FN Thomson Reuters Web of Science™ VR 1.0 PT J AU Watters, TR Nimmo, F Robinson, MS AF Watters, TR Nimmo, F Robinson, MS TI Extensional troughs in the Caloris basin of Mercury: Evidence of lateral crustal flow SO GEOLOGY LA English DT Article DE Mercury; caloris basin; tectonics; uplift; crustal flow ID MARE SERENITATIS; THICKNESS; TECTONICS; RIDGES; ORIGIN; LITHOSPHERE; TOPOGRAPHY; FRACTURES; GRAVITY; HISTORY AB Thirty years ago Mariner 10 revealed extensional troughs that form giant polygons in the floor material of the Caloris impact basin, Mercury. The polygonal troughs occur in the interior of the basin and overprint wrinkle ridges formed in an earlier stage of compression. In contrast, lunar and martian basins exhibit extensional troughs that are circumferential and confined to basin margins. Loading by basin-filling material can explain the extensional and compressional features seen in deformed lunar and martian basins, but not the existence of the Caloris polygonal troughs. Here we suggest that the Caloris troughs formed from late-stage basin uplift and extension due to lateral flow of a relatively thick crust toward the basin center. If such lateral flow occurs, the resulting timing, location, and magnitude of the extensional stresses predicted by our model are consistent with those inferred from the polygonal troughs. These results are not strongly dependent on the degree of lateral How or the assumed crustal rigidity. For a dry plagioclase rheology and likely radiogenic heat fluxes, the crustal thickness around Calloris is 90-140 km. Similar late-stage uplift and extension probably do not occur in basins on the Moon and Mars because their crusts are too thin to allow analogous lateral flow. C1 Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. Univ Calif Santa Cruz, Dept Earth Sci, Santa Cruz, CA 95064 USA. Northwestern Univ, Ctr Planetary Sci, Evanston, IL 60208 USA. RP Watters, TR (reprint author), Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. NR 38 TC 29 Z9 29 U1 0 U2 3 PU GEOLOGICAL SOC AMER, INC PI BOULDER PA PO BOX 9140, BOULDER, CO 80301-9140 USA SN 0016-8505 J9 GEOLOGY JI Geology PD AUG PY 2005 VL 33 IS 8 BP 669 EP 672 DI 10.1130/G21678 PG 4 WC Geology SC Geology GA 949IU UT WOS:000230779400014 ER PT J AU Suarez-Morales, E Iliffe, TM AF Suarez-Morales, E Iliffe, TM TI A new Stygonitocrella Petkovski (Copepoda : Harpacticoida) from a cave in Northern Mexico with comments on the taxonomy of the genus SO HYDROBIOLOGIA LA English DT Article DE cave fauna; freshwater copepods; troglobitic; invertebrate taxonomy ID FRESH-WATER; CRUSTACEA; COLONIZATION; AMEIRIDAE AB The cave-dwelling harpacticoid copepod fauna of Mexico is still yet to be known. There are only a few records related to karstic caves, but most refer to epigean forms. The analysis of samples collected in a cave system in Northern Mexico yielded two female specimens of an unknown harpacticoid copepod species which is described herein. It was assigned to the genus Stygonitocrella Petkovski, 1976 mainly because of the presence of a single endopodal segment on legs 1-4; the new species, S. mexicana n. sp. differs from its congeners by a combination of characters related to the segmentation and armature of the swimming legs 1-4, the fifth leg of the female, and the strcture of the antennae. Based on the current limits of Stygonitocrella, two new subgenera, are proposed to recognize different morphological patterns based on the presence or absence of an inner baseoendopodal lobe in the female fifth leg, a character not evaluated before. This lobe is absent in the new species and in other five species now contained in the subgenus Eustygonitocrella. A lobe is present in the new subgenus Fiersiella, also with six species. This is the second record of Stygonitocrella in North America, after S. (Fiersiella) sequoyahi Reid, Hunt & Stanley, 2003; it is the only North American cave-dwelling species of the genus. It is suggested that the influence of marine transgressions in Northern Mexico was related to the origin of the new species as part of a group of troglobitic forms originated from marine interstitial ancestors that colonized the freshwater caves. A key for the identification of all the known species of Stygonitocrella is also provided. C1 ECOSUR, Unidad Chetumal, Chetumal 77000, Quintana Roo, Mexico. Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. Texas A&M Univ, Dept Marine Biol, Galveston, TX 77553 USA. RP Suarez-Morales, E (reprint author), ECOSUR, Unidad Chetumal, AP 424, Chetumal 77000, Quintana Roo, Mexico. EM esuarez@ecosur-qroo.mx NR 36 TC 9 Z9 9 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0018-8158 J9 HYDROBIOLOGIA JI Hydrobiologia PD AUG 1 PY 2005 VL 544 BP 215 EP 228 DI 10.1007/s10750-005-0621-7 PG 14 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 965NX UT WOS:000231958500017 ER PT J AU Gingerich, O AF Gingerich, O TI The Copernicus biographies from the 16th to the 19th century. SO JOURNAL FOR THE HISTORY OF ASTRONOMY LA English DT Book Review C1 Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Gingerich, O (reprint author), Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU SCIENCE HISTORY PUBLICATIONS LTD PI CAMBRIDGE PA 16 RUTHERFORD RD, CAMBRIDGE CB2 2HH, ENGLAND SN 0021-8286 J9 J HIST ASTRON JI J. Hist. Astron. PD AUG PY 2005 VL 36 BP 343 EP 345 PN 3 PG 3 WC History & Philosophy Of Science SC History & Philosophy of Science GA 953UG UT WOS:000231105500010 ER PT J AU DeVorkin, D AF DeVorkin, D TI A concise history of solar and stellar physics. SO JOURNAL FOR THE HISTORY OF ASTRONOMY LA English DT Book Review C1 Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA. RP DeVorkin, D (reprint author), Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 2 PU SCIENCE HISTORY PUBLICATIONS LTD PI CAMBRIDGE PA 16 RUTHERFORD RD, CAMBRIDGE CB2 2HH, ENGLAND SN 0021-8286 J9 J HIST ASTRON JI J. Hist. Astron. PD AUG PY 2005 VL 36 BP 349 EP 351 PN 3 PG 3 WC History & Philosophy Of Science SC History & Philosophy of Science GA 953UG UT WOS:000231105500014 ER PT J AU Novotny, V Miller, SE Basset, Y Cizek, L Darrow, K Kaupa, B Kua, J Weiblen, GD AF Novotny, V Miller, SE Basset, Y Cizek, L Darrow, K Kaupa, B Kua, J Weiblen, GD TI An altitudinal comparison of caterpillar (Lepidoptera) assemblages on Ficus trees in Papua New Guinea SO JOURNAL OF BIOGEOGRAPHY LA English DT Article DE beta diversity; cryptic species; elevation gradient; Ficus; host specificity; Lepidoptera; Malesia; rain forest; species diversity; species turnover ID MONTANE RAIN-FOREST; LEAF-CHEWING INSECTS; SPECIES RICHNESS; ELEVATIONAL GRADIENT; GEOMETRID MOTHS; HERBIVOROUS INSECTS; COMMUNITIES; DIVERSITY; PATTERNS AB Aim This analysis of caterpillar (Lepidoptera) beta-diversity between tropical lowlands and highlands attempts to separate the effects of between-site (1) turnover of herbivore species on particular host plants, (2) changes in host use by herbivores, and (3) turnover of plant species on changes in herbivore assemblages. Location Two rain forest areas 130 km and 1700 altitudinal metres apart were studied in Papua New Guinea: one in the lowlands (100 m a.s.l.) on the northern coast of the island and one in the central New Guinean cordillera at 1800 m a.s.l. Methods The analysis is based on caterpillar feeding records obtained by quantitative sampling and rearing of caterpillars from four Ficus species studied in the mountains and 21 Ficus species and 62 plant species from other genera and families studied in the lowlands, including three Ficus species studied in both areas. Results Only 17% of species feeding on Ficus in the highlands also occurred in the lowlands. These species represented 1-46% of individuals in caterpillar assemblages on particular Ficus hosts. Widespread species included both Ficus specialists and generalists feeding on numerous plant families. Some of the Ficus specialists changed their preferred host species with altitude. High species turnover was not explained by changes in the species composition of host plants with altitude as lowland and montane assemblages feeding on the same Ficus species showed high turnover. Despite the rarity of widespread caterpillars, the lowland and montane Ficus assemblages were remarkably similar in their dominance structure, species richness, host specificity, generic composition and familial composition. Main conclusions Ficus-feeding Lepidoptera assemblages between tropical lowlands and highlands are characterized by substantial species turnover not explained by altitudinal changes in the composition of the vegetation. Further, species-rich plant genera can support caterpillar assemblages with relatively low beta-diversity compared with species-poor genera as caterpillars can switch their host preferences from one congeneric host species to another along an altitudinal gradient. Closely related plant species can thus represent a broad, continuously distributed resource along such gradients. C1 Acad Sci Czech Republ, Inst Entomol, CZ-37005 Ceske Budejovice, Czech Republic. Univ S Bohemia, Fac Biol, Ceske Budejovice, Czech Republic. Smithsonian Inst, Natl Zool Pk, Washington, DC 20008 USA. Natl Museum Nat Hist, Washington, DC 20560 USA. Smithsonian Trop Res Inst, Balboa, Ancon, Panama. New Guinea Binatang Res Ctr, Madang, Papua N Guinea. Univ Minnesota, Dept Plant Biol, St Paul, MN 55108 USA. RP Novotny, V (reprint author), Acad Sci Czech Republ, Inst Entomol, Branisovska 31, CZ-37005 Ceske Budejovice, Czech Republic. EM novotny@entu.cas.cz RI Basset, Yves/B-6642-2014; Cizek, Lukas/G-7905-2014; Novotny, Vojtech/G-9434-2014; Cizek, Lukas/K-7111-2015; OI Novotny, Vojtech/0000-0001-7918-8023; Miller, Scott/0000-0002-4138-1378 NR 57 TC 40 Z9 40 U1 0 U2 24 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0305-0270 J9 J BIOGEOGR JI J. Biogeogr. PD AUG PY 2005 VL 32 IS 8 BP 1303 EP 1314 DI 10.1111/j.1365-2699.2004.01225.x PG 12 WC Ecology; Geography, Physical SC Environmental Sciences & Ecology; Physical Geography GA 948OX UT WOS:000230726700003 ER PT J AU Thorwirth, S McCarthy, MC Gottlieb, CA Thaddeus, P Gupta, H Stanton, JF AF Thorwirth, S McCarthy, MC Gottlieb, CA Thaddeus, P Gupta, H Stanton, JF TI Rotational spectroscopy and equilibrium structures of S-3 and S-4 SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID GEOMETRICAL STRUCTURE; FLASH-PHOTOLYSIS; ELEMENTAL SULFUR; 2ND DERIVATIVES; SOLID ARGON; AB-INITIO; SPECTRA; TETRASULFUR; PERTURBATION; FREQUENCIES AB The sulfur molecules thiozone S-3 and tetrasulfur S-4 have been observed in a supersonic molecular beam in the centimeter-wave band by Fourier transform microwave spectroscopy, and in the millimeter- and submillimeter-wave bands in a low-pressure glow discharge. For S-3 over 150 rotational transitions between 10 and 458 GHz were measured, and for S-4 a comparable number between 6 and 271 GHz. The spectrum of S-3 is reproduced to within the measurement uncertainties by an asymmetric top Hamiltonian with three rotational and 12 centrifugal distortion constants; ten distortion constants, but an additional term to account for very small level shifts caused by interchange tunneling, are required to reproduce to comparable accuracy the spectrum of S-4. Empirical equilibrium (r(e)(emp)) structures of S-3 and S-4 were derived from experimental rotational constants of the normal and sulfur-34 species and vibrational corrections from coupled-cluster theory calculations. Quantum chemical calculations show that interchange tunneling occurs because S-4 automerizes through a transition state with D-2h symmetry which lies about 500 cm(-1) above the two equivalent C-2 upsilon minima on the potential energy surface. (C) 2005 American Institute of Physics. