Res Ctr, Dept Educ, Edgewater, MD 21037 USA. RP Erb, AS (reprint author), Smithsonian Environm Res Ctr, Dept Educ, 647 Contees Wharf Rd, Edgewater, MD 21037 USA. EM erba@si.edu NR 0 TC 0 Z9 0 U1 0 U2 1 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 0197-7385 BN 0-933957-34-3 J9 OCEANS-IEEE PY 2005 BP 549 EP 554 PG 6 WC Engineering, Ocean; Oceanography SC Engineering; Oceanography GA BEQ88 UT WOS:000238978700087 ER PT S AU Lang, MA AF Lang, Michael A. TI Smithsonian Institution coral reef research SO OCEANS 2005, VOLS 1-3 SE OCEANS-IEEE LA English DT Proceedings Paper CT Oceans 2005 Conference CY SEP 17-23, 2005 CL Washington, DC SP IEEE AB Through the Caribbean Coral Reef Ecosystems program in Belize and the Smithsonian Marine Station in Florida we are involved in systematic studies of marine organisms. STRI coral reef studies have revealed that marine tropical environments contain 4-5 times more species on average than has been generally realized and that the diversity of Caribbean reefs is an order of magnitude greater than previously assumed. SERC scientists are investigating the biocomplexity of mangroves, systems that are integrally linked to coral reefs. Perhaps the most dramatic revelation of long-term major reef changes was the 95% demise of the long-spined sea urchin (Diadem population throughout the western Atlantic. The sea urchin saga demonstrates how even extraordinarily abundant organisms are potentially vulnerable to rapid elimination by diseases that combine the lethality of Ebola with the contagion of the common cold. Mass spawning events, in which hundreds of organisms release eggs and sperm simultaneously, have been documented in Panamanian corals. Many green seaweeds also spawn in synchrony just before sunrise. The Smithsonian seeks to guide the conservation and management of coral reef re sources by making research results available through the scientific literature, by sharing information gained from documentation of its millions of collections, and by active collaborative work with conservation organizations and other government agencies. C1 Smithsonian Inst, Off Secretary Sci, Washington, DC 20013 USA. RP Lang, MA (reprint author), Smithsonian Inst, Off Secretary Sci, POB 37012, Washington, DC 20013 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 0197-7385 BN 0-933957-34-3 J9 OCEANS-IEEE PY 2005 BP 2850 EP 2852 PG 3 WC Engineering, Ocean; Oceanography SC Engineering; Oceanography GA BEQ88 UT WOS:000238978702165 ER PT S AU Lang, MA Hines, AH AF Lang, Michael A. Hines, Anson H. TI Smithsonian Institution Marine Science Network SO OCEANS 2005, VOLS 1-3 SE OCEANS-IEEE LA English DT Proceedings Paper CT Oceans 2005 Conference CY SEP 17-23, 2005 CL Washington, DC SP IEEE ID MASS MORTALITY AB The Smithsonian Marine Science Network (MSN) operates a unique array of laboratories and research vessels that spans the latitudinal gradient of the western Atlantic (Chesapeake Bay, Indian River Lagoon, Meso-American Barrier Reel) and crosses the isthmus of Panama. The Network is dedicated to understanding the rich biodiversity and complex ecosystem dynamics that sustain coastal processes and productivity. We study evolutionary, ecological, and environmental change in the ocean's coastal zones, increasing scientific knowledge of these environments and improving society's appreciation of the ocean's effect on our lives. Coastal environments are of immense economic and environmental importance and comprise 95% of the ocean's fisheries. Our coastal communities are the most densely populated and fastest growing areas in the U.S. The Network ensures integrated support of "Discovering and Understanding Life's Diversity," a core Smithsonian scientific mission. MSN goals are to ensure that the whole of the integrated Network is larger than the sum of its parts leading to enhanced productivity through: collaborative and comparative research, marine infrastructure development and supports professional training and outreach, and effective allocation of resources. C1 Smithsonian Inst, Off Secretary Sci, Washington, DC 20013 USA. RP Lang, MA (reprint author), Smithsonian Inst, Off Secretary Sci, POB 37012, Washington, DC 20013 USA. NR 14 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 0197-7385 BN 0-933957-34-3 J9 OCEANS-IEEE PY 2005 BP 2853 EP 2859 PG 7 WC Engineering, Ocean; Oceanography SC Engineering; Oceanography GA BEQ88 UT WOS:000238978702166 ER PT J AU Marra, PP Francis, CM Mulvihill, RS Moore, FR AF Marra, PP Francis, CM Mulvihill, RS Moore, FR TI The influence of climate on the timing and rate of spring bird migration SO OECOLOGIA LA English DT Article DE climate change; migratory birds; phenology; temperature; timing of migration ID EGG-LAYING TRENDS; GULF-OF-MEXICO; FAT DEPOSITION; GREEN-WAVE; WARBLERS; PHENOLOGY; STOPOVER; ARRIVAL; RESPONSES; PATTERNS AB Ecological processes are changing in response to climatic warming. Birds, in particular, have been documented to arrive and breed earlier in spring and this has been attributed to elevated spring temperatures. It is not clear, however, how long-distance migratory birds that overwinter thousands of kilometers to the south in the tropics cue into changes in temperature or plant phenology on northern breeding areas. We explored the relationships between the timing and rate of spring migration of long-distance migratory birds, and variables such as temperature, the North Atlantic Oscillation (NAO) and plant phenology, using mist net capture data from three ringing stations in North America over a 40-year period. Mean April/May temperatures in eastern North America varied over a 5degreesC range., but with no significant trend during this period. Similarly, we found few significant trends toward earlier median capture dates of birds. Median capture dates were not related to the NAO, but were inversely correlated to spring temperatures for almost all species. For every 1degreesC increase in spring temperature, median capture dates of migratory birds averaged, across species, one day earlier. Lilac (Syringa vulgaris) budburst. however, averaged 3 days earlier for every 1degreesC increase in spring temperature, suggesting that the impact of temperature on plant phenology is three times greater than on bird phenology. To address whether migratory birds adjust their rate of northward migration to changes in temperature.. we compared median capture dates for 15 species between a ringing station on the Gulf Coast of Louisiana in the southern USA with two stations approximately 2,500 km to the north. The interval between median capture dates in Louisiana and at the other two ringing stations was inversely correlated with temperature, with an average interval of 22 days, that decreased by 0.8 days per PC increase in temperature. Our results suggest that, although the onset of migration may be determined endogenously, the timing of migration is flexible and can be adjusted in response to variation in weather and/or phenology along migration routes. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Bird Studies Canada, Port Rowan, ON N0E 1M0, Canada. Carnegie Museum Nat Hist, Powdermill Nat Reserve, Rector, PA 15677 USA. Univ So Mississippi, Dept Biol Sci, Hattiesburg, MS 39406 USA. RP Marra, PP (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM marrap@si.edu NR 60 TC 187 Z9 197 U1 18 U2 139 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013 USA SN 0029-8549 J9 OECOLOGIA JI Oecologia PD JAN PY 2005 VL 142 IS 2 BP 307 EP 315 DI 10.1007/s00442-004-1725-x PG 9 WC Ecology SC Environmental Sciences & Ecology GA 887DH UT WOS:000226285000016 PM 15480801 ER PT S AU Cosmo, ML DeLuca, EE Golub, L Austin, GK Chappell, JH Barbera, M Bookbinder, JA Cheimets, PN Cirtain, J Podgorski, WA Davis, W Varisco, S Weber, MA AF Cosmo, Mario L. DeLuca, Edward E. Golub, Leon Austin, Gerald K. Chappell, Jon H. Barbera, Marco Bookbinder, Jay A. Cheimets, Peter N. Cirtain, Jonathan Podgorski, William A. Davis, William Varisco, Salvatore Weber, Mark A. BE Citterio, O ODell, SL TI The Calibration of the Solar-B X-ray Optics SO OPTICS FOR EUV, X-RAY, AND GAMMA-RAY ASTRONOMY II SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on Optics for EUV, X-Ray and Gamma-Ray Astronomy II CY AUG 03, 2005 CL San Diego, CA DE X-ray optics; solar astronomy; optical testing AB The Solar-B X-ray telescope (XRT) is a grazing-incidence modified Wolter I X-ray telescope, of 35 cm inner diameter and 2.7 m focal length. XRT, designed for full sun imaging over the wavelength 6-60 Angstroms, will be the highest resolution solar X-Ray telescope ever flown. Images will be recorded by a 2048 X 2048 back-illuminated CCD with 13.5 mu m pixels (1 arc-sec/pixel) with full sun field of view. XRT will have a wide temperature sensitivity in order to observe and discriminate both the high (5-10 MK) and low temperature (1-5 MK) phenomena in the coronal plasma. This paper presents preliminary results of the XRT mirror calibration performed at the X-ray Calibration Facility, NASA-MSFC, Huntsville, Alabama during January and February 2005. We discuss the methods and the most significant results of the XRT mirror performance, namely: characteristics of the point response function (PSF), the encircled energy and the effective area. The mirror FWHM is 0.8 '' when corrected for 1-g, finite source distance, and CCD pixelization. With the above corrections the encircled energy at 27 mu m and 1keV is 52%. The effective area is greater than 2cm(2) at 0.5keV and greater than 1.7cm(2) at 1.0keV. C1 [Cosmo, Mario L.; DeLuca, Edward E.; Golub, Leon; Austin, Gerald K.; Chappell, Jon H.; Bookbinder, Jay A.; Cheimets, Peter N.; Cirtain, Jonathan; Podgorski, William A.; Davis, William; Weber, Mark A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Cosmo, ML (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mcosmo@cfa.harvard.edu RI DeLuca, Edward/L-7534-2013; OI DeLuca, Edward/0000-0001-7416-2895; Barbera, Marco/0000-0002-3188-7420 NR 7 TC 0 Z9 0 U1 0 U2 1 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 978-0-8194-5905-3 J9 PROC SPIE PY 2005 VL 5900 AR 59000E DI 10.1117/12.618822 PG 7 WC Astronomy & Astrophysics; Optics SC Astronomy & Astrophysics; Optics GA BRX39 UT WOS:000283844000013 ER PT S AU Gorenstein, P Phillips, JD Reasenberg, RD AF Gorenstein, P. Phillips, J. D. Reasenberg, R. D. BE Citterio, O ODell, SL TI Refractive/diffractive telescope with very high angular resolution for X-ray astronomy SO OPTICS FOR EUV, X-RAY, AND GAMMA-RAY ASTRONOMY II SE Proceedings of SPIE-The International Society for Optical Engineering LA English DT Proceedings Paper CT Conference on Optics for EUV, X-Ray and Gamma-Ray Astronomy II CY AUG 03, 2005 CL San Diego, CA DE X-ray telescopes; X-ray astronomy; diffractive optics; formation flying AB The 0.5 arcsec angular resolution of the Chandra X-Ray Observatory is likely to be the best that a grazing incidence telescope with substantial collecting area will ever attain. We describe a concept for a telescope composed of diffractive and refractive components that transmit rather than reflect X-rays. Therefore, its angular resolution would be relatively insensitive to figure errors and surface roughness. With appropriately selected values for the two focal lengths the chromatic aberration that is inherent in both the diffractive and refractive components individually would compensate each other within a limited but not insignificant energy band. The system has a focal length of about 104 km because the refractive component is rather weak. The long focal length requires a very demanding type of formation flying between an optics spacecraft and a detector spacecraft. We simulate the simplest diffractive/refractive imaging system where chromatic aberration is corrected to first order at 6 keV. The angular resolution is expected to be better than a miliarcsec within a 10 % bandwidth. The energy band could be broadened either by employing an array of smaller systems with the same total area or by modifying the diffractive component in situ. The components are lightweight, not difficult to fabricate and can probably be made in a machine shop. We also consider possible sites for the system. C1 [Gorenstein, P.; Phillips, J. D.; Reasenberg, R. D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Gorenstein, P (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM pgorenstein@cfa.harvard.edu NR 6 TC 1 Z9 1 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 978-0-8194-5905-3 J9 P SOC PHOTO-OPT INS PY 2005 VL 5900 DI 10.1117/12.620144 PG 8 WC Astronomy & Astrophysics; Optics SC Astronomy & Astrophysics; Optics GA BRX39 UT WOS:000283844000041 ER PT S AU Reid, PB Glenn, P Bookbinder, J AF Reid, Paul B. Glenn, Paul Bookbinder, Jay BE Citterio, O ODell, SL TI Optical Design and Requirements for the Normal Incidence X-ray Telescope of the Reconnection and Microscale Solar Probe SO OPTICS FOR EUV, X-RAY, AND GAMMA-RAY ASTRONOMY II SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on Optics for EUV, X-Ray and Gamma-Ray Astronomy II CY AUG 03, 2005 CL San Diego, CA DE x-ray optics; normal incidence optics; EUV imaging; Sun; corona AB One of the key instruments on the Reconnection and Microscale (RAM) Solar-Terrestrial Probe mission is a normal incidence multilayer x-ray telescope designed to provide 10 milli-arc-sec imaging of the solar corona. To achieve this level of imaging it will be necessary to fabricate meter-class reflective optics with diffraction limited performance at 193 Angstroms. Because of the use of multilayer optics, surface micro-roughness must also be maintained at very low levels (a few Angstroms rms) to maintain good reflectance. To ease fabrication constraints and the sometimes competing requirements of micro-roughness and figure, we have explored a number of potential designs and fabrication approaches for RAM. Figure error budgets and optical designs are shown, demonstrating that RAM can be built with existing mirror fabrication technology. C1 [Reid, Paul B.; Bookbinder, Jay] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Reid, PB (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM preid@cfa.harvard.edu NR 5 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 978-0-8194-5905-3 J9 PROC SPIE PY 2005 VL 5900 AR 59000K DI 10.1117/12.613951 PG 8 WC Astronomy & Astrophysics; Optics SC Astronomy & Astrophysics; Optics GA BRX39 UT WOS:000283844000018 ER PT S AU Reid, PB Garcia, M Stewart, J AF Reid, Paul B. Garcia, Michael Stewart, Jeffrey BE Citterio, O ODell, SL TI Stray Light Shielding for Formation Flying X-ray Telescopes SO OPTICS FOR EUV, X-RAY, AND GAMMA-RAY ASTRONOMY II SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on Optics for EUV, X-Ray and Gamma-Ray Astronomy II CY AUG 03, 2005 CL San Diego, CA DE x-ray optics; straylight; baffling; Con-X; formation flying ID CONSTELLATION-X; XEUS MISSION AB Recent studies and planning for a variety of x-ray astronomy missions (Constellation-X, XEUS, Generation-X) have driven astronomers to explore grazing incidence telescopes with focal lengths of 50 m or greater. One approach to implementing such long focal lengths is to employ formation flying: separate optic and detector spacecraft travel in formation. Formation flying removes the "telescope tube" which was an integral part of shielding the telescope from straylight. We consider the implications of formation flying with respect to straylight, and discuss some design guidelines for baffling the straylight. The Constellation-X mission is used as an example. C1 [Reid, Paul B.; Garcia, Michael] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Reid, PB (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM preid@cfa.harvard.edu NR 9 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 978-0-8194-5905-3 J9 PROC SPIE PY 2005 VL 5900 AR 59000L DI 10.1117/12.613945 PG 14 WC Astronomy & Astrophysics; Optics SC Astronomy & Astrophysics; Optics GA BRX39 UT WOS:000283844000019 ER PT S AU Romaine, S Basso, S Bruni, RJ Burkert, W Citterio, O Conti, G Engelhaupt, D Freyberg, M Ghigo, M Gorenstein, P Gubarev, M Hartner, G Mazzoleni, F O'Dell, S Pareschi, G Ramsey, BD Speegle, C Spiga, D AF Romaine, S. Basso, S. Bruni, R. J. Burkert, W. Citterio, O. Conti, G. Engelhaupt, D. Freyberg, M. Ghigo, M. Gorenstein, P. Gubarev, M. Hartner, G. Mazzoleni, F. O'Dell, S. Pareschi, G. Ramsey, B. D. Speegle, C. Spiga, D. BE Citterio, O ODell, SL TI Development of a Prototype Nickel Optic for the Constellation-X Hard X-Ray Telescope: III SO OPTICS FOR EUV, X-RAY, AND GAMMA-RAY ASTRONOMY II SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on Optics for EUV, X-Ray and Gamma-Ray Astronomy II CY AUG 03, 2005 CL San Diego, CA DE X-ray Telescopes; X-ray optics; multilayers; electroformed optics ID MISSION; MIRRORS AB The Constellation-X (Con-X) mission(1) planned for launch in 2015, will feature an array of Hard X-ray telescopes (HXT) with a total collecting area greater than 1500 cm(2) at 40 keV. Two technologies are being investigated for the optics of these telescopes, including multilayer coated Electroformed-Nickel-Replicated (ENR) shells. The attraction of the ENR process is that the resulting full-shell optics are inherently stable and offer the prospect of better angular resolution which results in lower background and higher instrument sensitivity. We are building a prototype HXT mirror module using an ENR process to fabricate the individual shells. This prototype consists of 5 shells with diameters ranging from 150 mm to 280 mm with a length of 426 mm. The innermost of these will be coated with iridium, while the remainder will be coated with graded d-spaced W/Si multilayers. Parts I and II of this work were presented at the SPIE meetings in 2003 and 2004. This paper presents a progress update and focuses on accomplishments during this past year. In particular, we will present results from full illumination X-ray tests of multilayer coated shells, taken at the MPE-Panter X-ray facility. C1 [Romaine, S.; Bruni, R. J.; Gorenstein, P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Romaine, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM sromaine@cfa.harvard.edu OI Spiga, Daniele/0000-0003-1163-7843; O'Dell, Stephen/0000-0002-1868-8056; Ghigo, Mauro/0000-0003-2284-9251; Pareschi, Giovanni/0000-0003-3967-403X NR 13 TC 3 Z9 3 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 978-0-8194-5905-3 J9 PROC SPIE PY 2005 VL 5900 AR 59000S DI 10.1117/12.620438 PG 7 WC Astronomy & Astrophysics; Optics SC Astronomy & Astrophysics; Optics GA BRX39 UT WOS:000283844000026 ER PT S AU Vadawale, SV Hong, J Grindlay, JE Skinner, G AF Vadawale, S. V. Hong, J. Grindlay, J. E. Skinner, G. BE Citterio, O ODell, SL TI Monte-Carlo simulations of the expected imaging performance of the EXIST high-energy telescope SO OPTICS FOR EUV, X-RAY, AND GAMMA-RAY ASTRONOMY II SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on Optics for EUV, X-Ray and Gamma-Ray Astronomy II CY AUG 03, 2005 CL San Diego, CA DE Coded aperture imaging; EXIST; Monte-Carlo simulations ID UNIFORMLY REDUNDANT ARRAYS; MISSION AB EXIST is being studied as the Black Hole Finder Probe, one of the 3 Einstein Probe missions under NASA's Beyond Einstein program. The major science goals for EXIST include highly sensitive full-sky hard X-ray survey in a very wide energy band of 5 - 600 keV. The scientific requirements of wide energy band (10-600 keV for the High Energy Telescope considered for EXIST) and large field of view (approximately 130 degrees x 60 degrees in the current design, incorporating an array of 18 contiguous very large area coded aperture telescopes) presents significant imaging challenges. The requirement of achieving high imaging sensitivity puts stringent limits on the uniformity and knowledge of systematics for the detector plane. In order to accomplish the ambitious scientific requirements of EXIST, it is necessary to implement many novel techniques. Here we present the initial results of our extensive Monte-Carlo simulations of coded mask imaging for EXIST to estimate the performance degradation due to various factors affecting the imaging such as the non-ideal detector plane and bright partially coded sources. C1 [Vadawale, S. V.; Hong, J.; Grindlay, J. E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Vadawale, SV (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM svadawale@cfa.harvard.edu NR 12 TC 1 Z9 1 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 978-0-8194-5905-3 J9 PROC SPIE PY 2005 VL 5900 AR 590014 DI 10.1117/12.617671 PG 12 WC Astronomy & Astrophysics; Optics SC Astronomy & Astrophysics; Optics GA BRX39 UT WOS:000283844000038 ER PT J AU Olson, SL Irestedt, M Ericson, PGP Fjeldsa, J AF Olson, SL Irestedt, M Ericson, PGP Fjeldsa, J TI Independent evolution of two Darwinian marsh-dwelling ovenbirds (Furnariidae : Limnornis, Limnoctites) SO ORNITOLOGIA NEOTROPICAL LA English DT Article DE Furnariidae; Limnoctites; Limnornis; molecular systematics; nidification; ovenbirds ID BIRDS; PASSERIFORMES; INFERENCE; MRBAYES AB The Curve-billed Reedhaunter (Limnornis curvirostris) and the Straight-billed Reedhaunter (Limnoctites redirostris) are marsh-dwelling ovenbirds that were first collected by Charles Darwin in Uruguay. Each has a limited distribution in southernmost Brazil, Uruguay, and northern Argentina, within which the birds occupy very distinct habitats. Originally described as congeners because of overall similarity of plumage, the two species have been treated as close relatives through most of their history despite obvious structural differences. We analyzed DNA sequences from three different genes of these species, comparing them with a wide variety of other species of Furnariidae and several outgroup taxa. Limnoctites rectirostris belongs among the species traditionally placed in Cranioleuca, being most closely related to the marsh-dwelling Sulphur-throated Spinetail (C. sulphurifera) among the species we sampled. This is supported by vocalizations and nidification. Limnornis curvirostris forms a clade with the Wren-Eke Rushbird (Phleocryptes melanops), with the Sharp-tailed Streamcreeper (Lochmias nematura) as a rather distant sister-taxon. A close relationship between Limnornis and Phleocryptes is supported by the apparently unique nest architecture and blue-green egg color. C1 Smithsonian Inst, Div Birds, Natl Museum Nat Hist, Washington, DC 20013 USA. Swedish Museum Nat Hist, Dept Vertebrate Zool, SE-10405 Stockholm, Sweden. Swedish Museum Nat Hist, Mol Systemat Lab, SE-10405 Stockholm, Sweden. Stockholm Univ, Dept Zool, SE-10691 Stockholm, Sweden. Univ Copenhagen, Vertebrate Dept, Museum Zool, DK-2100 Copenhagen, Denmark. RP Olson, SL (reprint author), Smithsonian Inst, Div Birds, Natl Museum Nat Hist, POB 37012, Washington, DC 20013 USA. EM olsons@si.edu; martin.irestedt@nrm.se; per.edcson@nrm.se; jfjeldsaa@zmuc.ku.dk RI Fjeldsa, Jon/A-9699-2013; Research, NRM-BIG/F-2603-2013 OI Fjeldsa, Jon/0000-0003-0790-3600; NR 47 TC 9 Z9 11 U1 0 U2 3 PU NEOTROPICAL ORNITHOLOGICAL SOCIETY, USGS PATUXENT WILDLIFE RESEARCH CENTER PI ATHENS PA UNIVERSITY OF GEORGIA, WARNELL SCHOOL OF FOREST RESOURCES, ATHENS, GA USA SN 1075-4377 J9 ORNITOL NEOTROP JI ORNITOL. NEOTROP. PY 2005 VL 16 IS 3 BP 347 EP 359 PG 13 WC Ornithology SC Zoology GA 966JW UT WOS:000232017000005 ER PT J AU Stutchbury, BJM Woolfenden, BE Fedy, BC Morton, ES AF Stutchbury, BJM Woolfenden, BE Fedy, BC Morton, ES TI Nonbreeding territorial behavior of two congeneric antbirds, Chestnut-backed Antbird (Myrmeciza exsul) and White-bellied Antbird (M-longipes) SO ORNITOLOGIA NEOTROPICAL LA English DT Article DE territory defense; radiotelemetry; foraging; duetting; song; off-territory forays; Chestnut-backed Antbird; white-bellied Antbird; Myrmeciza exsul; Myrmeciza longipes ID TROPICAL PASSERINE; PANAMA AB We used radiotelemetry during the nonbreeding (dry) season to systematically compare the short-term movements, singing and territorial behavior of two antbirds that have a similar ecology but occupy different habitats. Both species are paired and territorial year round, but the White-bellied Antbird (Myrmeciza longipes) is common in second growth and edge habitat, while the Chestnut-backed Antbird (M. exsul) is found in mature forest. Although White-bellied Antbirds made off-territory forays during the dry season, we did not detect any off-territory forays in Chestnut-backed Antbirds. White-bellied Antbirds sang more and covered less area of their territories per hour (0.01 ha) compared with Chestnut-backed Antbirds (0.16 ha). Mated White-bellied antbirds often foraged < 5 m from each other and duetting occurred regularly, though at low frequency for most pairs. In Chestnut-backed Antbirds, pairs foraged farther apart and were often separated by over 20 m. Female Chestnut-backed Antbirds only occasionally sang and, when they did, it was immediately after their mate's song. We discuss whether these differences in territorial behavior and singing reflect greater food stability, and hence greater territorial stability, in the forest-dwelling Chestnut-backed Antbird. C1 Univ York, Dept Biol, Toronto, ON M3J 1P3, Canada. Univ British Columbia, Forest Sci Ctr, Ctr Appl Conservat Res, Vancouver, BC V6T 1Z4, Canada. Smithsonian Inst, Conservat & Res Ctr, Front Royal, VA 22630 USA. RP Stutchbury, BJM (reprint author), Univ York, Dept Biol, Toronto, ON M3J 1P3, Canada. EM bstutch@yorku.ca OI Fedy, Bradley/0000-0003-3933-4043 NR 14 TC 11 Z9 11 U1 0 U2 3 PU NEOTROPICAL ORNITHOLOGICAL SOCIETY, USGS PATUXENT WILDLIFE RESEARCH CENTER PI ATHENS PA UNIVERSITY OF GEORGIA, WARNELL SCHOOL OF FOREST RESOURCES, ATHENS, GA USA SN 1075-4377 J9 ORNITOL NEOTROP JI ORNITOL. NEOTROP. PY 2005 VL 16 IS 3 BP 397 EP 404 PG 8 WC Ornithology SC Zoology GA 966JW UT WOS:000232017000009 ER PT J AU Renner, SC AF Renner, SC TI The Mountain Guan (Penelopina nigra) in the Sierra Yalijux, Guatemala SO ORNITOLOGIA NEOTROPICAL LA English DT Article DE conservation; Guatemala; Mountain Guan; Penelopina Nigra; tropical montane cloud forest; habitat use ID CONSERVATION; BIODIVERSITY; MEXICO; BIRDS AB The Mountain Guan (Penelopina nigra) is restricted in distribution to the Central American Highlands (above 900 m). The species occurs from the southern Mexican states of Chiapas and Oaxaca to northern Nicaragua, but the largest populations are assumed to survive in Guatemala. Listed as a "Lower risk/near threatened species" (A1 cd + 2c) and in CITES Appendix 1, the Mountain Guan apparently is dependent for survival on primary cloud forest. A population of Mountain Guans in the northernmost Guatemalan mountain range (Chelemha, Sierra Yalijux, Alta Verapaz) was studied from March to July 2002 to analyze the species' habitat preferences. Most observations (81.6%) were made in primary forest areas. All juveniles were raised within the forest boundaries. I also observed successful breeding and followed at least two juveniles until the end of the study in September 2002. C1 Smithsonian Inst, Conservat & Res Ctr, Front Royal, VA 22630 USA. RP Renner, SC (reprint author), Smithsonian Inst, Conservat & Res Ctr, 1500 Remount Rd, Front Royal, VA 22630 USA. EM renners@crc.si.edu RI Renner, Swen/J-3502-2014 OI Renner, Swen/0000-0002-6893-4219 NR 35 TC 2 Z9 2 U1 0 U2 0 PU NEOTROPICAL ORNITHOLOGICAL SOCIETY, USGS PATUXENT WILDLIFE RESEARCH CENTER PI ATHENS PA UNIVERSITY OF GEORGIA, WARNELL SCHOOL OF FOREST RESOURCES, ATHENS, GA USA SN 1075-4377 J9 ORNITOL NEOTROP JI ORNITOL. NEOTROP. PY 2005 VL 16 IS 3 BP 419 EP 426 PG 8 WC Ornithology SC Zoology GA 966JW UT WOS:000232017000011 ER PT J AU Behrensmeyer, AK Barry, JC AF Behrensmeyer, AK Barry, JC TI Biostratigraphic surveys in the Siwaliks of Pakistan: A method for standardized surface sampling of the vertebrate fossil record SO PALAEONTOLOGIA ELECTRONICA LA English DT Article DE Siwaliks; Pakistan; Miocene; taphonomy; biostratigraphy; sampling methods; paleoecology ID NORTHERN PAKISTAN; DEPOSITS; MIOCENE; TAPHONOMY AB Much of the vertebrate fossil record consists of fragmentary specimens that are widely dispersed across eroding outcrops. This paper describes a method of standardized surface surveying that samples fragmentary surface fossil assemblages for information relating to biostratigraphy, taphonomy, and paleoecology that is not usually available from more traditional approaches to paleontological collecting. Biostratigraphic surveys have been used in the Miocene Siwalik sequence of northern Pakistan since 1979 to better define important faunal appearance and extinction events and to learn more about the taphonomy and overall productivity of the highly fossiliferous fluvial deposits. The surveys record all bones encountered during walking transects in specified stratigraphic intervals, which are well exposed and delimited by strike valleys between tilted sandstones. High quality or informative specimens are collected, and dense patches of fossils are designated as formal localities and treated separately. The resulting survey data permits analysis through time of variables such as fossil productivity per search hour, proportions of different skeletal parts and vertebrate groups, and ratios of abundant mammal families such as Equidae and Bovidae, as well as tests for correlations between these and other variables. Biostratigraphic survey data compliment other types of paleontological information about faunal evolution in the Siwalik sequence and provide new insights on biotic versus environmental correlates of changes in the abundances of particular groups through time. The methodology can be adapted and used for other fossiliferous sequences throughout the vertebrate record. C1 Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. Smithsonian Inst, Washington, DC 20013 USA. Harvard Univ, Peabody Museum, Cambridge, MA 02138 USA. RP Behrensmeyer, AK (reprint author), Natl Museum Nat Hist, Dept Paleobiol, MRC 121,POB 37012, Washington, DC 20013 USA. EM behrensa@si.edu; jcbarry@fas.harvard.edu NR 31 TC 2 Z9 2 U1 0 U2 0 PU COQUINA PRESS PI AMHERST PA C/O WHITEY HAGADORN, EXECUTIVE EDITOR, AMHERST COLLEGE, DEPT GEOLOGY, AMHERST, MA 01002 USA SN 1094-8074 J9 PALAEONTOL ELECTRON JI Palaeontol. electron. PY 2005 VL 8 IS 1 AR 13A PG 24 WC Paleontology SC Paleontology GA 018WW UT WOS:000235796500017 ER PT J AU Head, JJ AF Head, JJ TI Snakes of the Siwalik Group (Miocene of Pakistan): systematics and relationship to environmental change SO PALAEONTOLOGIA ELECTRONICA LA English DT Article DE snakes; faunal change; Siwalik Group; Miocene; Acrochordus ID NORTHERN PAKISTAN; ELAPID