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Harvard Univ, Div Engn & Appl Sci, Cambridge, MA 02138 USA. Univ Texas, Dept Chem & Biochem, Inst Theoret Chem, Austin, TX 78712 USA. RP Thorwirth, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM sthorwirth@cfa.harvard.edu RI Thorwirth, Sven/C-6217-2011; OI Thorwirth, Sven/0000-0001-8200-6710; McCarthy, Michael/0000-0001-9142-0008 NR 43 TC 36 Z9 37 U1 0 U2 8 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 AUG 1 PY 2005 VL 123 IS 5 AR 054326 DI 10.1063/1.1942495 PG 10 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 954QD UT WOS:000231168700042 PM 16108658 ER PT J AU Ferrari, FD Ueda, H AF Ferrari, FD Ueda, H TI Development of leg 5 of copepods belonging to the calanoid superfamily Centropagoidea (Crustacea) SO JOURNAL OF CRUSTACEAN BIOLOGY LA English DT Article ID MATING-BEHAVIOR; DIOITHONA-OCULATA; SWIMMING LEGS; PSEUDODIAPTOMUS; ZOOGEOGRAPHY; ANATOMY AB Leg 5 development is described for 10 species from 10 genera in 6 families of centropagoidean calanoid copepods. Segment homologies are inferred from the order in which arthrodial membranes, setae, and attenuations are added to ramal segments during late copepodid development. Among centropagoidean males, the grasping chela on the side opposite the male genital pore develops in three different ways. The fixed part of the chela may be a ventral attenuation of the basis, or of the proximal exopodal segment, or of the middle exopodal segment, suggesting that a male leg 5 chela is not a synapomorphy of the Centropagoidea because nonhomologous segments make up the convergent morphology. In like manner, a grasping subchela on the side opposite the male genital pore is expressed in three different ways: basis plus proximal, middle and distal exopodal segments; basis plus proximal and distal exopodal segments; or basis plus distal exopodal segment; so nonhomologous segments also result in a convergent subchela morphology. On leg 5 of adult females, a ventral attenuation of the middle exopodal segment, initially formed at copepodid stage V, is present on species of Centropagidae and Diaptomidae. A ventral attenuation of the exopod initially expressed at copepodid stage V on females of Temoridae is considered a homologous structure, although failure to express the proximal arthrodial membrane of the exopod complicates the interpretation of its origin. A ventral attenuation first appears on the exopod of Pontellidae and Acartiidae at copepodid stage V, but its homologies with the above families are more difficult to determine because neither proximal or distal arthrodial membranes nor setae are present on the adult exopod. The species of Tortanidae studied here does not express a ventral attenuation on the exopod at copepodid stage V or at the adult stage, but adults of some other species of Tortanus do. The ventral attenuation of the exopod of adult female leg 5, initially present at copepodid stage V, is a more likely synapomorphy for the superfamily although evidence for this homologous structure may be difficult to identify due to the secondary loss of setae and arthrodial membranes on the exopod of some species. Presence at copepodid stage V of the presumptive genital somite complex of the adult female is expressed among all centropagoideans studied here and appears to be an unambiguous synapomorphy for species of the superfamily. C1 Smithsonian Inst, Museum Natl Hist Nat, Dept Zool, Suitland, MD 20746 USA. Ehime Univ, Ctr Marine Environm Studies, Matsuyama, Ehime 7908577, Japan. RP Ferrari, FD (reprint author), Smithsonian Inst, Museum Natl Hist Nat, Dept Zool, MRC-534,4210 Silver Hill Rd, Suitland, MD 20746 USA. EM ferrari.frank@msc.si.edu; hueda@sci.ehime-u.ac.jp NR 51 TC 9 Z9 11 U1 0 U2 1 PU CRUSTACEAN SOC PI SAN ANTONIO PA 840 EAST MULBERRY, SAN ANTONIO, TX 78212 USA SN 0278-0372 J9 J CRUSTACEAN BIOL JI J. Crustac. Biol. PD AUG PY 2005 VL 25 IS 3 BP 333 EP 352 DI 10.1651/C2554 PG 20 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 959VB UT WOS:000231546300003 ER PT J AU Ferrari, FD Ivanenko, VN AF Ferrari, FD Ivanenko, VN TI Copepodid stages of Euryte longicauda (Cyclopoida, Cyclopidae, Euryteinae) from the white sea associated with the bryozoan Flustra foliacea SO JOURNAL OF CRUSTACEAN BIOLOGY LA English DT Article ID RIDGEWAYIA-KLAUSRUETZLERI; DIOITHONA-OCULATA; SWIMMING LEGS; CRUSTACEA; PATTERNS; PACIFIC; BELIZE AB The copepodid phase of development of Euryte longicauda Philippi, 1843, is described from six stages associated with the bryozoan Flustra foliacea Linnaeus, 1758 Distinctive character states of the species include: distal teeth of mandibular gnathobase perpendicular to proximal teeth: distal seta of maxillular praecoxa with multiple cusps is perpendicular to proximal setae with one cusp; coxa of maxillule as a gnathobase perpendicular to praecoxa; maxillular palp comprised of two setae; fluted setae medially on the distal segment complex of both rami of swimming legs 1-4. The segmental homologies of the maxilla of E. longicauda are an unarmed syncoxa, a basis with two setiferous lobes, and a ramus of three segments. A re-examination of type specimens of E. bellatula Humes, 199 1, and E. verecunda Humes, 1992, revealed a 2-segmented protopod for leg 5, confirming their inclusion in Euryte. Euryte longicauda retains the ancestral state for development of swimming legs 1-4. Development of the maxilliped suggests that E. longicaudata shares with Troglocyclops janstocki Rocha and IIiffe, 1994, and Neocyclops vicinus (Herbst, 1955) more states expressed during endopodal development of primitive cyclopoids, while endopodal development of the maxilliped of the remaining Cyclopidae is truncated. Euryte longicaudata, Tjanstocki, and N. vicinus appear to belong to a monophyletic lineage at the base of the Cyclopidae; T. janstocki is most closely related to E. longicaudata. C1 Smithsonian Inst, Museum Natl Hist Nat, Dept Zool, Suitland, MD 20746 USA. Moscow MV Lomonosov State Univ, Fac Biol, Dept Invertebrate Zool, Moscow 119899, Russia. RP Ferrari, FD (reprint author), Smithsonian Inst, Museum Natl Hist Nat, Dept Zool, MRC-534,4210 Silver Hill Rd, Suitland, MD 20746 USA. EM ferrari.frank@msc.si.edu; ivanenko@soil.msu.ru RI Ivanenko, Viatcheslav/B-8198-2008 OI Ivanenko, Viatcheslav/0000-0003-1255-0491 NR 58 TC 5 Z9 7 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 AUG PY 2005 VL 25 IS 3 BP 353 EP 374 DI 10.1651/C-2533 PG 22 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 959VB UT WOS:000231546300004 ER PT J AU Benfield, SL Guzman, HM Mair, JM AF Benfield, SL Guzman, HM Mair, JM TI Temporal mangrove dynamics in relation to coastal development in Pacific Panama SO JOURNAL OF ENVIRONMENTAL MANAGEMENT LA English DT Article DE mangrove; aerial photography; dynamics; coastal development ID REMOTE-SENSING TECHNIQUES; TIDAL FORESTS; ECOSYSTEMS; MANAGEMENT; SEEDLINGS; GROWTH; COLONIZATION; CONSERVATION; REGENERATION; RESTORATION AB This study assessed the changes in extent of fringing mangrove located in Punta Mala Bay, Panama in relation to coastal development over a period of two decades. Punta Mala Bay was chosen for this study, due to its social importance and its biological significance, as it is one of the few mangrove areas left around Panama City. Fieldwork confirmed the importance of Laguncularia racemosa in the bay, which formed nearly monospecific stands with a large number of seedlings indicating that the forest was rejuvenating. The mangrove was mapped from 1980 to 2002 using digitised aerial photographs and a GIS was used to determine the location and rates of mangrove growth and loss before and after the construction of a road and water treatment works in 1998. The land use maps were produced with an overall accuracy of 83.8%. The user's accuracy of the maps for L. racemosa dominated stands was 89.7%, although the producer's accuracy was lower due to the omission of seedlings on intertidal areas. It was found that the mangrove was spatially dynamic and had grown substantially in the bay at a rate ranging from 6 to 215% per year until the construction commenced. Between 1997 and 2002 there were 100% loss of mangrove in some areas due to the coastal development. The resilience of the dominant species L. racemosa at this locality was shown by the continued growth of two mangrove zones during the construction period 1997-2002, with one zone increasing in area by 61%. The pioneering ability of L. racemosa after disturbance was demonstrated by the development of two new mangrove zones of 498 and 1254 m(2) on bare intertidal areas after construction finished. Future mapping and fieldwork could provide information on the development of mangrove communities and their response to reoccurring human impacts. (c) 2005 Elsevier Ltd. All rights reserved. C1 Heriot Watt Univ, Sch Life Sci, Sch Built Environm, Edinburgh EH14 4AS, Midlothian, Scotland. Smithsonian Trop Res Inst, Balboa, Panama. RP Benfield, SL (reprint author), Heriot Watt Univ, Sch Life Sci, Sch Built Environm, Edinburgh EH14 4AS, Midlothian, Scotland. EM s.l.benfield@hw.ac.uk NR 47 TC 28 Z9 31 U1 3 U2 21 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0301-4797 EI 1095-8630 J9 J ENVIRON MANAGE JI J. Environ. Manage. PD AUG PY 2005 VL 76 IS 3 BP 263 EP 276 DI 10.1016/j.jenvman.2005.02.004 PG 14 WC Environmental Sciences SC Environmental Sciences & Ecology GA 948KF UT WOS:000230714000009 PM 15927354 ER PT J AU Borrell, BJ Goldbogen, JA Dudley, R AF Borrell, BJ Goldbogen, JA Dudley, R TI Aquatic wing flapping at low Reynolds numbers: swimming kinematics of the Antarctic pteropod, Clione antarctica SO JOURNAL OF EXPERIMENTAL BIOLOGY LA English DT Article DE Clione antarctica; drag; flapping flight; kinematics; lift; pteropod; swimming ID HOVERING INSECT FLIGHT; HYMENOCHIRUS-BOETTGERI; ARTEMIA LARVAE; LOCOMOTION; AERODYNAMICS; MOLLUSK; PROPULSION; LIMACINA; FORCE; MORPHOLOGY AB We studied swimming kinematics of the Antarctic pteropod, Clione antarctica, to investigate how propulsive forces are generated by flexible oscillating appendages operating at low Reynolds numbers (10 < Re < 100). We filmed ten ascending individuals at 125 frames s(-1) from two orthogonal views, and reconstructed three-dimensional coordinates of the wing tip and body. Each half-stroke of flapping consisted of distinct power and recovery phases, which were of approximately equal duration in both the upstroke and the downstroke. As pteropods ascended, the body traced a sawtooth path when viewed laterally. The magnitude of these oscillations decreased with body mass, and larger animals (operating at Re > 25) exhibited gliding during the recovery phase of each half-stroke. Maximum translational and rotational accelerations of the body occurred at the initiation of each power phase, suggesting that rotational circulation, the acceleration reaction, and wake recapture may all potentially contribute to vertical force production. Individual contributions of these mechanisms cannot, however, be assessed from these kinematic data alone. During recovery phases of each half-stroke, C antarctica minimized adverse drag forces by orienting the wings parallel to flow and by moving them along the body surface, possibly taking advantage of boundary layer effects. Vertical force production was altered through changes in the hydrodynamic angle of attack of the wing that augmented drag during the power phase of each half-stroke. At higher translational velocities of the body, the inclination of the power phase also became more nearly vertical. These results indicate that, in addition to serotonin-mediated modulation of wingbeat frequency reported previously in Clione, geometric alteration of wingbeat kinematics offers a precise means of controlling swimming forces. C1 Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. Smithsonian Trop Res Inst, Balboa, Panama. RP Borrell, BJ (reprint author), Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. EM bborrell@berkeley.edu NR 50 TC 13 Z9 13 U1 2 U2 9 PU COMPANY OF BIOLOGISTS LTD PI CAMBRIDGE PA BIDDER BUILDING CAMBRIDGE COMMERCIAL PARK COWLEY RD, CAMBRIDGE CB4 4DL, CAMBS, ENGLAND SN 0022-0949 J9 J EXP BIOL JI J. Exp. Biol. PD AUG PY 2005 VL 208 IS 15 BP 2939 EP 2949 DI 10.1242/jeb.01733 PG 11 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 960FO UT WOS:000231575800023 PM 16043599 ER PT J AU Carleton, MD Lawlor, TE AF Carleton, MD Lawlor, TE TI Peromyscus from Santa Catalina Island, Sea of Cortez, Mexico: Taxonomic identities and biogeographic implications SO JOURNAL OF MAMMALOGY LA English DT Article DE biogeography; Peromyscus slevini; Sea of Cortez; taxonomy ID SPECIES GROUP RODENTIA; GULF-OF-CALIFORNIA; EVOLUTIONARY RELATIONSHIPS; BAJA-CALIFORNIA; DEER-MOUSE; MURIDAE; PHYLOGEOGRAPHY; SYSTEMATICS; EXTINCTION; KARYOTYPE AB Peromyscus slevini Mailliard (1924) is endemic to Santa Catalina Island, a small oceanic island in the southern Sea of Cortez. The species has been variously associated, formally or informally, with 2 subgenera-Haplomylomys and Peromyscus-and 5 species-groups-californicus, eremicus, maniculatus, and boylii or mexicanus. Based upon our taxonomic evaluations, we document that 2 species of Peromyscus, P. slevini and P. fraterculus, occur among the samples that authors have identified as P. slevini, clarify the diagnosis of P. slevini proper and allocate it to membership in the P. melanophrys species-group, and discuss biogeographic implications of this proposed relationship. C1 Smithsonian Inst, Natl Museum Nat Hist, Mammal Div, Washington, DC 20560 USA. Humboldt State Univ, Dept Biol Sci, Arcata, CA 95521 USA. RP Carleton, MD (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Mammal Div, Washington, DC 20560 USA. EM carleton.michael@nmnh.si.edu NR 49 TC 1 Z9 2 U1 0 U2 3 PU ALLIANCE COMMUNICATIONS GROUP DIVISION ALLEN PRESS PI LAWRENCE PA 810 EAST 10TH STREET, LAWRENCE, KS 66044 USA SN 0022-2372 J9 J MAMMAL JI J. Mammal. PD AUG PY 2005 VL 86 IS 4 BP 814 EP 825 DI 10.1644/1545-1542(2005)086[0814:PFSCIS]2.0.CO;2 PG 12 WC Zoology SC Zoology GA 958OR UT WOS:000231458100021 ER PT J AU McCarthy, MC Thaddeus, P AF McCarthy, MC Thaddeus, P TI The rotational spectrum of HC8N, a linear molecule with a triplet ground state SO JOURNAL OF MOLECULAR SPECTROSCOPY LA English DT Article DE molecular spectroscopy; FTMW technique ID TRANSFORM MICROWAVE SPECTROSCOPY; LABORATORY DETECTION; CARBON-CHAIN; HCCN; HC4N; HC6N; CARBENE; CLOUDS AB By means of Fourier transform microwave spectroscopy of a supersonic molecular beam, we report here the laboratory detection of HC8N, a carbon chain with a triplet electronic ground state. A total of 71 hyperfine components from six rotational transitions between 8 and 13 GHz were measured to an uncertainty of 5 kHz or better. Eight spectroscopic constants, including six fine and hyperfine coupling constants, were determined to high accuracy, despite a complex spectrum which consists of many closely spaced lines. Like the shorter HC2nN chains, the linear triplet isomer detected here is highly polar and is almost certainly the ground state of HC8N; in our molecular beam discharge source, it is 10 times less abundant than triplet HC6N, but more than 100 times less abundant than the well-studied closed-shell cyanopolyyne HC7N. Owing to the collapse of the hyperfine structure with increasing chain length, still longer chains may be detectable. Published by Elsevier Inc. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Harvard Univ, Div Engn & Appl Sci, Cambridge, MA 02138 USA. RP McCarthy, MC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mccarthy@cfa.harvard.edu; pthaddeus@cfa.harvard.edu OI McCarthy, Michael/0000-0001-9142-0008 NR 24 TC 4 Z9 5 U1 1 U2 4 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0022-2852 J9 J MOL SPECTROSC JI J. Mol. Spectrosc. PD AUG PY 2005 VL 232 IS 2 BP 351 EP 357 DI 10.1016/j.jms.2005.05.001 PG 7 WC Physics, Atomic, Molecular & Chemical; Spectroscopy SC Physics; Spectroscopy GA 949EW UT WOS:000230768700023 ER PT J AU Ireland, RR Bellolio, G Bednarek-Ochyra, H Ochyra, R AF Ireland, RR Bellolio, G Bednarek-Ochyra, H Ochyra, R TI Fertile plants of Racomitrium patagonicum (Bryopsida, Grimmiaceae) SO JOURNAL OF THE HATTORI BOTANICAL LABORATORY LA English DT Article AB Fertile plants of Racomitrium patagonicum Bednarek-Ochyra & Ochyra, known only from southern South America, are described and illustrated from collections made in Chile. The species was originally described as new from sterile plants collected in Argentina, Chile and the Falkland Islands. A map showing the revised distribution of the species is presented. C1 Museum Natl Hist Nat, Smithsonian Inst, Dept Bot, Washington, DC 20013 USA. Univ Concepcion, Fac Ciencias Nat & Oceanog, Dept Bot, Flora Chile Project, Concepcion, Chile. Polish Acad Sci, Inst Bot, Lab Bryol, PL-310512 Krakow, Poland. RP Ireland, RR (reprint author), Museum Natl Hist Nat, Smithsonian Inst, Dept Bot, MRC-166,POB 37012, Washington, DC 20013 USA. NR 6 TC 1 Z9 1 U1 0 U2 0 PU HATTORI BOTANICAL LABORATORY PI MIYAZAKI-KEN PA OBI, NICHINAN-SHI, MIYAZAKI-KEN, 889-2535, JAPAN SN 0073-0912 J9 J HATTORI BOT LAB JI J. Hattori Bot. Lab. PD AUG PY 2005 IS 98 BP 205 EP 211 PG 7 WC Plant Sciences SC Plant Sciences GA 959AA UT WOS:000231488100008 ER PT J AU Breedy, O Guzman, HM AF Breedy, O Guzman, HM TI A new species of alcyonacean octocoral from the Galapagos Archipelago SO JOURNAL OF THE MARINE BIOLOGICAL ASSOCIATION OF THE UNITED KINGDOM LA English DT Article AB The genus Heterogorgia is reported for the first time from the shallow waters of the Galapagos Archipelago, and a new species found in the southern islands is described. The new species is distinguished from the other species of the genus described thus far by having thick branches with large, densely packed calyces, being mostly unbranched, and having larger sclerites. The occurrence of Heterogorgia verrucosa is also reported. C1 Univ Costa Rica, Escuela Biol, Museo Zool, San Jose, Costa Rica. Smithsonian Trop Res Inst, Balboa, Panama. RP Breedy, O (reprint author), Univ Costa Rica, Escuela Biol, Museo Zool, San Jose, Costa Rica. EM odalisca@racsa.co.cr; guzmanh@naos.si.edu NR 21 TC 9 Z9 9 U1 2 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 AUG PY 2005 VL 85 IS 4 BP 801 EP 807 DI 10.1017/S0025315405011732 PG 7 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 955CB UT WOS:000231201300009 ER PT J AU Cardini, A Hoffmann, RS Thorington, RW AF Cardini, A Hoffmann, RS Thorington, RW TI Morphological evolution in marmots (Rodentia, Sciuridae): size and shape of the dorsal and lateral surfaces of the cranium SO JOURNAL OF ZOOLOGICAL SYSTEMATICS AND EVOLUTIONARY RESEARCH LA English DT Article DE marmot evolution; cranium; geometric morphometrics; divergence; conservation ID GEOMETRIC MORPHOMETRICS; GROUND-SQUIRRELS; PHYLOGENY; SOCIALITY; PATTERNS; MAMMALIA AB Marmots are the largest ground squirrels and have been extensively studied by sociobiologists investigating the evolution of mammal societies. Being a member of the sciurid clade, traditionally considered inclined to convergence, they are also a group on which to test the hypothesis of sciurid propensity to homoplasy of osteological characters. In the present analysis, the dorsal and lateral surfaces of the cranium of all living marmot species are compared with geometric morphometric techniques. Phenetic groups are found which reflect the subgeneric classification of marmots and are consistent with previous morphometric analyses of the mandible and ventral cranium. Two species have distinctive morphologies and phenetic relationships not congruent with phylogeny. Marmota vancouverensis is highly divergent for osteological characters, fur colour and behaviour despite its young age and close genetic similarity to Marmota caligata. Its small population may represent a rare chance to study evolutionary processes during rapid allopatric speciation in mammals, but strong conservation efforts are required to preserve this unique component of the Vancouver Island biodiversity. Also, Marmota monax has distinctive cranial traits. These are possibly related to its long separate evolutionary history and unique ecology and behaviour. Size-related convergence is not evident in Marmota. When outgroup species are included, Spermophilus, Cynomys, Tamias, and Sciurus group together on one branch, Marmota on the other. This is best explained as a retention of the ancestral morphology in the smaller members of the Marmotini (Spermophilus, Cynomys, and Tamias) and the evolution of derived morphology in Marmota. C1 Univ York, Hull York Med Sch, York YO10 5DD, N Yorkshire, England. Univ Hull, Kingston Upon Hull HU6 7RX, N Humberside, England. Smithsonian Inst, Dept Vertebrate Zool, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Cardini, A (reprint author), Univ York, Hull York Med Sch, York YO10 5DD, N Yorkshire, England. EM alcardini@interfree.it; hoffmann.robert@nmnh.si.edu; thorington.richard@nmnh.si.edu RI Rohlf, F/A-8710-2008; cardini, andrea/G-9951-2011 OI cardini, andrea/0000-0003-2910-632X NR 41 TC 21 Z9 25 U1 2 U2 16 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0947-5745 J9 J ZOOL SYST EVOL RES JI J. Zool. Syst. Evol. Res. PD AUG PY 2005 VL 43 IS 3 BP 258 EP 268 DI 10.1111/j.1439-0469.2005.00316.258-268 PG 11 WC Evolutionary Biology; Zoology SC Evolutionary Biology; Zoology GA 949CU UT WOS:000230763300008 ER PT J AU Aiello, A AF Aiello, A TI A dazzle of dragonflies. SO LIBRARY JOURNAL LA English DT Book Review C1 Smithsonian Trop Res Inst, Ancon, Panama. RP Aiello, A (reprint author), Smithsonian Trop Res Inst, Ancon, Panama. NR 1 TC 0 Z9 0 U1 0 U2 0 PU 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 AUG PY 2005 VL 130 IS 13 BP 118 EP 118 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 956KF UT WOS:000231297900389 ER PT J AU Li, C Wilkerson, RC AF Li, C Wilkerson, RC TI Identification of Anopheles (Nyssorhynchus) albitarsis complex species (Diptera : Culicidae) using rDNA internal transcribed spacer 2-based polymerase chain reaction primes SO MEMORIAS DO INSTITUTO OSWALDO CRUZ LA English DT Article DE Anopheles albitarsis; species complex; polymerase chain reaction identification; malaria; internal transcribed spacer 2 ID DNA ITS2 SEQUENCES; MALARIA VECTOR; DIFFERENTIATE; BRAZIL; ARGENTINA; MOSQUITOS; ASSAY AB Anopheles (Nyssorhynchus) marajoara is a proven primary vector of malaria parasites in Northeast Brazil, and An. deaneorum is a suspected vector in Western Brazil. Both are members of the morphologically similar Albitarsis Complex, which also includes An. albitarsis and an undescribed species, An. albitarsis "B". These four species were recognized and can be identified using random amplified polymorphic DNA (RAPD) markers, but various other methodologies also point to multiple species under the name An. albitarsis. We describe here a technique for identification of these species employing polymerase chain reaction (PCR) primers based on ribosomal DNA internal transcribed spacer 2 (rDNA ITS2) sequence. Since this method is based on known sequence it is simpler than the sometimes problematical RAPD-PCR. Primers were tested on samples previously identified using RAPD markers with complete correlation. C1 Walter Reed Army Inst Res, Dept Entomol, Silver Spring, MD 20910 USA. RP Wilkerson, RC (reprint author), Smithsonian Inst, Museum Support Ctr, 4210 Silver Hill Rd, Suitland, MD 20746 USA. EM wilkersonr@si.edu FU NIAID NIH HHS [AI RO154139] NR 27 TC 41 Z9 42 U1 0 U2 1 PU FUNDACO OSWALDO CRUZ PI RIO DE JANEIRO, RJ PA AV BRASIL 4365, 21045-900 RIO DE JANEIRO, RJ, BRAZIL SN 0074-0276 J9 MEM I OSWALDO CRUZ JI Mem. Inst. Oswaldo Cruz PY 2005 VL 100 IS 5 BP 495 EP 500 DI 10.1590/S0074-02762005000500009 PG 6 WC Parasitology; Tropical Medicine SC Parasitology; Tropical Medicine GA 965YK UT WOS:000231986600009 PM 16184227 ER PT J AU Eberhard, JR Bermingham, E AF Eberhard, JR Bermingham, E TI Phylogeny and comparative biogeography of Pionopsitta parrots and Pteroglossus toucans SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article DE neotropics; refuge hypothesis; systematics; Amazonia; birds; biogeography; phylogeny; mtDNA ID MITOCHONDRIAL-DNA; MOLECULAR SYSTEMATICS; NONSYNONYMOUS SUBSTITUTION; NEOTROPICAL BIRDS; SPECIATION; EVOLUTION; AVES; DIVERGENCE; COMPLEX; MODEL AB Studies of Neotropical birds, and their distributions and areas of endemism, in particular, have been central in the formulation of hypotheses proposed to explain the high species diversity in the Neotropics. We used mtDNA sequence data (ATPase 6 and 8, COI, and cyt b) to reconstruct the species-level phylogenies for two genera, Pionopsitta (Aves: Psittacidae) and Pteroglossus (Aves: Ramphastidae), compare our results with previous morphology-based phylogenetic analyses, and estimate the absolute timing of lineage and biogeographic divergences. Both the Pionopsitta and Pteroglossus phylogenies support a hypothesis of area relationships in which a divergence of the Serra do Mar (Atlantic Forest, Brazil) region of endemism is followed by the divergence of cis- and trans-Andean regions, then a split between the upper and lower Amazon basin, next the divergence of the Guyana area, and finally diversification of taxa in the upper Amazon basin's areas of endemism. Phylogenies of both genera support a hypothesis of area relationships that is similar to that proposed by Prum [XIX International Ornithological Congress (1988), 2562] for high-vagility species, but while they agree on the relative timing of area divergence (vicariance) events, they yield different absolute time estimates for those divergences when the typical avian mtDNA clock calibration is used. Taken at face value, the time estimates indicate that both genera began to diversify before the start of the Pleistocene, and that climatic and habitat shifts alone do not account for the diversification of these taxa. (c) 2005 Elsevier Inc. All rights reserved. C1 Smithsonian Trop Res Inst, Balboa, Panama. RP Eberhard, JR (reprint author), Louisiana State Univ, Dept Biol Sci, 202 Life Sci, Baton Rouge, LA 70803 USA. EM eberhard@lsu.edu NR 70 TC 51 Z9 52 U1 3 U2 14 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 1055-7903 J9 MOL PHYLOGENET EVOL JI Mol. Phylogenet. Evol. PD AUG PY 2005 VL 36 IS 2 BP 288 EP 304 DI 10.1016/j.ympev.2005.01.022 PG 17 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 942EO UT WOS:000230265900008 PM 15955511 ER PT J AU Roelofs, GHA Groot, PJ Marsh, TR Steeghs, D Barros, SCC Nelemans, G AF Roelofs, GHA Groot, PJ Marsh, TR Steeghs, D Barros, SCC Nelemans, G TI SDSS J124058.03-015919.2: a new AM CVn star with a 37-min orbital period SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; binaries : close; stars : individual : AM CVn; stars : individual : SDSS J124058.03-015919.2; novae, cataclysmic variables ID DOUBLE-DEGENERATE BINARY; CATACLYSMIC VARIABLES; GP COM AB We present high time-resolution spectroscopy with the Very Large Telescope of SDSS J124058.03-015919.2, anew helium-transferring binary star identified in the Sloan Digital Sky Survey. We measure an orbital period of 37.355 +/- 0.002 min, confirming the AM CVn nature of the system. From the velocity amplitudes of the accretor and the accretion stream-disc impact, we derive amass ratio q = 0.039 +/- 0.010. Our spectral coverage extends from lambda 3700-9500 angstrom and shows the presence of helium, nitrogen, silicon and iron in the accretion disc, plus the redshifted, low-velocity 'central spikes' in the helium lines, known from the low-state AM CVn stars GP Com and CE 315. Doppler tomography of the helium and silicon emission lines reveals an unusual pattern of two bright emission sites in the tomograms, instead of the usual one emission site identified with the impact of the mass stream into the accretion disc. One of the two is preferred as the conventional stream-disc impact point in velocity space, at the 3a confidence level. We speculate briefly on the origin of the second. C1 Radboud Univ, Dept Astrophys, NL-6500 GL Nijmegen, Netherlands. Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02318 USA. Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. RP Roelofs, GHA (reprint author), Radboud Univ, Dept Astrophys, POB 9010, NL-6500 GL Nijmegen, Netherlands. EM g.roelofs@astro.ru.nl RI Nelemans, Gijs/D-3177-2012; Steeghs, Danny/C-5468-2009; Groot, Paul/K-4391-2016; OI Nelemans, Gijs/0000-0002-0752-2974; Steeghs, Danny/0000-0003-0771-4746; Groot, Paul/0000-0002-4488-726X; Barros, Susana/0000-0003-2434-3625 NR 25 TC 44 Z9 44 U1 0 U2 3 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 AUG 1 PY 2005 VL 361 IS 2 BP 487 EP 494 DI 10.1111/j.1365-2966.2005.09186.x PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 952JT UT WOS:000231000500012 ER PT J AU Jonker, PG Campana, S Steeghs, D Torres, MAP Galloway, DK Markwardt, CB Chakrabarty, D Swank, J AF Jonker, PG Campana, S Steeghs, D Torres, MAP Galloway, DK Markwardt, CB Chakrabarty, D Swank, J TI Chandra observations of the millisecond X-ray pulsar IGR J00291+5934 in quiescence SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion : accretion discs; binaries : general; stars : individual : IGR J00291+5934; stars : neutron; X-rays : binaries ID NEUTRON-STAR; THERMAL EMISSION; AQUILA X-1; XMM-NEWTON; TRANSIENT; SPECTRUM; KS-1731-260; VARIABILITY; DISCOVERY AB In this paper we report on our analysis of three Chandra observations of the accretion-powered millisecond X-ray pulsar IGR J00291+5934 obtained during the late stages of the 2004 outburst. We also report the serendipitous detection of the source in quiescence by ROSAT during MID 48830-48839 (1992 July 26-August 4). The detected 0.3-10 keV source count rates varied significantly between the Chandra observations from (7.2 +/- 1.2) x 10(-3), (6.8 +/- 0.9) x 10(-3) and (1.4 +/- 0. 1) x 10(-2) counts s(-1) for the first, second and third Chandra observations, on MJD 53371.88 (2005 January 1), 53383.99 (2005 January 13) and 53407.57 (2005 February 6), respectively. The count rate for the third observation is 2.0 +/- 0.4 times as high as that of the average of the first two observations. The unabsorbed 0.5-10 keV source fluxes for the bestfitting power-law model to the source spectrum were (7.9 +/- 2.5) x 10(-14), (7.3 +/- 2.0) x 10(-14), and (1.17 +/- 0.22) x 10(-13) erg cm(-2) s(-1) for the first, second and third Chandra observations, respectively. We find that this source flux is consistent with that found by ROSAT [ approximate to (5.4 +/- 2.4) x 10(-14) erg cm(-2) s(-1)]. Under the assumption that the interstellar extinction, NH, does not vary between the observations, we find that the blackbody temperature during the second Chandra observation is significantly higher than that during the first and third observations. Furthermore, the effective temperature of the neutron star derived from fitting an absorbed blackbody or neutron star atmosphere model to the data is rather high in comparison with many other neutron star soft X-ray transients in quiescence, even during the first and third observations. If we assume that the source quiescent luminosity is similar to that measured for two other accretion powered millisecond pulsars in quiescence, the distance to IGR J00291+5934 is 2.6-3.6 kpc. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. SRON, Natl Inst Space Res, NL-3584 CA Utrecht, Netherlands. Osserv Astron Brera, INAF, I-23807 Merate, LC, Italy. MIT, Ctr Space Res, Cambridge, MA 02139 USA. NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM pjonker@cfa.harvard.edu RI Swank, Jean/F-2693-2012; Steeghs, Danny/C-5468-2009; OI Steeghs, Danny/0000-0003-0771-4746; Galloway, Duncan/0000-0002-6558-5121 NR 38 TC 22 Z9 22 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD AUG 1 PY 2005 VL 361 IS 2 BP 511 EP 516 DI 10.1111/j.1365-2966.2005.09171.x PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 952JT UT WOS:000231000500015 ER PT J AU Edge, WRT Coe, MJ Galache, JL McBride, VA Corbet, RHD Okazaki, AT Laycock, S Markwardt, CB Marshall, FE Udalski, A AF Edge, WRT Coe, MJ Galache, JL McBride, VA Corbet, RHD Okazaki, AT Laycock, S Markwardt, CB Marshall, FE Udalski, A TI The binary period and outburst behaviour of the Small Magellanic Cloud X-ray binary pulsar system SXP504 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars : emission-line, Be; Magellanic Clouds; X-rays : binaries ID NEUTRON-STAR; SMC AB A probable binary period has been detected in the optical counterpart to the X-ray source CXOUJ005455.6-724510 = RXJ0054.9-7245 = AXJ0054.8-7244 = SXP504 in the Small Magellanic Cloud. This source was detected by Chandra on 2002 July 4 and subsequently observed by XMM-Newton on 2003 December 18. The source is coincident with an Optical Gravitational Lensing object in the light curves of which several optical outburst peaks are visible at similar to 268-d intervals. Timing analysis shows a period of 268.6 +/- 0.1 d at > 99 per cent significance. Archival Rossi X-ray Timing Explorer data for the 504-s pulse-period have revealed detections which correspond closely with predicted or actual peaks in the optical data. The relationship between this orbital period and the pulse period of 504 s is within the normal variance found in the Corbet diagram. C1 Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Space Res Assoc, Columbia, MD 21044 USA. Hokkai Gakuen Univ, Fac Engn, Sapporo, Hokkaido, Japan. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Maryland, Dept Astron, College Pk, MD 20742 USA. Univ Warsaw Observ, PL-00478 Warsaw, Poland. RP Edge, WRT (reprint author), Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. EM wrte@astro.soton.ac.uk NR 19 TC 5 Z9 5 U1 0 U2 1 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 AUG 1 PY 2005 VL 361 IS 2 BP 743 EP 747 DI 10.1111/j.1365-2966.2005.09205.x PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 952JT UT WOS:000231000500037 ER PT J AU Sack, L Tyree, MT Holbrook, NM AF Sack, L Tyree, MT Holbrook, NM TI Leaf hydraulic architecture correlates with regeneration irradiance in tropical rainforest trees SO NEW PHYTOLOGIST LA English DT Article DE Barro Colorado Island (BCI); biological networks; high pressure flowmeter (HPFM); leaf hydraulics; shade tolerance; vasculature ID PHOTOSYNTHETIC TRAITS; STOMATAL CONDUCTANCE; XYLEM CAVITATION; SHADE TOLERANCE; WOODY-PLANTS; GROWTH-RATE; WATER-FLOW; LEAVES; RESISTANCE; SEEDLINGS AB (.) The leaf hydraulic conductance ( K leaf) is a major determinant of plant water transport capacity. Here, we measured K leaf, and its basis in the resistances of leaf components, for fully illuminated leaves of five tree species that regenerate in deep shade, and five that regenerate in gaps or clearings, in Panamanian lowland tropical rainforest. We also determined coordination with stomatal characters and leaf mass per area. (.) K-leaf varied 10- fold across species, and was 3- fold higher in sun- than in shade-establishing species. On average, 12% of leaf hydraulic resistance (= 1/ K-leaf) was located in the petiole, 25% in the major veins, 25% in the minor veins, and 39% outside the xylem. Sun- establishing species had a higher proportion of leaf resistance in the xylem. Across species, component resistances correlated linearly with total leaf resistance. (.) K-leaf correlated tightly with indices of stomatal pore area, indicating a coordination of liquid- and vapor- phase conductances shifted relative to that of temperate woody species. (.) Leaf hydraulic properties are integrally linked in the complex of traits that define differences in water use and carbon economy across habitats and vegetation zones. (c) New Phytologist ( 2005). C1 Univ Hawaii Manoa, Dept Bot, Honolulu, HI 96822 USA. Smithsonian Trop Res Inst, Balboa, Ancon, Panama. Harvard Univ, Dept Organism & Evolutionary Biol, Cambridge, MA 02138 USA. Harvard Univ, Arnold Arboretum, Jamaica Plain, MA 02130 USA. USDA Forest Serv, Burlington, VT 05402 USA. RP Sack, L (reprint author), Univ Hawaii Manoa, Dept Bot, 3190 Maile Way, Honolulu, HI 96822 USA. EM Lsack@hawaii.edu RI Sack, Lawren/A-5492-2008 OI Sack, Lawren/0000-0002-7009-7202 NR 46 TC 118 Z9 125 U1 1 U2 35 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0028-646X J9 NEW PHYTOL JI New Phytol. PD AUG PY 2005 VL 167 IS 2 BP 403 EP 413 DI 10.1111/j.1469-8137.2005.01432.x PG 11 WC Plant Sciences SC Plant Sciences GA 942MP UT WOS:000230286800010 PM 15998394 ER PT J AU Babich, D AF Babich, D TI Optimal estimation of non-Gaussianity SO PHYSICAL REVIEW D LA English DT Article ID POWER SPECTRUM; BISPECTRUM AB We systematically analyze the primordial non-Gaussianity estimator used by the Wilkinson Microwave Anisotropy Probe (WMAP) science team with the basic ideas of estimation theory in order to see if the limited cosmic microwave background (CMB) data is being optimally utilized. The WMAP estimator is based on the implicit assumption that the CMB bispectrum, the harmonic transform of the three-point correlation function, contains all of the primordial non-Gaussianity information in a CMB map. We first demonstrate that the signal-to-noise (S/N) of an estimator based on CMB three-point correlation functions is significantly larger than the S/N of any estimator based on higher-order correlation functions; justifying our choice to focus on the three-point correlation function. We then conclude that the estimator based on the three-point correlation function, which was used by WMAP, is optimal, meaning it saturates the Cramer-Rao inequality when the underlying CMB map is nearly Gaussian. We quantify this restriction by demonstrating that the suboptimal character of our estimator is proportional to the square of the fiducial non-Gaussianity, which is already constrained to be extremely small, so we can consider the WMAP estimator to be optimal in practice. Our conclusions do not depend on the form of the primordial bispectrum, only on the observationally established weak levels of primordial non-Gaussianity. C1 Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. EM babich@physics.harvard.edu NR 33 TC 65 Z9 65 U1 0 U2 1 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 AUG PY 2005 VL 72 IS 4 AR 043003 DI 10.1103/PhysRevD.043003 PG 13 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 960BK UT WOS:000231565000008 ER PT J AU Stritzinger, M Suntzeff, NB Hamuy, M Challis, P Demarco, R Germany, L Soderberg, AM AF Stritzinger, M Suntzeff, NB Hamuy, M Challis, P Demarco, R Germany, L Soderberg, AM TI An atlas of spectrophotometric Landolt standard stars SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID INFRARED PHOTOMETRY; OPTICAL PHOTOMETRY; CELESTIAL EQUATOR; IA SUPERNOVAE; CALIBRATION; 1999EE; SYSTEM; SUN AB We present CCD observations of 102 Landolt standard stars obtained with the Ritchey-Chretien spectrograph on the Cerro Tololo Inter-American Observatory 1.5 m telescope. Using stellar atmosphere models, we have extended the flux points to our six spectrophotometric secondary standards, in both the blue and the red, allowing us to produce flux-calibrated spectra that span a wavelength range from 3050 angstrom to 1.1 mu m. Mean differences between UBVRI spectrophotometry computed using Bessell's standard passbands and Landolt's published photometry were determined to be 1% or less. Observers in both hemispheres will find these spectra useful for flux-calibrating spectra, and through the use of accurately constructed instrumental passbands, will be able to compute accurate corrections to bring instrumental magnitudes to any desired standard photometric system (S-corrections). In addition, by combining empirical and modeled spectra of the Sun, Sirius, and Vega, we calculate and compare synthetic photometry to observed photometry taken from the literature for these three stars. C1 Max Planck Inst Astrophys, D-85741 Garching, Germany. Cerro Tololo Interamer Observ, La Serena, Chile. Carnegie Observ, Campanas Observ, La Serena, Chile. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. European So Observ, Vitacura Santiago, Chile. CALTECH, Pasadena, CA 91125 USA. RP Stritzinger, M (reprint author), Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85741 Garching, Germany. EM stritzin@mpa-garching.mpg.de; nsuntzeff@noao.edu; mhamuy@lco.cl; pchallis@cfa.harvard.edu; demarco@pha.jhu.edu; lgermany@eso.org; ams@astro.caltech.edu RI Hamuy, Mario/G-7541-2016; OI stritzinger, maximilian/0000-0002-5571-1833 NR 33 TC 37 Z9 37 U1 1 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6280 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD AUG PY 2005 VL 117 IS 834 BP 810 EP 822 DI 10.1086/431468 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 953WW UT WOS:000231113400004 ER PT J AU Small, LM AF Small, LM TI The price of ambition (Smithson) 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 AUG PY 2005 VL 36 IS 5 BP 11 EP 11 PG 1 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA 948IX UT WOS:000230710500002 ER PT J AU James, HF Olson, SL AF James, HF Olson, SL TI The diversity and biogeography of koa-finches (Drepanidini : Rhodacanthis), with descriptions of two new species SO ZOOLOGICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Article DE Acacia koa; character displacement; extinction; evolutionary rates; fossils; Hawaiian honeycreepers; Hawaiian Islands; island biogeography; Quaternary; speciation ID EXTINCT BIRDS; ECOLOGY; HAWAII; RECORD; MAUI; JAW AB All known populations of koa-finches, genus Rhodacanthis, became extinct in the Holocene epoch. Two new species are described here from Quaternary fossil sites in the Hawaiian Islands. One new species, from Kauai and Maui, is roughly the size of the historically known greater koa-finch (R. palmeri) but differs in having a more robust skull and in bill morphology. The second new species, from Oahu and Maui, is similar in size to the lesser koa-finch (R. flaviceps) but closer to R. palmeri in qualitative osteological traits. The two species of koa-finches known historically from the island of Hawaii are distinct in osteology from the fossil koa-finches on the older Hawaiian islands, indicating that at least two of the four known speciation events in the genus took place within approximately the past 500 kyr. However, the similarity of maxillae from Pleistocene and Holocene sites on Oahu suggests that the Oahu population maintained morphological stasis through the climate changes of the late Quaternary. The evidence that speciation occurred on the youngest island in the archipelago suggests that the process of community assembly on newly emergent Hawaiian landscapes was a stimulus to evolutionary diversification in Rhodacanthis. (C) 2005 The Linnean Society of London. C1 Smithsonian Inst, Natl Museum Nat Hist, Div Birds, Washington, DC 20013 USA. RP James, HF (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Div Birds, POB 37012, Washington, DC 20013 USA. EM jamesh@si.edu NR 30 TC 6 Z9 6 U1 0 U2 3 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0024-4082 EI 1096-3642 J9 ZOOL J LINN SOC-LOND JI Zool. J. Linn. Soc. PD AUG PY 2005 VL 144 IS 4 BP 527 EP 541 DI 10.1111/j.1096-3642.2005.00173.x PG 15 WC Zoology SC Zoology GA 955NR UT WOS:000231233200003 ER PT J AU Reisz, RR Scott, D Sues, HD Evans, DC Raath, MA AF Reisz, RR Scott, D Sues, HD Evans, DC Raath, MA TI Embryos of an Early Jurassic prosauropod dinosaur and their evolutionary significance SO SCIENCE LA English DT Article ID SAUROPOD DINOSAURS; LOCOMOTION AB Articulated embryos from the Lower Jurassic Elliot Formation of South Africa are referable to the prosauropod Massospondylus carinatus and, together with other material, provide substantial insights into the ontogenetic development in this early dinosaur. The large forelimbs and head and the horizontally held neck indicate that the hatchlings were obligate quadrupeds. In contrast, adult Massospondylus were at least facultatively bipedal. This suggests that the quadrupedal gait of giant sauropods may have evolved by retardation of postnatal negative allometry of the forelimbs. Embryonic body proportions and an absence of well-developed teeth suggest that hatchlings of this dinosaur may have required parental care. C1 Univ Toronto, Dept Biol, Mississauga, ON L5L 1C6, Canada. Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. Univ Witwatersrand, Bernard Price Inst Palaeontol Res, ZA-2050 Wits, Johannesburg, South Africa. RP Reisz, RR (reprint author), Univ Toronto, Dept Biol, Mississauga, ON L5L 1C6, Canada. EM rreisz@utm.utoronto.ca NR 18 TC 65 Z9 72 U1 2 U2 20 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD JUL 29 PY 2005 VL 309 IS 5735 BP 761 EP 764 DI 10.1126/science.1114942 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 951NU UT WOS:000230938200047 PM 16051793 ER PT J AU Drake, JJ Testa, P AF Drake, JJ Testa, P TI The 'solar model problem' solved by the abundance of neon in nearby stars SO NATURE LA English DT Article ID GAMMA-RAY SPECTROSCOPY; CORONAL ABUNDANCES; HELIOSEISMOLOGY; ELEMENTS; CAPELLA; CHANDRA; PLASMA; RATIO; IONS AB The interior structure of the Sun can be studied with great accuracy using observations of its oscillations, similar to seismology of the Earth. Precise agreement between helioseismological measurements and predictions of theoretical solar models(1) has been a triumph of modern astrophysics. A recent downward revision by 25-35 per cent of the solar abundances of light elements such as C, N, O and Ne (ref. 2) has, however, broken this accordance: models adopting the new abundances incorrectly predict the depth of the convection zone, the depth profiles of sound speed and density, and the helium abundance(1,3). The discrepancies are far beyond the uncertainties in either the data or the model predictions(4). Here we report neon-to-oxygen ratios measured in a sample of nearby solar-like stars, using their X-ray spectra. The abundance ratios are all very similar and substantially larger than the recently revised solar value. The neon abundance in the Sun is quite poorly determined. If the Ne/O abundance in these stars is adopted for the Sun, the models are brought back into agreement with helioseismology measurements(5,6). C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. MIT, MIT Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. RP Drake, JJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jdrake@cfa.harvard.edu NR 30 TC 150 Z9 151 U1 0 U2 2 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD JUL 28 PY 2005 VL 436 IS 7050 BP 525 EP 528 DI 10.1038/nature03803 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 949LE UT WOS:000230788800054 PM 16049481 ER PT J AU Hoke, KL Ryan, MJ Wilczynski, W AF Hoke, KL Ryan, MJ Wilczynski, W TI Social cues shift functional connectivity in the hypothalamus SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE amphibian; immediate early gene; mate choice; neural network; tungara frog ID TREEFROG HYLA-CINEREA; GREEN TREEFROG; VENTRAL HYPOTHALAMUS; ACOUSTIC MODULATION; ANURAN AMPHIBIANS; NEOTROPICAL FROG; GENE-EXPRESSION; AUDITORY-SYSTEM; NEURAL ACTIVITY; TUNGARA FROGS AB We determined how social stimuli that vary in behavioral relevance differentially activate functional networks in the frog hypothalamus. As measured by egr-1 mRNA levels, activity in three hypothalamic nuclei varied with acoustic stimulus, and these responses were correlated with egr-1 responses in different auditory regions regardless of stimulus. The correlations among hypothalamic nuclei, however, varied as a function of the behavioral relevance of the stimuli. Thus relevant social cues shift the functional connectivity within the hypothalamus, consistent with principles that underlie the simultaneous processing of sensory information in cognitive tasks. C1 Univ Texas, Sect Integrat Biol, Austin, TX 78712 USA. Smithsonian Trop Res Inst, Balboa, Panama. Univ Texas, Dept Psychol, Austin, TX 78712 USA. RP Hoke, KL (reprint author), Univ Texas, Sect Integrat Biol, 1 Univ Stn C0930, Austin, TX 78712 USA. EM khoke@psych.stanford.edu NR 46 TC 44 Z9 45 U1 0 U2 12 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 JUL 26 PY 2005 VL 102 IS 30 BP 10712 EP 10717 DI 10.1073/pnas.0502261102 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 950JL UT WOS:000230853300055 PM 16020531 ER PT J AU Emmons, LH Patton, JL AF Emmons, LH Patton, JL TI A new species of Oryzomys (Rodentia : Muridae) from eastern Bolivia SO AMERICAN MUSEUM NOVITATES LA English DT Article ID PHYLOGENY; SEQUENCES; MAMMALS; BRAZIL AB Specimens of Oryzomys referable to the megacephalus complex (Musser et al., 1998) collected in the Parque Nacional Noel Kempff Mercado (PNNKM), eastern Bolivia, are discriminated from three other currently recognized species of that group (O. megacephalus, O. perenensis, O. laticeps) by analysis of cranial morphometrics and molecular sequence of the cytochrome b gene. The Bolivian sample has the closest genetic relationship to O. perenensis (Kimura 2-parameter genetic distance X 100: 14.8) and O. laticeps (distance 12.0), but the genetic distance is large. The Bolivian sample is clearly separated from the others by both principal component and discriminant function analyses of cranial and body variables. We here describe it as a new species. Morphologically, it is intermediate in size, along with O. perenensis, between the smaller O. megacephalus and the larger-bodied O. laticeps. In pelage color and occlusal pattern it closely resembles O. megacephalus. The geographic range appears to be a relatively small area of the western basin of the Rio Itenez that drains easternmost Santa Cruz and Beni Departments. Genetically verified populations of the four species are thus far allopatric, with the known range of the new species wedged between the geographic ranges of O. perenensis to the west and O. megacephalus to the east. C1 Smithsonian Inst, Div Mammals, Washington, DC 20013 USA. Univ Calif Berkeley, Museum Vertebrate Zool, Berkeley, CA 94720 USA. RP Emmons, LH (reprint author), Smithsonian Inst, Div Mammals, NHB390 MRC108,POB 37012, Washington, DC 20013 USA. EM emmons.louise@nmnh.si.edu; patton@berkeley.edu NR 26 TC 11 Z9 16 U1 0 U2 8 PU AMER MUSEUM NATURAL HISTORY PI NEW YORK PA ATTN: LIBRARY-SCIENTIFIC PUBLICATIONS DISTRIBUTION, CENTRAL PK WEST AT 79TH ST, NEW YORK, NY 10024-5192 USA SN 0003-0082 EI 1937-352X J9 AM MUS NOVIT JI Am. Mus. Novit. PD JUL 25 PY 2005 IS 3478 BP 1 EP 26 DI 10.1206/0003-0082(2005)478[0001:ANSOOR]2.0.CO;2 PG 26 WC Biodiversity Conservation; Zoology SC Biodiversity & Conservation; Zoology GA 950IZ UT WOS:000230852100001 ER PT J AU Givnish, TJ Pires, JC Graham, SW McPherson, MA Prince, LM Patterson, TB Rai, HS Roalson, EH Evans, TM Hahn, WJ Millam, KC Meerow, AW Molvray, M Kores, PJ O'Brien, HE Hall, JC Kress, WJ Sytsma, KJ AF Givnish, TJ Pires, JC Graham, SW McPherson, MA Prince, LM Patterson, TB Rai, HS Roalson, EH Evans, TM Hahn, WJ Millam, KC Meerow, AW Molvray, M Kores, PJ O'Brien, HE Hall, JC Kress, WJ Sytsma, KJ TI Repeated evolution of net venation and fleshy fruits among monocots in shaded habitats confirms a priori predictions: evidence from an ndhF phylogeny SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE adaptation; correlated evolution; molecular systematics; monocotyledons ID SEED PLANT PHYLOGENY; FLOWERING PLANTS; SEQUENCE DATA; SPECIES-DIVERSITY; DIVERGENCE TIMES; RBCL; ANGIOSPERMS; FAMILIES; GNETALES; CONIFERS AB We present a well-resolved, highly inclusive phylogeny for monocots, based on ndhF sequence variation, and use it to test a priori hypotheses that net venation and vertebrate-dispersed fleshy fruits should undergo concerted convergence, representing independent but often concurrent adaptations to shaded conditions. Our data demonstrate that net venation arose at least 26 times and was lost eight times over the past 90 million years; fleshy fruits arose at least 21 times and disappeared I I times. Both traits show a highly significant pattern of concerted convergence (p < 10(-9)), arising 16 times and disappearing four times in tandem. This phenomenon appears driven by even stronger tendencies for both traits to evolve in shade and be lost in open habitats (p < 10(-13)-10(-29)). These patterns are among the strongest ever demonstrated for evolutionary convergence in individual traits and the predictability of evolution, and the strongest evidence yet uncovered for concerted convergence. The rate of adaptive shifts per taxon has declined exponentially over the past 90 million years, as expected when large-scale radiations fill adaptive zones. C1 Univ Wisconsin, Dept Bot, Madison, WI 53706 USA. Univ Wisconsin, Dept Agron, Madison, WI 53706 USA. Univ British Columbia, Bot Garden, Ctr Plant Res, Vancouver, BC V6T 1Z4, Canada. Univ British Columbia, Dept Bot, Vancouver, BC V6T 1Z4, Canada. Rancho Santa Ana Bot Garden, Claremont, CA 91711 