SNAKES; RATTLESNAKE; PHYLOGENY; SERPENTES; PALEOGENE; TAPHONOMY; MONSOON; EOCENE AB The lower and middle Siwalik Group of the Potwar Plateau, Pakistan ( Miocene, approximately 18 to 3.5 Ma) is a continuous fluvial sequence that preserves a dense fossil record of snakes. The record consists of approximately 1,500 vertebrae derived from surface-collection and screen-washing of bulk matrix. This record represents 12 identifiable taxa and morphotypes, including Python sp., Acrochordus dehmi, Gansophis potwarensis gen. et sp. nov., Bungarus sp., Chotaophis padhriensis, gen. et sp. nov., and Sivaophis downsi gen. et sp. nov. The record is dominated by Acrochordus dehmi, a fully-aquatic taxon, but diversity increases among terrestrial and semi-aquatic taxa beginning at approximately 10 Ma, roughly coeval with proxy data indicating the inception of the Asian monsoons and increasing seasonality on the Potwar Plateau. Taxonomic differences between the Siwalik Group and coeval European faunas indicate that South Asia was a distinct biogeographic theater from Europe by the middle Miocene. Differences between the Siwalik Group and extant snake faunas indicate significant environmental changes on the Plateau after the last fossil snake occurrences in the Siwalik section. C1 Natl Museum Nat Hist, Smithsonian Inst, Dept Paleobiol, Washington, DC 20013 USA. Univ London Queen Mary Coll, Sch Biol Sci, London E1 4NS, England. RP Head, JJ (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Dept Paleobiol, POB 37012, Washington, DC 20013 USA. EM headj@si.edu NR 96 TC 1 Z9 1 U1 1 U2 1 PU COQUINA PRESS PI AMHERST PA C/O WHITEY HAGADORN, EXECUTIVE EDITOR, AMHERST COLLEGE, DEPT GEOLOGY, AMHERST, MA 01002 USA SN 1094-8074 J9 PALAEONTOL ELECTRON JI Palaeontol. electron. PY 2005 VL 8 IS 1 AR UNSP 18A PG 33 WC Paleontology SC Paleontology GA 018WW UT WOS:000235796500020 ER PT J AU Hubbell, SP AF Hubbell, SP TI The neutral theory of biodiversity and biogeography and Stephen Jay Gould SO PALEOBIOLOGY LA English DT Article ID SPECIES ABUNDANCE; MASS EXTINCTIONS; EVOLUTION; SPECIATION; ECOLOGY AB Neutral theory in ecology is based on the symmetry assumption that ecologically similar species in a community can be treated as demographically equivalent on a per capita basis-equivalent in birth and death rates, in rates of dispersal, and even in the probability of speciating. Although only a first approximation, the symmetry assumption allows the development of a quantitative neutral theory of relative species abundance and dynamic null hypotheses for the assembly of communities in ecological time and for phylogeny and phylogeography in evolutionary time. Although Steve Gould was not a neutralist, he made use of ideas of symmetry and of null models in his science, both of which are fundamental to neutral theory in ecology. Here I give a brief overview of the current status of neural theory in ecology and phylogeny and, where relevant, connect these newer ideas to Gould ' s work. In particular, I focus on modes of speciation under neutrality, particularly peripheral isolate speciation, and their implications for relative species abundance and species life spans. Gould was one of the pioneers in the study of neutral models of phylogeny, but the modern theory suggests that at least some of the conclusions from these early neutral models were premature. Modern neutral theory is a remarkably rich source of new ideas to test in ecology and paleobiology, the potential of which has only begun to be realized. C1 Univ Georgia, Dept Plant Biol, Athens, GA 30602 USA. Smithsonian Trop Res Inst, Miami, FL 34002 USA. RP Univ Georgia, Dept Plant Biol, Athens, GA 30602 USA. EM shubbell@plantbio.uga.edu NR 44 TC 16 Z9 20 U1 2 U2 38 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0094-8373 EI 1938-5331 J9 PALEOBIOLOGY JI Paleobiology PY 2005 VL 31 IS 2 SU S BP 122 EP 132 DI 10.1666/0094-8373(2005)031[0122:TNTOBA]2.0.CO;2 PG 11 WC Biodiversity Conservation; Ecology; Evolutionary Biology; Paleontology SC Biodiversity & Conservation; Environmental Sciences & Ecology; Evolutionary Biology; Paleontology GA 938BB UT WOS:000229973800010 ER PT B AU Goddard, I AF Goddard, Ives BE Wolfart, HC TI Modal attraction and other cases of functional overlap in Meskwaki modes SO Papers of the Thirty-Sixth Algonquian Conference SE PAPERS OF THE ALGONQUIAN CONFERENCE LA English DT Proceedings Paper CT 36th Algonquian Conference CY OCT 28-31, 2004 CL Univ Wisconsin, Madison, WI HO Univ Wisconsin C1 Smithsonian Inst, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU UNIV MANITOBA PRESS PI WINNIPEG PA 244 ENGINEERING BLDG, WINNIPEG, MANITOBA R3T 2N2, CANADA J9 PAP ALGON CONF PY 2005 VL 36 BP 207 EP 221 PG 15 WC Anthropology; Language & Linguistics SC Anthropology; Linguistics GA BFQ45 UT WOS:000243840000010 ER PT B AU Thomason, L AF Thomason, Lucy BE Wolfart, HC TI Meskwaki prenouns SO Papers of the Thirty-Sixth Algonquian Conference SE PAPERS OF THE ALGONQUIAN CONFERENCE LA English DT Proceedings Paper CT 36th Algonquian Conference CY OCT 28-31, 2004 CL Univ Wisconsin, Madison, WI HO Univ Wisconsin C1 Smithsonian Inst, Washington, DC 20560 USA. NR 49 TC 0 Z9 0 U1 0 U2 0 PU UNIV MANITOBA PRESS PI WINNIPEG PA 244 ENGINEERING BLDG, WINNIPEG, MANITOBA R3T 2N2, CANADA J9 PAP ALGON CONF PY 2005 VL 36 BP 425 EP 448 PG 24 WC Anthropology; Language & Linguistics SC Anthropology; Linguistics GA BFQ45 UT WOS:000243840000021 ER PT B AU Geller, MJ AF Geller, MJ BE Alverson, G Barberis, E Nath, P Vaughn, MT TI Where the dark matter is... and isn't SO PASCOS 2004: Proceedings of the 10th International Symposium on Particles, Strings and Cosmology, Pt 1 LA English DT Proceedings Paper CT 10th International Symposium on Particles, Strings and Cosmology (PASCOS 2004) CY AUG 16-22, 2004 CL NE Univ, Boston, MA SP US Natl Sci Fdn, US DOE HO NE Univ ID REGION NEARBY SURVEY; GALAXY CLUSTERS; LUMINOSITY; CAIRNS AB Observations of the cosmic microwave background combined with large redshift surveys suggest that Omega(m) similar to 0.3. Direct dynamical measurements combined with estimated of the universal luminosity density suggest Omega(m) = 0.1 - 0.2. The apparent discrepancy may result from variations in the dark matter fraction with mass and scale. Traditional techniques already indicate that these variations are present. Gravitational lensing maps combined with large redshift surveys promise to measure the dark matter distribution. The Hectopsec Survey of a field in the Deep Lens Survey is a first approach to this kind of measurement. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Geller, MJ (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. NR 15 TC 0 Z9 0 U1 0 U2 0 PU WORLD SCIENTIFIC PUBL CO PTE LTD PI SINGAPORE PA PO BOX 128 FARRER RD, SINGAPORE 9128, SINGAPORE BN 981-256-391-1 PY 2005 BP 18 EP 26 DI 10.1142/9789812701756_0002 PG 9 WC Physics, Multidisciplinary SC Physics GA BDM88 UT WOS:000234374500002 ER PT J AU Tan, JN Silver, E Pomeroy, J Laming, JM Gillaspy, J AF Tan, JN Silver, E Pomeroy, J Laming, JM Gillaspy, J TI An electron beam ion trap (EBIT) plus a microcalorimeter: A good combination for laboratory astrophysics SO PHYSICA SCRIPTA LA English DT Article; Proceedings Paper CT 8th International Colloquium on Atomic Spectra and Oscillator Strengths for Astrophysical and Laboratory Plasmas CY AUG 08-12, 2004 CL Univ Wisconsin, Madison, WI HO Univ Wisconsin ID HIGHLY-CHARGED IONS; X-RAY ASTRONOMY; FE-XVII; SPECTRA; HYDROGENLIKE; SPECTROSCOPY; TRANSITIONS; INTENSITY; CAPELLA; PHYSICS AB An EBIT can selectively create, in principle, any charge state of every naturally occurring element, has good control on atomic collision processes, and can produce nearly ideal conditions for the analysis of highly ionized plasmas of astrophysical importance. A microcalorimeter enables the broadband detection of X- ray emission with high energy resolution and near- unity quantum efficiency in the energy range wherein many cosmic X- ray sources emit the bulk of their energy ( 0.2 keV - 10 keV). The combination ( EBIT+ microcalorimeter) provides a powerful tool for laboratory studies of the atomic/ plasma processes underlying the energy release mechanisms in cosmic X- ray sources. We briefly describe some early experiments with a microcalorimeter built by the Smithsonian Astrophysical Observatory ( SAO) and deployed on the NIST EBIT. We also present some very recent observations with a more advanced microcalorimeter built by SAO that can obtain an energy resolution of 4.5eV. The higher spectral quality produced by the new system will be useful in laboratory measurements of interest in X- ray astronomy. C1 Natl Inst Stand & Technol, Gaithersburg, MD 20899 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. USN, Res Lab, Washington, DC 20375 USA. RP Tan, JN (reprint author), Natl Inst Stand & Technol, 100 Bur Dr, Gaithersburg, MD 20899 USA. NR 37 TC 9 Z9 9 U1 0 U2 2 PU ROYAL SWEDISH ACAD SCIENCES PI STOCKHOLM PA PUBL DEPT BOX 50005, S-104 05 STOCKHOLM, SWEDEN SN 0031-8949 J9 PHYS SCRIPTA JI Phys. Scr. PY 2005 VL T119 BP 30 EP 34 DI 10.1088/0031-8949/2005/T119/005 PG 5 WC Physics, Multidisciplinary SC Physics GA 034DR UT WOS:000236906900006 ER PT J AU Desyatnyk, O Pszczolkowski, L Thorwirth, S Krygowski, TM Kisiel, Z AF Desyatnyk, O Pszczolkowski, L Thorwirth, S Krygowski, TM Kisiel, Z TI The rotational spectra, electric dipole moments and molecular structures of anisole and benzaldehyde SO PHYSICAL CHEMISTRY CHEMICAL PHYSICS LA English DT Article ID CENTRIFUGAL-DISTORTION; MICROWAVE-SPECTRUM; MILLIMETER-WAVE; BANDS; SPECTROMETER; SPECTROSCOPY; DERIVATIVES; CONSTANTS; GEOMETRY; BENZENE AB The rotational spectra of anisole and of benzaldehyde were investigated in supersonic expansion at frequencies up to 41 GHz, and at room temperature in the millimetre-wave region, from 170 to 330 GHz. Accurate spectroscopic constants for the parent isotopomers in the ground vibrational state and for the first excited torsional state were determined for both molecules. The supersonic expansion spectrum allowed measurement, in natural abundance, of all singly substituted C-13 isotopomers, as well as of the O-18 isotopomer for both anisole and benzaldehyde. The rotational constants were used to determine the r(s) and the r(m)((1)) gas-phase geometries, which are found to be consistent with prediction of bond length alternation in the phenyl ring induced by the asymmetric substituent. Stark measurements were made on the supersonic expansion spectrum resulting in electric dipole moment determination, vertical bar mu(a)vertical bar = 2.9061(22) D, vertical bar mu(b)vertical bar = 1.1883(10) D, mu(tot) = 3.1397(24) D for benzaldehyde and vertical bar mu(a)vertical bar = 0.6937(12) D, vertical bar mu(b)vertical bar = 1.0547(8) D, mu(tot) = 1.2623(14) D for anisole. During the investigation it was found that use of a carrier gas mixture consisting of 30% Ar in He carries significant advantages for studies of weak lines, and pertinent experimental details are reported. C1 Polish Acad Sci, Inst Phys, PL-02668 Warsaw, Poland. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Harvard Univ, Div Engn & Appl Sci, Cambridge, MA 02138 USA. Univ Warsaw, Dept Chem, PL-02093 Warsaw, Poland. RP Polish Acad Sci, Inst Phys, Al Lotnikow 32-46, PL-02668 Warsaw, Poland. EM kisiel@ifpan.edu.pl RI Thorwirth, Sven/C-6217-2011; Kisiel, Zbigniew/K-8798-2016; Pszczolkowski, Lech/S-3018-2016 OI Thorwirth, Sven/0000-0001-8200-6710; Kisiel, Zbigniew/0000-0002-2570-3154; NR 45 TC 32 Z9 33 U1 5 U2 18 PU ROYAL SOC CHEMISTRY PI CAMBRIDGE PA THOMAS GRAHAM HOUSE, SCIENCE PARK, MILTON RD, CAMBRIDGE CB4 0WF, CAMBS, ENGLAND SN 1463-9076 EI 1463-9084 J9 PHYS CHEM CHEM PHYS JI Phys. Chem. Chem. Phys. PY 2005 VL 7 IS 8 BP 1708 EP 1715 DI 10.1039/b501041a PG 8 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 914QB UT WOS:000228241500015 PM 19787929 ER PT J AU Petrov, DS Salomon, C Shlyapnikov, GV AF Petrov, DS Salomon, C Shlyapnikov, GV TI Scattering properties of weakly bound dimers of fermionic atoms SO PHYSICAL REVIEW A LA English DT Article ID SHORT-RANGE FORCES; INTERACTING PARTICLES; GAS; CONDENSATION; COLLISIONS; RESONANCE; SUPERCONDUCTIVITY; NEUTRONS; STATE; PAIRS AB . We consider weakly bound diatomic molecules (dimers) formed in a two-component atomic Fermi gas with a large positive scattering length for the interspecies interaction. We develop a theoretical approach for calculating atom-dimer and dimer-dimer elastic scattering and for analyzing the inelastic collisional relaxation of the molecules into deep bound states. This approach is based on the single-channel zero-range approximation, and we find that it is applicable in the vicinity of a wide two-body Feshbach resonance. Our results draw prospects for various interesting manipulations of weakly bound dimers of fermionic atoms. C1 Harvard Univ, Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. Harvard Univ, Dept Phys, Harvard MIT Ctr Ultracold Atoms, Cambridge, MA 02138 USA. Univ Calif Santa Barbara, Kavli Inst Theoret Phys, Santa Barbara, CA 93106 USA. Russian Res Ctr, Kurchatov Inst, Moscow 123182, Russia. Ecole Normale Super, Lab Kastler Brossel, F-75005 Paris, France. Univ Paris 11, Lab Phys Theor & Modeles Stat, F-91405 Orsay, France. Univ Amsterdam, Van der Waals Zeeman Inst, NL-1018 XE Amsterdam, Netherlands. RP Harvard Univ, Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. NR 72 TC 114 Z9 115 U1 0 U2 5 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2469-9926 EI 2469-9934 J9 PHYS REV A JI Phys. Rev. A PD JAN PY 2005 VL 71 IS 1 AR 012708 DI 10.1103/PhysRevA.71.012708 PG 15 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 901LF UT WOS:000227283300081 ER PT J AU Zotz, G AF Zotz, G TI Vascular epiphytes in the temperate zones - a review SO PLANT ECOLOGY LA English DT Review DE accidental epiphytes; biodiversity; ferns; frost; latitude; temperate forests; tropical forests; water relations ID RAIN-FOREST; NEW-ZEALAND; SPECIES RICHNESS; DRY FOREST; VEGETATION; DIVERSITY; PATTERNS; ECOLOGY; BIOMASS; BIOGEOGRAPHY AB Vascular epiphytes are typically associated with tropical rainforests, whereas their occurrence in temperate forests is little appreciated. This review summarises the available information on epiphytism in the temperate zones ( > 23.5 degrees latitude), which has not been reviewed comprehensively for more than a century, and critically analyses the proposed mechanisms behind the observed biogeographical patterns. Although in the temperate zone epiphytic vascular plants are rarely as impressive as in tropical forests, there are noteworthy exceptions. Temperate rain forests of Chile and New Zealand, or montane forests in the Himalayas are comparable to many tropical forests in terms of epiphyte biomass and diversity, but differ in their taxonomic spectrum: temperate epiphyte communities are generally dominated by ferns and fern-allies. Other,temperate areas are not, however, necessarily barren of epiphytes, as repeatedly implied. Quite in contrast, local populations of epiphytes in a large number of other non-tropical areas in both the southern and the northern hemisphere can be quite conspicuous. The proposed reasons for the latitudinal gradients in epiphyte abundance and,diversity (water scarcity or low temperatures) are not fully convincing and, moreover, still await experimental verification. Other factors, both historical (e.g., Pleistocene extinctions) and ecological (e.g., prevalence of conifers in the northern hemisphere), should also be taken into consideration to obtain a comprehensive explanation of the extant global distribution of vascular epiphytes. C1 Univ Basel, Inst Bot, CH-4056 Basel, Switzerland. Smithsonian Trop Res Inst, Balboa, Panama. RP Zotz, G (reprint author), Univ Basel, Inst Bot, Schonbeinstr 6, CH-4056 Basel, Switzerland. EM gerhard.zotz@unibas.ch NR 114 TC 26 Z9 32 U1 3 U2 36 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 1385-0237 J9 PLANT ECOL JI Plant Ecol. PY 2005 VL 176 IS 2 BP 173 EP 183 DI 10.1007/s11258-004-0066-5 PG 11 WC Plant Sciences; Ecology; Forestry SC Plant Sciences; Environmental Sciences & Ecology; Forestry GA 908ID UT WOS:000227779800004 ER PT S AU Luhman, KL Fazio, G Megeath, T Hartmann, L Calvet, N Stauffer, J AF Luhman, KL Fazio, G Megeath, T Hartmann, L Calvet, N Stauffer, J BE Favata, F Hussain, GAJ Battrick, B TI Spitzer observations of brown dwarf disks SO PROCEEDINGS OF THE 13TH CAMBRIDGE WORKSHOP ON COOL STARS, STELLAR SYSTEMS AND THE SUN - PROCEEDINGS, VOLS 1 AND 2 SE ESA Special Publications LA English DT Proceedings Paper CT 13th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun CY JUL 05-09, 2004 CL Hamburg, GERMANY DE sStars : low-mass; brown dwarfs; planetary systems; protoplanetary disks; stars : formation ID LOW-MASS STARS; EVOLUTIONARY MODELS; FORMING REGION AB Through the Spitzer IRAC GTO program, we have recently begun extremely sensitive mid-infrared imaging of young brown dwarfs in the nearest star-forming regions. The spectral energy distributions measured from these data provide unprecedented measurements of the fraction of known young brown dwarfs that have circumstellar disks. These Spitzer data are also the first observations capable of detecting Class I brown dwarfs, or proto-brown dwarfs. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. EM kluhman@cfa.harvard.edu NR 12 TC 0 Z9 0 U1 0 U2 0 PU EUROPEAN SPACE AGENCY PI PARIS PA 8-10 RUE MARIO NIKIS, 75738 PARIS, FRANCE SN 0379-6566 BN 92-9092-871-9 J9 ESA SPEC PUBL PY 2005 VL 560 BP 257 EP 260 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BCU73 UT WOS:000231306900034 ER PT S AU Cranmer, SR AF Cranmer, SR BE Favata, F Hussain, GAJ Battrick, B TI New insights into solar wind physics from SOHO SO Proceedings of the 13th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun - Proceedings, Vols 1 and 2 SE ESA SPECIAL PUBLICATIONS LA English DT Proceedings Paper CT 13th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun CY JUL 05-09, 2004 CL Hamburg, GERMANY DE solar corona; solar wind; SOHO; MHD waves; plasma physics; UV spectroscopy ID ULTRAVIOLET CORONAGRAPH SPECTROMETER; SLOW MAGNETOSONIC WAVES; ION-CYCLOTRON WAVES; R-CIRCLE-DOT; MAGNETIC-FIELD; POLAR PLUMES; TRANSITION REGION; TEMPERATURE ANISOTROPY; VELOCITY DISTRIBUTIONS; SUMER INSTRUMENT AB The Solar and Heliospheric Observatory (SOHO) was launched in December 1995 with a suite of instruments designed to answer long-standing questions about the Sun's internal structure, its extensive outer atmosphere and the solar wind. This paper reviews the new understanding of the physical processes responsible for the solar wind that have come from the past 8 years of SOHO observations, analysis, and theoretical work. For example, the UVCS instrument on SOHO has revealed the acceleration region of the fast solar wind to be far from simple thermal equilibrium. Evidence for preferential acceleration of ions, 100 million K ion temperatures, and marked departures from Maxwellian velocity distributions all point to specific types of collisionless heating processes. The slow solar wind, typically associated with bright helmet streamers, has been found to share some of the nonthermal characteristics of the fast wind. Abundance measurements from spectroscopy and visible-light coronagraphic movies from LASCO have led to a better census of the plasma components making up the slow wind. The origins of the solar wind in the photosphere and chromosphere have been better elucidated with disk spectroscopy from the SUMER and CDS instruments. Finally, the impact of the solar wind on spacecraft systems, ground-based technology, and astronauts has been greatly aided by having continuous solar observations at the Earth-Sun L1 point, and SOHO has set a strong precedent for future studies of space weather. 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 119 TC 1 Z9 1 U1 0 U2 1 PU EUROPEAN SPACE AGENCY PI PARIS PA 8-10 RUE MARIO NIKIS, 75738 PARIS, FRANCE SN 0379-6566 BN 92-9092-871-9 J9 ESA SP PUBL PY 2005 VL 560 BP 299 EP 307 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BCU73 UT WOS:000231306900040 ER PT S AU Lobel, A AF Lobel, A BE Favata, F Hussain, GAJ Battrick, B TI Spatially resolved STIS spectra of Betelgeuse's upper chromosphere and circumstellar dust envelope SO PROCEEDINGS OF THE 13TH CAMBRIDGE WORKSHOP ON COOL STARS, STELLAR SYSTEMS AND THE SUN - PROCEEDINGS, VOLS 1 AND 2 SE ESA Special Publications LA English DT Proceedings Paper CT 13th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun CY JUL 05-09, 2004 CL Hamburg, GERMANY DE stars : alpha Orionis; chromospheres; dust; winds; mass-loss; spectroscopy; radiative transport ID LATE-TYPE STARS; ALPHA-ORIONIS; SPECTROSCOPY; OSCILLATION; EMISSION AB The Hubble Space Telescope observed red supergiant Betelgeuse (alpha Ori) with the Space Telescope Imaging Spectrograph to investigate the outer atmosphere from spatially resolved spectra. We present a new set of seven high-resolution near-UV spectra observed with HST-STIS in fall 2002 and spring 2003, by scanning at chromospheric intensity peak-up position and six off-limb target positions up to three arcseconds away from the star. A small aperture is used to study and determine the thermal conditions and flow dynamics in the upper chromosphere and inner circumstellar dust envelope of this important nearby cool supergiant (M2 Iab). We provide the first evidence for the presence of warm chromospheric plasma at least 3" away from Betelgeuse at similar to 120 R. (1 R-* similar or equal to 700 R-circle dot) based on detailed spectroscopic observations of the Mg II h & k emission lines. Many other weak chromospheric emission lines as Fe II lambda 2716, C II lambda 2327, Al II] lambda 2669, and Fe I lambda 2823, are detected out to at least V in the spatially resolved STIS observations. The recent spectra reveal that a Ori's upper chromosphere extends far beyond the circumstellar Ha envelope of similar to 5 R., determined from previous ground-based images. The changes of shape of the detailed Mg II line profiles observed in Betelgeuse's outer atmosphere are compared with detailed Mg II line profiles previously observed above the limb of the average quiet Sun. The profiles of the Mg II h & k, and the Si I resonance emission lines reveal a strong increase of asymmetry by scanning off-limb, signaling the outward acceleration of wind expansion in Betelgeuse's upper chromosphere beyond 200 mas (similar to 8 R.). We discuss detailed radiative transfer models that fit the STIS observations showing that the local kinetic gas temperature in the upper chromosphere exceeds 2600 K. Our radiation transport models for the IR silicate dust emission at 9.8 mu m in the upper chromosphere show however that the ambient gas temperature remains below 600 K to sustain the presence of dust grains. Hence, the STIS spectra of Betelgeuse's upper chromosphere directly demonstrate that warm chromospheric plasma must coexist with cool dusty plasma in its outer atmosphere. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM alobel@cfa.harvard.edu NR 12 TC 1 Z9 1 U1 0 U2 0 PU EUROPEAN SPACE AGENCY PI PARIS PA 8-10 RUE MARIO NIKIS, 75738 PARIS, FRANCE SN 0379-6566 BN 92-9092-871-9 J9 ESA SPEC PUBL PY 2005 VL 560 BP 327 EP 334 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BCU73 UT WOS:000231306900043 ER PT S AU Brickhouse, NS Dupree, AK Hoogerwerf, R AF Brickhouse, NS Dupree, AK Hoogerwerf, R BE Favata, F Hussain, GAJ Battrick, B TI Chandra x-ray spectra of contact binaries SO Proceedings of the 13th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun - Proceedings, Vols 1 and 2 SE ESA SPECIAL PUBLICATIONS LA English DT Proceedings Paper CT 13th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun CY JUL 05-09, 2004 CL Hamburg, GERMANY DE stars : coronae; stars : individual (44i Boo, VW Cep); stars : late-type AB We present Chandra LETG/HRC-S spectra of the bright eclipsing contact binary 44i Boo. Chandra began observing the target on 22 Sept 2003 for an exposure time of 118.524 ks. This observation continuously covers 5.12 epochs of the binary system. Analysis of phase-binned spectra is compared with previous results from HETG/ACIS-S, which showed Doppler line shifts as a function of orbital phase (Brickhouse, Dupree, & Young 2001). We confirm the presence of the high latitude features found in 2000 in this remarkably stable corona. We expect these new data to provide additional information on the size, location, and variability of the high latitude emission. We also compare results with LETG/HRC-S spectra of the complementary contact binary system VW Cep. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Brickhouse, NS (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 8 TC 0 Z9 0 U1 0 U2 0 PU EUROPEAN SPACE AGENCY PI PARIS PA 8-10 RUE MARIO NIKIS, 75738 PARIS, FRANCE SN 0379-6566 BN 92-9092-871-9 J9 ESA SP PUBL PY 2005 VL 560 BP 457 EP 460 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BCU73 UT WOS:000231306900069 ER PT S AU Drake, JJ AF Drake, JJ BE Favata, F Hussain, GAJ Battrick, B TI Trouble on the shock front: TW hydrae, x-rays and accretion SO Proceedings of the 13th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun - Proceedings, Vols 1 and 2 SE ESA SPECIAL PUBLICATIONS LA English DT Proceedings Paper CT 13th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun CY JUL 05-09, 2004 CL Hamburg, GERMANY DE stars : T tauri; stars : TW hydrae; stars : x-ray; x-ray : spectroscopy; processes : accretion ID MAIN-SEQUENCE STARS; TAURI STARS; IUE ATLAS AB The classical T Tauri star TW Hydrae has an X-ray spectrum quite unlike that of any other active star or T Tauri star so far observed at high spectral resolution. Density-sensitive O VII and Ne IX fines seen in both XMM-Newton and Chandra spectra indicate plasma densities of order 10(13) cm(-3) when interpreted in terms of collisional excitation, while the dominant plasma temperature is a rather cool 3 x 10(6) K. It has been suggested in the recent literature that these characteristics are indicative of emission from an accretion shock rather than from a coronal plasma. Simple models suggest that such a shock should occur deep in the photosphere from which copious X-rays should not escape. Excitation of the O VII and Ne IX S-3(1) ->(3) P transitions by the ambient UV radiation field might alleviate this problem and I show that photoexcitation likely affects the observed f/i ratios. O and Ne Ly alpha/beta line ratios indicate an absorbing column of 3-6 x 10(21) cm(-1), which corresponds to a photospheric depth of similar to 100 km. These results combined suggest a postshock density slightly lower than 10(13) cm(-3), and in the range of a few 10(12) cm(-3). The observed X-rays then originate from only the top few percent of the post-shock region; X-rays formed deeper axe absorbed and reprocessed to longer wavelengths. More detailed calculations axe required to fully understand the shock region and to interpret properly the observed X-ray and UV characteristics of TW Hya. One conclusion is clear: X-ray shocks from T Tauri stars accreting at higher rates that TW Hya are likely to be invisible in general, because accretion shocks will occur too deep in the atmosphere; X-ray shocks axe then only expected for accretion rates of similar to 10(-9) Me or less. Combined with orientation effects, this might explain the apparent rareity of TW Hya-like X-ray spectra. C1 Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Drake, JJ (reprint author), Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. NR 12 TC 25 Z9 25 U1 0 U2 0 PU EUROPEAN SPACE AGENCY PI PARIS PA 8-10 RUE MARIO NIKIS, 75738 PARIS, FRANCE SN 0379-6566 BN 92-9092-871-9 J9 ESA SP PUBL PY 2005 VL 560 BP 519 EP 522 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BCU73 UT WOS:000231306900084 ER PT S AU Dupree, AK Brickhouse, NS AF Dupree, AK Brickhouse, NS BE Favata, F Hussain, GAJ Battrick, B TI Evolution of stellar coronae SO Proceedings of the 13th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun - Proceedings, Vols 1 and 2 SE ESA SPECIAL PUBLICATIONS LA English DT Proceedings Paper CT 13th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun CY JUL 05-09, 2004 CL Hamburg, GERMANY DE stars : coronae; stars : hybrid ID STARS; SUPERGIANTS; GIANTS AB Two single cool stars, Beta Dra and Alpha TrA offer a contrast in the structure and evolution of their outer atmospheres. Alpha TrA is a hybrid object, from a class of cool luminous stars originally identified based on C IV emission accompanied by absorption features indicating a massive stellar wind and circumstellar material. The atmosphere of Beta Dra appears to be similar to the Sun with high temperature emission, and lacking a massive wind. Spectra of these stars obtained with RGS-XMM/Newton show high temperature emission T similar to 10(7)K in their steady (non-flaring) state. A 1-T fit to the spectra suggests that the corona of Beta Dra is slightly hotter than that of Alpha TrA. Abundances of 0, Ne, and Fe axe 'solar' in Beta Dra, but 0 and Ne are enhanced with respect to solar in Alpha TrA. The density sensitive ratio of O VII transitions suggests that the densities are comparable. These spectra demonstrate that slowly-rotating giants and supergiants can have coronae hotter than the Sun. These spectra also give the first evidence that coronal structure changes, becoming cooler as luminous stars evolve to the hybrid phase. 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 8 TC 0 Z9 0 U1 0 U2 0 PU EUROPEAN SPACE AGENCY PI PARIS PA 8-10 RUE MARIO NIKIS, 75738 PARIS, FRANCE SN 0379-6566 BN 92-9092-871-9 J9 ESA SP PUBL PY 2005 VL 560 BP 523 EP 526 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BCU73 UT WOS:000231306900085 ER PT S AU Kalkofen, W AF Kalkofen, W BE Favata, F Hussain, GAJ Battrick, B TI The structure of the quiet solar chromosphere SO PROCEEDINGS OF THE 13TH CAMBRIDGE WORKSHOP ON COOL STARS, STELLAR SYSTEMS AND THE SUN - PROCEEDINGS, VOLS 1 AND 2 SE ESA Special Publications LA English DT Proceedings Paper CT 13th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun CY JUL 05-09, 2004 CL Hamburg, GERMANY DE solar chromosphere; acoustic waves; CaII bright points; dynamics and heating ID OSCILLATIONS; PROPAGATION; ATMOSPHERE; GRAINS; ENERGY; MODELS; WAVES AB The quiet solar atmosphere is described by two types of model that differ fundamentally in the manner in which acoustic waves heat their chromospheres, viz., an empirical model, whose temperature structure implies steady heating, with the temperature rising monotonically in the outward direction; and a wave model, in which heating occurs intermittently in space and time, with the time-averaged temperature dropping and the emission-averaged temperature rising monotonically in the upward direction. When the wave model is corrected for the geometry of three-dimensional wave propagation in a stratified atmosphere, the emission-averaged temperature as well drops monotonically in the upward direction. The wave model provides an accurate, if only qualitative, description of the dynamics of Ca II bright-point oscillations. But it falls as a model of chromospheric heating, supplying only a fraction of 10(-3) to 10(-2) of the energy required. The shortfall is partly due to the spatial intermittence of bright-point dynamics, whose filling factor varies from similar to 1% at the base of the chromosphere to similar to 50% at its top, and partly due to the temporal intermittence of the shock waves that produce the bright points. The analysis of the wave model shows that chromospheric dynamics and chromospheric heating axe separate and independent processes. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. EM wolf@cfa.harvard.edu NR 19 TC 0 Z9 0 U1 0 U2 0 PU EUROPEAN SPACE AGENCY PI PARIS PA 8-10 RUE MARIO NIKIS, 75738 PARIS, FRANCE SN 0379-6566 BN 92-9092-871-9 J9 ESA SPEC PUBL PY 2005 VL 560 BP 695 EP 698 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BCU73 UT WOS:000231306900127 ER PT S AU Lin, L Kashyap, VL Drake, JJ DeLuca, EE Weber, M Sette, AL AF Lin, L Kashyap, VL Drake, JJ DeLuca, EE Weber, M Sette, AL BE Favata, F Hussain, GAJ Battrick, B TI The nearest star: Resolving the building blocks of the coronal DEM SO PROCEEDINGS OF THE 13TH CAMBRIDGE WORKSHOP ON COOL STARS, STELLAR SYSTEMS AND THE SUN - PROCEEDINGS, VOLS 1 AND 2 SE ESA Special Publications LA English DT Proceedings Paper CT 13th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun CY JUL 05-09, 2004 CL Hamburg, GERMANY DE corona : emission measure; software : PINTofALE,MCMC ID X-RAY STAR; EMISSION MEASURE; SOLAR CORONA; SUN; TEMPERATURE AB We have constructed differential emission measures (DEMs) of different structures in the solar corona using data from multiple instruments. We apply a sophisticated DEM reconstruction technique to solar imaging and spectral data obtained contemporaneously using Yohkoh/SXT, TRACE, SoHO/EIT, SoHO/CDS, and GOES. The method is easily adapted to any combination of observations with different instruments and filters. We employ the technique to characterize the DEM in the solar active region AR8232 (June 1998) for which data axe available from all five instruments. We compare DEMs spatially averaged over large regions with those derived for individually resolved features and discuss the results. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM llin@cfa.haravard.edu; jdrake@cfa.harvard.edu; mweber@aip.de OI DeLuca, Edward/0000-0001-7416-2895 NR 19 TC 0 Z9 0 U1 0 U2 0 PU EUROPEAN SPACE AGENCY PI PARIS PA 8-10 RUE MARIO NIKIS, 75738 PARIS, FRANCE SN 0379-6566 BN 92-9092-871-9 J9 ESA SPEC PUBL PY 2005 VL 560 BP 757 EP 761 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BCU73 UT WOS:000231306900143 ER PT S AU Lobel, A Aufdenberg, JP Ilyin, I Rosenbush, AE AF Lobel, A Aufdenberg, JP Ilyin, I Rosenbush, AE BE Favata, F Hussain, GAJ Battrick, B TI Mass-loss and recent spectral changes in the yellow hypergiant rho Cassiopeiae SO PROCEEDINGS OF THE 13TH CAMBRIDGE WORKSHOP ON COOL STARS, STELLAR SYSTEMS AND THE SUN - PROCEEDINGS, VOLS 1 AND 2 SE ESA Special Publications LA English DT Proceedings Paper CT 13th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun CY JUL 05-09, 2004 CL Hamburg, GERMANY DE stars; rho Cassiopeiae; stellar winds; pulsation; mass-loss; spectroscopy; supergiants; emission lines AB The yellow hypergiant rho Cassiopeiae (F-G Ia0) has recently become very active with a tremendous outburst event in the fall of 2000. During the event the pulsating supergiant dimmed by more than a visual magnitude, while its effective temperature decreased from 7000 K to below 4000 K over about 200 d, and we directly observed the largest mass-loss rate of about 5% of the solar mass in a single stellar outburst so far. Over the past three years since the eruption we observed a very prominent inverse P Cygni profile in Balmer H alpha, signaling a strong collapse of the upper atmosphere, also observed before the 2000 event. Continuous spectroscopic monitoring reveals that the Ha line profile has transformed into a P Cygni profile since June 2003, presently (Sept 2004) signaling supersonic expansion velocities up to similar to 120 km s(-1) in the extended upper atmosphere, comparable to the 2000 outburst. With the new fast atmospheric expansion many strong neutral atomic emission lines have appeared in the optical and near-IR spectrum over the past half year. Based on the very recent unique spectral evolution we observed the far-UV spectrum with the FUSE satellite in July 2004. The FUSE spectrum reveals that high-temperature plasma emission lines of O vi and C III are absent in the hypergiant, also observed for the red supergiant alpha Ori (M2 Iab). On the other hand, we observe prominent transition region emission lines in the smaller (less luminous) classical Cepheid variable beta Dor (F-G Iab-Ia), indicating that the mean atmospheric extension and surface gravity acceleration (as compared to effective temperature and atmospheric pulsation) play a major role for the formation of high-temperature stellar atmospheric plasmas. We present an overview of the recent spectral vaxiability phases of p Cas with enhanced mass-loss from this enigmatic cool star. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM alobel@cfa.harvard.edu; jasona@noao.edu; ilyin@aip.de NR 11 TC 0 Z9 0 U1 0 U2 0 PU EUROPEAN SPACE AGENCY PI PARIS PA 8-10 RUE MARIO NIKIS, 75738 PARIS, FRANCE SN 0379-6566 BN 92-9092-871-9 J9 ESA SPEC PUBL PY 2005 VL 560 BP 771 EP 774 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BCU73 UT WOS:000231306900146 ER PT S AU Cranmer, SR AF Cranmer, SR BE Lacoste, H TI Why is the fast solar wind fast and the slow solar wind slow? A survey of geometrical models SO Proceedings of the Conference Solar Wind 11 - SOHO 16: CONNECTING SUN AND HELIOSPHERE SE ESA SPECIAL PUBLICATIONS LA English DT Proceedings Paper CT Solar Wind 11 - SOHO 16 Conference CY JUN 12-17, 2005 CL Whistler, CANADA SP European Space Agcy, NASA, CSA ASC, NSF, Univ Michigan ID INTERPLANETARY MAGNETIC-FIELD; POLAR CORONAL HOLE; ALFVEN WAVES; VELOCITY DISTRIBUTIONS; LOW-FREQUENCY; FLUX TUBES; ACCELERATION; SPEED; FLOW; TURBULENCE AB Four decades have gone by since the discovery that the solar wind at 1 AU seems to exist in two relatively distinct states: slow and fast. There is still no universal agreement concerning the primary physical cause of this apparently bimodal distribution, even in its simplest manifestation at solar minimum. In this presentation we review and extend a series of ideas that link the different states of solar wind to the varying superradial geometry of magnetic flux tubes in the extended corona. Past researchers have emphasized different aspects of this relationship, and we attempt to disentangle some of the seemingly contradictory results. We apply the hypothesis of Wang and Sheeley (as well as Kovalenko) that Alfven wave fluxes at the base are the same for all flux tubes to a recent model of non-WKB Alfven wave reflection and turbulent heating, and we predict coronal heating rates as a function of flux tube geometry. We compare the feedback of these heating rates on the locations of Parker-type critical points, and we discuss the ranges of parameters that yield a realistic bifurcation of wind solutions into fast and slow. Finally, we discuss the need for next-generation coronagraph spectroscopy of the extended corona-especially measurements of the electron temperature above 1.5 solar radii-in order to confirm and refine these ideas. 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 74 TC 5 Z9 5 U1 0 U2 2 PU ESA PUBLICATIONS DIVISION C/O ESTEC PI 2200 AG NOORDWIJK PA PO BOX 299, 2200 AG NOORDWIJK, NETHERLANDS SN 0379-6566 BN 92-9092-903-0 J9 ESA SP PUBL PY 2005 VL 592 BP 159 EP 164 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BDU58 UT WOS:000235471300024 ER PT S AU Kohl, JL Cranmer, SR Gardner, LD Lin, J Raymond, JC Strachan, L AF Kohl, JL Cranmer, SR Gardner, LD Lin, J Raymond, JC Strachan, L BE Lacoste, H TI Capabilities of UV coronagraphic spectroscopy for studying the source regions of solar energetic particles and the solar wind SO PROCEEDINGS OF THE CONFERENCE SOLAR WIND 11 - SOHO 16: CONNECTING SUN AND HELIOSPHERE SE ESA Special Publications LA English DT Proceedings Paper CT Solar Wind 11 - SOHO 16 Conference CY JUN 12-17, 2005 CL Whistler, CANADA SP European Space Agcy, NASA, CSA ASC, NSF, Univ Michigan ID CORONAL MASS EJECTION; MAGNETIC RECONNECTION; DRIVEN SHOCKS; ACTIVE-REGION; VELOCITY DISTRIBUTIONS; CURRENT SHEETS; ALFVEN WAVES; ACCELERATION; MODEL; FLARES AB We summarize the unique capabilities of UV coronagraphic spectroscopy for determining the detailed plasma properties (e.g., density, temperature, outflow speed, composition) of the source regions of both transient phenomena such as CMEs, flares, and solar energetic particles (SEPs) and more time-steady solar wind streams. UVCS/SOHO observations have provided the first detailed diagnostics of the physical conditions of CME plasma in the extended corona. It provided new insights into the roles of shock waves, reconnection, and magnetic helicity in CME eruptions. We summarize past observations and discuss the diagnostic potential of UV coronagraphic spectroscopy for characterizing two possible sites of SEP production: CME shocks and reconnection current sheets. UVCS/SOHO has also led to fundamentally new views of the acceleration region of the solar wind. Understanding the physical processes in this region, which ranges from the low corona (r = 1.1-1.5 R(circle dot)) past the sonic points (r > 5 R(circle dot)), is key to linking the results of solar imaging to in situ particle and field detection. Despite the advances that have resulted from UVCS/SOHO, more advanced instrumentation could determine properties of additional ions with a wider sampling of charge/mass combinations. This would provide much better constraints on the specific kinds of waves that are present as well as the specific collisionless damping modes. Electron temperatures and departures from Maxwellian velocity distributions could also be measured. The instrumentation capable of making the above observations will be described. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kohl, JL (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jkohl@cfa.harvard.edu; scranmer@cfa.harvard.edu; jlin@cfa.harvard.edu; jraymond@cfa.hardard.edu; lstrachan@cfa.harvard.edu RI LIN, JUN/B-9890-2017 NR 66 TC 0 Z9 0 U1 0 U2 0 PU ESA PUBLICATIONS DIVISION C/O ESTEC PI 2200 AG NOORDWIJK PA PO BOX 299, 2200 AG NOORDWIJK, NETHERLANDS SN 0379-6566 BN 92-9092-903-0 J9 ESA SPEC PUBL PY 2005 VL 592 BP 677 EP 680 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BDU58 UT WOS:000235471300135 ER PT S AU Smith, HA Allen, L Megeath, T Barmby, P Calvet, N Fazio, G Hartmann, L Myers, P Marengo, M Gutermuth, R Pipher, J D'Alessio, P Merin, B Reach, B Noriega-Crespo, A Marston, T Muzerolle, J AF Smith, HA Allen, L Megeath, T Barmby, P Calvet, N Fazio, G Hartmann, L Myers, P Marengo, M Gutermuth, R Pipher, J D'Alessio, P Merin, B Reach, B Noriega-Crespo, A Marston, T Muzerolle, J BE Wilson, A TI Star formation as seen by the Infrared Array Camera on Spitzer SO PROCEEDINGS OF THE DUSTY AND MOLECULAR UNIVERSE: A PRELUDE TO HERSCHEL AND ALMA SE ESA SPECIAL PUBLICATIONS LA English DT Proceedings Paper CT Conference on the Dusty and Molecular Universe CY OCT 27-29, 2004 CL Paris, FRANCE SP Minist Rech, Observ Paris, Minist Educ Natl, CNES, Inst Natl Sci Univers, CNRS, European So Observ, European Space Agcy ID HII-REGIONS; DR-21; OUTFLOW AB The Infrared Array Camera (IRAC) onboard Spitzer has imaged regions of star formation (SF) in its four IR bands with spatial resolutions of similar to 2"/ pixel. IRAC is sensitive enough to detect very faint, embedded young stars at levels of tens of mu Jy, and IRAC photometry can categorize their stages of development: from young protostars with infalling envelopes (Class 0/I) to stars whose infrared excesses derive from accreting circumstellar disks (Class II) to evolved stars dominated by photospheric emission. The IRAC images also clearly reveal and help diagnose associated regions of shocked and/or PDR emission in the clouds; we find existing models provide a good start at explaining the continuum of the SF regions IRAC observes. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02139 USA. RP Smith, HA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02139 USA. NR 26 TC 2 Z9 2 U1 0 U2 0 PU ESA PUBLICATIONS DIVISION C/O ESTEC PI 2200 AG NOORDWIJK PA PO BOX 299, 2200 AG NOORDWIJK, NETHERLANDS SN 0379-6566 J9 ESA SP PUBL PY 2005 VL 577 BP 197 EP 200 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BBR24 UT WOS:000227350800035 ER PT S AU Bensch, F Bergin, EA AF Bensch, F Bergin, EA BE Wilson, A TI Rat4com: A radiative transfer model for water in comets SO PROCEEDINGS OF THE DUSTY AND MOLECULAR UNIVERSE: A PRELUDE TO HERSCHEL AND ALMA SE ESA SPECIAL PUBLICATIONS LA English DT Proceedings Paper CT Conference on the Dusty and Molecular Universe CY OCT 27-29, 2004 CL Paris, FRANCE SP Minist Rech, Observ Paris, Minist Educ Natl, CNES, Inst Natl Sci Univers, CNRS, European So Observ, European Space Agcy DE comets : general; radiative transfer; methods : numerical; radio lines : solar system ID C/1999 H1 LEE; EXCITATION AB We present an improved version of rat4com, a radiation transfer model for water rotational line emission in cometary coma. The original model is limited to the rotational transitions of ortho-water for a comet with a constant water production rate (Bensch & Bergin, 2004). With the improved version of rat4com we include para-water levels and study the impact of ne,er, more accurate water-electron collision rates on the predicted line emission. Additionally, we present results for a model where the water production rate is temporarily elevated. It is an initial attempt to model the emission of a comet undergoing an outburst. The prospects of water rotational line observations with HIFI on the Herschel Space Observatory are discussed. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Bensch, F (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 10 TC 2 Z9 2 U1 0 U2 0 PU ESA PUBLICATIONS DIVISION C/O ESTEC PI 2200 AG NOORDWIJK PA PO BOX 299, 2200 AG NOORDWIJK, NETHERLANDS SN 0379-6566 J9 ESA SP PUBL PY 2005 VL 577 BP 465 EP 466 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BBR24 UT WOS:000227350800140 ER PT J AU Edmiston, JF Mathis, WN AF Edmiston, JF Mathis, WN TI A review of two nearctic species of the shore-fly genus Philygria Stenhammar: P-debilis Loew and P-nigrescens (Cresson) (Diptera : Ephydridae) SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Review DE review; Diptera; ephydridae; ilytheinae; hyadinini; shore flies; Philygria debilis; P. nigrescens; lectotype designations ID COMMUNITY STRUCTURE; FLIES DIPTERA; WASHINGTON AB Two species of the shore-fly genus Philygria Stenhammar. P. debilis Loew and P. nigrescens (Cresson), are reviewed to reassess their taxonomic status. which Was recently questioned by Hollmann-Schirrmacher. Both species are distinct. and evidence is presented to support their revised status. For perspective and to facilitate their identification, the appropriate subfamily, tribe, genus, and species are diagnosed and keys to the,genera of the tribe Hyadinini and to the Nearctic species of Philygria are presented. Lectotypes, as appropriate, are designated. C1 Franciscan Project Russia & Kazakhstan, Novosibirsk, Russia. Smithsonian Inst, Dept Entomol, Washington, DC 20013 USA. RP Edmiston, JF (reprint author), Franciscan Project Russia & Kazakhstan, Novosibirsk, Russia. EM edmisja@att.net; mathis.wayne@nmnh.si.edu NR 48 TC 1 Z9 2 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 JAN PY 2005 VL 107 IS 1 BP 7 EP 20 PG 14 WC Entomology SC Entomology GA 887QC UT WOS:000226319600002 ER PT J AU Gates, MW Myartseva, SN Schauff, ME AF Gates, MW Myartseva, SN Schauff, ME TI A new Baryscapus Forster (Hymenoptera : Eulophidae) parasitic on Diorhabda elongata Brulle (Coleoptera : Chrysomelidae) and implications for the biological control of Saltcedar (Tamaricaceae : Tamarix spp.) in the southwestern United States SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Hymenoptera; Eulophidae; Baryscapus; Diorhabda; Tamarix; biocontrol AB Baryscapus diorhabdivorus Gates and Myartseva, new species, (Hymenoptera: Eulophidae) is described and illustrated. This species was reared from the salt-cedar leaf beetle, Diorhabda elongata Brulle (Coleoptera: Chrysomelidae), in Turkmenistan. It is compared to closely related species, and its implications for the biological control of Tamarix spp. are discussed. C1 USDA ARS, Systemat Entomol Lab, PSI, Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20013 USA. RP Gates, MW (reprint author), USDA ARS, Systemat Entomol Lab, PSI, Natl Museum Nat Hist,Smithsonian Inst, POB 37012,MRC 168, Washington, DC 20013 USA. EM mgates@sel.barc.usda.gov; smyartse@uamac.uat.mx; mschauff@sel.barc.usda.gov NR 8 TC 1 Z9 2 U1 1 U2 1 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD JAN PY 2005 VL 107 IS 1 BP 28 EP 33 PG 6 WC Entomology SC Entomology GA 887QC UT WOS:000226319600004 ER PT J AU Mawdsley, JR AF Mawdsley, JR TI Extirpation of a population of Cicindela patruela Dejean (Coleoptera : Carabidae : Cicindelini) in suburban Washington, DC, USA SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Cicindela patruela; tiger beetle; extirpation; conservation; restoration; management AB A population of Cicindela patruela patruela DeJean (Coleoptera: Carabidae: Cicindelini) existed until at least 1950 in a small area of eastern Washington, D.C., and adjacent Prince George's County, Maryland, USA. Suitable habitat for this population consisted of open sandy barrens with soils derived from Cretaceous sediments of the Potomac Group and vegetation characterized by oak and pine species, particularly Quercus marilandica Munchhausen and Pinus rigida Miller. This habitat was eliminated in the Washington area by extensive suburban housing construction, which was driven by rapid growth in the human population. Recommendations are provided for the reintroduction of C. patruela and for the restoration of suitable habitat at remnant natural areas. C1 Natl Museum Nat Hist, Smithsonian Inst, Dept Entomol, Washington, DC 20560 USA. RP Mawdsley, JR (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Dept Entomol, Washington, DC 20560 USA. EM jonathan.mawdsle@nfwf.org NR 25 TC 6 Z9 9 U1 1 U2 2 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD JAN PY 2005 VL 107 IS 1 BP 64 EP 70 PG 7 WC Entomology SC Entomology GA 887QC UT WOS:000226319600008 ER PT J AU Neunzig, HH Solis, MA AF Neunzig, HH Solis, MA TI Tumoriala, a new neotropical phycitine genus (Lepidoptera : Pyralidae) SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Phycitinae; Guatemala; Costa Rica; Brazil AB Tumoriala n. gen., is proposed for the Neotropical phycitine T. subaquilella (Ragonot 1888), n. comb. The previously unknown male is described and the occurrence of this species in Costa Rica and Brazil is reported for the first time. Males in the genus are characterized by a unique, raised cluster of scales on the upper surface of the forewing, and slender genitalia with a tegumen bearing earlike lobes. Females have a strongly developed diverticulum about midway on the ductus bursae. Photographs of the adults. and line drawings of male wing venation, labial palpus and antenna, and male and female genitalia are included. C1 N Carolina State Univ, Dept Entomol, Raleigh, NC 27695 USA. USDA ARS, PSI, Systemat Entomol Lab, Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20013 USA. RP Neunzig, HH (reprint author), N Carolina State Univ, Dept Entomol, Raleigh, NC 27695 USA. EM asolis@sel.barc.usda.gov NR 3 TC 2 Z9 2 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 JAN PY 2005 VL 107 IS 1 BP 84 EP 89 PG 6 WC Entomology SC Entomology GA 887QC UT WOS:000226319600011 ER PT J AU Smith, DR AF Smith, DR TI Review of the genus Acordulecera Say (Hymenoptera : Pergidae) of the West Indies, and the first records of symphyta from Montserrat and St. Kitts SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Review DE St. Vincent; Dominica; Lesser Antilles; neotropical; symphyta AB Three species of the pergid genus Acordulecera Say are recorded from the West Indies, A. montserratensis, n. sp.. from Montserrat. St. Kitts, and Dominica. A. longica, n. sp., from Dominica and Montserrat, and A. insularis Ashmead from St. Vincent and Dominica. Acordulecera montserratensis and A. longica are the first sawflies recorded from Montserrat, and A. montserratensis is the first sawfly known front St. Kitts. The species are keyed, described, illustrated, and separated from other species of Acordulecera. C1 USDA ARS, PSI, Systemat Entomol Lab, Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20013 USA. RP Smith, DR (reprint author), USDA ARS, PSI, Systemat Entomol Lab, Natl Museum Nat Hist,Smithsonian Inst, POB 37012,MRC 168, Washington, DC 20013 USA. EM dsmith@sel.barc.usda.gov NR 10 TC 3 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 JAN PY 2005 VL 107 IS 1 BP 99 EP 107 PG 9 WC Entomology SC Entomology GA 887QC UT WOS:000226319600013 ER PT J AU Hall, JPW AF Hall, JPW TI A review of the Metacharis syloes group (Lepidoptera : Riodinidae), with the description of two new species from west of The Andes SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Review DE allopatry; Andes; Ecuador; Metacharis; montane forest; Panama AB On the basis of male genitalia and wing pattern, the Neotropical riodinid genus Metacharis Butler is tentatively divided into four species groups, whose phylogenetic, inter-relation ships are briefly discussed. With this taxonomic framework established, the derived syloes group is here characterized and taxonomically elaborated. It contains one described species, M. syloes Hewitson, and two that are described here, M. fergusi, n. sp., and M. smalli, n. sp. These are the only Metacharis species to exclusively inhabit montane forest, and they are distributed allopatrically in the eastern Andes, western Andes, and mountains of central and eastern Panama, respectively. The elevation of M. umbrata Stichel to species status (n. stat.) is also discussed. C1 Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Hall, JPW (reprint author), Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, Washington, DC 20560 USA. NR 15 TC 3 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 JAN PY 2005 VL 107 IS 1 BP 200 EP 208 PG 9 WC Entomology SC Entomology GA 887QC UT WOS:000226319600022 ER PT J AU Wheeler, AG Henry, TJ AF Wheeler, AG Henry, TJ TI Description of the adult and fifth instar of a myrmecomorphic plant bug, Bicuspidatiella conica Maldonado (Hemiptera : Miridae : Deraeocorenae), with notes on its habits SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Heteroptera; myrmecomorphy; Puerto Rico; Sternorrhyncha; Nectandra turbacensis ID HETEROPTERA; ANTS AB The deraeocorine plant bug Bicuspidatiella conica Maldonado, belonging, to a monotypic genus in the tribe Hyaliodini, has been known only from five adults taken at three localities in Puerto Rico. Previous biological information consists of a record from guaba (Inga vera Willd.). The fifth instar and adult of this myrmecomorphic mirid, collected at Cayey, Puerto Rico, are described and figured. The species was found on laurel amarillo (Nectandra turbacensis (Kunth) Nees) in association with the formicine ant Myrmelachista ramulorum. Wheeler, the ant-attended mealybug Nipaecoccus nipae (Maskell) (Pseudococcidae), the soft scale Coccus moestus De Lotto (Coccidae), and an unidentified whitefly (Aleyrodidae). Bicuspidatiella conica, a member of an almost exclusively predacious group, probably feeds on ant-attended sternorrhynchans. C1 Clemson Univ, Dept Entomol Soils & Plant Sci, Clemson, SC 29634 USA. Smithsonian Inst, USDA, Systemat Ecol Lab, ARS,PSI,Natl Museum Nat Hist, Washington, DC 20560 USA. RP Wheeler, AG (reprint author), Clemson Univ, Dept Entomol Soils & Plant Sci, Clemson, SC 29634 USA. EM awhlr@clemson.edu; thenry@sel.barc.usda.gov NR 16 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 JAN PY 2005 VL 107 IS 1 BP 209 EP 213 PG 5 WC Entomology SC Entomology GA 887QC UT WOS:000226319600023 ER PT J AU Smith, DR AF Smith, DR TI A new sawfly (Hymenoptera : Pergidae) feeding on guava, Psidium guajava L. (Myrtaceae), in Costa Rica SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE symphyta; guava; Taiwanese guava C1 Smithsonian Inst, Natl Museum Nat Hist, Systemat Entomol Lab, PSI,Agr Res Serv,USDA, Washington, DC 20013 USA. RP Smith, DR (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Systemat Entomol Lab, PSI,Agr Res Serv,USDA, POB 37012,MRC 168, Washington, DC 20013 USA. EM dsmith@sel.barc.usda.gov NR 3 TC 1 Z9 2 U1 1 U2 2 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD JAN PY 2005 VL 107 IS 1 BP 214 EP 217 PG 4 WC Entomology SC Entomology GA 887QC UT WOS:000226319600024 ER PT J AU Cambra, RA Gonzalez, VH Wcislo, WT AF Cambra, RA Gonzalez, VH Wcislo, WT TI Description of the male, host associations, and new distribution records for Lophostigma cincta (du Buysson) (Hymenoptera : Mutillidae) SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Sphaeropthalminae; parasitism; Halictidae; Megalopta ID MEGALOPTA-GENALIS; ECUADORIA HYMENOPTERA; SWEAT BEES; HALICTIDAE AB The male of the mutillid wasp genus Lophostigma Mickel is described for the first time based on specimens of Lophostigma cincta (du Buysson). The sex association for L. cincta is based on individuals reared from nests of nocturnal sweat bees, Megalopta genalis (Meade-Waldo) and M. ecuadoria Friese (Hymenoptera: Halictidae). These bees are the first confirmed hosts for Lophostigma. We summarize the geographical distribution of L. cincta. C1 Smithsonian Trop Res Inst, Unit 0948, Balboa, Panama. Univ Kansas, Dept Ecol & Evolutionary Biol, Lawrence, KS 66045 USA. Univ Panama, Estafeta Univ, Museo Invertebrados GB Fairchild, Panama City, Panama. RP Cambra, RA (reprint author), Smithsonian Trop Res Inst, Unit 0948, APO AA 34002,Apartado 2072, Balboa, Panama. EM rcambra@ancon.up.ac.pa; vhgonza@ku.edu; wcislow@si.edu RI Gonzalez, Victor/B-4072-2015 NR 13 TC 4 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 JAN PY 2005 VL 107 IS 1 BP 229 EP 234 PG 6 WC Entomology SC Entomology GA 887QC UT WOS:000226319600026 ER PT J AU Rueda, LM Ma, Y Song, GH Gao, Q AF Rueda, LM Ma, Y Song, GH Gao, Q TI Notes on the distribution of Anopheles (Anopheles) sinensis Wiedemann (Diptera : Culicidae) in China and the status of some Anopheles hyrcanus group type specimens from China SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article C1 Walter Reed Army Inst Res, Dept Entomol, Walter Reed Biosystemat Unit, Silver Spring, MD 20910 USA. 2nd Mil Med Univ, Dept Etiol Biol, Shanghai 200433, Peoples R China. 2nd Mil Med Univ, Dept Parasitol, Shanghai 200433, Peoples R China. Inst Parasit Dis, Wuxi 214064, Jiangsu, Peoples R China. RP Rueda, LM (reprint author), Smithsonian Inst, Walter Reed Biosystemat Unit, MSC MRC 534, 4210 Silver Hill Rd, Suitland, MD 20746 USA. EM ruedapol@msc.si.edu NR 8 TC 6 Z9 6 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 JAN PY 2005 VL 107 IS 1 BP 235 EP 238 PG 4 WC Entomology SC Entomology GA 887QC UT WOS:000226319600027 ER PT J AU Lada, CJ AF Lada, CJ TI Star formation in the galaxy: An observational overview SO PROGRESS OF THEORETICAL PHYSICS SUPPLEMENT LA English DT Article; Proceedings Paper CT 19th Nishinomiya Yukawa Memorial Symposium CY NOV 01-02, 2004 CL Nishinomiya, JAPAN SP Nishinomiya City Board Educ, Phys Soc Japan, Ctr Divers & Univ Phys ID YOUNG STELLAR OBJECTS; L1630 MOLECULAR CLOUD; INITIAL MASS FUNCTION; ORION NEBULA CLUSTER; DENSE CORES; LUMINOSITY FUNCTIONS; TRAPEZIUM CLUSTER; CIRCUMSTELLAR DISKS; NANTEN OBSERVATIONS; PLANET FORMATION AB The problems of star and planet formation are among the most important challenges facing modern astrophysical research. Stars and their accompanying planetary systems are continuously being formed in the Galaxy enabling direct observation and investigation of the star forming process. However, stars form invisibly deep within cold and dark molecular clouds. Observations of these stellar birth sites at infrared and millimeter wavelengths from space and the ground have resulted in considerable progress toward a physical understanding of stellar origins. In this contribution I will review the empirical basis for our current understanding of the process of star formation with an emphasis on the origin of low mass (sunlike) stars. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Lada, CJ (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. EM clada@cfa.harvard.edu NR 76 TC 2 Z9 2 U1 0 U2 0 PU PROGRESS THEORETICAL PHYSICS PUBLICATION OFFICE PI KYOTO PA C/O KYOTO UNIV, YUKAWA HALL, KYOTO, 606-8502, JAPAN SN 0375-9687 J9 PROG THEOR PHYS SUPP JI Prog. Theor. Phys. Suppl. PY 2005 IS 158 BP 1 EP 23 PG 23 GA 955BK UT WOS:000231199500003 ER PT S AU Schwartz, DA AF Schwartz, DA BE Gurvits, LI Frey, S Rawlings, S TI An X-ray view of radio sources SO Radio Astronomy from Karl Jansky to Microjansky SE EAS PUBLICATIONS SERIES LA English DT Proceedings Paper CT Symposium on Radio Astronomy at 70 - From Karl Jansky to Microjansky CY AUG 27-30, 2003 CL Budapest, HUNGARY SP European Astron Soc, Hungarian Acad Sci, Eotvos Lorand Univ, Konkoly Observ, Eotvos Lorand Phys Soc, Netherlands Fdn Res Astron, Joint Inst VLBI, Hungarian Sci Res Fund, EC FP5 Infrastruct Cooperat Network RadioNET, EC FP6 Integrated Infrastruct Initiat RadioNET ID ACTIVE GALACTIC NUCLEI; HYDRA-A; COOLING FLOWS; CHANDRA OBSERVATIONS; INTRACLUSTER MEDIUM; PERSEUS CLUSTER; CRAB-NEBULA; LARGE-SCALE; SKY SURVEY; GALAXIES AB We review recent examples where the synergy between radio and X-ray observations has led to substantial progress in understanding astronomical systems. The sub-arcsecond imaging capabilities of the Chandra X-ray observatory provides a 100-fold improvement for comparing X-ray and radio structures. We specifically discuss examples which provide insight into the outflow of material and energy from pulsars and supernovae, the centers of clusters of galaxies, and the nuclei of quasars. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Schwartz, DA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 62 TC 1 Z9 1 U1 0 U2 0 PU E D P SCIENCES PI CEDEX A PA 17 AVE DU HOGGAR PARC D ACTIVITES COUTABOEUF BP 112, F-91944 CEDEX A, FRANCE SN 1633-4760 BN 2-86883-735-2 J9 EAS PUBLICATIONS PY 2005 VL 15 BP 353 EP 368 DI 10.1051/eas:2005163 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BED05 UT WOS:000236854400021 ER PT B AU Jaramillo, CA Munoz, F Cogollo, M De La Parra, F AF Jaramillo, CA Munoz, F Cogollo, M De La Parra, F BE Powell, AJ Riding, JB TI Quantitative biostratigraphy for the Cuervos Formation (Paleocene) of the Llanos foothills, Colombia: improving palynological resolution for oil exploration SO RECENT DEVELOPMENTS IN APPLIED BIOSTRATIGRAPHY SE MICROPALAEONTOLOGICAL SOCIETY SPECIAL PUBLICATIONS LA English DT Proceedings Paper CT Joint Meeting of the TMS/35th Annual Meeting of the American-Association-of-Stratigraphic-Palynologists/North American Micropaleontology Section of the SEPM CY SEP 11-13, 2002 CL Univ Coll London, London, ENGLAND SP TMS, Amer Assoc Stratigraph Palynol, SEPM, Amer Micropaleontol Sect HO Univ Coll London ID EASTERN CORDILLERA; ILANOS BASIN AB Oil exploration in Colombia has traditionally taken place in areas with relatively few structural complexities. However. in the last decade, exploration has moved to regions characterized by complex structural deformation, poor seismic resolution, and many stratigraphic problems, such as in the Llanos foothills. In this region, the major reservoirs occur in mostly continental Paleogene sequences, where palynomorphs are usually the only fossil group found. Tins, palynology has become an important tool in controlling the stratigraphic position of a well during drilling, in testing diverse seismic and structural interpretations, and correlating reservoirs. This study provides a biostratigraphic framework for the Cuervos Formation (Late Paleocene to earliest Eocene) of the Llanos and Llanos foothills, making use of graphic correlation. We used 14 sections with palynological information from outcrops, well cores, and well ditch cuttings. Five informal palynological zones are proposed. Based on the biostratigraphic model produced by this analysis, we reinterpreted a recently drilled well in the Llanos foothills upon which several previous interpretations had been made. A sidetrack of that well was subsequently drilled, validating the proposed model. This is a positive test that the biostratigraphic framework developed for the Cuervos Formation is reliable and can be successfully applied to exploration in the Llanos foothills. C1 Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. RP Jaramillo, CA (reprint author), Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. EM carlos@flmnh.ufl.edu NR 45 TC 8 Z9 8 U1 0 U2 1 PU GEOLOGICAL SOC PUBLISHING HOUSE PI BATH PA UNIT 7, BRASSMILL ENTERPRISE CTR, BRASSMILL LANE, BATH BA1 3JN, AVON, ENGLAND BN 1-86239-187-4 J9 MICROPAL SOC SPEC PU PY 2005 BP 145 EP 159 PG 15 WC Geology; Paleontology SC Geology; Paleontology GA BDM08 UT WOS:000234239500009 ER PT S AU Steinetz, BG Brown, JL Roth, TL Czekala, N AF Steinetz, BG Brown, JL Roth, TL Czekala, N BE Sherwood, OD Fields, PA Steinetz, BG TI Relaxin concentrations in serum and urine of endangered species - Correlations with physiologic events and use as a marker of pregnancy SO RELAXIN AND RELATED PEPTIDES: FOURTH INTERNATIONAL CONFERENCE SE ANNALS OF THE NEW YORK ACADEMY OF SCIENCES LA English DT Article; Proceedings Paper CT 4th International Conference on Relaxin and Related Peptides CY SEP, 2004 CL Moran, WY SP Univ Illinois Urbana Champaign Sch Mol & Cellular Biol, Bas Med, Immunodiagnostik AG, Lalor Fdn, March Dimes, NICHD, USDA, CSREES, Univ Guelph DE relaxin; endangered species; elephant; rhinoceros; giant panda; pregnancy ID PANDA AILUROPODA-MELANOLEUCA; ELEPHANT ELEPHAS-MAXIMUS; LOXODONTA-AFRICANA; DICERORHINUS-SUMATRENSIS; SUMATRAN-RHINOCEROS; LUTEINIZING-HORMONE; OVARIAN-FUNCTION; ASIAN ELEPHANTS; PROGESTERONE; RADIOIMMUNOASSAY AB Many mammalian species are facing extinction due to problems created by human encroachment, agriculture, pollution, and willful slaughter. Among those at risk are the Asian and African elephant, Sumatran rhinoceros, and giant panda. Conservation groups try to save species in the wild by preserving habitat and limiting animal-human conflicts, often with limited success. Another alternative is to preserve the extant gene pool through captive breeding as a hedge against extinction. Measurement of circulating reproductive hormones is impractical for most wildlife species; determination of urinary or fecal hormone metabolites provides a more viable approach. To aid breeding management, one important tool is the ability to diagnose and monitor pregnancy, especially in species with long gestations (e.g., rhinos over 15 mo and elephants over 20 mo). Unfortunately, measuring progestins often is not useful diagnostically, because concentrations are similar during at least part of the pregnancy and the nonpregnant luteal phase in some species (e.g., elephants, rhinoceroses, and giant pandas). As serum relaxin reliably distinguishes between pregnancy and pseudopregnancy in bitches, relaxin measurement might also provide a method for detecting a successful pregnancy in endangered species. Appropriate immunoassay reagents have enabled the estimation of relaxin concentrations in the serum of elephants and rhinos and the determination of pregnancy establishment and the outcome. Relaxin was also detected in panda serum and urine. However, the extreme variability of the time between observed mating and parturition and the confounding factors of delayed implantation, pseudopregnancy, and frequent fetal resorptions made it impossible to use the panda relaxin data as a specific marker of pregnancy. C1 NYU, Sch Med, Nelson Inst Environm Med, Dept Environm Med, Tuxedo Pk, NY 10987 USA. Smithsonian Inst, Conservat & Res Ctr, Dept Reprod Sci, Front Royal, VA 22630 USA. Ctr Conservat & Res Endangered Wildlife, Cincinnati, OH 45220 USA. Zool Soc San Diego, Ctr Reprod Endangered Species, San Diego, CA USA. RP Steinetz, BG (reprint author), NYU, Sch Med, Nelson Inst Environm Med, Dept Environm Med, Tuxedo Pk, NY 10987 USA. EM Steinetz@env.med.nyu.edu; Steinetz@env.med.nyu.edu NR 36 TC 13 Z9 14 U1 4 U2 18 PU NEW YORK ACAD SCIENCES PI NEW YORK PA 2 EAST 63RD ST, NEW YORK, NY 10021 USA SN 0077-8923 BN 1-57331-484-6 J9 ANN NY ACAD SCI JI Ann.NY Acad.Sci. PY 2005 VL 1041 BP 367 EP 378 DI 10.1196/annals.1282.057 PG 12 WC Biochemistry & Molecular Biology; Endocrinology & Metabolism; Multidisciplinary Sciences; Physiology SC Biochemistry & Molecular Biology; Endocrinology & Metabolism; Science & Technology - Other Topics; Physiology GA BCY07 UT WOS:000231831000057 PM 15956734 ER PT B AU Herken, G AF Herken, G BE Kelly, CC TI Science in the service of the state: The cautionary tale of Robert Oppenheimer SO REMEMBERING THE MANHATTAN PROJECT: PERSPECTIVES ON THE MAKING OF THE ATOMIC BOMB AND ITS LEGACY LA English DT Proceedings Paper CT Symposium on the Manhattan Project CY APR 27, 2002 CL Carnegie Inst Washington, Washington, DC SP Atom Heritage Fdn HO Carnegie Inst Washington C1 Smithsonian Inst, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 1 PU WORLD SCIENTIFIC PUBL CO PTE LTD PI SINGAPORE PA PO BOX 128 FARRER RD, SINGAPORE 9128, SINGAPORE BN 981-256-040-8 PY 2005 BP 69 EP 71 PG 3 WC History & Philosophy Of Science SC History & Philosophy of Science GA BDF74 UT WOS:000233299300010 ER PT J AU Penfold, LM Monfort, SL Wolfe, BA Citino, SB Wildt, DE AF Penfold, LM Monfort, SL Wolfe, BA Citino, SB Wildt, DE TI Reproductive physiology and artificial insemination studies in wild and captive gerenuk (Litocranius walleri walleri) SO REPRODUCTION FERTILITY AND DEVELOPMENT LA English DT Article DE artificial insemination; gerenuk; progestagen; progesterone; spermatozoa; testosterone AB Gerenuk antelope in North American zoos are descended from 28 founders imported from Kenya similar to 20 years ago. Intensive management is required to prevent inbreeding depression. Artificial insemination has potential for augmenting genetic management, but successful application requires a thorough understanding of species' reproductive norms. Semen collected from captive (n= 10) and wild ( n= 6) gerenuk contained low numbers of morphologically normal spermatozoa (similar to 40%). Age, but not season, influenced (P < 0.05) the proportion of morphologically normal spermatozoa (mean +/- s.e.m., 12-17 months of age, 10.3 +/- 1.9%; 18-26 months of age, 34.4 +/- 6.2%; 3-6 years of age, 40.0 +/- 4.7%). Seasonality was investigated by analysing faecal testosterone and progesterone in males and females, respectively, by radioimmunoassays. Females cycled all year ( ovarian cycle length, 18.7 +/- 0.9 days). Testosterone in males did not vary (P > 0.05) with time of year. Three females (3/9, 33%) became pregnant by insemination with 9.75 - 54.0 x 10(6) motile fresh or frozen sperm after oestrus synchronisation with two prostaglandin F-2 alpha injections, 12 days apart. One female inseminated with frozen - thawed sperm delivered a full-term stillborn calf after 213 days gestation. These results characterise gerenuk reproductive norms and indicate that artificial insemination may be a useful tool in the genetic management of gerenuk. C1 White Oak Conservat Ctr, Yulee, FL 32097 USA. Smithsonians Natl Zool Pk, Conservat & Res Ctr, Dept Reprod Sci, Front Royal, VA 22630 USA. N Carolina Zool Pk, Asheboro, NC 27205 USA. RP Penfold, LM (reprint author), White Oak Conservat Ctr, 581705 White Oak Rd, Yulee, FL 32097 USA. EM lindap@wogilman.com NR 26 TC 17 Z9 19 U1 1 U2 7 PU C S I R O PUBLISHING PI COLLINGWOOD PA 150 OXFORD ST, PO BOX 1139, COLLINGWOOD, VICTORIA 3066, AUSTRALIA SN 1031-3613 J9 REPROD FERT DEVELOP JI Reprod. Fertil. Dev. PY 2005 VL 17 IS 7 BP 707 EP 714 DI 10.1071/RD05077 PG 8 WC Developmental Biology; Reproductive Biology; Zoology SC Developmental Biology; Reproductive Biology; Zoology GA 979XX UT WOS:000232979600006 PM 16364224 ER PT S AU Heckadon-Moreno, S AF Heckadon-Moreno, S BE Harmon, RS TI Light and shadows in the management of the Panama Canal Watershed SO RIO CHAGRES, PANAMA: A MULTIDISCIPLINARY PROFILE OF A TROPICAL WATERSHED SE Water Science and Technology Library LA English DT Proceedings Paper CT International Scientific Symposium on Rio Chagres Panama - A Multidisciplinary Profile of a Tropical Watershed CY FEB 24-26, 2003 CL Gamboa, PANAMA DE Panama; Panama Canal Watershed; Rio Chagres; Proyecto de Monitoreo de la Cuenca del Canal AB This paper reviews the history of settlement in Panama and then summarizes the important findings of the Panama Canal Watershed Natural Resources Monitoring Project, a multidisciplinary study was conducted between 1996-1999. C1 Smithsonian Trop Res Inst, Balboa, Panama. RP Heckadon-Moreno, S (reprint author), Smithsonian Trop Res Inst, Balboa, Panama. NR 24 TC 3 Z9 3 U1 0 U2 4 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 0921-092X BN 1-4020-3298-6 J9 WATER SCI TECHNOL LI PY 2005 VL 52 BP 29 EP 44 PG 16 WC Forestry; Soil Science; Water Resources SC Forestry; Agriculture; Water Resources GA BDE87 UT WOS:000233165300003 ER PT S AU Perez, R Aguilar, S Somoza, A Condit, R Tejada, I Camargo, C Lao, S AF Perez, R Aguilar, S Somoza, A Condit, R Tejada, I Camargo, C Lao, S BE Harmon, RS TI Tree species composition and beta diversity in the upper Rio Chagres basin, Panama SO Rio Chagres, Panama: A Multidisciplinary Profile of a Tropical Watershed SE WATER SCIENCE AND TECHNOLOGY LIBRARY LA English DT Proceedings Paper CT International Scientific Symposium on Rio Chagres Panama - A Multidisciplinary Profile of a Tropical Watershed CY FEB 24-26, 2003 CL Gamboa, PANAMA DE Panama; Panama Canal Watershed; upper Rio Chagres basin; rain forest; tree species; beta-diversity ID FOREST; DROUGHT; IMPACT AB Tree species composition at two sites in the upper Rio Chagres basin of central Panama was evaluated using rapid inventory methods. At each site, two 40x40 in quadrats were demarcated, and each was thoroughly searched for tree and shrub species. The 40x40 in quadrats had a mean of 155 species each, and the four pooled had 285 species; 29 other species were noted along trails near the survey plots. These inventories were compared to 81 others within the Panama Canal Watershed, and forest composition and diversity was evaluated relative to mean dry season duration. The upper Rio Chagres sites have high rainfall and are rich in tree species relative to most of the area; the only area with higher diversity is the Santa Rita Ridge, along the Caribbean coast, which is even wetter. Many tree species are restricted to these wet areas of central Panama, not occurring in drier areas of the Pacific slope or central Panama. C1 Smithsonian Trop Res Inst, Balboa, Panama. RP Perez, R (reprint author), Smithsonian Trop Res Inst, Balboa, Panama. NR 15 TC 4 Z9 4 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 0921-092X BN 1-4020-3298-6 J9 WATER TRANS PY 2005 VL 52 BP 227 EP 235 PG 9 WC Forestry; Soil Science; Water Resources SC Forestry; Agriculture; Water Resources GA BDE87 UT WOS:000233165300014 ER PT S AU Ibanez, RD AF Ibanez, RD BE Harmon, RS TI A note on amphibians and reptiles in the upper Rio Chagres basin, Panama SO RIO CHAGRES, PANAMA: A MULTIDISCIPLINARY PROFILE OF A TROPICAL WATERSHED SE Water Science and Technology Library LA English DT Proceedings Paper CT International Scientific Symposium on Rio Chagres Panama - A Multidisciplinary Profile of a Tropical Watershed CY FEB 24-26, 2003 CL Gamboa, PANAMA DE Panama; Rio Chagres; herpetofauna; amphibians; reptiles AB Twenty-nine amphibians and six reptiles were recorded at a site in the upper Rio Chagres basin at the confluence of the Rio Chagrecito with the upper Rio Chagres. Most of them are assumed to be the common species, partly due to the brief time and search effort spent at the site. The amphibians and reptiles found at this site are also present in nearby sites, such as Las Pavas stream and along the Piedras-Pacora ridge. This survey provides information on the herpetofauna present in a virtually unexplored area of the upper Rio Chagres basin. The treefrog Hyla boons was not previously known from the upper Rio Chagres region. C1 Smithsonian Trop Res Inst, Balboa, Panama. RP Ibanez, RD (reprint author), Smithsonian Trop Res Inst, Balboa, Panama. NR 12 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 0921-092X BN 1-4020-3298-6 J9 WATER SCI TECHNOL LI PY 2005 VL 52 BP 237 EP 242 PG 6 WC Forestry; Soil Science; Water Resources SC Forestry; Agriculture; Water Resources GA BDE87 UT WOS:000233165300015 ER PT S AU Dick, CW Condit, R Bermingham, E AF Dick, CW Condit, R Bermingham, E BE Harmon, RS TI Biogeographic history and the high beta-diversity of rainforest trees in Panama SO RIO CHAGRES, PANAMA: A MULTIDISCIPLINARY PROFILE OF A TROPICAL WATERSHED SE Water Science and Technology Library LA English DT Proceedings Paper CT International Scientific Symposium on Rio Chagres Panama - A Multidisciplinary Profile of a Tropical Watershed CY FEB 24-26, 2003 CL Gamboa, PANAMA DE Panama; rain forest; tree species; biotic interchange; beta-diversity; biogeography ID DIVERSIFICATION; AMERICA AB In a recent study examining the degree to which tree species composition differs among rainforest sites (i.e., beta-diversity), Condit et al. (2002) found that plots in the Panama Canal Watershed separated by 50 km were more highly differentiated than plots in western Amazonia separated by nearly 1400 km. The high beta-diversity of trees in Panama was attributed to sharp environmental gradients between the Atlantic and Pacific coasts. However, the pattern may also result from Panama's history as a land bridge over which floras from Central America and South America mixed during the Great American Biotic Interchange (GABI) roughly 3 million years ago. Under this scenario, it would be expected that wetter Panamanian forests would contain more trees of South American origin, whereas drier Panamanian forests would have more trees of Mesoamerican origin due to the historical prevalence of dry habitats in Mesoamerica. This idea was tested by quantifying the geographic distributions of 714 tree species found in three sites in the Panama Canal Watershed, which represent a gradient in annual rainfall. Nearly identical proportions of geographic representation of trees among the three sites, with species distributions of ca. 15% Mesoamerican, 17% South American, 9% Panama endemic, and 59% widespread. These data do not support the biotic interchange hypothesis. However, this analysis found that 433 of the 714 tree species (61%) have a cross-Andean distribution, which suggests that these tree species may be sufficiently old to have participated in the GABI. C1 Smithsonian Trop Res Inst, Balboa, Panama. RP Dick, CW (reprint author), Smithsonian Trop Res Inst, Balboa, Panama. NR 22 TC 4 Z9 4 U1 1 U2 3 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 0921-092X BN 1-4020-3298-6 J9 WATER SCI TECHNOL LI PY 2005 VL 52 BP 259 EP 269 PG 11 WC Forestry; Soil Science; Water Resources SC Forestry; Agriculture; Water Resources GA BDE87 UT WOS:000233165300017 ER PT S AU Gurtner, W Noomen, R Pearlman, MR AF Gurtner, W Noomen, R Pearlman, MR BE Moore, P TI The International Laser Ranging Service: current status and future developments SO SATELLITE DYNAMICS IN THE ERA OF INTREDISCIPLINARY SPACE GEODESY SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT 35th COSPAR Scientific Assembly CY JUL 18-25, 2004 CL Paris, FRANCE SP Comm Space Res DE space geodesy; satellite laser ranging; geodynamics; terrestrial reference systems AB In 1998 the International Laser Ranging Service (ILRS) was founded as the second space geodesy service of the International Association of Geodesy (IAG). In order to fulfill the requirements of modern space geodetic applications and in accordance with the other services, the ILRS is in the process of improving its capabilities of data and product delivery with shorter latencies and better inter-service compatibilities. Observing and data analysis strategies are optimized in order to accentuate the inherent strengths of laser ranging, especially in the subsequent combination with products of the other space geodetic techniques. Operational costs of the laser ranging network are being reduced by an increased degree of automation of the tracking stations, which requires improvements in station hardware and software, operational procedures, communication, and prediction accuracy. (c) 2004 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 Univ Bern, Astron Inst, CH-3012 Bern, Switzerland. Delft Univ Technol, Fac Aerosp Engn, NL-2629 HS Delft, Netherlands. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Gurtner, W (reprint author), Univ Bern, Astron Inst, Sidlerstr 5, CH-3012 Bern, Switzerland. EM gurtner@aiub.unibe.ch NR 5 TC 4 Z9 9 U1 4 U2 5 PU ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD 0X5 1GB, OXON, ENGLAND SN 0273-1177 J9 ADV SPACE RES PY 2005 VL 36 IS 3 SI 2005 BP 327 EP 332 DI 10.1016/j.asr.2004.12.012 PG 6 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BDT66 UT WOS:000235247800002 ER PT J AU Carrano, MT AF Carrano, Matthew T. BE Rogers, KAC Wilson, JA TI The Evolution of Sauropod Locomotion MORPHOLOGICAL DIVERSITY OF A SECONDARILY QUADRUPEDAL RADIATION SO SAUROPODS: EVOLUTION AND PALEOBIOLOGY LA English DT Article; Book Chapter ID NON-AVIAN DINOSAURS; MAMMALS; HABITS; TRENDS; DIPLODOCUS; WEIGHT; ORIGIN; BIRDS C1 Smithsonian Inst, Dept Paleobiol, Washington, DC 20013 USA. RP Carrano, MT (reprint author), Smithsonian Inst, Dept Paleobiol, POB 37012,MRC 121, Washington, DC 20013 USA. EM carranom@si.edu RI Carrano, Matthew/C-7601-2011 OI Carrano, Matthew/0000-0003-2129-1612 NR 63 TC 26 Z9 27 U1 0 U2 4 PU UNIV CALIFORNIA PRESS PI BERKELEY PA 2120 BERKELEY WAY, BERKELEY, CA 94720 USA BN 978-0-520-93233-3 PY 2005 BP 229 EP 251 PG 23 WC Evolutionary Biology; Paleontology SC Evolutionary Biology; Paleontology GA BWD78 UT WOS:000293686700009 ER PT S AU DeLuca, EE Weber, MA Sette, AL Golub, L Shibasaki, K Sakao, T Kano, R AF DeLuca, EE Weber, MA Sette, AL Golub, L Shibasaki, K Sakao, T Kano, R BE Harra, LK Culhane, JL Harruson, RA TI Science of the X-ray Sun: The X-ray telescope on Solar-B SO SOLAR ENCOUNTER, SOLAR-B AND STEREO SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT 35th COSPAR Scientific Assembly CY JUL 18-25, 2004 CL Paris, FRANCE SP Comm Space Res DE solar corona; X-ray telescope; Solar-B AB The X-Ray Telescope (XRT) on Solar-B is designed to provide high resolution, high cadence observations of the X-ray corona through a wide range of filters. The XRT science team has identified four general problems in coronal physics as the primary science goals for our instrument. Each of these goals will require collaborative observations from the other Solar-B instruments: EUV Imaging Spectrograph (EIS) and Solar Optical Telescope Focal Plane Package (SOT). We will discuss the science goals and observations needed to address those goals. (c) 2005 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Natl Astron Observ, Nobeyama Radio Observ, Nagano 6841305, Japan. Natl Astron Observ, Mitaka, Tokyo 1818588, Japan. RP DeLuca, EE (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 58, Cambridge, MA 02138 USA. EM edeluca@cfa.harvard.edu; mweber@cfa.harvard.edu RI DeLuca, Edward/L-7534-2013 OI DeLuca, Edward/0000-0001-7416-2895 NR 6 TC 6 Z9 6 U1 0 U2 4 PU ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD 0X5 1GB, OXON, ENGLAND SN 0273-1177 J9 ADV SPACE RES PY 2005 VL 36 IS 8 SI 2005 BP 1489 EP 1493 DI 10.1016/j.asr.2004.12.073 PG 5 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BEC66 UT WOS:000236807600021 ER PT J AU Wilson, GL Ernst, CH AF Wilson, GL Ernst, CH TI Reproductive ecology of the Terrapene carolina carolina (Eastern Box Turtle) in Central Virginia SO SOUTHEASTERN NATURALIST LA English DT Article ID SEXUAL SIZE DIMORPHISM; POPULATION AB The reproductive ecology of Terrapene carolina carolina (Eastern Box Turtle) was studied in an 11-ha woods in Lynchburg, VA. Estimated population demographics included a population size of 176 turtles with a 1: 1 male to female sex ratio, population density of 16 turtles/ha, mean clutch size of 3.15 eggs, and a proportion of adult females gravid per year of 0.405. Reproductive output was 112 eggs per year. A positive significant relationship existed between female carapace width and clutch size, as well as female shell height and clutch size. However, no significant relationship existed between female carapace length (CL) and clutch size. When mean clutch size was compared to those of other investigators of T. c. carolina, a slight positive correlation with latitude was indicated. though it was not statistically significant. Mean female CL and clutch size in a Long Island population were both significantly larger than the means from the Virginia population. C1 Smithsonian Inst, Div Amphibians & Reptiles, Washington, DC 20013 USA. RP Wilson, GL (reprint author), 702 Jefferson St, Moscow, ID 83843 USA. EM gwilson@nsa.edu NR 39 TC 9 Z9 11 U1 2 U2 14 PU HUMBOLDT FIELD RESEARCH INST PI STEUBEN PA PO BOX 9, STEUBEN, ME 04680-0009 USA SN 1528-7092 J9 SOUTHEAST NAT JI Southeast. Nat. PY 2005 VL 4 IS 4 BP 689 EP 702 DI 10.1656/1528-7092(2005)004[0689:REOTTC]2.0.CO;2 PG 14 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 000XY UT WOS:000234496900009 ER PT S AU Huang, HC Kuan, YJ Charnley, SB Hirano, N Takakuwa, S Bourke, TL AF Huang, HC Kuan, YJ Charnley, SB Hirano, N Takakuwa, S Bourke, TL BE Bernstein, M NavarroGonzalez, R Raulin, R TI Organic molecules in the hot corinos and circumstellar disks of IRAS 16293-2422 SO SPACE LIFE SCIENCES: ASTROBIOLOGY: STEPS TOWARD ORIGIN OF LIFE AND TITAN BEFORE CASSINI SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT 35th COSPAR Scientific Assembly CY JUL 18-25, 2004 CL Paris, FRANCE SP Comm Space Res DE astrochemistry; ISM : abundances; ISM : individual (IRAS 16293-2422); ISM : molecules; radio lines; ISM - stars : formation ID PROTOSTAR IRAS 16293-2422; MASS STAR-FORMATION; YOUNG BINARY-SYSTEM; LINE SURVEY; DEUTERATED METHANOL; FORMING REGIONS; EARLY EARTH; CORE; ABUNDANCES; EMISSION AB Using the recently commissioned Submillimeter Array (SMA), we have detected several complex organic molecules, including (CH3)(2)O, C2H5OH, C2H5CN, and tentatively CH2CDCN, toward the protostellar hot cores of IRAS 16293-2422 at arcsecond-resolution (<= 400 AU in radius). Vibrationally excited transitions of SO, SO2 and HCN with energy levels up to 1800 K were also observed. In addition to the other organic molecules (HC3N, CH2CO, CH3OH, CH2CHCN and HCOOCH3) previously reported by us (Kuan, Y.-J., Huang, H.-C., Charnley, S.B., Hirano, H., Takakuwa, S., et al. Organic molecules in low-mass protostellar hot cores: submillitimeter imaging of IRAS 16293-2422. Astrophys. J. 616, 127-L30, 2004) these results clearly indicate the existence of a rich organic chemistry in low-mass 'hot corinos'. From the observation of optically thin (HCN)-N-15 emission, we conclude 116293A is a rotating circumstellar disk lying along the north-south direction similar to 10 degrees to the east and with an inclination similar to 30 degrees to the sky. We suggest that the observed vibrational SO and SO, emission may originate from shock waves near or in the circumstellar disks. Between the two cores, we find a strong anticorrelation in emission from C2H5OH and CH5CN. The relative contribution of gas phase and grain-surface chemistries to the production of the observed complex molecules is discussed. We point out the shortcomings underlying recent claims that all the O-bearing organics are formed on grains. The presence of so many well-known interstellar molecules in solar-type hot corinos strengthens the link between molecular cloud chemistry, the starting materials of protoplanetary disks such as the protosolar nebula.. and the composition of comets. Establishing the fine details of this connection is crucial in answering fundamental questions concerning the importance of galactic astrochemistry for astrobiology. (c) 2005 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 Natl Taiwan Normal Univ, Dept Earth Sci, Taipei 116, Taiwan. NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. Harvard Smithsonian Ctr Astrophys, Submillimeter Array Project, Hilo, HI 96721 USA. Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan. RP Huang, HC (reprint author), Natl Taiwan Normal Univ, Dept Earth Sci, 88 Sec 4 Tug Chou Rd, Taipei 116, Taiwan. EM hspring@sgrb2.geos.ntnu.edu.tw RI Charnley, Steven/C-9538-2012 NR 41 TC 13 Z9 13 U1 0 U2 2 PU ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD 0X5 1GB, OXON, ENGLAND SN 0273-1177 J9 ADV SPACE RES PY 2005 VL 36 IS 2 SI 2005 BP 146 EP 155 DI 10.1016/j.asr.2005.03.115 PG 10 WC Engineering, Aerospace; Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology; Meteorology & Atmospheric Sciences GA BDT05 UT WOS:000235191500003 ER PT S AU Cosmo, ML Lorenzini, EC Bombardelli, C AF Cosmo, ML Lorenzini, EC Bombardelli, C BE Coffey, SL Coffey, SL Mazzoleni, AP Luu, KK Glover, RA TI Space tethers as testbeds for spacecraft formation-flying SO Spaceflight Mechanics 2004, Vol 119, Pt 1-3 SE ADVANCES IN THE ASTRONAUTICAL SCIENCES LA English DT Proceedings Paper CT AAS/AIAA 14th Space Flight Mechanics Meeting CY FEB 08-12, 2004 CL Maui, HI SP AAS, Amer Inst Aeronaut & Astronaut ID ORBITING INTERFEROMETER SATELLITE AB We analyze the dynamics of a tethered demonstrator proposed for testing elements of formation flying for space-based interferometry. A tether connecting the space vehicles offers the dual advantage of being the main structural component that keeps the spacecraft together and acting as the control actuator to reposition the formation. Moreover, when used for a spinning formation the tethered configuration can hold an inertial pointing while keeping the formation together with no expenditure of fuel. In order to minimize the disturbance of the environmental perturbations, the proposed intererometric missions are planned to fly at the Sun-Earth Lagrangian points or in Earth trailing orbit. The demonstrator is meant as a low-cost mission to be flown in low Earth orbit to test actuators, sensors and control algorithms required for formation flying in a representative dynamic environment. The orbital characteristics have been chosen with the goal of minimizing dynamic effects due to Earth's oblateness and to provide over a relatively long period of time almost constant thermal inputs and solar pressure which typical of higher orbits. In this paper, we analyze the effect of external perturbations on the inertial pointing of the formation and preliminary control strategies for deploying the tethered demonstrator. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Cosmo, ML (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS80, Cambridge, MA 02138 USA. NR 10 TC 0 Z9 0 U1 0 U2 0 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 0-87703-515-6 J9 ADV ASTRONAUT SCI PY 2005 VL 119 BP 1083 EP 1094 PN 1-3 PG 12 WC Automation & Control Systems; Engineering, Aerospace; Mechanics SC Automation & Control Systems; Engineering; Mechanics GA BBZ98 UT WOS:000228444908066 ER PT S AU Wang, Z Penprase, BE Fazio, GG Willner, SP Ashby, MLN Smith, HA AF Wang, Z Penprase, BE Fazio, GG Willner, SP Ashby, MLN Smith, HA BE Popescu, CC Tuffs, RJ TI Measuring star forming activities in the antennae: Region-by-region SO Spectral Energy Distributions of Gas-Rich Galaxies: Confronting Models with Data SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT International Workshop on Spectral Energy Distributions of Gas-Rich Galaxies CY OCT 04-08, 2004 CL Max Planck Inst, Nucl Phys, Heidelberg, GERMANY HO Max Planck Inst, Nucl Phys ID GALAXIES AB The Antennae is a proto-typical case of a pair of gas-rich galaxies in the process of merging, while experiencing active star formation. Recently obtained mid-IR data with the Spitzer Space Telescope provide new information on the nature of star forming regions in this system, complementary to the high resolution optical images from the Hubble and earlier IR data from ISO. By cross-referencing the optical emission line regions, individual star clusters can be identified and their colors and SEDs measured and compared with theoretical models. With this approach we are able to study previously unremarkable regions of active star formation, and find evidence that star formation may be triggered by the gravitational interaction in a sequential process. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Wang, Z (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. 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 0-7354-0246-9 J9 AIP CONF PROC PY 2005 VL 761 BP 433 EP 436 PG 4 WC Astronomy & Astrophysics; Spectroscopy SC Astronomy & Astrophysics; Spectroscopy GA BCE89 UT WOS:000228963700051 ER PT J AU Ballard, MW AF Ballard, MW TI Dyes in history and archaeology 19: Including papers presented at the 19th meeting held at the Royal Museum, National Museums of Scotland, Edinburgh, 19-20 October 2000 SO STUDIES IN CONSERVATION LA English DT Book Review C1 Smithsonian Ctr Mat Res & Educ, Washington, DC USA. RP Ballard, MW (reprint author), Smithsonian Ctr Mat Res & Educ, Washington, DC USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU INT INST CONSERVATION HISTORIC ARTISTIC WORKS PI LONDON PA 6 BUCKINGHAM ST, LONDON WC2N 6BA, ENGLAND SN 0039-3630 J9 STUD CONSERV JI Stud. Conserv. PY 2005 VL 50 IS 3 BP 235 EP 236 PG 2 WC Archaeology; Art; Chemistry, Applied; Chemistry, Analytical; Spectroscopy SC Archaeology; Art; Chemistry; Spectroscopy GA 026SG UT WOS:000236361900008 ER PT J AU Gillespie, LJ Soreng, RJ AF Gillespie, LJ Soreng, RJ TI A phylogenetic analysis of the bluegrass genus Poa based on cpDNA restriction site data SO SYSTEMATIC BOTANY LA English DT Article ID CHLOROPLAST-DNA; NONCODING REGIONS; UNIVERSAL PRIMERS; POACEAE; GRAMINEAE; SEQUENCES; TRITICEAE; ORIGIN; AMPLIFICATION; LOCALIZATION AB oa, with about 575 species, is the largest genus of grasses, and has diversified throughout temperate, boreal, and arctic regions, and similar habitats through the tropics. This new phylogenetic study of Poa based on analysis of restriction site data from PCR amplified regions of chloroplast DNA (trnT-trnF trnF-trnV trnV-rbcL, rbcL-ORF106, trnH-trnK) expands previous sampling in the genus to where 1/5 to 1/6 of the species have been characterized for chloroplast DNA, types. A broad phylogenetic structure detected in a previous study using restriction site mapping of Poa chloroplast DNA, gained additional and robust support. Accounting for extended intra- and extrageneric sampling, Poa remains monophyletic if Austrofestuca and Parodiochloa are included as sections within P subg. Poa, and if Poa subg. Andinae is removed from the genus. Two new combinations are made: Poa sect. Austrofestuca and Poa secL Parodiochloa. This new analysis supports the recognition of five major clades within Poa: 1) ArcSyl, Pea subg. Arctopoa sects. Arctopoa and Aphydris, and P subg. Poa sect. Sylvestres; 2) BAPO, R subg. Poa sects. (Bolbophorum + Alpinae) (Parodiochloa + Ochlopoa); 3) SPOSTA, P subg. Poa sects. (Secundae (Pandemos (Orienos + Stenopoa + Tichopoa + Abbreviatae))); 4) PoM, P. subg. Poa sects. (Poa + Macropoa); 5) HAM-BADD, R subg. Poa sects. (Homalopoa, Acutifolae, Brizoides, Madropoa, Austrofestuca, Dasypoa, Dioicopoa, and informal groups "Punapoa" and "Australopoa"). These clades diverge in the following arrangement from the outgroups: ArcSyl (BAPO (SPOSTA ((PoM) (HAMBADD))). C1 Canadian Museum Nat, Div Res, Ottawa, ON K1P 6P4, Canada. Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Gillespie, LJ (reprint author), Canadian Museum Nat, Div Res, POB 3443 Stn D, Ottawa, ON K1P 6P4, Canada. EM lgillespie@mus-nature.ca; sorengr@si.edu NR 93 TC 41 Z9 60 U1 0 U2 11 PU AMER SOC PLANT TAXONOMISTS PI BRONX PA NEW YORK BOTANICAL GARDEN, BRONX, NY 10458-5126 USA SN 0363-6445 J9 SYST BOT JI Syst. Bot. PD JAN-MAR PY 2005 VL 30 IS 1 BP 84 EP 105 DI 10.1600/0363644053661940 PG 22 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA 901PA UT WOS:000227293200007 ER PT J AU Ferrucci, MS Acevedo-Rodriguez, P AF Ferrucci, MS Acevedo-Rodriguez, P TI Three new species of Serjania (Sapindaceae) from south America SO SYSTEMATIC BOTANY LA English DT Article AB The new species Serjania chacoensis from Bolivia and Brazil, Serjania souzana from Bolivia, Brazil, and Peru, and Serjania paranensis from the state of Parana, Brazil, all belonging to Serjania sect. Serjania, are described, illustrated and contrasted to their putatively closest relatives. C1 Consejo Nacl Invest Cient & Tecn, UNNE, Inst Bot Nordeste, RA-3400 Corrientes, Argentina. Smithsonian Inst, Dept Bot, Washington, DC 20013 USA. RP Ferrucci, MS (reprint author), Consejo Nacl Invest Cient & Tecn, UNNE, Inst Bot Nordeste, Casilla Correo 209, RA-3400 Corrientes, Argentina. EM ibone@agr.unne.edu.ar; acevedo.pedro@nmnh.si.edu NR 15 TC 8 Z9 9 U1 0 U2 0 PU AMER SOC PLANT TAXONOMISTS PI BRONX PA NEW YORK BOTANICAL GARDEN, BRONX, NY 10458-5126 USA SN 0363-6445 J9 SYST BOT JI Syst. Bot. PD JAN-MAR PY 2005 VL 30 IS 1 BP 153 EP 162 DI 10.1600/0363644053661904 PG 10 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA 901PA UT WOS:000227293200012 ER PT J AU Basset, Y Springate, ND Charles, E AF Basset, Yves Springate, Neil D. Charles, Elroy BE Hammond, DS TI Folivorous Insects in the Rainforests of the Guianas SO TROPICAL FORESTS OF THE GUIANA SHIELD: ANCIENT FORESTS IN A MODERN WORLD LA English DT Article; Book Chapter ID ATTA-CEPHALOTES L; L HYMENOPTERA-FORMICIDAE; LEAF-CUTTING ANTS; FRENCH-GUIANA; NEOTROPICAL FOREST; MORABALLI CREEK; BRITISH GUIANA; LIMITED-AREA; HERBIVORY; GUYANA C1 [Basset, Yves] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Springate, Neil D.] Nat Hist Museum, Dept Entomol, London SW7 5BD, England. [Charles, Elroy] Univ Guyana, Fac Agr Forestry, Georgetown, Guyana. RP Basset, Y (reprint author), Smithsonian Trop Res Inst, Apartado 2072, Balboa, Ancon, Panama. EM bassety@tivoli.si.edu; nds@nhm.ac.uk; elroy_c@yahoo.co.uk NR 159 TC 3 Z9 3 U1 0 U2 1 PU CABI PUBLISHING-C A B INT PI WALLINGFORD PA CABI PUBLISHING, WALLINGFORD 0X10 8DE, OXON, ENGLAND BN 978-0-85199-536-6 PY 2005 BP 295 EP 320 DI 10.1079/9780851995366.0295 D2 10.1079/9780851995366.0000 PG 26 WC Ecology; Forestry SC Environmental Sciences & Ecology; Forestry GA BVZ69 UT WOS:000293215500005 ER PT S AU Desai, P Brickhouse, NS Drake, JJ Edgar, RJ Hoogerwerf, R Kashyap, V Wargelin, BJ Smith, RK Huenemoerder, DP Liedahl, DA AF Desai, P Brickhouse, NS Drake, JJ Edgar, RJ Hoogerwerf, R Kashyap, V Wargelin, BJ Smith, RK Huenemoerder, DP Liedahl, DA BE Smith, RK TI Comparison of Fe XVIII and Fe XIX line emissions with spectral models SO X-RAY DIAGNOSTICS OF ASTROPHYSICAL PLASMAS: THEORY, EXPERIMENT, AND OBSERVATION SE AIP Conference Proceedings LA English DT Proceedings Paper CT Conference on X-Ray Diagnostics of Astrophysical Plasmas - Theory, Experiment, and Observation CY NOV 15-17, 2004 CL Cambridge, MA ID CAPELLA AB We discuss here the observations of Fe XVIII and XIX emission lines and compare the X-ray, EUV and FUV lines with the spectral codes widely used today (e.g. FAC and APEC). We assess the relative accuracy of these spectral models and try to identify the critical atomic data and processes. Capella with a narrow enhancement in its emission measure distribution at 6 MK provides a unique opportunity to test the Fe XVIII and Fe XIX model emissivities which peak from 6 to 8 MK. We use the summed spectra from Chandra HETG/ACIS-S and LETG/HRC-S, as well as contemporaneous EUVE and FUSE observations, to measure line ratios for comparison with predictions. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 8 TC 0 Z9 0 U1 1 U2 1 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0259-0 J9 AIP CONF PROC PY 2005 VL 774 BP 155 EP 157 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BCS46 UT WOS:000231041800017 ER PT S AU Rakowski, CE AF Rakowski, CE BE Smith, RK TI X-ray diagnostics of ionizing plasmas in collisionless shocks SO X-RAY DIAGNOSTICS OF ASTROPHYSICAL PLASMAS: THEORY, EXPERIMENT, AND OBSERVATION SE AIP Conference Proceedings LA English DT Proceedings Paper CT Conference on X-Ray Diagnostics of Astrophysical Plasmas - Theory, Experiment, and Observation CY NOV 15-17, 2004 CL Cambridge, MA DE collisionless shocks; non-equilibrium ionization; supemova remnants; Li-like ions ID INNER-SHELL TRANSITIONS; HELIUM-LIKE IONS; SOLAR-FLARES; TRANSIENT PLASMAS; ATOMIC PHYSICS; LINE RATIOS; SPECTRA; SPECTROSCOPY; EMISSION; TEMPERATURE AB Although collisional ionization equilibrium conditions have been much more thoroughly studied, many astrophysical situations involve timescales that are shorter than the time it would take for ionization equilibrium to have been achieved. In plasmas out of equilibrium ionization the ion fractions cannot be assumed to be a simple function of the electron temperature, but rather must be independently assessed before comparisons can be made of the relative abundances of different elements. The emission spectrum is a function of both the temperature of the surrounding electrons, U, as well as the ionization timescale, n(e)t which, together with kTe determines the current charge state distribution. The accuracy of measuring an ionization timescale from the X-ray spectrum depends strongly on our knowledge of the ionization and recombination rates as well the emission processes. However, lines that are only strong in a rapidly ionizing plasma could provide a separate proof of non-equilibrium conditions distinct from diagnostics that are indicative of the temperature or ion fractions. In this talk I will present examples of both traditional temperature diagnostics as well as lines that would be undetectable in anything other than a rapidly ionizing plasma. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-70, 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 0-7354-0259-0 J9 AIP CONF PROC PY 2005 VL 774 BP 203 EP 211 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BCS46 UT WOS:000231041800023 ER PT S AU Kharchenko, V AF Kharchenko, V BE Smith, RK TI Charge-exchange mechanism of X-ray emission SO X-RAY DIAGNOSTICS OF ASTROPHYSICAL PLASMAS: THEORY, EXPERIMENT, AND OBSERVATION SE AIP Conference Proceedings LA English DT Proceedings Paper CT Conference on X-Ray Diagnostics of Astrophysical Plasmas - Theory, Experiment, and Observation CY NOV 15-17, 2004 CL Cambridge, MA DE cometary and heliospheric X-rays; highly charged solar wind ions; charge-exchange collisions ID SOLAR-WIND IONS; EXTREME-ULTRAVIOLET EMISSION; LOCAL INTERSTELLAR-MEDIUM; COMET HYAKUTAKE; XMM-NEWTON; C/1999 S4; SPECTRA; JUPITER; DISCOVERY; NEUTRALS AB The charge-exchange mechanism of X-ray emissions induced by the solar wind ions from cometary and planetary atmospheres and interstellar gas is discussed. The X-ray photon spectra of individual ions, such as highly charged Oq+, Cq+, Nq+ Neq+ and other ions, are described in detail. Cascading spectra of X-ray and EUV emissions of heavy solar wind ions are calculated for different ion velocities and compared with the results of laboratory measurements. Relative intensities of different spectral lines of the charge-exchange X-ray/EUV emission are used for the remote diagnostic of the compositions and velocities of the solar wind plasma. Synthetic X-ray spectra, computed for the slow and fast solar winds, are applied for the analysis of observed cometary and planetary X-rays and predictions of X-ray spectra from interstellar gas. The contribution of charge-transfer emission to the X-ray diffuse background is discussed. Brightness maps of the charge-exchange source of X-ray in the heliosphere are constructed taking into account the anisotropy of the solar wind plasma and a realistic distribution of the H and He gas. C1 Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. RP Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. NR 44 TC 7 Z9 7 U1 0 U2 2 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0259-0 J9 AIP CONF PROC PY 2005 VL 774 BP 271 EP 280 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BCS46 UT WOS:000231041800031 ER PT S AU Silver, E Schnopper, HW Jones, C Forman, W Romaine, S Madden, N Landis, D Beeman, J Haller, EE Barbera, M Christensen, F Ramsey, B Woosley, S Diehl, R AF Silver, E Schnopper, HW Jones, C Forman, W Romaine, S Madden, N Landis, D Beeman, J Haller, EE Barbera, M Christensen, F Ramsey, B Woosley, S Diehl, R BE Smith, RK TI High energy, high resolution X-ray spectroscopy: Microcalorimeters for nuclear line astrophysics SO X-RAY DIAGNOSTICS OF ASTROPHYSICAL PLASMAS: THEORY, EXPERIMENT, AND OBSERVATION SE AIP Conference Proceedings LA English DT Proceedings Paper CT Conference on X-Ray Diagnostics of Astrophysical Plasmas - Theory, Experiment, and Observation CY NOV 15-17, 2004 CL Cambridge, MA AB We introduce focusing optics and microcalorimeter spectroscopy to nuclear line emission astrophysics with a balloon payload concept called, B-MINE. It is designed to probe the deepest regions of a supernova explosion by detecting Ti-44 emission at 68 keV with spatial and spectral resolutions that are sufficient to determine the velocity distribution of the Ti-44 emitting region. B-MINE has a thin plastic foil telescope multilayered to maximize the reflectivity in a 20 keV band centered at 68 keV and a microcalorimeter array optimized for the same energy band. This combination provides a reduced background, an energy resolution of 50 eV and a 3 sigma sensitivity in 10(6) s of 6 x 10(-8) ph cm(-2) s(-1) at 68 keV. During the course of a long duration balloon flight, B-MINE could carry out a detailed study of the Ti-44 emission line centroids and width in CAS A. Details of the spectrometer and simulated results are presented. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. OI Barbera, Marco/0000-0002-3188-7420; Forman, William/0000-0002-9478-1682 NR 7 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 0-7354-0259-0 J9 AIP CONF PROC PY 2005 VL 774 BP 391 EP 399 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BCS46 UT WOS:000231041800052 ER PT S AU Brickhouse, NS Desai, P Hoogerwerf, R Liedahl, DA Smith, RK AF Brickhouse, NS Desai, P Hoogerwerf, R Liedahl, DA Smith, RK BE Smith, RK TI Progress and plans for the astrophysical plasma emission code (APEC) SO X-RAY DIAGNOSTICS OF ASTROPHYSICAL PLASMAS: THEORY, EXPERIMENT, AND OBSERVATION SE AIP Conference Proceedings LA English DT Proceedings Paper CT Conference on X-Ray Diagnostics of Astrophysical Plasmas - Theory, Experiment, and Observation CY NOV 15-17, 2004 CL Cambridge, MA DE atomic processes; X-rays ID LABORATORY MEASUREMENTS; FE-XVII; TRANSITIONS; INTENSITY AB APEC models for collisional ionization equilibrium are now available. These basic models have been benchmarked against astrophysical coronal spectra and show reasonable agreement; however, several atomic data issues need to be addressed. We plan to conduct an atomic data needs assessment and set priorities over the next year. New tools are under development to broaden the applicability of APEC models. We discuss the status of this development. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 9 TC 4 Z9 4 U1 1 U2 1 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0259-0 J9 AIP CONF PROC PY 2005 VL 774 BP 405 EP 407 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BCS46 UT WOS:000231041800054 ER PT S AU Ousley, SD Billeck, WT Hollinger, RE AF Ousley, SD Billeck, WT Hollinger, RE BE Stinson, S TI Federal repatriation legislation and the role of physical anthropology in repatriation SO YEARBOOK OF PHYSICAL ANTHROPOLOGY, VOL 48 SE Yearbook of Physical Anthropology LA English DT Article; Book Chapter DE NAGPRA; NMAIA; forensic anthropology; cultural affiliation ID MANDIBULAR RAMUS FLEXURE; MULTIVARIATE-ANALYSIS; SKELETAL REMAINS; MORPHOLOGIC INDICATOR; SEXUAL-DIMORPHISM; TECHNICAL NOTE; SECULAR CHANGE; UNITED-STATES; ANCIENT DNA; BLIND TEST AB Two laws governing the disposition of Native American human remains in museums and institutions have had a profound impact on anthropology, and especially physical anthropology. In contrast to the perception of constant conflict between Native Americans and physical anthropologists, the repatriation process based on these laws has been in large part harmonious between institutions and Native peoples in the US. Despite misconceptions, the Native American Graves Protection and Repatriation Act (NAPGRA; 25 United States Code (U.S.C.) 3001-3013) was not intended to halt further research on Native American remains in museums. In fact, court decisions have affirmed that the documentation of human remains produces information no other methods can provide, and provides necessary evidence to be incorporated and weighed, along with other evidence, in evaluating "cultural affiliation," the legal term for the required connection from federally recognized Native American groups to their ancestors. The wide variety of osteological data collected at the National Museum of Natural History (NMNH), Smithsonian Institution, have proven indispensable when evaluating cultural affiliation, especially when other information sources are unhelpful or ambiguous, and provide an empirical basis for determining the ancestry of individuals whose remains will be discovered in the future. To date, the claim-driven process at the NMNH has resulted in the affiliation and repatriation of more Native American remains than any other institution in the country. Repatriation experiences at the NMNH demonstrate the changing relationships between museums and Native peoples, the continuing important contributions that physical anthropology makes to the repatriation process, and the importance of physical anthropology in understanding the recent and ancient history of North America. C1 Smithsonian Inst, Natl Museum Nat Hist, Repatriat Off, Dept Anthropol, Washington, DC 20013 USA. RP Ousley, SD (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Repatriat Off, Dept Anthropol, MRC 138,POB 37012, Washington, DC 20013 USA. EM ousleys@si.edu NR 171 TC 20 Z9 21 U1 2 U2 15 PU WILEY-LISS, INC PI NEW YORK PA 605 THIRD AVE, NEW YORK, NY 10158-0012 USA SN 0096-848X J9 YEARB PHYS ANTHROPOL JI Yearb. Phys. Anthropol. PY 2005 VL 48 BP 2 EP 32 DI 10.1002/ajpa.20354 PG 31 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA BDS04 UT WOS:000235159600002 ER PT S AU Chen, Y Su, Y Slane, PO Wang, QD AF Chen, Y Su, Y Slane, PO Wang, QD BE Rakowski, C Chatterjee, S TI Highly clumpy structure of the thermal composite supernova remnant 3C 391 unveiled by Chandra SO YOUNG NEUTRON STARS AND SUPERNOVA REMNANTS SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT 35th COSPAR Scientific Assembly CY JUL 18-25, 2004 CL Paris, FRANCE SP Comm Space Res DE radiation mechanism; thermal radiation; ISM; supernova remnants; 3C391(G31.9+0.0); X-rays ID 3C 391; CASSIOPEIA AB The nature of the internal thermal X-ray emission seen in "thermal composite" supernova remnants is still uncertain. Chandra observation of the 3091 shows a southeast-northwest elongated morphology and unveils a highly clumpy structure of the remnant. Detailed spatially resolved spectral analysis for the small-scale features reveals normal metal abundance and uniform temperature for the interior gas. The properties of the hot gas comparatively favor the cloudlet evaporation model as a main mechanism for the "thermal composite" X-ray appearance, though radiative rim and thermal conduction may also be effective. A faint protrusion is found in Si and S lines out of the southwest radio border. (c) 2005 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 Nanjing Univ, Dept Astron, Nanjing 210093, Jiangsu, Peoples R China. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. RP Chen, Y (reprint author), Nanjing Univ, Dept Astron, 22 Hankou Rd, Nanjing 210093, Jiangsu, Peoples R China. EM ygchen@nju.edu.cn NR 13 TC 0 Z9 0 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI KIDLINGTON PA THE BOULEVARD, LANGFORD LANE,, KIDLINGTON OX5 1GB, OXFORD, ENGLAND SN 0273-1177 J9 ADV SPACE RES PY 2005 VL 35 IS 6 BP 1007 EP 1011 DI 10.1016/j.asr.2005.01.005 PG 5 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BCX77 UT WOS:000231793600006 ER PT S AU Rakowski, CE AF Rakowski, CE BE Rakowski, C Chatterjee, S TI Electron-ion temperature equilibration at collisionless shocks in supernova remnants SO YOUNG NEUTRON STARS AND SUPERNOVA REMNANTS SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT 35th COSPAR Scientific Assembly CY JUL 18-25, 2004 CL Paris, FRANCE SP Comm Space Res DE shock waves; supernova remnants; cosmic rays; X-rays : ISM; ISM : individual (Cygnus Loop, RCW 86, DEM L71, Tycho's supernova remnant, SN 1006, 1E 0102.2-7219); supernovae : individual (SN 1987A) ID X-RAY-EMISSION; LARGE-MAGELLANIC-CLOUD; NONRADIATIVE SHOCKS; BLAST WAVES; CYGNUS LOOP; PHYSICS; EXPANSION; SPECTRUM; SN-1006 AB The topic of this review is the current state of our knowledge about the degree of initial equilibration between electrons, protons and ions at supernova remnant (SNR) shocks. Specifically, the question has been raised as to whether there is an inverse relationship between the shock velocity and the equilibration. This review aims to compile every method that has been used to measure the equilibration and every SNR on which they have been tested. I review each method, its problems and uncertainties and how those would effect the degree of equilibration (or velocity) inferred. The final compilation of observed electron to proton temperature ratios as a function of shock velocity gives an accurate, conservative picture of the state of our knowledge and the avenues we need to pursue to make progress in our understanding of the relation between the velocity of a shock and the degree of equilibration. (c) 2005 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 Harvard Univ, Smithsonian Ctr Astrophys, High Energy Astrophy Div, Cambridge, MA 02138 USA. RP Rakowski, CE (reprint author), Harvard Univ, Smithsonian Ctr Astrophys, High Energy Astrophy Div, 60 Garden St,MS-70, Cambridge, MA 02138 USA. EM crakowski@cfa.harvard.edu NR 20 TC 37 Z9 38 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI KIDLINGTON PA THE BOULEVARD, LANGFORD LANE,, KIDLINGTON OX5 1GB, OXFORD, ENGLAND SN 0273-1177 J9 ADV SPACE RES PY 2005 VL 35 IS 6 BP 1017 EP 1026 DI 10.1016/j.asr.2005.03.131 PG 10 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BCX77 UT WOS:000231793600008 ER PT S AU Baring, MG Ellison, DC Slane, PO AF Baring, MG Ellison, DC Slane, PO BE Rakowski, C Chatterjee, S TI Multiwavelength spectral models for SNR G347.3-0.5 from non-linear shock acceleration SO YOUNG NEUTRON STARS AND SUPERNOVA REMNANTS SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT 35th COSPAR Scientific Assembly CY JUL 18-25, 2004 CL Paris, FRANCE SP Comm Space Res DE supernova remnants; shock acceleration; cosmic rays; inverse Compton scattering; synchrotron radiation; imaging atmospheric Cerenkov telescopes ID GAMMA-RAY EMISSION; SUPERNOVA REMNANT G347.3-0.5; PARTICLE-ACCELERATION; RX J1713.7-3946; COSMIC-RAYS; SHELL; DISCOVERY; ORIGIN; RADIO AB The remnant G347.3-0.5 exhibits strong shell emission in the radio and X-ray bands, and has a purported detection in the TeV gamma-ray band by the CANGAROO-II telescope. The CANGAROO results were touted as evidence for the production of cosmic ray ions, a claim that has proven controversial due to constraining fluxes associated with a proximate unidentified EGRET source 3EG J1714-3857. HESS has now seen this source in the TeV band. The complex environment of the remnant renders modeling of its broadband spectrum sensitive to assumptions concerning the nature and parameters of the circurnremnant medium. This paper explores a sampling of reasonable possibilities for multiwavelength spectral predictions from this source, using a non-linear model of diffusive particle acceleration at the shocked shell. The magnetic field strength, shell size and degree of particle cross-field diffusion act as variables to which the radio to X-ray to gamma-ray signal is sensitive. The modeling of the extant data constrains these variables, and the potential impact of the recent HESS detection on such parameters is addressed. Putative pion decay signals in hard gamma-rays resulting from hadronic interactions in dense molecular clouds are briefly discussed; the requisite suppression of the GeV component needed to accommodate the 3EG J1714-3857 EGRET data provides potential bounds on the diffusive distance from the shell to the proximate clouds. (c) 2005 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 Rice Univ, Dept Phys & Astron, Houston, TX 77251 USA. N Carolina State Univ, Dept Phys, Raleigh, NC 27695 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Baring, MG (reprint author), Rice Univ, Dept Phys & Astron, MS-108,POB 1892, Houston, TX 77251 USA. EM baring@rice.edu; don_ellison@ncsu.edu; slane@head.cfa.harvard.edu NR 34 TC 4 Z9 4 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI KIDLINGTON PA THE BOULEVARD, LANGFORD LANE,, KIDLINGTON OX5 1GB, OXFORD, ENGLAND SN 0273-1177 J9 ADV SPACE RES PY 2005 VL 35 IS 6 BP 1041 EP 1046 DI 10.1016/j.asr.2005.02.067 PG 6 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BCX77 UT WOS:000231793600011 ER PT S AU Slane, P AF Slane, P BE Rakowski, C Chatterjee, S TI The devil is in the details: Compact structures in pulsar wind nebulae SO YOUNG NEUTRON STARS AND SUPERNOVA REMNANTS SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT 35th COSPAR Scientific Assembly CY JUL 18-25, 2004 CL Paris, FRANCE SP Comm Space Res DE ISM : general; stars : neutron; stars : winds,outflows ID X-RAY-EMISSION; CRAB-NEBULA; SUPERNOVA REMNANT; MAGNETOHYDRODYNAMIC MODEL; SYNCHROTRON NEBULA; MAGNETIC-FIELD; VELA PULSAR; 3C 58; DISCOVERY; ORIGIN AB The large-scale structure of pulsar wind nebulae (PWNe) tells us a considerable amount about their average magnetic fields, the total particle input from the pulsar winds, and the confining pressure at their outer boundaries. However, the details of the pulsar outflow, the sites of shocks and particle acceleration, the effects of instabilities in the magnetic field, and the interaction between the relativistic wind and the surrounding ejecta are contained in small-scale structures, where we observe jets and toroidal structures, time-varying emission from compact clumps, and filaments in both the inner and outer regions of the nebulae. Here, I review recent observational studies of compact structures in PWNe and present current scenarios (and questions) regarding their origin. (c) 2005 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Slane, P (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM slane@cfa.harvard.edu NR 38 TC 6 Z9 6 U1 1 U2 1 PU PERGAMON-ELSEVIER SCIENCE LTD PI KIDLINGTON PA THE BOULEVARD, LANGFORD LANE,, KIDLINGTON OX5 1GB, OXFORD, ENGLAND SN 0273-1177 J9 ADV SPACE RES PY 2005 VL 35 IS 6 BP 1092 EP 1098 DI 10.1016/j.asr.2005.04.029 PG 7 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BCX77 UT WOS:000231793600020 ER PT S AU Gaensler, BM AF Gaensler, BM BE Rakowski, C Chatterjee, S TI Bow shocks around pulsars and neutron stars SO YOUNG NEUTRON STARS AND SUPERNOVA REMNANTS SE ADVANCES IN SPACE RESEARCH-SERIES LA English DT Article; Proceedings Paper CT 35th COSPAR Scientific Assembly CY JUL 18-25, 2004 CL Paris, FRANCE SP Comm Space Res DE ISM : general; stars : neutron; stars : winds,outflows ID X-RAY NEBULA; INTERSTELLAR-MEDIUM; WIND; G359.23-0.82; DISCOVERY; EMISSION; GUITAR; MOUSE AB Pulsar wind nebulae are now well-established as important probes both of neutron stars' relativistic winds and of the surrounding interstellar medium. Amongst this diverse group of objects, pulsar bow shocks have long been regarded as an oddity, only seen around a handful of rapidly moving neutron stars. However, recent efforts at optical, radio and X-ray wavelengths have identified many new pulsar bow shocks, and these results have consequently motivated renewed theoretical efforts to model these systems. Here, I review the new results and ideas which have emerged on these spectacular systems, and explain how bow shocks and "Crab-like" nebulae now form a consistent picture within our understanding of pulsar winds. (c) 2005 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Gaensler, BM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-6, Cambridge, MA 02138 USA. EM bgaensler@cfa.harvard.edu RI Gaensler, Bryan/F-8655-2010; OI Gaensler, Bryan/0000-0002-3382-9558 NR 37 TC 6 Z9 6 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI KIDLINGTON PA THE BOULEVARD, LANGFORD LANE,, KIDLINGTON OX5 1GB, OXFORD, ENGLAND SN 0273-1177 J9 ADV SPACE RES-SERIES PY 2005 VL 35 IS 6 BP 1116 EP 1122 DI 10.1016/j.asr.2005.01.026 PG 7 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BCX77 UT WOS:000231793600024 ER PT S AU Yusef-Zadeh, F Gaensler, BM AF Yusef-Zadeh, F Gaensler, BM BE Rakowski, C Chatterjee, S TI A radio study of the mouse, G359.23-0.82 SO YOUNG NEUTRON STARS AND SUPERNOVA REMNANTS SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT 35th COSPAR Scientific Assembly CY JUL 18-25, 2004 CL Paris, FRANCE SP Comm Space Res DE ISM : individual :(G359.23-0.82); pulsars : individual (J1747-2958); stars : neutron; stars : winds; outflows ID GALACTIC-CENTER REGION; POWERED BOW SHOCK AB The recent detection of a young pulsar powering "the Mouse", G359.23 - 0.82, as well as detailed imaging of surrounding nebular X-ray emission, have motivated us to investigate the structural details and polarization characteristics of the radio emission from this axisymmetric source with a supersonic bow shock. Using polarization data at 3.6 and 6 cm, we find that the magnetic field wraps around the bow-shock structure near the apex of the system, but downnstrearn runs parallel to the inferred direction of the pulsar's motion. The rotation measure (RM) distribution of the Mouse also suggests that the low degree of polarization combined with a high RM ahead of the pulsar result from internal plasma within the bow-shock region. In addition, using sub-arcsecond radio image of the Mouse, we identify modulations in the brightness distribution of the Mouse that may be associated with the unshocked pulsar wind behind the pulsar. Lastly, we discuss the relationship between the Mouse and its neighboring shell-type supernova remnant G359.1 - 0.5 and argue that these two sources could potentially have the same origin. (c) 2005 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Yusef-Zadeh, F (reprint author), Northwestern Univ, Dept Phys & Astron, 2145 Sheridan Rd, Evanston, IL 60208 USA. EM zadeh@northwestern.edu RI Gaensler, Bryan/F-8655-2010; OI Gaensler, Bryan/0000-0002-3382-9558 NR 17 TC 10 Z9 10 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI KIDLINGTON PA THE BOULEVARD, LANGFORD LANE,, KIDLINGTON OX5 1GB, OXFORD, ENGLAND SN 0273-1177 J9 ADV SPACE RES PY 2005 VL 35 IS 6 BP 1129 EP 1136 DI 10.1016/j.asr.2005.03.003 PG 8 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BCX77 UT WOS:000231793600026 ER PT J AU Robeck, TR Monfort, SL Calle, PP Dunn, JL Jensen, E Boehm, JR Young, S Clark, ST AF Robeck, TR Monfort, SL Calle, PP Dunn, JL Jensen, E Boehm, JR Young, S Clark, ST TI Reproduction, growth and development in captive beluga (Delphinapterus leucas) SO ZOO BIOLOGY LA English DT Article DE mondontidae; cetacean age and growth; testosterone; progesterone; captive cetaceans ID BOTTLE-NOSED DOLPHINS; WHALES ORCINUS-ORCA; TURSIOPS-TRUNCATUS; HARBOR-PORPOISES; BAY; METABOLITES; EXCRETION; PREGNANCY; BEHAVIOR; HORMONE AB Recent success propagating captive beluga has resulted from combined efforts by North American zoos and aquariums to manage disparate collections as a single population. This success has provided a tremendous opportunity to increase our understanding of beluga reproductive biology. Blood samples were collected on a weekly to biweekly basis from 23 female and 12 male beluga, ranging in age from 2-15 years, for analysis of serum progesterone (P) and testosterone (T), respectively. Peri-parturient observational data, including food intake, duration and signs of labor, and nursing patterns were collected from 15 days prepartum to 30 days postpartum during 21 births. Total body lengths and weights were collected from 10 captive-born beluga. For female beluga, the mean ( SD) age, body length, and weight at first conceptions were 9.1 +/- 2.8 years, 318.0 +/- 9.1 cm, and 519 +/- 84 kg. Thirty-five luteal phases and 13 conceptions were detected from January-June, and 70% of luteal phases and 80% conceptions occurred from March-May. The mean luteal phase and total estrous cycle lengths were 30.0 +/- 6.5 days and 48.0 +/- 4.6 days, respectively. For male beluga, the mean age that males sired their first calf was 13.3 +/- 2.6 years. Compared to younger males (< 8 years of age, 0.95 ng/ml), levels of T secretion in older males (> 8 years of age, 5.0 ng/ml) were elevated significantly only during the interval from January-April. Highest T concentrations (6.2 +/- 4.9 ng/ml) were recorded from January-March, whereas nadir concentrations (1.1 +/- 1.0 ng/ml) were detected from August-September. The mean gestation length was 475.0 +/- 20.4 days (n = 9). For parturition, the mean time from the first appearance of fluke or rostrum to delivery, delivery to placental passage, and delivery to nursing were 4.4 +/- 2.9 hr, 7.6 +/- 1.8 hr, and 43 +/- 45 hr, respectively. All cows had decreased food intake on the day of delivery, with 44% having zero intake. Peak 24-hr nursing activity occurred 3.9 +/- 2.7 days post-partum. Growth (i.e., body weight and length) as a function of age were well described by the Gompertz model (r(2) = 0.91, 0.93). Based on the model, growth in body weight and length were significantly greater in males compared to females. Predicted birth weight (88.9 kg) was similar for both sexes, however, and male calves were predicted to be shorter (154.3 cm) than female calves (160.7 cm). The results provide the first descriptions of captive beluga reproductive physiology, including endocrinology, peri-parturient behavior, growth, and reproductive maturity. This knowledge is important for helping to maintain genetically diverse, self-sustaining populations of captive beluga whales. C1 SeaWorld Texas, San Antonio, TX 78251 USA. Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, Front Royal, VA USA. Wildlife Conservat Soc, Bronx, NY USA. Myst Aquarium, Mystic, CT USA. USN Marine Mammal Program, San Diego, CA USA. John G Shedd Aquarium, Chicago, IL USA. Vancouver Aquarium Marine Sci Ctr, Vancouver, BC, Canada. Corp Zool Operat, Orlando, FL USA. RP Robeck, TR (reprint author), SeaWorld Texas, 10500 SeaWorld Dr, San Antonio, TX 78251 USA. EM Todd.Robeck@SeaWorld.com NR 47 TC 39 Z9 46 U1 9 U2 69 PU WILEY-LISS PI HOBOKEN PA DIV JOHN WILEY & SONS INC, 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 0733-3188 J9 ZOO BIOL JI Zoo Biol. PD JAN-FEB PY 2005 VL 24 IS 1 BP 29 EP 49 DI 10.1002/zoo.20037 PG 21 WC Veterinary Sciences; Zoology SC Veterinary Sciences; Zoology GA 903TL UT WOS:000227448400003 ER PT J AU Collins, AG Winikelmann, S Hadrys, H Schierwater, B AF Collins, AG Winikelmann, S Hadrys, H Schierwater, B TI Phylogeny of Capitata and Corynidae (Cnidaria, Hydrozoa) in light of mitochondrial 16S rDNA data SO ZOOLOGICA SCRIPTA LA English DT Article ID LIFE-CYCLE; ANTHOMEDUSAE; SEQUENCES; MEDUSOZOA; EVOLUTION AB New sequences of the partial rDNA gene coding for the mitochondrial large ribosomal subunit, 16S, are derived from 47 diverse hydrozoan species and used to investigate phylogenetic relationships among families of the group Capitata and among species of the capitate family Corynidae. Our analyses identify a well-supported clade, herein named Aplanulata, of capitate hydrozoans that are united by the synapomorphy of undergoing direct development without the ciliated planula stage that is typical of cnidarians. Aplanulata includes the important model organisms of the group Hydridae, as well as species of Candelabridae, Corymorphidae, and Tubulariidae. The hypothesis that Hydridae is closely related to brackish water species of Moerisiidae is strongly controverted by 16S rDNA data, as has been shown for nuclear 18S rDNA data. The consistent phylogenetic signal derived front 16S and 18S data suggest that both markers would be useful for broad-scale multimarker analyses of hydrozoan relationships. Corynidae is revealed as paraphyletic with respect to Polyorchidae, a group for which information about the hydroid stage is lacking. Bicorona, which has been classified both within and outside of Corynidae, is shown to have a close relationship with all but one sampled species of Coryne. The corynid genera Coryne, Dipurena, and Sarsia are not revealed as monophyletic, further calling into question the morphological criteria used to classify them. The attached gonophores of the corynid species Sarsia lovenii are confirmed as being derived from an ancestral state of liberated medusae. Our results indicate that the 16S rDNA market could be useful for a DNA-based identification system for Cnidaria, for which it has been shown that the commonly used cytochrome c oxidase subunit 1 gene does not work. C1 German Res Ctr Biotechnol Epigenet Regulat, D-38124 Braunschweig, Germany. ITZ, D-30559 Hannover, Germany. RP Collins, AG (reprint author), NMFS, Natl Museum Nat Hist, MRC 153 Smithsonian Inst, POB 37012, Washington, DC 20013 USA. EM allen.collins@ecolevol.de RI Collins, Allen/A-7944-2008 OI Collins, Allen/0000-0002-3664-9691 NR 30 TC 49 Z9 52 U1 0 U2 1 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0300-3256 J9 ZOOL SCR JI Zool. Scr. PD JAN PY 2005 VL 34 IS 1 BP 91 EP 99 DI 10.1111/j.1463-6409.2005.00172.x PG 9 WC Evolutionary Biology; Zoology SC Evolutionary Biology; Zoology GA 892UL UT WOS:000226675400008 ER PT J AU Sues, HD Reisz, RR Hinic, S Raath, MA AF Sues, HD Reisz, RR Hinic, S Raath, MA TI On the skull of Massospondylus carinatus Owen, 1854 (Dinosauria : Sauropodomorpha) from the Elliot and Clarens formations (Lower Jurassic) of South Africa SO ANNALS OF CARNEGIE MUSEUM LA English DT Article DE Dinosauria; Saurischia; Sauropodomorpha; Lower Jurassic; Elliot formation; Clarens formation; South Africa AB This paper presents a comprehensive description of the cranial structure of the sauropodomorph dinosaur Massospondylus carinatus, based oil four well-preserved skulls (including one of a juvenile individual) from the Lower Jurassic Elliot and Clarens formations of South Africa. Massospondylus can be distinguished from other basal sauropodomorph dinosaurs by the following combination of primitive and derived cranial character-states: The greatest transverse width of the skull exceeds its dorsoventral height by at least 10 percent. Even in adult specimens, the orbit is proportionately large and the antorbital region proportionately short. The maxilla has a tall, nearly vertical dorsal process, and its medial sheet is narrow anteroposteriorly. A long posterior process of the prefrontal extends along the dorsal margin of the orbit, but the frontal still participates significantly in the formation of the orbital margin. There is a distinct ridge on the dorsolateral aspect of the lacrimal and a knob on the lateral surface of the prefrontal. A partial skull from the Lower Jurassic Kayenta Formation of Arizona previously attributed to Massospondylus differs from the South African material in several cranial and dental features and is not referable to this taxon. C1 Smithsonian Inst, Natl Museum Nat Hist, Sect Vertebrate Paleontol, Washington, DC 20013 USA. Univ Toronto, Dept Biol, Sect Vertebrate Paleontol, Mississauga, ON L5L 1C6, Canada. Univ Calif Davis, Dept Geol, Davis, CA 95616 USA. Univ Witwatersrand, Bernard Price Inst Palaeontol Res, ZA-2050 Wits, South Africa. RP Sues, HD (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Sect Vertebrate Paleontol, NHB MRC 106,POB 37012, Washington, DC 20013 USA. EM suesh@si.edu NR 38 TC 34 Z9 37 U1 1 U2 5 PU CARNEGIE MUSEUM NATURAL HISTORY PI PITTSBURGH PA 4400 FORBES AVE, PITTSBURGH, PA 15213 USA SN 0097-4463 J9 ANN CARNEGIE MUS JI Ann. Carnegie Mus. PD DEC 31 PY 2004 VL 73 IS 4 BP 239 EP 257 PG 19 WC Paleontology; Zoology SC Paleontology; Zoology GA 903VP UT WOS:000227454000003 ER PT J AU Lim, C Kafatos, M Megonigal, P AF Lim, C Kafatos, M Megonigal, P TI Correlation between atmospheric CO2 concentration and vegetation greenness in North America: CO2 fertilization effect SO CLIMATE RESEARCH LA English DT Article DE global change; climate change; CO2 fertilization effect; NDVI; remote sensing; vegetation ID NET PRIMARY PRODUCTION; CLIMATE-CHANGE; CARBON SEQUESTRATION; VARIABILITY; RESPONSES; FOREST; ECOSYSTEMS; ENRICHMENT; NITROGEN; GROWTH AB The possibility that rising atmospheric CO2 concentrations are influencing plant growth in contemporary ecosystems has received little attention, and the studies that exist have been done on a small spatial scale. We correlated the monthly rate of relative change in normalized differenced vegetation index (NDVI) from advanced very high resolution radiometer (AVHRR) data to the rate of change in atmospheric CO2 concentration during the natural vegetation growing season for evidence of a possible CO2 fertilization effect on vegetation development. The study addressed seasonal and annual patterns in spatially averaged NDVI for 3 different ecological regions in North America from 1982 to 1992. Correlations between CO2 and NDVI were calculated for 3 different lag conditions. Relatively high and positive correlation coefficients were found when the monthly rate of change in NDVI was 1 mo lagged to that for CO2, which suggests, but does not prove, a CO2 fertilization effect on natural vegetation development. Generally, the correlation coefficients changed from relatively high and positive correlations when NDVI was lagged 1 mo behind CO2 to relatively high and negative correlations when CO2 was lagged 1 mo behind NDVI. A general increase in the annual maximum greenness of the vegetation was also found in most of the regions studied from 1982 to 2001. The desert and humid temperate regions in the eastern part of North America showed an increase in the annual minimum vegetation greenness, while the southern humid temperate regions showed relatively high correlations between the minimum NDVI and atmospheric CO2 concentration in interannual comparisons. The results of this study are generally consistent with the notion of a contemporary CO2 fertilization effect, but they also demonstrate how remotely-sensed data can be used to explore the effects of global change at large scales in order to complement experimental results obtained on smaller temporal and spatial scales. C1 George Mason Univ, SCS, CEOSR, Fairfax, VA 22030 USA. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Lim, C (reprint author), George Mason Univ, SCS, CEOSR, Fairfax, VA 22030 USA. EM clim1@gmu.edu NR 32 TC 9 Z9 9 U1 0 U2 9 PU INTER-RESEARCH PI OLDENDORF LUHE PA NORDBUNTE 23, D-21385 OLDENDORF LUHE, GERMANY SN 0936-577X J9 CLIMATE RES JI Clim. Res. PD DEC 31 PY 2004 VL 28 IS 1 BP 11 EP 22 DI 10.3354/cr028011 PG 12 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 906JZ UT WOS:000227638300002 ER PT J AU Li, XZ Bruce, AJ Manning, RB AF Li, XZ Bruce, AJ Manning, RB TI Some palaemonid shrimps (Crustacea : Decapoda) from northern South China Sea, with descripitions of two new species SO RAFFLES BULLETIN OF ZOOLOGY LA English DT Review DE South China Sea; Crustacea; Decapoda; Palaemonidae; taxonomy ID PERICLIMENAEUS-BORRADAILE; REDESCRIPTION; DESIGNATION; PONTONIINAE; TERRITORY; AUSTRALIA; ISLANDS; DANA AB Thirty-four palaemonid species from the northern area of South China Sea are reported in the present paper, including two new species, Paranchistus lini, new species, and Periclimenes chacei, new species, and eight other species are reported for the first time from South China Sea: Leander tenuicornis (Say, 1818), Leandrites stenopus Holthuis, 1950, Palaemon debilis Dana, 1852, Urocaridella antonbrurnii (Bruce, 1967), Kemponia platycheles (Holthuis, 1952), Paraclimenes franklini (Bruce, 1990b), Paranchistus spondylis Suzuki, 1971, Periclimenes hirsutus Bruce, 1971. C1 Smithsonian Inst, Dept Invertebrate Zool, Museum Natl Hist Nat, Washington, DC 20560 USA. Queensland Museum, Brisbane, Qld, Australia. Chinese Acad Sci, Inst Oceanol, Qingdao 266071, Peoples R China. RP Li, XZ (reprint author), Smithsonian Inst, Dept Invertebrate Zool, Museum Natl Hist Nat, Washington, DC 20560 USA. EM lixzh@ms.qdio.ac.cn; abruce@broad.net.au NR 113 TC 19 Z9 23 U1 2 U2 9 PU NATL UNIV SINGAPORE, SCHOOL BIOLOGICAL SCIENCES PI SINGAPORE PA DEPT ZOOLOGY, KENT RIDGE, SINGAPORE 0511, SINGAPORE SN 0217-2445 J9 RAFFLES B ZOOL JI Raffles Bull. Zool. PD DEC 31 PY 2004 VL 52 IS 2 BP 513 EP 553 PG 41 WC Zoology SC Zoology GA 889ES UT WOS:000226426900018 ER PT J AU Quinteros, RB Behrensmeyer, AK Ormazabal, GC AF Quinteros, RB Behrensmeyer, AK Ormazabal, GC TI Paleoclimate and faunal evolution in the Plio-Pleistocene of Africa and South America SO AMEGHINIANA LA Spanish DT Article DE paleoclimate; mammals; Pliocene; Pleistocene; Argentina; Africa ID EAST-AFRICA; MAMMAL FAUNAS; CLIMATE; RESPONSES; COMMUNITIES; VARIABILITY; KENYA AB PALEOCLIMATE AND FAUNAL EVOLUTION IN THE PLIO-PLEISTOCENE OF AFRICA AND SOUTH AMERICA. Climatic change is often hypothesized to be a major variable in forcing evolutionary change. Recent work on Pliocene and Pleistocene fossil mammals from the Turkana Basin of Kenya and Ethiopia shows that climate may play an important role in the spread of savanna environments, and thus in the increasing abundance of mammals adapted to open and seasonally and conditions. If global climate change is behind some of these trends in East Africa, we hypothesize that similar patterns of faunal change may occur elsewhere. An analysis of fossil mammals from the Pampean region of Argentina shows an increase in the number of species adapted to open and seasonally and conditions through the Plio-Pleistocene. The South American pattern is not identical to the East African pattern, but both show a significant increase in open and and adapted mammals shortly after 2 million years ago, at the very beginning of the Pleistocene. Although global climate change may be invoked as a common cause of these intercontinental trends, local and regional geography and tectonics play a critical role in modulating the global signal. C1 SUNY Buffalo, Dept Anthropol, Buffalo, NY 14261 USA. Smithsonian Inst Evolut, Terr Ecosyst Program, Washington, DC 20013 USA. Ctr Divulgac Biogeog, San Bernardo, Chile. RP Quinteros, RB (reprint author), SUNY Buffalo, Dept Anthropol, 380 MFAC,Ellicott Complex, Buffalo, NY 14261 USA. EM renebobe@buffalo.edu; behrensmeyer.kay@nmnh.si.edu; chlamyphorus@yahzoo.com NR 71 TC 7 Z9 7 U1 0 U2 4 PU ASOCIACION PALEONTOLOGICA ARGENTINA PI BUENOS AIRES PA MAIPU 645, 1ER PISO, 1006 BUENOS AIRES, ARGENTINA SN 0002-7014 EI 1851-8044 J9 AMEGHINIANA JI Ameghiniana PD DEC 30 PY 2004 VL 41 IS 4 BP 641 EP 649 PG 9 WC Paleontology SC Paleontology GA 898TX UT WOS:000227100200016 ER PT J AU Schloder, C D'Croz, L AF Schloder, C D'Croz, L TI Responses of massive and branching coral species to the combined effects of water temperature and nitrate enrichment SO JOURNAL OF EXPERIMENTAL MARINE BIOLOGY AND ECOLOGY LA English DT Article DE coral-zooxanthella symbiosis; nitrate enrichment; ENSO; sea-warming; upwelling ID EL-NINO; REEF CORALS; POCILLOPORA-DAMICORNIS; POPULATION-DENSITY; SEA-WATER; ZOOXANTHELLAE; MORTALITY; NITROGEN; ISLANDS; PANAMA AB The branching coral species Pocillopora damicornis (Linnaeus) and the massive coral species Porites lobata Dana were exposed for 30 days to different temperatures and nitrate concentrations to study the response of the coral-zooxanthella symbiosis. Results suggest that the effect of nitrate enrichment on the polyp-zooxanthella symbiosis varies according to the coral morphology. After the experimental period only 30% of P. damicornis colonies remained healthy, in contrast to 90% of P. lobata. The branching P damicornis was significantly affected by the addition of nitrate, whereas P. lobata was significantly influenced by water temperature. The two species showed enhanced zooxanthella volume, and chlorophyll contents per cell under high nitrate concentrations. The reduced zooxanthellae density in both species indicated a detrimental influence of the interaction of high nitrate and high temperature. Tissue soluble proteins in P. lobata were significantly reduced by elevated temperature. Results showed that tissue soluble proteins and chlorophylls in P. lobata were from two- to three-fold higher than in P. damicornis. The number of zooxanthellae in P. lobata was double that of P. damicornis. Therefore, we suggest that the slow-growing species R lobata is better able to cope with changing environmental conditions than the fast-growing coral R damicornis. (C) 2004 Elsevier B.V. All rights reserved. C1 Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. Univ Kaiserslautern, D-67663 Kaiserslautern, Germany. Estafeta Univ, Dept Biol Marina & Limnol, Panama City, Panama. RP Schloder, C (reprint author), Smithsonian Trop Res Inst, Apartado 2072, Panama City, Panama. EM carmen_schloeder@hotmail.com NR 51 TC 20 Z9 21 U1 0 U2 7 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0022-0981 J9 J EXP MAR BIOL ECOL JI J. Exp. Mar. Biol. Ecol. PD DEC 30 PY 2004 VL 313 IS 2 BP 255 EP 268 DI 10.1016/j.jembe.2004.08.012 PG 14 WC Ecology; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 874UT UT WOS:000225376300004 ER PT J AU Irwin, RP Howard, AD Maxwell, TA AF Irwin, RP Howard, AD Maxwell, TA TI Geomorphology of Ma'adim Vallis, Mars, and associated paleolake basins SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Review DE flood; lake; valley networks ID GUSEV CRATER; SEDIMENT TRANSPORT; MARGARITIFER SINUS; MARTIAN HIGHLANDS; BEDROCK CHANNELS; OUTFLOW CHANNELS; IMPACT CRATERS; GROUND ICE; EVOLUTION; WATER AB Ma'adim Vallis, one of the largest valleys in the Martian highlands, appears to have originated by catastrophic overflow of a large paleolake located south of the valley heads. Ma'adim Vallis debouched to Gusev crater, 900 km to the north, the landing site for the Spirit Mars Exploration Rover. Support for the paleolake overflow hypothesis comes from the following characteristics: (1) With a channel width of 3 km at its head, Ma'adim Vallis originates at two (eastern and western) gaps incised into the divide of the similar to1.1 M km(2) enclosed Eridania head basin, which suggests a lake as the water source. (2) The sinuous course of Ma'adim Vallis is consistent with overland flow controlled by preexisting surface topography, and structural control is not evident or required to explain the valley course. (3) The nearly constant similar to5 km width of the inner channel through crater rim breaches, the anastomosing course of the wide western tributary, the migration of the inner channel to the outer margins of bends in the valley's lower reach, a medial sedimentary bar similar to200 m in height, and a step-pool sequence are consistent with modeled flows of 1-5 x 10(6) m(3)/s. Peak discharges were likely higher but are poorly constrained by the relict channel geometry. (4) Small direct tributary valleys to Ma'adim Vallis have convex-up longitudinal profiles, suggesting a hanging relationship to a valley that was incised quickly relative to the timescales of tributary development. (5) The Eridania basin had adequate volume between the initial divide and the incised gap elevations to carve Ma'adim Vallis during a single flood. (6) The Eridania basin is composed of many overlapping, highly degraded and deeply buried impact craters. The floor materials of the six largest craters have an unusually high internal relief (similar to1 km) and slope (similar to0.5-1.5degrees) among degraded Martian craters, which are usually flat-floored. Long-term, fluvial sediment transport appears to have been inhibited within these craters, and the topography is inconsistent with basaltic infilling. (7) Fluvial valleys do not dissect the slopes of these deeper crater floor depressions, unlike similar slopes that are dissected at higher levels in the watershed. These characteristics (6, 7) suggest that water mantled at least the lower parts of the Eridania basin floor throughout the period of relatively intense erosion early in Martian history. The lake level increased and an overflow occurred near the close of the Noachian (age determined using >5 km crater counts). Initially, the Eridania basin debouched northward at two locations into the intermediate basin, a highly degraded impact crater similar to500 km in diameter. As this intermediate basin was temporarily filled with water, erosion took place first along the lower (northern) reach of Ma'adim Vallis, debouching to Gusev crater. The western overflow point was later abandoned, and erosion of the intermediate basin interior was concentrated along the eastern pathway. Subsequent air fall deposition, impact gardening, tectonism, and limited fluvial erosion modified the Eridania basin region, so evidence for a paleolake is restricted to larger landforms that could survive post-Noachian degradation processes. C1 Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20013 USA. Univ Virginia, Dept Environm Sci, Charlottesville, VA 22903 USA. RP Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, MRC 315, Washington, DC 20013 USA. EM irwinr@nasm.si.edu NR 105 TC 43 Z9 43 U1 1 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD DEC 30 PY 2004 VL 109 IS E12 AR E12009 DI 10.1029/2004JE002287 PG 33 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 885CQ UT WOS:000226135000001 ER PT J AU Rijkenberg, MJA Gerringa, LJA Neale, PJ Timmermans, KR Buma, AGJ de Baar, HJW AF Rijkenberg, MJA Gerringa, LJA Neale, PJ Timmermans, KR Buma, AGJ de Baar, HJW TI UVA variability overrules UVB ozone depletion effects on the photoreduction of iron in the Southern Ocean SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID ULTRAVIOLET-RADIATION; EQUATORIAL PACIFIC; WATERS; PHOTOSYNTHESIS; PHYTOPLANKTON; INHIBITION; SEAWATER; ICE AB [ 1] A spectral weighting function describing the wavelength dependency of the photoproduction of Fe( II) in Antarctic seawater was established. The strong wavelength-dependent photoproduction of Fe( II) from amorphous ferric hydroxides can be described as an exponential function: epsilon(lambda) = 3.57 . 10(3) . e (-0.02)((lambda-300)). Solar spectra recorded during the 2000 Antarctic ozone depletion season were used to demonstrate that daily and seasonal variability of the ultraviolet A ( UVA: 315-400 nm) and the visible part of the light spectrum ( VIS: 400-700 nm) dominates Fe( II) production rates in surface waters ( respectively > 60% and about 30%) and in the water column. Although ultraviolet B ( UVB: 280-315 nm) is the most effective wavelength region for Fe( II) photoproduction, the impact of UVB was small due to the relatively low flux of UVB into the ocean surface waters. However, the impact of UVB did indeed increase significantly from 3.54 to 6.15 % during the austral ozone minimum. C1 Univ Groningen, Ctr Ecol & Evolutionary Studies, Dept Marine Biol, NL-9750 AA Haren, Netherlands. Royal Netherlands Inst Sea Res, Dept Marine Chem & Geol, NL-1790 AB Den Burg, Netherlands. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Rijkenberg, MJA (reprint author), Univ Groningen, Ctr Ecol & Evolutionary Studies, Dept Marine Biol, POB 14, NL-9750 AA Haren, Netherlands. EM rijken@nioz.nl RI Neale, Patrick/A-3683-2012; Rijkenberg, Micha/C-3245-2012; Buma, Anita/E-8372-2015 NR 18 TC 4 Z9 4 U1 1 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD DEC 29 PY 2004 VL 31 IS 24 AR L24310 DI 10.1029/2004GL020829 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 885BZ UT WOS:000226133100002 ER PT J AU Norris, DR Marra, PP Montgomerie, R Kyser, TK Ratcliffe, LM AF Norris, DR Marra, PP Montgomerie, R Kyser, TK Ratcliffe, LM TI Reproductive effort molting latitude, and feather color in a migratory songbird SO SCIENCE LA English DT Article ID ISOTOPES; GROUNDS; WINTER; BIRD AB Toward the end of the breeding season, migratory songbirds face crucial tradeoffs between the timing of reproduction, molt, and migration. Using stable hydrogen isotopes, we show that male American redstarts investing in high levels of reproduction late in the season adopt a unique strategy of combining molt and migration. Tail feathers molted during migration also reflect less orange-red light, indicating reduced carotenoid concentration. Thus, we show how reproduction in a migratory animal can influence both life history strategies (location of molt) and social signals (feather color) during subsequent periods of the annual cycle. C1 Queens Univ, Dept Biol, Kingston, ON K7L 3N6, Canada. Queens Univ, Dept Geol Sci & Engn, Kingston, ON K7L 3N6, Canada. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Univ British Columbia, Ctr Appl Conservat Res, Forest Sci Ctr, Vancouver, BC V6T 1Z4, Canada. RP Norris, DR (reprint author), Queens Univ, Dept Biol, Kingston, ON K7L 3N6, Canada. EM ryann@biology.queensu.ca RI Montgomerie, Robert/C-6516-2008; Norris, Ryan/F-4720-2011 OI Montgomerie, Robert/0000-0003-4701-4525; NR 13 TC 80 Z9 82 U1 4 U2 32 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 DEC 24 PY 2004 VL 306 IS 5705 BP 2249 EP 2250 DI 10.1126/science.1103542 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 882PE UT WOS:000225950000044 PM 15618516 ER PT J AU Martin, RV Parrish, DD Ryerson, TB Nicks, DK Chance, K Kurosu, TP Jacob, DJ Sturges, ED Fried, A Wert, BP AF Martin, RV Parrish, DD Ryerson, TB Nicks, DK Chance, K Kurosu, TP Jacob, DJ Sturges, ED Fried, A Wert, BP TI Evaluation of GOME satellite measurements of tropospheric NO2 and HCHO using regional data from aircraft campaigns in the southeastern United States SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE ozone; GOME; TEXAQS; Houston; nitrogen dioxide; formaldehyde ID OZONE MONITORING EXPERIMENT; AIRBORNE FORMALDEHYDE MEASUREMENTS; NORTH-AMERICA; ISOPRENE EMISSIONS; MODEL DESCRIPTION; OXIDE EMISSIONS; GOCART MODEL; GLOBAL-MODEL; CHEMISTRY; NITROGEN AB We compare tropospheric measurements of nitrogen dioxide (NO2) and formaldehyde ( HCHO) from the Global Ozone Monitoring Experiment (GOME) satellite instrument with in situ measurements over eastern Texas and the southeast United States. On average, the GOME and in situ measurements of tropospheric NO2 and HCHO columns are consistent despite pronounced sampling differences. The geometric mean in situ to GOME ratios over the campaign are 1.08 for NO2 and 0.84 for HCHO, with corresponding geometric standard deviations of 1.27 and 1.38. The correlation of the observed column spatial variability between the two NO2 measurement sets is encouraging before (r(2) = 0.54, n = 18) and after (r(2) = 0.67, n = 18) correcting for a sampling bias. Mean relative vertical profiles of HCHO and NO2 calculated with a global three-dimensional model (GEOS-CHEM) and used in the GOME retrieval are highly consistent with in situ measurements; differences would affect the retrieved NO2 and HCHO columns by a few percent. GOME HCHO columns over eastern Texas include contributions from anthropogenic volatile organic compound (VOC) emissions but are dominated by biogenic VOC emissions at the regional scale in August-September when HCHO columns are within 20% of those over the southeastern United States. In situ measurements show that during summer the lowest 1500 m ( the lower mixed layer) contains 75% of the tropospheric NO2 column over Houston and Nashville, and 60% of the HCHO column over Houston. Future validation of space-based measurements of tropospheric NO2 and HCHO columns over polluted regions should include coincident in situ measurements that span the entire satellite footprint, especially in the heterogeneous mixed layer. C1 Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 3J5, Canada. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. NOAA, Aeron Lab, Boulder, CO 80305 USA. Harvard Univ, Div Engn & Appl Sci, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA. Natl Ctr Atmospher Res, Div Atmospher Chem, Boulder, CO 80303 USA. RP Martin, RV (reprint author), Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 3J5, Canada. EM randall.martin@dal.ca RI Martin, Randall/A-2051-2008; Parrish, David/E-8957-2010; Ryerson, Tom/C-9611-2009; Martin, Randall/C-1205-2014; Chem, GEOS/C-5595-2014 OI Parrish, David/0000-0001-6312-2724; Martin, Randall/0000-0003-2632-8402; NR 43 TC 62 Z9 64 U1 0 U2 13 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD DEC 23 PY 2004 VL 109 IS D24 AR D24307 DI 10.1029/2004JD004869 PG 11 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 883PQ UT WOS:000226027000005 ER PT J AU Mlynczak, MG Martin-Torres, FJ Johnson, DG Kratz, DP Traub, WA Jucks, K AF Mlynczak, MG Martin-Torres, FJ Johnson, DG Kratz, DP Traub, WA Jucks, K TI Observations of the O(P-3) fine structure line at 63 mu m in the upper mesosphere and lower thermosphere SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE atomic oxygen; far-infrared; oxygen emissions; thermospheric energy balance ID ATOMIC OXYGEN; TRANSLATIONAL TEMPERATURE; TERRESTRIAL THERMOSPHERE; UPPER-ATMOSPHERE; MIDDLE; ENERGETICS; EMISSION AB Observations of the O(P-3) fine structure line at 63 mum originating in the upper mesosphere and lower thermosphere have been obtained by the far-infrared spectrometer (FIRS-2) instrument, a Fourier transform spectrometer that flies periodically on high-altitude balloons. FIRS-2 primarily observes stratospheric ozone photochemistry using the technique of limb emission spectroscopy. As part of the routine operation of FIRS-2, up-looking views are made, during which the emission from the atomic oxygen is recorded. Using the Mass Spectrometer Incoherent Scatter (MSIS) empirical model to provide temperature and atomic oxygen concentrations, we compute radiances for comparison with the FIRS-2 observations. The computed radiances agree with the FIRS-2 measurements, which encompass 31 observations during nine flights over a span of 14 years, to within 10% on average, with 23 of the 31 observations agreeing to within measurement and calculation uncertainty. The consistency between the observed and computed radiances suggests that the MSIS model provides a reasonably accurate representation of temperature and atomic oxygen in the upper mesosphere and lower thermosphere. C1 NASA, Climate Sci Branch, Langley Res Ctr, Hampton, VA 23681 USA. NASA, Analyt Mat & Serv Corp, Langley Res Ctr, Hampton, VA 23681 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Mlynczak, MG (reprint author), NASA, Climate Sci Branch, Langley Res Ctr, 21 Langley Blvd,Mail Stop 420, Hampton, VA 23681 USA. EM m.g.mlynczak@nasa.gov RI Mlynczak, Martin/K-3396-2012; Johnson, David/F-2376-2015; Martin-Torres, Francisco Javier/G-6329-2015 OI Johnson, David/0000-0003-4399-5653; Martin-Torres, Francisco Javier/0000-0001-6479-2236 NR 17 TC 8 Z9 8 U1 0 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD DEC 23 PY 2004 VL 109 IS A12 AR A12306 DI 10.1029/2004JA010595 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 883QE UT WOS:000226028600001 ER PT J AU Davis, JL Elosegui, P Mitrovica, JX Tamisiea, ME AF Davis, JL Elosegui, P Mitrovica, JX Tamisiea, ME TI Climate-driven deformation of the solid Earth from GRACE and GPS SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID VARIABILITY; GRAVITY; WATER AB GRACE data indicate large seasonal variations in gravity that are assumed to be related to climate-driven fluxes of surface water. Seasonal redistribution of surface mass should deform the Earth, and our calculations using GRACE data suggest vertical deformations of similar to13 mm in the region of greatest flux, the Amazon River Basin. To test the GRACE gravity-hydrology connection, we analyzed GPS data acquired from sites in this region. After accounting for degree 1 variations not observable with GRACE, we find that annual deformation measured with GPS correlates highly with predictions calculated from GRACE measurements. These results confirm the variations in surface water sensed by GRACE, which are significantly larger than those predicted by some hydrology models. The results also demonstrate that GRACE can be an important tool for monitoring deformation of the Earth, and suggest that combined analysis of GRACE and GPS may be a useful approach for estimation of geocenter variations. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CSIC, Inst Estudis Espacials Catalunya, Barcelona, Spain. Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada. RP Davis, JL (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 42, Cambridge, MA 02138 USA. EM jdavis@cfa.harvard.edu; pelosegui@cfa.harvard.edu; jxm@physics.utoronto.ca; jxm@physics.utoronto.ca RI Davis, James/D-8766-2013 OI Davis, James/0000-0003-3057-477X NR 16 TC 156 Z9 162 U1 4 U2 18 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 DEC 22 PY 2004 VL 31 IS 24 AR L24605 DI 10.1029/2004GL021435 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 883PK UT WOS:000226026300005 ER PT J AU Erwin, TL AF Erwin, TL TI The beetle family Carabidae of Costa Rica: The genus Epikastea Liebke of the Plochonida Group, with new Neotropical species and notes on their way of life (Insecta : Coleoptera, Lebiini, Agrina) SO ZOOTAXA LA English DT Article DE Costa Rica; Peru; Ecuador; INBio; Carabidae; Lebiini; Epikastea Liebke ID CLASSIFICATION; TAXONOMY AB Genus Epikastea Liebke 1936, of the Plochionida Group of Subtribe Agrina, Lebiini, with six species is revised. Subtribe Agrina consists of those species formerly included in the Subtribe Calleidina. The species of Epikastea Liebke 1936 are diagnosed, described, and illustrated. One species occurs in Costa Rica; five are new South American species and are here assigned to this genus. The five new species described are: Epikastea biolat Erwin, n. sp. (PERU, MADRE DE DIOS, Rio Manu, BIOLAT Biodiversity Station, Pakitza Guard Station, 356m, 11degrees 56' 47" S, 071degrees 17' 00" W), Epikastea grace Erwin, n. sp. (PERU, LORETO, Samiria River, Camp Manco Capac, 04degrees 43' 0 S, 074degrees 18' 0 W), Epikastea mancocapac Erwin, n. sp. ( PERU, LORETO, Samiria River, Camp Manco Capac, 04degrees 43' 0 S, 074degrees 18' 0 W), Epikastea piranha Erwin, n. sp. (ECUADOR. ORELLANA, Hauorani Territory, Camp Pirana, 0degrees 39' 25.685" S, 76degrees 27' 10.813" W), Epikastea poguei Erwin, n. sp. ( PERU, MADRE DE DIOS, Rio Manu, BIOLAT Biodiversity Station, Pakitza Guard Station, 356m, 11degrees 56' 47" S, 071degrees 17' 00" W). A definition of the Plochionida Group and an identification key to the Western Hemisphere genera included are provided. A key to the known species of Epikastea Liebke is given. Distribution data are provided for all species and a map is provided for the Costa Rican taxon. Adults of Epikastea Liebke have been found on rotting logs in rainforests and fogged from the canopy of tropical trees and palms. C1 Smithsonian Inst, Dept Entomol, Hyperdivers Grp, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Erwin, TL (reprint author), Smithsonian Inst, Dept Entomol, Hyperdivers Grp, Natl Museum Nat Hist, MRC-187,POB 37012, Washington, DC 20013 USA. EM erwin.terry@nmnh.si.edu NR 26 TC 12 Z9 14 U1 1 U2 1 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, 1030, NEW ZEALAND SN 1175-5334 J9 ZOOTAXA JI Zootaxa PD DEC 22 PY 2004 IS 790 BP 1 EP 20 PG 20 WC Zoology SC Zoology GA 883GW UT WOS:000226000600001 ER PT J AU Pogue, MG AF Pogue, MG TI A new species of Schinia Hubner from riparian habitats in the Grand Canyon (Lepidoptera : Noctuidae : Heliothinae) SO ZOOTAXA LA English DT Article DE systematics; genitalia; tamarisk; mesquite; acacia AB Schinia immaculata, new species, is described from riparian habitats along the Colorado River in the Grand Canyon. Habitats include the shoreline, new high water dominated by tamarisk (Tamarix sp., Tamaricaceae), and old high water characterized by mesquite (Prosopis sp., Fabaceae), acacia (Acacia sp., Fabaceae), and desert shrubs. Adult and male genitalia are illustrated and compared with Schinia biundulata Smith. C1 Smithsonian Inst, USDA, Agr Res Serv, Systemat Entomol Lab, Washington, DC 20013 USA. RP Pogue, MG (reprint author), Smithsonian Inst, USDA, Agr Res Serv, Systemat Entomol Lab, POB 37012,NMNH,MRC-168, Washington, DC 20013 USA. EM mpogue@sel.barc.usda.gov NR 6 TC 6 Z9 6 U1 0 U2 1 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, 1030, NEW ZEALAND SN 1175-5334 J9 ZOOTAXA JI Zootaxa PD DEC 22 PY 2004 IS 788 BP 1 EP 4 PG 4 WC Zoology SC Zoology GA 883GU UT WOS:000226000300001 ER PT J AU Luhman, KL AF Luhman, KL TI New brown dwarfs and an updated initial mass function in Taurus SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared : stars; stars : evolution; stars : formation; stars : low-mass, brown dwarfs; stars : luminosity function, mass function; stars : pre-main-sequence ID ORION NEBULA CLUSTER; STAR-FORMING REGION; AURIGA MOLECULAR CLOUD; YOUNG STELLAR OBJECTS; SPACE-TELESCOPE WFPC2; MAIN-SEQUENCE STARS; EVOLUTIONARY MODELS; LUMINOSITY FUNCTION; TRAPEZIUM CLUSTER; COOL NEIGHBORS AB By combining infrared photometry from the Two Micron All Sky Survey with new optical imaging and spectroscopy, I have performed a search for young low-mass stars and brown dwarfs in two regions encompassing a total area of 4 deg(2) in the Taurus star-forming region (tau similar to 1 Myr). From this work I have discovered 15 new members of Taurus. In addition, I present seven new members outside of these areas from the initial stage of a survey of all of Taurus. These 22 objects exhibit spectral types of M4.5-M9.25 and masses of 0.3-0.015 M-circle dot according to the theoretical evolutionary models of Baraffe & Chabrier, seven of which are likely to be brown dwarfs. Emission in Halpha, He I, Ca II, [O I], and [S II] and excess emission in optical and near-infrared bands among some of these objects suggest the presence of accretion, outflows, and circumstellar disks. These results add to the body of work-initiated by the first detections of brown dwarf disks by Comeron and coworkers in 1998 and Luhman in 1999 - indicating that disks around young brown dwarfs are relatively common. The results from the 4 deg(2) survey have been combined with previous studies of Taurus to arrive at an initial mass function ( IMF) for a total area of 12.4 deg(2). As in the previous IMFs for Taurus, the updated IMF peaks at a higher mass (0.8 M-circle dot) than the mass functions in IC 348 and Orion (0.1-0.2 M-circle dot). Meanwhile, the deficit of brown dwarfs in Taurus appears to be less significant (; 1: 4 1: 8) than that found in earlier studies (x2) because of a slightly higher brown dwarf fraction in the new IMF for Taurus and a lower brown dwarf fraction in the new spectroscopic IMF for the Trapezium from Slesnick and coworkers. The spatial distribution of the low-mass stars and brown dwarfs discovered in the two new survey areas closely matches that of the more massive members. Thus, on the degree size scales (similar to3 pc) probed to date, there is no indication that brown dwarfs form through ejection. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Luhman, KL (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM kluhman@cfa.harvard.edu NR 77 TC 160 Z9 160 U1 2 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 2004 VL 617 IS 2 BP 1216 EP 1232 DI 10.1086/425647 PN 1 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 882VS UT WOS:000225968200037 ER PT J AU Jiang, GF DePoy, DL Gal-Yam, A Gaudi, BS Gould, A Han, C Lipkin, Y Maoz, D Ofek, EO Park, BG Pogge, RW Udalski, A Kubiak, M Szymanski, MK Szewczyk, O Zerbrun, K Wyrzykowski, L Soszynski, I Pietrzynski, G Albrow, MD Beaulieu, JP Caldwell, JAR Cassan, A Coutures, C Dominik, M Donatowicz, J Fouque, P Greenhill, J Hill, K Horne, K Jorgensen, SF Jorgensen, UG Kane, S Kubas, D Martin, R Menzies, J Pollard, KR Sahu, KC Wambsganss, J Watson, R Williams, A AF Jiang, GF DePoy, DL Gal-Yam, A Gaudi, BS Gould, A Han, C Lipkin, Y Maoz, D Ofek, EO Park, BG Pogge, RW Udalski, A Kubiak, M Szymanski, MK Szewczyk, O Zerbrun, K Wyrzykowski, L Soszynski, I Pietrzynski, G Albrow, MD Beaulieu, JP Caldwell, JAR Cassan, A Coutures, C Dominik, M Donatowicz, J Fouque, P Greenhill, J Hill, K Horne, K Jorgensen, SF Jorgensen, UG Kane, S Kubas, D Martin, R Menzies, J Pollard, KR Sahu, KC Wambsganss, J Watson, R Williams, A CA FUN Collaboration OGLE Collaboration PLANET Collaboration TI OGLE-2003-BLG-238: Microlensing mass estimate of an isolated star SO ASTROPHYSICAL JOURNAL LA English DT Article DE gravitational lensing; stars : fundamental parameters ID SPACE-INTERFEROMETRY-MISSION; GRAVITATIONAL LENSING EXPERIMENT; LARGE-MAGELLANIC-CLOUD; GALACTIC BULGE; EVENTS; PHOTOMETRY; HALO; DEGENERACY; PARALLAXES; CANDIDATES AB Microlensing is the only known direct method to measure the masses of stars that lack visible companions. In terms of microlensing observables, the mass is given by M (c(2)/4G)(r) over tilde (E)theta(E) and so requires the measurement of both the angular Einstein radius theta(E) and the projected Einstein radius (r) over tilde (E). Simultaneous measurement of these two parameters is extremely rare. Here we analyze OGLE-2003-BLG-238, a spectacularly bright (I-min 10.3), high-magnification (A(max) 170) microlensing event. Pronounced finite-source effects permit a measurement of theta(E) = 650 muas. Although the timescale of the event is only t(E) 38 days, one can still obtain weak constraints on the microlens parallax: 4.4 AU < <(r)over tilde>(E) < 18 AU at the 1 sigma level. Together these two parameter measurements yield a range for the lens mass of 0.36 M-circle dot < M < 1.48 M-circle dot. As was the case for MACHO-LMC-5, the only other single star (apart from the Sun) whose mass has been determined from its gravitational effects, this estimate is rather crude. It does, however, demonstrate the viability of the technique. We also discuss future prospects for single-lens mass measurements. C1 Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. CALTECH, Dept Astron, Pasadena, CA 91025 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Chungbuk Natl Univ, Inst Basic Sci Res, Dept Phys, Chonju 361763, South Korea. Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. Tel Aviv Univ, Wise Observ, IL-69978 Tel Aviv, Israel. Korea Astron Observ, Taejon 305348, South Korea. Univ Warsaw Observ, PL-00478 Warsaw, Poland. Univ Concepcion, Dept Fis, Concepcion, Chile. Univ Canterbury, Dept Phys & Astron, Christchurch 1, New Zealand. Inst Astrophys, F-75014 Paris, France. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Univ Texas, McDonald Observ, Ft Davis, TX 79734 USA. CEA Saclay, DSM, DAPNIA, F-91191 Gif Sur Yvette, France. Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. Vienna Univ Technol, Dept Comp, A-1060 Vienna, Austria. Observ Midi Pyrenees, UMR 5572, F-31400 Toulouse, France. Univ Tasmania, Sch Math & Phys, Hobart, Tas 7001, Australia. Niels Bohr Inst, Astron Observ, DK-2100 Copenhagen, Denmark. Univ Potsdam, D-14469 Potsdam, Germany. Perth Observ, Perth, WA 6076, Australia. S African Astron Observ, ZA-7935 Cape Town, South Africa. RP Ohio State Univ, Dept Astron, 140 W 18th Ave, Columbus, OH 43210 USA. EM jiang@astronomy.ohio-state.edu; depoy@astronomy.ohio-state.edu; avishay@astro.caltech.edu; sgaudi@cfa.harvard.edu; gould@astronomy.ohio-state.edu; cheongho@astroph.chungbuk.ac.kr; yiftah@wise.tau.ac.il; dani@wise.tau.ac.il; eran@wise.tau.ac.il; bgpark@boao.re.kr; pogge@astronomy.ohio-state.edu; udalski@astrouw.edu.pl; mk@astrouw.edu.pl; msz@astrouw.edu.pl; szewczyk@astrouw.edu.pl; zebrun@astrouw.edu.pl; wyrzykow@astrouw.edu.pl; soszynsk@astrouw.edu.pl; pietrzyn@astrouw.edu.pl; sfj@astro.ku.dk RI Gaudi, Bernard/I-7732-2012; Kane, Stephen/B-4798-2013; Greenhill, John/C-8367-2013; Williams, Andrew/K-2931-2013; OI Williams, Andrew/0000-0001-9080-0105; Dominik, Martin/0000-0002-3202-0343 NR 44 TC 27 Z9 27 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 2004 VL 617 IS 2 BP 1307 EP 1315 DI 10.1086/425678 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 882VS UT WOS:000225968200045 ER PT J AU Pepino, R Kharchenko, V Dalgarno, A Lallement, R AF Pepino, R Kharchenko, V Dalgarno, A Lallement, R TI Spectra of the X-ray emission induced in the interaction between the solar wind and the heliospheric gas SO ASTROPHYSICAL JOURNAL LA English DT Article DE atomic data; solar wind; X-rays : general ID LOCAL INTERSTELLAR-MEDIUM; CHARGE-TRANSFER; ULTRAVIOLET EMISSION; COMET INTERACTIONS; STELLAR WINDS; EXCHANGE; SUN; NEUTRALS/; HELIUM; IONS AB Spectra of the heliospheric EUV and X-ray emission induced in the charge transfer collisions of the highly charged solar wind ions with the interstellar gas have been calculated. Cascading photon spectra of individual Oq+, Cq+, Nq+, and Neq+ ions have been constructed using recent data on ion radiative transition probabilities and the state-selective population cross sections for charge transfer collisions of the most abundant heavy solar wind ions with H and He atoms. Emission spectra have been calculated for slow and fast solar winds interacting with the heliospheric H and He gas. Relative intensities of the brightest lines have been predicted. The volume power distribution of the charge transfer EUV and X-ray emission has been computed for simplified models of the solar winds and the interstellar gas. X-ray images of the heliosphere have been composed for the region inside 10 AU from the Sun. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CNRS, Serv Aeron, F-91371 Verrieres Le Buisson, France. RP Pepino, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 37 TC 48 Z9 48 U1 0 U2 8 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 2004 VL 617 IS 2 BP 1347 EP 1352 DI 10.1086/425682 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 882VS UT WOS:000225968200049 ER PT J AU Zubko, V Li, D Lim, T Feuchtgruber, H Harwit, M AF Zubko, V Li, D Lim, T Feuchtgruber, H Harwit, M TI Observations of water vapor outflow from NML Cygnus (vol 610, pg 427, 2004) SO ASTROPHYSICAL JOURNAL LA English DT Correction C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Rutherford Appleton Lab, Didcot OX11 0QX, Oxon, England. Max Planck Inst Extraterr Phys, Garching, Germany. Cornell Univ, Ithaca, NY 14853 USA. RP Zubko, V (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. NR 1 TC 0 Z9 0 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 2004 VL 617 IS 2 BP 1371 EP 1371 DI 10.1086/425655 PN 1 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 882VS UT WOS:000225968200052 ER PT J AU Cairns, SD Bayer, FM AF Cairns, SD Bayer, FM TI Studies on western Atlantic Octocorallia (Coelenterata : Anthozoa). Part 5: The genera Plumarella Gray, 1870; Acanthoprimnoa, n. gen.; and Candidella Bayer, 1954 SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article AB The nine western Atlantic species belonging to three genera, Plumarella, Acanthoprimnoa, and Candidella, are described and illustrated. Four new species of Plumarella are described, as well as one new species of Acanthoprimnoa; the genus Acanthoprimnoa is also described as new, differentiated from Plumarella by lacking tubercles on the undersurfaces of its sclerites. Two western Pacific species are transferred to Acanthoprimnoa: A. serta and A. cristata. Three varieties are recognized of the common Plumarella pourtalesii, one previously described as a variety (P. p. robusta) and another proposed herein (P. p. var. obtusa). A dichotomous key and table of comparisons is provided for the species and forms of Plumarella, as are a table of comparisons for the two Atlantic species of Acanthoprimnoa, and an indented key to the eleven genera of western Atlantic Primnoidae. Specimens of these genera were found to be extremely common at lower shelf and upper slope depths primarily in the temperate western Atlantic; over 1500 specimens were examined in this study, including types of all included species. C1 Smithsonian Inst, Dept Zool, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Cairns, SD (reprint author), Smithsonian Inst, Dept Zool, Natl Museum Nat Hist, POB 37012, Washington, DC 20013 USA. EM cairns.stephen@nmnh.si.edu NR 51 TC 9 Z9 12 U1 1 U2 1 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD DEC 20 PY 2004 VL 117 IS 4 BP 447 EP 487 PG 41 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 895RM UT WOS:000226880700001 ER PT J AU Von Sternberg, R Schotte, M AF Von Sternberg, R Schotte, M TI A new anchialine shrimp of the genus Procaris (Crustacea : Decapoda : Procarididae) from the Yucatan Peninsula SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article ID MARINE CAVES; AGOSTOCARIDIDAE; SUPERFAMILY; ATLANTIC; FAMILY AB A fourth species of the anchialine shrimp genus Procaris is described from Cozumel Island, Quintana Roo, Mexico. The combination of character states observed for the abdomen, antennal scale/stylocerite, second antennular segment, carapace, eyes, rostrum, and telson is unique in the genus. The new species appears to be morphologically most closely related to P. ascensionis from Ascension Island. Cladistic analysis of differentiating character states supports a sister group relationship between P. ascensionis and the Mexican species, in two out of three most parsimonious hypotheses. In addition, the Bermudan P. chacei and Hawaiian P. hawaiiana are positioned as sister taxa in all minimal length trees. While the discovery of a new Procaris species adds to our biogeographical knowledge of the genus, it has pointed to the possibility that the Atlantic taxa may be a paraphyletic assemblage. C1 NCBI GenBank, NIH, Bethesda, MD 20892 USA. Smithsonian Inst, Dept Zool, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Von Sternberg, R (reprint author), NCBI GenBank, NIH, Bldg 45,Room 6An,18D-30, Bethesda, MD 20892 USA. EM sternber@ncbi.nlm.nih.gov; Schottem@si.edu NR 15 TC 4 Z9 5 U1 0 U2 1 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD DEC 20 PY 2004 VL 117 IS 4 BP 514 EP 522 PG 9 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 895RM UT WOS:000226880700004 ER PT J AU Knapp, LW Imamura, H AF Knapp, LW Imamura, H TI Sunagocia sainsburyi, a new flathead fish (Scorpaeniformes : Platycephalidae) from northwestern Australia SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article AB Based on two specimens taken by bottom trawl from northwestern Australia, Sunagocia sainsburyi differs from its congeners in having: 4-5 preorbital spines; 5 total gill rakers on first arch; a bony expansion of suborbital ridge base on cheek bearing 1-2 rows of small spines; and no papillae on upper surface of eye. It also tends to have more spines on the ethmoid and on the supraorbital and suborbital ridges. A table compares features of the new species to the other three species currently included in the genus Sunagocia. C1 Smithsonian Inst, Dept Zool, Natl Museum Nat Hist, Washington, DC 20560 USA. Hokkaido Univ, Fac Fisheries, Hokkaido Univ Museum, Hakodate, Hokkaido 0418611, Japan. RP Knapp, LW (reprint author), Smithsonian Inst, Dept Zool, Natl Museum Nat Hist, Washington, DC 20560 USA. EM knappl@si.edu; imamura@museum.hukudai.ac.jp NR 10 TC 2 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 J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD DEC 20 PY 2004 VL 117 IS 4 BP 545 EP 550 PG 6 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 895RM UT WOS:000226880700008 ER PT J AU Vari, RP Ferraris, CJ AF Vari, RP Ferraris, CJ TI A new species of Nannocharax (Characiformes : Distichodontidae) from Cameroon, with the description of contact organs and breeding tubercles in the genus SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article AB Nannocharax reidi, new species, is described from several localities in the upper Cross River basin in Cameroon. The species possesses the synapomorphies of the clade comprising Nannocharax and Hemigrammocharax. It is assigned to Nannocharax on the basis of its possession of a completely-pored lateral line, a feature distinguishing that questionably monophyletic genus within the clade composed of these two genera. Nannocharax reidi is distinguished from its congeners on the basis of a combination of meristic and morphometric features and details of pigmentation on the body. Comparative studies revealed the presence of hook-shaped contact organs on the pectoral fins of some species of Nannocharax and epidermal breeding tubercles on the head, body, and fins of at least one species of the genus. These observations represent the first reports of contact organs and breeding tubercles in African members of the order Characiformes. Some species of Nannocharax were found also to possess variably-developed fields of hook-shaped contact organs on the exposed surfaces of scales of the midlateral portion of the body posterior of the pectoral girdle. This latter feature has not been previously reported among fishes. C1 Smithsonian Inst, Dept Zool, Div Fishes, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Vari, RP (reprint author), Smithsonian Inst, Dept Zool, Div Fishes, Natl Museum Nat Hist, Washington, DC 20560 USA. EM vari.richard@nmnh.si.edu; cferraris@msn.com NR 20 TC 8 Z9 9 U1 0 U2 2 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD DEC 20 PY 2004 VL 117 IS 4 BP 551 EP 563 PG 13 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 895RM UT WOS:000226880700009 ER PT J AU Olson, SL AF Olson, SL TI Taxonomic review of the fossil Procellariidae (Aves : Procellariiformes) described from Bermuda by R. W. Shufeldt SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article AB The literature and specimens relevant to the three new species of petrels (Procellariidae) proposed by R. W. Shufeldt from Quaternary fossils from Bermuda were re-examined. A case is made for citing all three binomials as dating from Shufeldt's earlier preliminary publication (1916) rather than his later monograph (1922). Aestrelata vociferans Shufeldt, 2 October 1916, was correctly synonymized with Aestrelata cahow Nichols & Mowbray, 31 March 1916, and a lectotype is designated here. Puffinis mcgalli Shufeldt, 1916, was correctly synonymized with Puffinus puffinus Brunnich, 1764, with the holotype evidently representing a casual occurrence. A lectotype is designated for Puffinus parvus Shufeldt, 1916. This taxon is not synonymous with Puffinus lherminieri Lesson, 1839, being much smaller, and is provisionally retained until its status relative to other taxa in the Puffinus assimilis/lherminieri complex can be assessed. C1 Smithsonian Inst, Div Birds, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Olson, SL (reprint author), Smithsonian Inst, Div Birds, Natl Museum Nat Hist, Washington, DC 20560 USA. EM olsons@si.edu NR 18 TC 5 Z9 5 U1 0 U2 1 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD DEC 20 PY 2004 VL 117 IS 4 BP 575 EP 581 PG 7 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 895RM UT WOS:000226880700011 ER PT J AU Santamore, DH Gaudio, S Timmermans, E AF Santamore, DH Gaudio, S Timmermans, E TI Zero sound in a mixture of a single-component fermion gas and a Bose-Einstein condensate SO PHYSICAL REVIEW LETTERS LA English DT Article ID ATOMS AB The resonant dynamics of mediated interactions supports zero sound in a cold atom degenerate mixture of a single-component fermion gas and a Bose-Einstein condensate. We characterize the onset of instability in the phase separation of an unstable mixture and we find a rich collective mode structure for stable mixtures with one undamped mode that exhibits an avoided crossing and a Landau-damped mode that terminates. C1 Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. Boston Coll, Dept Phys, Chestnut Hill, MA 02467 USA. Los Alamos Natl Lab, Div Theory, Los Alamos, NM 87545 USA. RP Santamore, DH (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. NR 29 TC 11 Z9 11 U1 0 U2 2 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 EI 1079-7114 J9 PHYS REV LETT JI Phys. Rev. Lett. PD DEC 17 PY 2004 VL 93 IS 25 AR 250402 DI 10.1103/PhysRevLett.93.250402 PG 4 WC Physics, Multidisciplinary SC Physics GA 880JD UT WOS:000225785200002 PM 15697876 ER PT J AU Rocha, LA AF Rocha, LA TI Mitochondrial DNA and color pattern variation in three western Atlantic Halichoeres (labridae), with the revalidation of two species SO COPEIA LA English DT Article ID LIFE-HISTORY TRAITS; REEF FISHES; SEXUAL SELECTION; SOUTH ATLANTIC; SHORE FISHES; AMAZON RIVER; EVOLUTION; ECOLOGY; PHYLOGEOGRAPHY; BIOGEOGRAPHY AB Genetic surveys of widely distributed marine species often find previously undetected biodiversity. In the present study, populations of three species of Halichoeres were sampled across their entire geographical ranges: Halichoeres cyanocephalus and Halichoeres maculipinna were sampled on both sides of the Amazon freshwater outflow, the main biogeographic barrier in the tropical western Atlantic; and Halichoeres garnoti was sampled in the Caribbean and Bermuda. Genetic divergences between populations separated by the Amazon ranged from 2.3% in H. cyanocephalus to 6.5% in H. maculipinna. There is inconsistency between color differences and genetic partitions in the species surveyed. The color differences between populations of H. cyanocephalus and H. maculipinna correspond to deep genetic partitions at the cytochrome b locus. However, genetic similarity at this same locus was observed between populations of H. garnoti with striking color differences. Based on the combination of the observed genetic differences with diagnostic color differences, the Brazilian species Halichoeres dimidiatus (Agassiz) and Halichoeres penrosei Starks, 1913 are revalidated. In addition, a neotype is designated to H. cyanocephalus (Bloch, 1791), to clarify its taxonomic status and type locality. All species analyzed have a similar larval dispersal potential, but varying degrees of genetic divergences were observed, indicating that benthic stage ecology may also play a role in speciation in this group. C1 Smithsonian Trop Res Inst, NAOS Lab, Unit 0948, Miami, FL 34002 USA. RP Rocha, LA (reprint author), Smithsonian Trop Res Inst, NAOS Lab, Unit 0948, APO AA, Miami, FL 34002 USA. EM rochal@naos.si.edu RI Rocha, Luiz/C-5107-2011 NR 61 TC 60 Z9 66 U1 0 U2 7 PU AMER SOC ICHTHYOLOGISTS & HERPETOLOGISTS PI MIAMI PA MAUREEN DONNELLY, SECRETARY FLORIDA INT UNIV BIOLOGICAL SCIENCES, 11200 SW 8TH STREET, MIAMI, FL 33199 USA SN 0045-8511 EI 1938-5110 J9 COPEIA JI Copeia PD DEC 15 PY 2004 IS 4 BP 770 EP 782 DI 10.1643/CG-04-106 PG 13 WC Zoology SC Zoology GA 880QU UT WOS:000225805100004 ER PT J AU Fernandez, L Vari, RP AF Fernandez, L Vari, RP TI New species of Trichomycterus from midelevation localities of northwestern Argentina (Siluriformes : Trichomycteridae) SO COPEIA LA English DT Article ID TELEOSTEI; ANDES AB Trichomycterus pseudosilvinichthys, new species, is described from midelevation drainages in the Provincia de La Rioja, Argentina. The new species is distinguished from other members of the apparently nomnonophyletic genus Trichomycterus by having the insertion of the first proximal dorsal-fin pterygiophore at, or posterior to, vertebra 20 to 22; the presence of the pelvic fin and girdle; a fronto-lachrymal tendon bone with a lateral expansion but an incomplete laterosensory canal segment; the absence of a portion of the supraorbital laterosensory canal running between the frontal and nasal bones with the resultant loss of pore 3; the possession of 17-19 ribs; a first pectoral-fin ray that is not prolonged as a short filament; and the tip of the pelvic fin falling short of the anus. C1 Smithsonian Inst, Div Fishes, Natl Museum Nat Hist, Washington, DC 20013 USA. Fdn Miguel Lillo, Dept Zool, Div Ictiol, RA-4000 San Miguel De Tucuman, Argentina. RP Vari, RP (reprint author), Smithsonian Inst, Div Fishes, Natl Museum Nat Hist, POB 37012,WG-14,MRC-159, Washington, DC 20013 USA. EM vari.richard@nmnh.si.edu NR 18 TC 6 Z9 6 U1 0 U2 1 PU AMER SOC ICHTHYOLOGISTS & HERPETOLOGISTS PI MIAMI PA MAUREEN DONNELLY, SECRETARY FLORIDA INT UNIV BIOLOGICAL SCIENCES, 11200 SW 8TH STREET, MIAMI, FL 33199 USA SN 0045-8511 EI 1938-5110 J9 COPEIA JI Copeia PD DEC 15 PY 2004 IS 4 BP 876 EP 882 DI 10.1643/CI-04-094R1 PG 7 WC Zoology SC Zoology GA 880QU UT WOS:000225805100013 ER PT J AU Root, DB Hacker, BR Mattinson, JM Wooden, JL AF Root, DB Hacker, BR Mattinson, JM Wooden, JL TI Zircon geochronology and ca. 400 Ma exhumation of Norwegian ultrahigh-pressure rocks: an ion microprobe and chemical abrasion study SO EARTH AND PLANETARY SCIENCE LETTERS LA English DT Article DE zircon; U/Pb; UHP; REE; eclogite; Norway ID WESTERN GNEISS REGION; HIGH-GRADE METAMORPHISM; SM-ND AGES; U-PB; ECLOGITE TRANSITION; NORWAY; CALEDONIDES; GARNET; RECRYSTALLIZATION; PRESERVATION AB Understanding the formation and exhumation of the remarkable ultrahigh-pressure (UHP) rocks of the Western Gneiss Region, Norway, hinges oil precise determination of the time of eclogite recrystallization. We conducted detailed thermal ionization mass spectrometry, chemical abrasion analysis and sensitive high-resolution ion-microprobe analysis of zircons from four ultrahigh- and high-pressure (HP) rocks. Ion-microprobe analyses from the Flatraket eclogite yielded a broad range of apparently concordant Caledonian ages, suggesting long-term growth. In contrast. higher precision thermal ionization mass spectrometry analysis of zircon subject to combined thermal annealing and multi-step chemical abrasion yielded moderate Pb loss front the first (lowest temperature) abrasion step.. possible minor Pb loss or minor growth at 400 Ma from the second step and a 407-404 Ma cluster of slightly discordant - Pb-206/(238) U ages, most likely free from Ph loss, from the remaining abrasion steps. We interpret the latter to reflect zircon crystallization at similar to405-400 Ma with minor discordance from inherited cores. Zircon crystallization occurred at eclogite-facies, possibly post-peak conditions, based on compositions of garnet inclusions in zircon as well as nearly flat HREE profiles and lack of Eu anomalies in zircon fractions subjected to chemical abrasion. These ages are significantly younger than the 425 Ma age often cited for western Norway eclogite recrysiallization, implying faster of exhumation (>2.5-8.5 km/Myr), and coeval formation of eclogites across the UHP portion of the Western Gneiss Region. (C) 2004 Published by Elsevier B.V. C1 Univ Calif Santa Barbara, Dept Geol Sci, Santa Barbara, CA 93106 USA. US Geol Survey, Menlo Pk, CA 94025 USA. RP Root, DB (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. EM rootd@si.edu; hacker@geol.ucsb.edu; mattinson@geol.ucsb.edu; jwooden@usgs.gov RI Hacker, Bradley/E-7750-2011 NR 43 TC 79 Z9 79 U1 0 U2 7 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0012-821X J9 EARTH PLANET SC LETT JI Earth Planet. Sci. Lett. PD DEC 15 PY 2004 VL 228 IS 3-4 BP 325 EP 341 DI 10.1016/j.epsl.2004.10.019 PG 17 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 882JV UT WOS:000225936100009 ER PT J AU King, RS Beaman, JR Whigham, DF Hines, AH Baker, ME Weller, DE AF King, RS Beaman, JR Whigham, DF Hines, AH Baker, ME Weller, DE TI Watershed land use is strongly linked to PCBs in white perch in Chesapeake Bay subestuaries SO ENVIRONMENTAL SCIENCE & TECHNOLOGY LA English DT Article ID RIVER STRIPED BASS; SEDIMENT CONTAMINATION; ORGANIC CONTAMINANTS; STREAM ECOSYSTEMS; HABITAT USE; INDICATORS; ESTUARINE; HUDSON; QUALITY; COVER AB We related total PCBs (t-PCBs) in white perch (Morone americana), an abundant estuarine resident that supports a valuable recreational and commercial fishery in the mid-Atlantic region, to the amount and spatial arrangement of developed land in watersheds that discharge into 14 subestuaries of Chesapeake Bay. We considered the intensity of development in watersheds using four developed land-use measures (% impervious surface, % total developed land, % high-intensity residential + commercial [%high-res/comm], and % commercial) to represent potential source areas of PCBs to the subestuaries. We further evaluated the importance of source proximity by calculating three inverse-distance weighted (IDW) metrics of development, an approach that weighted developed land near the shoreline more heavily than developed land farther away. Unweighted percentages of each of the four measures of developed land explained 51-69% of the variance in t-PCBs. However, IDWs markedly improved the relationships between % developed land measures and t-PCBs. Percent commercial land, weighted by its simple inverse distance, explained 99% of the variance in t-PCBs, whereas the other three measures explained as much as 93-97%. PCBs historically produced or used in commercial and residential areas are apparently persisting in the environment at the scale of the watersheds and subestuaries examined in this study, and developed land close to the subestuary has the greatest unit effect on t-PCBs in fish. These findings provide compelling evidence for a strikingly strong linkage between watershed land use and t-PCBs in white perch, and this relationship may prove useful for identifying unsampled subestuaries with a high risk of PCB contamination. C1 Baylor Univ, Dept Biol, Ctr Reservoir & Aquat Syst Res, Waco, TX 76798 USA. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Maryland Dept Environm, Tech & Regulatory Serv Adm, Baltimore, MD 21224 USA. RP King, RS (reprint author), Baylor Univ, Dept Biol, Ctr Reservoir & Aquat Syst Res, Waco, TX 76798 USA. EM Ryan_S_King@baylor.edu RI Baker, Matthew/I-2839-2014; OI Baker, Matthew/0000-0001-5069-0204; Weller, Donald/0000-0002-7629-5437; Whigham, Dennis/0000-0003-1488-820X NR 35 TC 31 Z9 33 U1 4 U2 15 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0013-936X J9 ENVIRON SCI TECHNOL JI Environ. Sci. Technol. PD DEC 15 PY 2004 VL 38 IS 24 BP 6546 EP 6552 DI 10.1021/es049059m PG 7 WC Engineering, Environmental; Environmental Sciences SC Engineering; Environmental Sciences & Ecology GA 880AX UT WOS:000225761800020 PM 15669311 ER PT J AU Wernicke, B Davis, JL Bennett, RA Normandeau, JE Friedrich, AM Niemi, NA AF Wernicke, B Davis, JL Bennett, RA Normandeau, JE Friedrich, AM Niemi, NA TI Tectonic implications of a dense continuous GPS velocity field at Yucca Mountain, Nevada SO JOURNAL OF GEOPHYSICAL RESEARCH-SOLID EARTH LA English DT Article DE geodesy; tectonics; Yucca Mountain ID CALIFORNIA SHEAR ZONE; LITTLE-SKULL-MOUNTAIN; GLOBAL POSITIONING SYSTEM; VALLEY FAULT ZONE; STRAIN ACCUMULATION; SLIP RATES; RANGE PROVINCE; EARTHQUAKE SEQUENCE; NORTHERN BASIN; 1992 LANDERS AB A dense, continuous GPS network was established in the Yucca Mountain area in 1999 to provide the most reliable measurements possible of geodetic strain patterns across the nation's only proposed permanent repository for high-level radioactive waste. The network lies astride a boundary between the geodetically stable central Great Basin and the active western Great Basin, which at the latitude of Yucca Mountain is undergoing distributed right-lateral shear at a rate of similar to60 nstrain/yr. Monitoring from 1999 to 2003 (3.75 years) yields a velocity field characterized by nearly homogenous N20degreesW right-lateral shear of 20+/-2 nstrain/yr (net velocity contrast of similar to1.2 mm/yr across a 60 km aperture) in the vicinity of the proposed repository site. Comparison of time series of continuous results with earlier campaign surveys indicating similar to50 nstrain/yr of west-northwest extension from 1991 to 1997 suggests that the more rapid rates were in part transient motions associated with the 1992 M-s 5.4 Little Skull Mountain earthquake. Postseismic motions do not appear to affect the 1999-2003 velocity field in either campaign or continuous data. The magnitude of the velocity contrast across the area, the overall linearity of the gradient, and the large area of undeforming crust to the east of Yucca Mountain are difficult to explain by elastic bending of the crust associated with the Death Valley fault zone, a major right-lateral strike-slip fault about 50 km west of the repository site. These observations, along with apparent local variations in the velocity gradient, suggest that significant right-lateral strain accumulation, with displacement rate in the 1 mm/yr range, may be associated with structures in the Yucca Mountain area. The absence of structures in the area with equivalent late Quaternary displacement rates underscores the problem of reconciling discrepancies between geologic and geodetic estimates of deformation rates. C1 CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Wernicke, B (reprint author), CALTECH, Div Geol & Planetary Sci, Mail Stop 100-23,1200 E Calif Blvd, Pasadena, CA 91125 USA. EM brian@gps.caltech.edu RI Niemi, Nathan/A-9996-2011; Friedrich, Anke/G-2921-2011; Davis, James/D-8766-2013; OI Friedrich, Anke/0000-0002-6938-8563; Davis, James/0000-0003-3057-477X; Niemi, Nathan/0000-0002-3380-3024 NR 50 TC 30 Z9 30 U1 0 U2 8 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9313 EI 2169-9356 J9 J GEOPHYS RES-SOL EA JI J. Geophys. Res.-Solid Earth PD DEC 15 PY 2004 VL 109 IS B12 AR B12404 DI 10.1029/2003JB002832 PG 13 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 881QO UT WOS:000225883100001 ER PT J AU Hoke, KL Burmeister, SS Fernald, RD Rand, AS Ryan, MJ Wilczynski, W AF Hoke, KL Burmeister, SS Fernald, RD Rand, AS Ryan, MJ Wilczynski, W TI Functional mapping of the auditory midbrain during mate call reception SO JOURNAL OF NEUROSCIENCE LA English DT Article DE auditory; midbrain; amphibian; egr-1; mating; tungara frogs ID EFFERENT INNERVATION PATTERNS; HORMONE-CONCENTRATING CELLS; SUPERIOR OLIVARY NUCLEUS; DRIVEN GENE-EXPRESSION; TORUS SEMICIRCULARIS; LEOPARD FROG; AUTORADIOGRAPHIC LOCALIZATION; SONG PRESENTATION; SEXUAL SELECTION; RANA-CATESBEIANA AB We examined patterns of neural activity as assayed by changes in gene expression to localize representation of acoustic mating signals in the auditory midbrain of frogs. We exposed wild-caught male Physalaemus pustulosus to conspecific mating calls that vary in their behavioral salience, nonsalient mating calls, or no sound. We measured expression of the immediate early gene egr-1 (also called ZENK, zif268, NGFI-A, and krox-24) throughout the torus semicircularis, the auditory midbrain homolog of the inferior colliculus. Differential egr-1 induction in response to the acoustic stimuli occurred in the laminar, midline, and principal nuclei of the torus semicircularis, whereas the ventral region did not show significant effects of stimulus. The laminar nucleus differentially responded to conspecific mating calls compared with nonsalient mating calls, whereas the midline and principal nuclei responded preferentially to one of two conspecific calls. These responses were not explained by simple acoustic properties of the stimuli, and they demonstrate a functional heterogeneity of auditory processing of complex biological signals within the frog midbrain. Moreover, using analyses that assess the ability of the torus semicircularis as a whole to discriminate among acoustic stimuli, we found that activity patterns in the four regions together provide more information about biologically relevant acoustic stimuli than activity in any single region. C1 Univ Texas, Sect Integrat Biol, Austin, TX 78712 USA. Univ Texas, Dept Psychol, Austin, TX 78712 USA. Stanford Univ, Dept Psychol, Stanford, CA 94305 USA. Stanford Univ, Neurosci Program, Stanford, CA 94305 USA. Smithsonian Trop Res Inst, Balboa, Panama. RP Hoke, KL (reprint author), Univ Texas, Sect Integrat Biol, 1 Univ Stn C0930, Austin, TX 78712 USA. NR 55 TC 51 Z9 51 U1 0 U2 15 PU SOC NEUROSCIENCE PI WASHINGTON PA 11 DUPONT CIRCLE, NW, STE 500, WASHINGTON, DC 20036 USA SN 0270-6474 J9 J NEUROSCI JI J. Neurosci. PD DEC 15 PY 2004 VL 24 IS 50 BP 11264 EP 11272 DI 10.1523/JNEUROSCI.2079-04.2004 PG 9 WC Neurosciences SC Neurosciences & Neurology GA 880CK UT WOS:000225766200010 PM 15601932 ER PT J AU Guimaraes, RZP Gasparini, JL Rocha, LA AF Guimaraes, RZP Gasparini, JL Rocha, LA TI A new cleaner goby of the genus Elacatinus (Teleostei : Gobiidae), from Trindade Island, off Brazil SO ZOOTAXA LA English DT Article DE Western South Atlantic; oceanic island; Brazil; reef fish; endemism; new species; Elacatinus; Gobiidae ID ATLANTIC; PACIFIC; FISHES AB Elacatinus pridisi n. sp., a cleaner goby from Trindade Island, off Brazil, differs from its congeners of the Horsti Complex that have a pale stripe extending from the eye to the caudal fin base by the following combination of characters: dark longitudinal stripe wide, reaching lower abdomen and base of anal fin (vs. never reaching lower abdomen or base of anal fin in all other species); pectoral-fin rays typically 18 (vs. typically 17 in E. randalli (Bohlke & Robins) and E. figaro Sazima et al. and typically 16 in E. atronasum (Bohlke Robins)); anal-fin rays typically 11 (vs. typically 10 in E. figaro); a pale oval spot present on snout (vs. no spot in E. atronasum and E. horsti (Bohlke & Robins), a "V"-shaped spot in E. prochilos (Bohlke & Robins), and a medial bar in E. xanthiprora (Bohlke & Robins), E. louisae (Bohlke & Robins) and E. lori Colin). The new species was recorded in depths ranging from 3 to 30 m, over rocky reefs and calcareous-algae banks around the island. It has been observed in cleaning activities during the day with clients varying from large-sized carnivores such as Carcharhinus perezi (Poey) to small-sized planktivores such as Chromis multilineata (Guichenot). The discovery of the new species reinforces recognition of the Trindade-Martin Vaz insular complex as an area of endemism in the Atlantic Ocean. C1 Univ Fed Rio de Janeiro, Lab Biodiversidade Recursos Pesqueiros, BR-21941569 Rio De Janeiro, Brazil. Oceansat Tecnol Espacial Monitoramento Ambiental, BR-20090001 Rio De Janeiro, Brazil. Univ Fed Espirito Santo, Dept Ecol & Recursos Nat, BR-29041970 Vitoria, Espirito Santo, Brazil. Smithsonian Trop Res Inst, APO, AA 34002 USA. RP Guimaraes, RZP (reprint author), Univ Fed Rio de Janeiro, Lab Biodiversidade Recursos Pesqueiros, Cidade Univ, BR-21941569 Rio De Janeiro, Brazil. EM ricardo@biologia.ufrj.br; gaspa.vix@terra.com.br; Rocha@naos.si.edu RI Rocha, Luiz/C-5107-2011 NR 11 TC 8 Z9 8 U1 1 U2 3 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, 1030, NEW ZEALAND SN 1175-5334 J9 ZOOTAXA JI Zootaxa PD DEC 14 PY 2004 IS 770 BP 1 EP 8 PG 8 WC Zoology SC Zoology GA 883GC UT WOS:000225998300001 ER PT J AU Wei, XM Rodriguez, AD Baran, P Raptis, RG Sanchez, JA Ortega-Barria, E Gonzalez, J AF Wei, XM Rodriguez, AD Baran, P Raptis, RG Sanchez, JA Ortega-Barria, E Gonzalez, J TI Antiplasmodial cembradiene diterpenoids from a Southwestern Caribbean gorgonian octocoral of the genus Eunicea SO TETRAHEDRON LA English DT Article DE diterpene; Eunicea sp.; single-crystal X-ray analysis; cytotoxicity; antimalarial; Caribbean gorgonian octocoral ID AUSTRALIAN SOFT CORALS; GLYCOSIDES AB Five new representatives of the cembrane class of marine natural products have been isolated as minor metabolites from an undescribed species of Eunicea, a sea whip collected near the Colombian Southwestern Caribbean Sea. The structure of the crystalline metabolite 1 was solved by single-crystal X-ray diffraction analysis. Structures could then be proposed for cembradienes 2-5 by comprehensive spectral analyses involving 2D NMR, IR, UV, and high-resolution mass spectrometry, as well as chemical interconversion studies. Compound 1 exhibited weak cytotoxicity in the NCI 3-cell line panel human cancer screening program, whereas compounds 1, 2 and 4 displayed significant antiplasmodial activity against Plasmodium falciparum. (C) 2004 Elsevier Ltd. All rights reserved. C1 Univ Puerto Rico, Dept Chem, San Juan, PR 00931 USA. Smithsonian Inst, Dept Systemat Biol, Washington, DC 20013 USA. Smithsonian Inst, Labs Analyt Biol, Washington, DC 20013 USA. Inst Invest Cientif Avanzadas & Serv Alta Tecnol, Cent Estudios Biomed, Panama City 5, Panama. RP Rodriguez, AD (reprint author), Univ Puerto Rico, Dept Chem, POB 23346,UPR Stn, San Juan, PR 00931 USA. EM arodrig@cnnet.upr.edu RI Gonzalez Santamaria, Jose/Q-2439-2015; Johnson, Selena/K-3541-2013 NR 13 TC 21 Z9 24 U1 1 U2 4 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0040-4020 J9 TETRAHEDRON JI Tetrahedron PD DEC 13 PY 2004 VL 60 IS 51 BP 11813 EP 11819 DI 10.1016/j.tet.2004.09.108 PG 7 WC Chemistry, Organic SC Chemistry GA 873WE UT WOS:000225311400015 ER PT J AU Maller, AH Bullock, JS AF Maller, AH Bullock, JS TI Multiphase galaxy formation: high-velocity clouds and the missing baryon problem SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Review DE galaxy : formation; cooling flows; galaxies : formation; intergalactic medium; quasars : absorption lines ID COLD DARK-MATTER; KELVIN-HELMHOLTZ INSTABILITIES; ALPHA ABSORPTION SYSTEMS; LYMAN-LIMIT SYSTEMS; X-RAY-CLUSTERS; GALACTIC HALO; LOCAL GROUP; STAR-FORMATION; MAGELLANIC STREAM; ANGULAR-MOMENTUM AB The standard treatment of cooling in cold dark matter haloes assumes that all of the gas within a 'cooling radius' cools and contracts monolithically to fuel galaxy formation. Here we take into account the expectation that the hot gas in galactic haloes is thermally unstable and prone to fragmentation during cooling and we show that the implications are more far-reaching than previously expected: allowing multiphase cooling fundamentally alters expectations about gas infall in galactic haloes and naturally gives rise to a characteristic upper limit on the masses of galaxies, as observed. Specifically, we argue that cooling should proceed via the formation of high-density, similar to 10(4) K clouds, pressure-confined within a hot gas background. The background medium that emerges has a low density, and can survive as a hydrostatically stable corona with a long cooling time. The fraction of halo baryons contained in the residual hot core component grows with halo mass because the cooling density increases with gas temperature, and this leads to an upper-mass limit in quiescent, non-merged galaxies of similar to10(11) Mcircle dot. In this scenario, galaxy formation is fuelled by the infall of pressure-supported clouds. For Milky-Way-size systems, clouds of mass similar to5 x 10(6) Mcircle dot that formed or merged within the last several Gyr should still exist as a residual population in the halo, with a total mass in clouds of similar to2 x 10(10) Mcircle dot. The baryonic mass of the Milky Way galaxy is explained naturally in this model, and is a factor of 2 smaller than would result in the standard treatment without feedback. We expect clouds in galactic haloes to be similar to1 kpc in size and to extend similar to150 kpc from galactic centres. The predicted properties of Milky Way clouds match well the observed radial velocity distribution, angular sizes, column densities and velocity widths of high-velocity clouds around our Galaxy. The clouds we predict are also of the type needed to explain high-ion absorption systems at z < 1, and the predicted covering factor around external galaxies is consistent with observations. C1 Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. RP Maller, AH (reprint author), Univ Massachusetts, Dept Astron, LGRT-B 619E,710 N Pleasant St, Amherst, MA 01003 USA. EM ari@astro.umass.edu; jbullock@cfa.harvard.edu RI Bullock, James/K-1928-2015 OI Bullock, James/0000-0003-4298-5082 NR 137 TC 259 Z9 259 U1 0 U2 2 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD DEC 11 PY 2004 VL 355 IS 3 BP 694 EP 712 DI 10.1111/j.1365-2966.2004.08349.x PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 884WA UT WOS:000226116200008 ER PT J AU Jones, DH Saunders, W Colless, M Read, MA Parker, QA Watson, FG Campbell, LA Burkey, D Mauch, T Moore, L Hartley, M Cass, P James, D Russell, K Fiegert, K Dawe, J Huchra, J Jarrett, T Lahav, O Lucey, J Mamon, GA Proust, D Sadler, EM Wakamatsu, K AF Jones, DH Saunders, W Colless, M Read, MA Parker, QA Watson, FG Campbell, LA Burkey, D Mauch, T Moore, L Hartley, M Cass, P James, D Russell, K Fiegert, K Dawe, J Huchra, J Jarrett, T Lahav, O Lucey, J Mamon, GA Proust, D Sadler, EM Wakamatsu, K TI The 6dF Galaxy Survey: samples, observational techniques and the first data release SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE surveys; galaxies : clusters : general; galaxies : distances and redshifts; cosmology : observations; large-scale structure of Universe ID DIGITAL SKY SURVEY; MULTIOBJECT FIBER-SPECTROSCOPY; REDSHIFT SURVEY; LUMINOSITY FUNCTIONS; PECULIAR VELOCITIES; ELLIPTIC GALAXIES; TILING ALGORITHM; POWER SPECTRUM; DENSITY; CLUSTERS AB The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z similar to 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K-tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J, r(F), b(J)) = (13.05, 13.75, 15.6, 16.75). Central to the survey is the Six-Degree Field (6dF) multifibre spectrograph, an instrument able to record 150 simultaneous spectra over the 5.7-field of the UK Schmidt Telescope. An adaptive tiling algorithm has been employed to ensure around 95 per cent fibring completeness over the 17 046 deg(2) of the southern sky with \b\ > 10degrees. Spectra are obtained in two observations using separate V and R gratings, that together give R similar to 1000 over at least 4000-7500 Angstrom and signal-to-noise ratio similar to10 per pixel. Redshift measurements are obtained semi-automatically, and are assigned a quality value based on visual inspection. The 6dFGS data base is available at http://www-wfau.roe.ac.uk/6dFGS/, with public data releases occurring after the completion of each third of the survey. C1 Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. Anglo Australian Observ, Epping, NSW 2121, Australia. Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. Macquarie Univ, Dept Phys, Sydney, NSW 2109, Australia. Univ Sydney, Sch Phys, Sydney, NSW 2006, Australia. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. UCL, Dept Phys & Astron, London WC1E 6BT, England. Univ Durham, Dept Phys, Durham DH1 3LE, England. Inst Astrophys, CNRS, UMR 7095, F-75014 Paris, France. Observ Paris, CNRS, UMR 8111, GEPI, F-92195 Meudon, France. Gifu Univ, Fac Engn, Gifu 5011192, Japan. RP Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. EM heath@mso.anu.edu.au; will@aao.gov.au; colless@aao.gov.au; fgw@aao.gov.au; lachlan@tnso.anu.edu.au OI Sadler, Elaine/0000-0002-1136-2555; Mamon, Gary/0000-0001-8956-5953; Colless, Matthew/0000-0001-9552-8075 NR 48 TC 251 Z9 256 U1 0 U2 6 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD DEC 11 PY 2004 VL 355 IS 3 BP 747 EP 763 DI 10.1111/j.1365-2966.2004.08353.x PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 884WA UT WOS:000226116200011 ER PT J AU Sobolewska, MA Siemiginowska, A Zycki, PT AF Sobolewska, MA Siemiginowska, A Zycki, PT TI High-redshift radio-quiet quasars: Exploring the parameter space of accretion models. II. Patchy corona model SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; galaxies : high-redshift; quasars : general; X-rays : galaxies ID OPTICALLY SELECTED QUASARS; BLACK-HOLE MASS; X-RAY-SPECTRA; CHANDRA; DISKS; MULTIWAVELENGTH; VARIABILITY; LUMINOSITY; EMISSION; GALAXIES AB We modeled the spectral energy distribution of high-redshift radio-quiet quasars (high-z RQQs). We computed spectra in a patchy corona geometry in which an accretion disk extends to the last stable orbit and the Comptonizing active regions (hot clouds) are distributed above the disk. We explored the model parameter space to find theoretical parameters that give spectra with an optical/UV luminosity, X-ray loudness, and X-ray photon index compatible with those of high-z RQQs observed with Chandra. We found that a range of solutions is possible, from high-kT(e) low-tau to low-kT(e) high-tau models. The solutions require a low level of energy dissipation in the hot clouds and a low disk covering factor. The modeled mass is on the order of 10(10) M-circle dot, and the accretion rate is. (M)over dot greater than or equal to 0.2 (M)over dot(Edd). We compare our results with those obtained previously for a hot inner flow geometry. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Nicholas Copernicus Astron Ctr, PL-00716 Warsaw, Poland. RP Sobolewska, MA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM msobolewska@cfa.harvard.edu; asiemiginowska@cfa.harvard.edu; ptz@camk.edu.pl NR 39 TC 18 Z9 18 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 10 PY 2004 VL 617 IS 1 BP 102 EP 112 DI 10.1086/425262 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 880CP UT WOS:000225766700006 ER PT J AU Mullis, CR Henry, JP Gioia, IM Bohringer, H Briel, UG Voges, W Huchra, JP AF Mullis, CR Henry, JP Gioia, IM Bohringer, H Briel, UG Voges, W Huchra, JP TI Spatial correlation function of X-ray-selected active galactic nuclei SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : observations; large-scale structure of universe; quasars : general; X-rays : general ID NORTH ECLIPTIC POLE; ANGULAR-CORRELATION FUNCTIONS; GALAXY REDSHIFT SURVEY; LARGE-SCALE STRUCTURE; OPTICAL IDENTIFICATIONS; SOURCE CATALOG; QUASAR SURVEY; EVOLUTION; UNIVERSE; BIAS AB We present a detailed description of the first direct measurement of the spatial correlation function of X-ray selected active galactic nuclei (AGNs). This result is based on an X-ray flux-limited sample of 219 AGNs discovered in the contiguous 80.7 deg(2) region of the ROSAT North Ecliptic Pole (NEP) Survey. Clustering is detected at the 4 sigma level at comoving scales in the interval r=5-60 h(-1) Mpc. Fitting the data with a power law of slope gamma=1.8, we find a correlation length of r(0)=7.4(-1.9)(+1.8) h(-1) Mpc (Omega(M)=0.3, Omega(Lambda)=0.7). The median redshift of the AGN contributing to the signal is z(xi)=0.22. This clustering amplitude implies that X-ray-selected AGNs are spatially distributed in a manner similar to that of optically selected AGNs. Furthermore, the ROSAT NEP determination establishes the local behavior of AGN clustering, a regime that is poorly sampled in general. Combined with high-redshift measures from optical studies, the ROSAT NEP results argue that the AGN correlation strength essentially does not evolve with redshift, at least out to zsimilar to2.2. In the local universe, X-ray-selected AGNs appear to be unbiased relative to galaxies, and the inferred X-ray bias parameter is near unity, b(X)similar to1. Hence, X-ray-selected AGNs closely trace the underlying mass distribution. The ROSAT NEP AGN catalog, presented here, features complete optical identifications and spectroscopic redshifts. The median redshift, X-ray flux, and X-ray luminosity are z=0.41, f(X)=1.1x10(-13) ergs cm(-2) s(-1), and L-X=9.2x10(43) h(70)(-2) ergs s(-1) (0.5-2.0 keV), respectively. Unobscured, type I AGNs are the dominant constituents (90%) of this soft X-ray-selected sample of AGNs. C1 European So Observ, D-85748 Garching, Germany. Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. CNR, Ist Radioastron, I-40129 Bologna, Italy. Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Univ Michigan, Dept Astron, 918 Denisson,501 E Univ Ave, Ann Arbor, MI 48109 USA. EM cmullis@umich.edu RI Gioia, Isabella/B-6982-2012 OI Gioia, Isabella/0000-0003-3127-498X NR 70 TC 43 Z9 44 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 10 PY 2004 VL 617 IS 1 BP 192 EP 208 DI 10.1086/425248 PN 1 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 880CP UT WOS:000225766700013 ER PT J AU Evans, IN Koratkar, AP AF Evans, IN Koratkar, AP TI Chandra X-ray observations of the inner optical filaments in Centaurus A SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : individual (NGC 5128); galaxies : ISM; X-rays : galaxies ID RADIO-LOBE; NGC 5128; NGC-5128; REGION; JETS AB We have obtained Chandra High Resolution Camera (0.1-10 keV) X-ray imaging of the inner optical filaments of Cen A. Faint X-ray emission is observed associated with the filaments with significance levels of 2-3.5 sigma when the data are adaptively smoothed. Comparison with optical [O III] lambda5007 emission-line imaging suggests that the X-ray-emitting gas is associated with the northwest edge of the optical line-emitting gas. This region of the filaments is closest to the radio jet and is therefore a candidate for shock heating induced by turbulent instabilities in the interstellar medium. The observed X-ray luminosity is significantly smaller than that predicted by purely radiative shock models of the filaments, implying that mechanical energy input does not provide 100% of the ionizing energy budget for the filaments. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21250 USA. RP Evans, IN (reprint author), Smithsonian Astrophys Observ, 60 Garden St,MS-81, Cambridge, MA 02138 USA. EM ievans@cfa.harvard.edu; koratkar@umbc.edu NR 27 TC 6 Z9 6 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 10 PY 2004 VL 617 IS 1 BP 209 EP 213 DI 10.1086/425164 PN 1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 880CP UT WOS:000225766700014 ER PT J AU Kobulnicky, HA Kewley, LJ AF Kobulnicky, HA Kewley, LJ TI Metallicities of 0.3 < z < 1.0 galaxies in the GOODS-North field SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : abundances; galaxies : evolution; galaxies : fundamental parameters; galaxies : starburst; HII regions; ISM : abundances ID STAR-FORMING GALAXIES; H-II REGIONS; DWARF IRREGULAR GALAXIES; EMISSION-LINE GALAXIES; HIGH-REDSHIFT GALAXIES; CHEMICAL EVOLUTION; FORMATION HISTORY; HII-REGIONS; DEEP SURVEY; ELECTRON TEMPERATURES AB We measure nebular oxygen abundances for 204 emission-line galaxies with redshifts 0.3&SIM;20), consistent with scenarios whereby the formation epoch for less massive galaxies is more recent than for massive galaxies. C1 Univ Wyoming, Dept Phys & Astron, Laramie, WY 82071 USA. Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Kobulnicky, HA (reprint author), Univ Wyoming, Dept Phys & Astron, Laramie, WY 82071 USA. EM chipk@uwyo.edu; lkewley@cfa.harvard.edu NR 75 TC 375 Z9 377 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 10 PY 2004 VL 617 IS 1 BP 240 EP 261 DI 10.1086/425299 PN 1 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 880CP UT WOS:000225766700017 ER EF