USA. Washington State Univ, Sch Biol Sci, Pullman, WA 99164 USA. Hope Coll, Dept Biol, Holland, MI 49422 USA. Georgetown Coll, Washington, DC 20057 USA. USDA ARS, SHRS, Natl Germplasm Repository & Fairchild Trop Garden, Miami, FL 33156 USA. Moorpark Coll, Dept Biol, Moorpark, CA 93021 USA. Harvard Univ, Arnold Arboretum, Cambridge, MA 02138 USA. Natl Museum Nat Hist, Dept Bot, Smithsonian Inst, Washington, DC 20013 USA. Australian Natl Univ, Res Sch Biol Sci, Canberra, ACT 2601, Australia. RP Givnish, TJ (reprint author), Univ Wisconsin, Dept Bot, Madison, WI 53706 USA. EM givnish@wisc.edu RI Graham, Sean/L-3944-2014; OI Graham, Sean/0000-0001-8209-5231; Pires, J Chris/0000-0001-9682-2639 NR 42 TC 59 Z9 60 U1 1 U2 24 PU ROYAL SOCIETY PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8452 J9 P ROY SOC B-BIOL SCI JI Proc. R. Soc. Lond. Ser. B-Biol. Sci. PD JUL 22 PY 2005 VL 272 IS 1571 BP 1481 EP 1490 DI 10.1098/rspb.2005.3067 PG 10 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 955ZM UT WOS:000231268700009 PM 16011923 ER PT J AU Meggers, BJ AF Meggers, BJ TI The origins of Olmec civilization SO SCIENCE LA English DT Letter C1 Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Meggers, BJ (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. NR 3 TC 1 Z9 1 U1 0 U2 2 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD JUL 22 PY 2005 VL 309 IS 5734 BP 556 EP 556 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 948SE UT WOS:000230735200016 PM 16040687 ER PT J AU Gansicke, BT Marsh, TR Edge, A Rodriguez-Gil, P Steeghs, D Araujo-Betancor, S Harlaftis, E Giannakis, O Pyrzas, S Morales-Rueda, L Aungwerojwit, A AF Gansicke, BT Marsh, TR Edge, A Rodriguez-Gil, P Steeghs, D Araujo-Betancor, S Harlaftis, E Giannakis, O Pyrzas, S Morales-Rueda, L Aungwerojwit, A TI Cataclysmic variables from a ROSAT/2MASS selection - I. Four new intermediate polars SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; binaries : close; novae, cataclysmic variables ID AE AQUARII; ORBITAL PERIOD; WHITE-DWARF; WZ SAGITTAE; SKY SURVEY; DW-CANCRI; H-I; CATALOG; BINARIES; MINIMUM AB We report the first results from a new search for cataclysmic variables (CVs) using a combined X-ray (ROSAT)/infrared (2MASS) target selection that discriminates against background active galactic nuclei. Identification spectra were obtained at the Isaac Newton Telescope for a total of 174 targets, leading to the discovery of 12 new CVs. Initially devised to find short-period low-mass-transfer CVs, this selection scheme has been very successful in identifying new intermediate polars. Photometric and spectroscopic follow-up observations identify four of the new CVs as intermediate polars: 1RXS J063631.9+353537 P(orb)similar or equal to 201 min, P-spin= 1008.3408 s or 930.5829 s), 1RXS J070407.9+262501 (P(orb)similar or equal to 250 min, P-spin= 480.708 s) 1RXS J173021.5-055933 (P-orb= 925.27 min, P-spin= 128.0 s), and 1RXS J180340.0+401214 (P-orb= 160.21 min, P-spin= 1520.51 s). RX J1730, also a moderately bright hard X-ray source in the INTEGRAL/IBIS Galactic plane survey, resembles the enigmatic AE Aqr. It is likely that its white dwarf is not rotating at the spin equilibrium period, and the system may represent a short-lived phase in CV evolution. C1 Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. Univ Durham, Dept Phys, Durham DH1 3LE, England. Inst Astrofis Canarias, E-38200 San Cristobal la Laguna, Spain. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Natl Observ Athens, Inst Space Applicat & Remote Sensing, Athens 11810, Greece. Natl Observ Athens, Astron Inst, Athens 11810, Greece. Univ Thessaloniki, Dept Phys, Sect Astrophys Astron & Mech, Thessaloniki 54124, Greece. Radboud Univ Nijmegen, Dept Astrophys, NL-6500 GL Nijmegen, Netherlands. RP Gansicke, BT (reprint author), Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. EM boris.gaensicke@warwick.ac.uk RI Gaensicke, Boris/A-9421-2012; Steeghs, Danny/C-5468-2009; Giannakis, Omiros/K-4420-2013; Rodriguez-Gil, Pablo/H-7709-2015; OI Gaensicke, Boris/0000-0002-2761-3005; Steeghs, Danny/0000-0003-0771-4746; Giannakis, Omiros/0000-0002-2470-1042; Rodriguez-Gil, Pablo/0000-0002-4717-5102; Edge, Alastair/0000-0002-3398-6916 NR 46 TC 36 Z9 36 U1 1 U2 1 PU BLACKWELL PUBLISHING 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 JUL 21 PY 2005 VL 361 IS 1 BP 141 EP 154 DI 10.1111/j.1365-2966.2005.09138.x PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 942TC UT WOS:000230304300009 ER PT J AU Young, KE Harvey, PM Brooke, TY Chapman, N Kauffmann, J Bertoldi, F Lai, SP Alcala, J Bourke, TL Spiesman, W Allen, LE Blake, GA Evans, NJ Koerner, DW Mundy, LG Myers, PC Padgett, DL Salinas, A Sargent, AI Stapelfeldt, KR Teuben, P van Dishoeck, EF Wahhaj, Z AF Young, KE Harvey, PM Brooke, TY Chapman, N Kauffmann, J Bertoldi, F Lai, SP Alcala, J Bourke, TL Spiesman, W Allen, LE Blake, GA Evans, NJ Koerner, DW Mundy, LG Myers, PC Padgett, DL Salinas, A Sargent, AI Stapelfeldt, KR Teuben, P van Dishoeck, EF Wahhaj, Z TI The Spitzer c2d survey of large, nearby, interstellar clouds. I. Chamaeleon II observed with MIPS SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared : stars; ISM : clouds; stars : formation ID MULTIBAND IMAGING PHOTOMETER; YOUNG STELLAR OBJECTS; MAIN-SEQUENCE STARS; DARK-CLOUD; MOLECULAR CLOUDS; REDUCTION ALGORITHMS; T-TAURI; HH 54; CORES; DUST AB We present maps of over 1.5 deg(2) in Chamaeleon (Cha) II at 24, 70, and 160 mu m observed with the Spitzer Space Telescope Multiband Imaging Photometer for Spitzer (MIPS) and a 1.2 deg(2) millimeter map from SIMBA on the Swedish-ESO Submillimetre Telescope (SEST). The c2d Spitzer Legacy Team's data reduction pipeline is described in detail. Over 1500 24 mu m sources and 41 70 mu m sources were detected by MIPS with fluxes greater than 10 sigma. More than 40 potential YSOs are identified with a MIPS and 2MASS color-color diagram and by their spectral indices, including two previously unknown sources with 24 mu m excesses. Our new SIMBA millimeter map of Cha II shows that only a small fraction of the gas is in compact structures with high column densities. The extended emission seen by MIPS is compared with previous CO observations. Some selected interesting sources, including two detected at 1 mm, associated with Cha II are discussed in detail, and their SEDs are presented. The classification of these sources using MIPS data is found to be consistent with that of previous studies. C1 Univ Texas, Dept Astron, Austin, TX 78712 USA. CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. Univ Maryland, Dept Astron, College Pk, MD 20742 USA. Max Planck Inst Radioastron, D-53121 Bonn, Germany. Univ Bonn, Inst Radioastron, D-53121 Bonn, Germany. Osserv Astron Capodimonte, INAF, I-80131 Naples, Italy. Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. No Arizona Univ, Dept Phys & Astron, Flagstaff, AZ 86011 USA. Spitzer Sci Ctr, Pasadena, CA 91125 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Leiden Observ, NL-2300 RA Leiden, Netherlands. RP Young, KE (reprint author), Univ Texas, Dept Astron, 1 Univ Stn C1400, Austin, TX 78712 USA. EM kaisa@astro.as.utexas.edu; pmh@astro.as.utexas.edu; tyb@astro.caltech.edu; chapman@astro.umd.edu; jkauffma@mpifr-bonn.mpg.de; bertoldi@uni-bonn.de; slai@astro.umd.edu; jmae@sun1.na.astro.it; tbourke@cfa.harvard.edu; spies@astro.as.utexas.edu; leallen@cfa.harvard.edu; gab@gps.caltech.edu; nje@astro.as.utexas.edu; koerner@physics.nau.edu; lgm@astro.umd.edu; pmyers@cfa.harvard.edu; dlp@ipac.caltech.edu; afs@astro.caltech.edu; krs@exoplanet.jpl.nasa.gov; zwahhaj@physics.nau.edu RI Stapelfeldt, Karl/D-2721-2012 NR 50 TC 44 Z9 44 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 JUL 20 PY 2005 VL 628 IS 1 BP 283 EP 297 DI 10.1086/430597 PN 1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 948MR UT WOS:000230720500023 ER PT J AU Williams, BF Garcia, MR McClintock, JE Kong, AKH Primini, FA Murray, SS AF Williams, BF Garcia, MR McClintock, JE Kong, AKH Primini, FA Murray, SS TI An X-ray transient and optical counterpart in the M31 bulge SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : individual (M31); X-rays : binaries ID BLACK-HOLE; CHANDRA; OUTBURST; BINARIES; NOVAE AB We have obtained snapshot images of a transient X-ray source in M31 from Chandra ACIS-I and the Hubble Space Telescope (HST) Advanced Camera for Surveys (ACS). The Chandra position of the X-ray nova was R.A. = 00(h)42(m)56.(s)038 +/- 0"08, decl: = +41 degrees 12'18."50 +/- 0."07. The transient was active for at least 6 months. Previous observations set an upper limit before the X-ray outburst, demonstrating variability by a factor of > 100 and confirming the transient nature of the source. For the first 6 months after the initial detection, the X-ray luminosity was similar to 6; 10(37) ergs s(-1); it then decayed to < 5; 10(36) ergs s(-1) over the following 2 months. An HST observation 29 days after the initial X-ray detection revealed a source at R.A. = 00(h)42(m)56.(s)042, decl. = +41 degrees 12'18,"45 that was B = 24.52 +/- 0.07. This optical source faded to B = 24: 95 +/- 0: 08 in 9 months. The HST identification of an optical source at the same position as the X- ray source, fading in concert with the X- ray source, indicates that this optical source is the counterpart of the X-ray transient. The lack of high-mass stars in the region suggests that this source is a low-mass X-ray binary, and the X-ray and optical luminosities provide a rough orbital period estimate of 8(-5)(+12) days for the system. 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; jem@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 24 TC 7 Z9 7 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 JUL 20 PY 2005 VL 628 IS 1 BP 382 EP 387 DI 10.1086/430876 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 948MR UT WOS:000230720500030 ER PT J AU Bosch-Ramon, V Paredes, JM Ribo, M Miller, JM Reig, P Marti, J AF Bosch-Ramon, V Paredes, JM Ribo, M Miller, JM Reig, P Marti, J TI Orbital X-ray variability of the microquasar LS 5039 SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion; accretion disks; binaries : close; stars : individual (LS 5039); X-rays : binaries; X-rays : individual (RX J1826.2-1450) ID INTERSTELLAR-MEDIUM; BINARY LS-5039; LOW/HARD STATE; GALACTIC PLANE; RADIO; EMISSION; ENERGY; J1826.2-1450; CANDIDATES; CATALOG AB The properties of the orbit and the donor star in the high-mass X-ray binary microquasar LS 5039 indicate that accretion processes should mainly occur via a radiatively driven wind. In such a scenario, significant X-ray variability would be expected due to the eccentricity of the orbit. The source has been observed at X-rays by several missions, although with a poor coverage that prevents reaching any conclusion about orbital variability. Therefore, we conducted RXTE observations of the microquasar system LS 5039 covering a full orbital period of 4 days. Individual observations are well fitted with an absorbed power law plus a Gaussian at 6.7 keV, to account for iron-line emission that is probably a diffuse background feature. In addition, we have taken into account that the continuum is also affected by significant diffuse background contamination. Our results show moderate power-law flux variations on timescales of days, as well as the presence of miniflares on shorter timescales. The new orbital ephemerides of the system recently obtained by Casares et al. have allowed us to show, for the first time, that an increase of emission is seen close to the periastron passage, as expected in an accretion scenario. Moreover, the detected orbital variability is a factor of similar to 4 smaller than the one expected by using a simple wind accretion model, and we suggest that an accretion disk around the compact object could be responsible for this discrepancy. On the other hand, significant changes in the photon index are also observed, clearly anticorrelated with the flux variations. We interpret the overall X-ray spectral characteristics of LS 5039 in the context of X-ray radiation produced by inverse Compton and/ or synchrotron processes in the jet of this microquasar. C1 Univ Barcelona, Dept Astron Meteorol, Barcelona 08028, Spain. CEA, Serv Astrophys, Commissariat Energie Atom, F-91191 Gif Sur Yvette, France. Univ Paris 07, CNRS, Unite Mixte Rech, CEA, Paris, France. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Valencia, Inst Ciencia Mat, Grp Astron & Ciencias Espacio, Valencia 46071, Spain. Univ Crete, Dept Phys, Iraklion 71003, Greece. Univ Crete, Inst Elect Struct & Laser, Fdn Res & Technol, Iraklion 71003, Greece. Univ Jaen, Dept Fis, Escuela Politecn Super, Jaen 23071, Spain. RP Bosch-Ramon, V (reprint author), Univ Barcelona, Dept Astron Meteorol, Avenida Diagonal 647, Barcelona 08028, Spain. EM vbosch@am.ub.es; jmparedes@ub.edu; mribo@discovery.saclay.cea.fr; jmmiller@head-cfa.harvard.edu; pablo.reig@uv.es; jmarti@ujaen.es RI Reig, Pablo/A-1198-2014; Ribo, Marc/B-3579-2015; OI Reig, Pablo/0000-0002-6446-3050; Ribo, Marc/0000-0002-9931-4557; Paredes, Josep M./0000-0002-1566-9044 NR 33 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 JUL 20 PY 2005 VL 628 IS 1 BP 388 EP 394 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 948MR UT WOS:000230720500031 ER PT J AU Devor, J AF Devor, J TI Solutions for 10,000 eclipsing binaries in the bulge fields of OGLE II using DEBiL SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : eclipsing; galaxy : bulge; stars : statistics; surveys ID GRAVITATIONAL LENSING EXPERIMENT; SYNOPTIC SURVEY TELESCOPE; SMALL-MAGELLANIC-CLOUD; GALACTIC BULGE; ABSOLUTE PROPERTIES; PHOTOMETRIC SOLUTIONS; DISTANCE INDICATORS; VARIABLE-STARS; PERIOD SEARCH; LIGHT-CURVE AB We have developed a fully automated pipeline for systematically identifying and analyzing eclipsing binaries within large data sets of light curves. The pipeline is made up of multiple tiers that subject the light curves to increasing levels of scrutiny. After each tier, light curves that did not conform to a given criteria were filtered out of the pipeline, reducing the load on the following, more computationally intensive tiers. As a central component of the pipeline, we created the fully automated Detached Eclipsing Binary Light curve fitter (DEBiL), which rapidly fits large numbers of light curves to a simple model. Using the results of DEBiL, light curves of interest can be flagged for follow-up analysis. As a test case, we analyzed the 218,699 light curves within the bulge fields of the OGLE II survey and produced 10,862 model fits. We point out a small number of extreme examples, as well as unexpected structure found in several of the population distributions. We expect this approach to become increasingly important as light-curve data sets continue growing in both size and number. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Devor, J (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jdevor@cfa.harvard.edu NR 54 TC 66 Z9 66 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 JUL 20 PY 2005 VL 628 IS 1 BP 411 EP 425 DI 10.1086/431170 PN 1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 948MR UT WOS:000230720500034 ER PT J AU Su, KYL Rieke, GH Misselt, KA Stansberry, JA Moro-Martin, A Stapelfeldt, KR Werner, MW Trilling, DE Bendo, GJ Gordon, KD Hines, DC Wyatt, MC Holland, WS Marengo, M Megeath, ST Fazio, GG AF Su, KYL Rieke, GH Misselt, KA Stansberry, JA Moro-Martin, A Stapelfeldt, KR Werner, MW Trilling, DE Bendo, GJ Gordon, KD Hines, DC Wyatt, MC Holland, WS Marengo, M Megeath, ST Fazio, GG TI The vega debris disk: A surprise from Spitzer SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; infrared : stars; planetary systems; stars : individual (Vega) ID MULTIBAND IMAGING PHOTOMETER; MAIN-SEQUENCE STARS; RADIATION PRESSURE; SPACE-TELESCOPE; REDUCTION ALGORITHMS; ACCRETION DISKS; SOLAR-SYSTEM; DUSTY DEBRIS; GRAINS; SUBMILLIMETER AB We present high spatial resolution mid- and far-infrared images of the Vega debris disk obtained with the Multiband Imaging Photometer for Spitzer ( MIPS). The disk is well resolved, and its angular size is much larger than found previously. The radius of the disk is at least 43" (330 AU), 70" (543 AU), and 105" (815 AU) in extent at 24, 70, and 160 mu m, respectively. The disk images are circular, smooth, and without clumpiness at all three wavelengths. The radial surface brightness profiles follow radial power laws of r(-3) or r(-4) and imply an inner boundary at a radius of 11" +/- 2" (86 AU). Assuming an amalgam of amorphous silicate and carbonaceous grains, the disk can be modeled as an axially symmetric and geometrically thin disk, viewed face-on, with the surface particle number density following an inverse radial power law. The disk radiometric properties are consistent with a range of models using grains of sizes similar to 1 to similar to 50 mu m. The exact minimum and maximum grain size limits depend on the adopted grain composition. However, all of these models require an r(-1) surface number density profile and a total mass of (3 +/- 1.5) x 10(-3) M-circle plus in grains. We find that a ring, containing grains larger than 180 mu m and at radii of 86 - 200 AU from the star, can reproduce the observed 850 mu m flux, while its emission does not violate the observed MIPS profiles. This ring could be associated with a population of larger asteroidal bodies analogous to our own Kuiper Belt. Cascades of collisions starting with encounters among these large bodies in the ring produce the small debris that is blown outward by radiation pressure to much larger distances, where we detect its thermal emission. The relatively short lifetime (< 1000 yr) of these small grains and the observed total mass, similar to 3 x 10(-3) M-circle plus, set a lower limit on the dust production rate, similar to 10(15) g s(-1). This rate would require a very massive asteroidal reservoir for the dust to be produced in a steady state throughout Vega's life. Instead, we suggest that the disk we imaged is ephemeral and that we are witnessing the aftermath of a large and relatively recent collisional event, and a subsequent collisional cascade. C1 Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Max Planck Inst Astron, D-69117 Heidelberg, Germany. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Space Sci Inst, Boulder, CO 80301 USA. Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Su, KYL (reprint author), Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA. EM ksu@as.arizona.edu RI Stapelfeldt, Karl/D-2721-2012; OI Su, Kate/0000-0002-3532-5580 NR 41 TC 144 Z9 144 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 JUL 20 PY 2005 VL 628 IS 1 BP 487 EP 500 DI 10.1086/430819 PN 1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 948MR UT WOS:000230720500041 ER PT J AU Furlan, E Calvet, N D'Alessio, P Hartmann, L Forrest, WJ Watson, DM Uchida, KI Sargent, B Green, JD Herter, TL AF Furlan, E Calvet, N D'Alessio, P Hartmann, L Forrest, WJ Watson, DM Uchida, KI Sargent, B Green, JD Herter, TL TI Colors of classical T Tauri stars in Taurus derived from Spitzer infrared spectrograph spectra: Indication of dust settling SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; infrared : stars; planetary systems : protoplanetary disks; stars : pre-main-sequence ID SPACE-TELESCOPE; ENERGY-DISTRIBUTIONS; ACCRETION DISKS; YOUNG OBJECTS; BROWN DWARFS; ARRAY CAMERA; AURIGA; CONSTRAINTS; EVOLUTION; MODELS AB We analyzed Spitzer Infrared Spectrograph data of a representative sample of classical T Tauri stars in the Taurus star-forming region by computing color indices in wave bands that characterize the continuum emission from dust in circumstellar disks. We compared these indices to those derived from a grid of accretion disk models with varying inclination angles, mass accretion rates, and amounts of dust settling. We conclude that most T Tauri stars in our sample have experienced some degree of dust settling and grain growth in their disks, indicating disk evolution. C1 Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Nacl Autonoma Mexico, Ctr Radioastron & Astrofis, Morelia 58089, Michoacan, Mexico. Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. RP Cornell Univ, Ctr Radiophys & Space Res, 208 Space Sci Bldg, Ithaca, NY 14853 USA. EM furlan@astro.cornell.edu; ncalvet@cfa.harvard.edu; p.dalessio@astrosmo.unam.mx; hartmann@cfa.harvard.edu; forrest@pas.rochester.edu; dmw@pas.rochester.edu; kuchida@astro.cornell.edu; bsargent@pas.rochester.edu; joel@pas.rochester.edu; tlh10@cornell.edu OI Furlan, Elise/0000-0001-9800-6248 NR 35 TC 38 Z9 38 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 JUL 20 PY 2005 VL 628 IS 1 BP L65 EP L68 DI 10.1086/432540 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 948MU UT WOS:000230720800017 ER PT J AU Gaudi, BS AF Gaudi, BS TI On the size distribution of close-in extrasolar giant planets SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; planets and satellites : general; stars : individual (HD 209458) ID GRAVITATIONAL LENSING EXPERIMENT; LUMINOSITY OBJECT TRANSITS; GALACTIC DISK; 2001 CAMPAIGN; FOLLOW-UP; STAR; RADIUS; CANDIDATES; EXOPLANET; EVOLUTION AB The precisions of extrasolar planet radius measurements are reaching the point at which meaningful and discriminatory comparisons with theoretical predictions can be made. However, care must be taken to account for selection effects in the transit surveys that detect the transiting planets for which radius measurements are possible. Here I identify one such selection effect, such that the number of planets with radius detected in R-p a signal-to-noise ratio limited transit survey is proportional to R-p(alpha), with alpha similar to 4-6. In the presence of a dispersion sigma in the intrinsic distribution of planet radii, this selection effect translates to bias b in the radii of observed planets. Detected planets are, on average, larger by a fractional amount b similar to alpha(sigma/< R-p>)(2) relative to the mean radius < R-p> of the underlying distribution. I argue that the intrinsic dispersion in planetary radii is likely to be in the range sigma = (0.05 - 0.12)R-J, where the lower bound is that expected theoretically solely from the variance in stellar insolation, and the upper bound is the 95% c.l. upper limit from the scatter in observed radii. Assuming an arbitrary but plausible value of sigma/< R-p> similar to 10%, and thus b similar to 6%, I infer a mean intrinsic radius of close-in massive extrasolar planets of < R-p> = (1.01 +/- 0.03)R-J. This value reinforces the case for HD 209458b having an anomAR alously large radius, and may be inconsistent with coreless models of irradiated giant planets. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Gaudi, BS (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM sgaudi@cfa.harvard.edu RI Gaudi, Bernard/I-7732-2012 NR 31 TC 27 Z9 27 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 JUL 20 PY 2005 VL 628 IS 1 BP L73 EP L76 DI 10.1086/432573 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 948MU UT WOS:000230720800019 ER PT J AU Luhman, KL Stauffer, JR Mamajek, EE AF Luhman, KL Stauffer, JR Mamajek, EE TI The age of AB Doradus SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared : stars; stars : formation; open clusters and associations : individual (IC 2391; Pleiades); stars : low-mass, brown dwarfs; stars : pre-main-sequence ID LOW-MASS STARS; YOUNG OPEN CLUSTERS; ACTIVE-CHROMOSPHERE STARS; F TYPE STARS; ROTATIONAL VELOCITIES; MAIN-SEQUENCE; BROWN DWARFS; EVOLUTIONARY MODELS; SOLAR NEIGHBORHOOD; LITHIUM-DEPLETION AB We have derived a new age estimate for the nearby young star AB Dor and have investigated the resulting implications for testing theoretical evolutionary models with the data reported by Close and coworkers for the low-mass companion AB Dor C. Using color-magnitude diagrams, we find that the AB Dor moving group is roughly coeval with the Pleiades (tau = 100-125 Myr) and is clearly older than IC 2391 (tau = 35-50 Myr). In fact, based on a comparison of the kinematics of AB Dor and the Pleiades, we suggest that the stars identified by Zuckerman and coworkers as members of a moving group with AB Dor are remnants of the large-scale star-formation event that formed the Pleiades. Using the age of tau = 50(-20)(+50) Myr adopted by Close, the luminosity predicted by the models of Chabrier and Baraffe for AB Dor C is larger than the value reported by Close but is still within the quoted uncertainties. Meanwhile, the agreement is good when our age estimate for AB Dor C is adopted. Thus, we find no evidence in the data presented by Close for AB Dor C to suggest that previous studies using the models of Chabrier and Baraffe and bolometric luminosity as the mass indicator have significantly underestimated the masses of young low-mass stars and brown dwarfs. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM kluhman@cfa.harvard.edu; stauffer@ipac.caltech.edu; emamajek@cfa.harvard.edu NR 49 TC 102 Z9 102 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 JUL 20 PY 2005 VL 628 IS 1 BP L69 EP L72 DI 10.1086/432617 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 948MU UT WOS:000230720800018 ER PT J AU Wu, YF Zhu, M Wei, Y Xu, DD Zhang, QZ Fiege, JD AF Wu, YF Zhu, M Wei, Y Xu, DD Zhang, QZ Fiege, JD TI The discovery of a massive scuba core with both inflow and outflow motions SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; ISM : clouds; ISM : kinematics and dynamics; ISM : molecules; stars : formation ID H-II REGIONS; STAR-FORMATION; PROTOSTELLAR CANDIDATES; MOLECULAR CLOUDS; DYNAMICAL COLLAPSE; IRAS SOURCES; HII-REGIONS; DUST; SEARCH; SAMPLE AB We report the discovery of a massive SCUBA core with evidence of inflow and outflow motions. This core is detected by SCUBA at both 450 and 850 mm. Barely resolved by the telescope beam at 450 mm, it has a size of 10", corresponding to 0.28 pc at a distance of 5.7 kpc. The dust temperature is estimated to be <= 29 K, the total mass is 820 M-circle dot, and the average density is cm(-3) in a region with a radius of 5". Follow-up 6 1.1 x 10 spectral line observations, including HCN (3-2), HCO+ (3-2), (HCO+)-C-13 (3-2), and (CO)-O-17 (2-1), reveal a typical blue profile indicating that this core is collapsing. The CO (3-2) line profile is as broad as 38 km s(-1), indicating outflow motions in this region. This core is approximately 1.5 pc away from the known H II region G25.4NW, but there are no obvious radio, IRAS, MSX, or Spitzer sources associated with it. We suggest that this core is at a very early stage of massive star or cluster formation. C1 Peking Univ, PKU, Dept Astron, Joint Beijing Astrophys Ctr,CAS, Beijing 100871, Peoples R China. Natl Res Council Canada, Joint Astron Ctr, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Manitoba, Dept Phys & Astron, Winnipeg, MB R3T 2N2, Canada. RP Wu, YF (reprint author), Peking Univ, PKU, Dept Astron, Joint Beijing Astrophys Ctr,CAS, 5 Haidian Lu, Beijing 100871, Peoples R China. EM yfwu@bac.pku.edu.cn OI Zhang, Qizhou/0000-0003-2384-6589 NR 25 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 JUL 20 PY 2005 VL 628 IS 1 BP L57 EP L60 DI 10.1086/432614 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 948MU UT WOS:000230720800015 ER PT J AU Stein, DL AF Stein, DL TI Descriptions of four new species, redescription of Paraliparis membranaceus, and additional data on species of the fish family Liparidae (Pisces, Scorpaeniformes) from the west coast of South America and the Indian Ocean SO ZOOTAXA LA English DT Article DE Chile; Peru; Southeastern Pacific Ocean; Indian Ocean; deep water; Liparidae; Enantioliparis; Paraliparis; Notoliparis; Careproctus; Psednos; new species ID TELEOSTEI; SLOPE; BLUE AB Liparids are a cottoid family of more than 350 species distributed worldwide in polar, temperate and deep tropical waters. About 20 species ( in six genera) are known from the west coast of South America south of Panama to Tierra del Fuego, and four ( in two genera) from the Indian Ocean. This paper describes an additional four species from existing collections: three from Peruvian and Chilean waters (Paraliparis carlbondi new species, Paraliparis skeliphrus new species, Notoliparis antonbruuni new species), and one from the Indian Ocean (Psednos carolinae new species). Paraliparis membranaceus Gunther is redescribed, a range extension and additional descriptive information is reported for Paraliparis merodontus Stein, additional descriptive information is provided for Careproctus pallidus (Vaillant) and Psednos steini Chernova, the known range of Careproctus longifilis Garman is extended to Peru from the Gulf of Panama, and a species of Psednos similar to Psednos dentatus Chernova and Stein is described, but not named. C1 NOAA, NMFS Systemat Lab, Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Stein, DL (reprint author), NOAA, NMFS Systemat Lab, Smithsonian Inst, Natl Museum Nat Hist, POB 37012, Washington, DC 20013 USA. EM steind@si.edu NR 53 TC 13 Z9 13 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 JUL 19 PY 2005 IS 1019 BP 1 EP 25 PG 25 WC Zoology SC Zoology GA 946RG UT WOS:000230589300001 ER PT J AU Cairns, SD Haussermann, V Forsterra, G AF Cairns, SD Haussermann, V Forsterra, G TI A review of the Scleractinia (Cnidaria : Anthozoa) of Chile, with the description of two new species SO ZOOTAXA LA English DT Review DE Cnidaria; Scleractinia; azooxanthellate corals; Chile; Juan Fernandez; new species ID AZOOXANTHELLATE SCLERACTINIA; CORALS AB All records of the 23 scleractinian species known to occur off Chile are reviewed, including the first records of seven for this coastline. Two species are described as new: Caryophyllia huinayensis and Tethocyathus endesa. Additional specimens of 15 of the 23 species are reported. All Chilean species are azooxanthellate, some occurring as deep as 4195 m; only six species occur at SCUBA depth. Three species are reported for the Juan Fernandez Islands. The Chilean scleractinian fauna is considered to be depauperate, consisting of only 3% of the known azooxanthellate species. C1 Natl Museum Nat Hist, Dept Invertebrate Zool, Smithsonian Inst, Washington, DC 20560 USA. Univ Munich, Dept Biol 2, D-80333 Munich, Germany. Zoolog Staatssammlung, Fdn Huinay, Munich, Germany. RP Cairns, SD (reprint author), Natl Museum Nat Hist, Dept Invertebrate Zool, Smithsonian Inst, POB 37012,W-329, Washington, DC 20560 USA. EM cairns.stephen@nmnh.si.edu; vreni_haeussermann@yahoo.de; gunter_forsterra@yahoo.com NR 53 TC 21 Z9 23 U1 0 U2 2 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD JUL 15 PY 2005 IS 1018 BP 15 EP 46 PG 32 WC Zoology SC Zoology GA 945HB UT WOS:000230492500002 ER PT J AU Riess, AG Li, WD Stetson, PB Filippenko, AV Jha, S Kirshner, RP Challis, PM Garnavich, PM Chornock, R AF Riess, AG Li, WD Stetson, PB Filippenko, AV Jha, S Kirshner, RP Challis, PM Garnavich, PM Chornock, R TI Cepheid calibrations from the Hubble Space Telescope of the luminosity of two recent type Ia supernovae and a redetermination of the hubble constant SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : observations; distance scale; galaxies : distances and redshifts; supernovae : general ID EXTRAGALACTIC DISTANCE SCALE; LARGE-MAGELLANIC-CLOUD; AUTOMATIC IMAGING TELESCOPE; PHOTOMETRIC STANDARD STARS; PROBE WMAP OBSERVATIONS; LIGHT-CURVE SHAPES; PEAK BRIGHTNESS; KEY PROJECT; COSMOLOGICAL PARAMETERS; STELLAR PHOTOMETRY AB We report observations of two nearby Type Ia supernovae (SNe Ia) for which observations of Cepheid variables in the host galaxies have been obtained with the Hubble Space Telescope: SN 1994ae in NGC 3370 and SN 1998aq in NGC 3982. For NCG 3370, we used the Advanced Camera for Surveys to observe 64 Cepheids that yield a distance of 29 Mpc, the farthest direct measurement of Cepheids. We have measured emission lines from H II regions in both host galaxies that provide metallicity-dependent corrections to their period-luminosity relations. These two SNe Ia double the sample of "ideal'' luminosity calibrators: objects with well-observed and well-calibrated light curves of typical shape and with low reddening. By comparing them to all similarly well-measured SNe Ia in the Hubble flow, we find that H-0 = 73 +/- 4 ( statistical) +/- 5 ( systematic) kms(-1) Mpc(-1). A detailed analysis demonstrates that most of the past disagreement over the value of H-0 as determined from SNe Ia is abated by the replacement of past, problematic data by more accurate and precise, modern data. C1 Space Telescope Sci Inst, Baltimore, MD 21218 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. RP Riess, AG (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. EM ariess@stsci.edu; weidong@astro.berkeley.edu; peter.stetson@nrc-cnrc.gc.ca; alex@astro.berkeley.edu; sjha@astro.berkeley.edu; kirshner@cfa.harvard.edu; pgarnavi@miranda.phys.nd.edu; rchornock@astro.berkeley.edu NR 87 TC 122 Z9 123 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 JUL 10 PY 2005 VL 627 IS 2 BP 579 EP 607 DI 10.1086/430497 PN 1 PG 29 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 941CH UT WOS:000230191800001 ER PT J AU Nagamine, K Cen, R Hernquist, L Ostriker, JP Springel, V AF Nagamine, K Cen, R Hernquist, L Ostriker, JP Springel, V TI Massive galaxies and extremely red objects at z=1-3 in cosmological hydrodynamic simulations: Near-infrared properties 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; HUBBLE DEEP FIELD; ULTRAVIOLET LUMINOSITY DENSITY; HIGH-REDSHIFT GALAXIES; STAR-FORMING GALAXIES; DARK-MATTER UNIVERSE; LY-ALPHA EMITTERS; EVOLVED GALAXIES; BLACK-HOLES AB Recent observations have revealed a population of red massive galaxies at high redshift that are challenging to explain in terms of hierarchical galaxy formation models. We analyze this "massive galaxy problem'' with two different types of hydrodynamic simulations - Eulerian total variation diminishing (TVD) and smoothed particle hydrodynamics (SPH) - of a concordance Lambda cold dark matter (Lambda CDM) universe. We consider two separate but connected aspects of the problem posed by these extremely red objects (EROs): ( 1) the mass scale of these galaxies and ( 2) their red colors. We perform spectrophotometric analyses of simulated galaxies in B; z; R; I; J(S); K-S; and K filters and compare their near-infrared (near-IR) properties with observations at redshift z = 1-3. We find that the simulated galaxies brighter than the magnitude limit of K-Vega = 20 mag have stellar masses M-star >= 10(11) h(-1) M-circle dot and a number density of a few times 10(-4) h(3) Mpc(-3) at z similar to 2, in good agreement with the observed number density in the K20 survey. Therefore, our hydrodynamic simulations do not exhibit the mass-scale problem. The answer to the "redness problem'' is less clear because of our poor knowledge of the amount of dust extinction in EROs and the uncertain fraction of star-forming EROs. However, our simulations can account for the observed comoving number density of similar to 1 x 10(-4) Mpc(-3) at z = 1-2 if we assume a uniform extinction of E( B - V) = 0.4 for the entire population of simulated galaxies. Upcoming observations of the thermal emission of dust in 24 mu m by the Spitzer Space Telescope will help to better estimate the dust content of EROs at z = 1-3 and thus to further constrain the star formation history of the universe and theoretical models of galaxy formation. C1 Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA. Princeton Univ Observ, Princeton, NJ 08544 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Max Planck Inst Astrophys, D-85740 Munich, Germany. RP Nagamine, K (reprint author), Univ Calif San Diego, Ctr Astrophys & Space Sci, 9500 Gilman Dr, La Jolla, CA 92093 USA. NR 122 TC 57 Z9 57 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 JUL 10 PY 2005 VL 627 IS 2 BP 608 EP 620 DI 10.1086/430699 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 941CH UT WOS:000230191800002 ER PT J AU Sawicki, M Stevenson, M Barrientos, LF Gladman, B Mallen-Ornelas, G van den Bergh, S AF Sawicki, M Stevenson, M Barrientos, LF Gladman, B Mallen-Ornelas, G van den Bergh, S TI Properties of extremely red objects in an overdense region SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : clusters : general; galaxies : evolution; galaxies : high-redshift; galaxies : statistics; infrared : galaxies ID RADIO-LOUD QUASARS; GALAXY COUNTS; MASSIVE GALAXIES; DENSITY RELATION; FAINT GALAXIES; NUMBER COUNTS; DEEP FIELD; SKY SURVEY; MORPHOLOGY; SIZE AB We use a serendipitously discovered overdensity of extremely red objects (EROs) to study the morphologies and cumulative surface number density of EROs in a dense environment. Our extremely deep imaging allows us to select very faint EROs, reaching K-S = 21, or similar to 2 mag fainter than the L-* of passively evolving ellipticals at z = 1: 5. We find that the shape of the ERO cumulative surface number density in our overdense field mimics that of the field ERO population over all magnitudes down to K-S = 21 but with a factor of 3-4 higher normalization. The excellent seeing in our images (0."4 in K-S and 0."6 in R) allows for morphological classification of the brighter (K-S < 19) EROs, and we find a mix of morphologies including interacting systems and disks; the fraction of pure bulges (at most 38 %), galaxies with disks ( at least 46 %), and interacting systems ( at least 21 %) is consistent with morphological fractions in field ERO studies. The similarity in the shape of the cumulative surface density and morphological mix between our overdense field and the field ERO population suggests that ERO galaxies in overdense regions at z similar to 1-2 may not have had an appreciably different history from those in the field. C1 Natl Res Council Canada, Herzberg Inst Astrophys, Dominion Astrophys Observ, Victoria, BC V9E 2E7, Canada. Univ Victoria, Dept Phys & Astron, Victoria, BC V8W 3P6, Canada. Catholic Univ Chile, Fac Fis, Dept Astron & Astrofis, Santiago, Chile. Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Sawicki, M (reprint author), Natl Res Council Canada, Herzberg Inst Astrophys, Dominion Astrophys Observ, 5071 W Saanich Rd, Victoria, BC V9E 2E7, Canada. NR 41 TC 12 Z9 13 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 JUL 10 PY 2005 VL 627 IS 2 BP 621 EP 631 DI 10.1086/430466 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 941CH UT WOS:000230191800003 ER PT J AU Zezas, A Birkinshaw, M Worrall, DM Peters, A Fabbiano, G AF Zezas, A Birkinshaw, M Worrall, DM Peters, A Fabbiano, G TI Chandra observations of NGC 4261 (3C 270): Revealing the jet and hidden active galactic nucleus in a type 2 liner SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : elliptical and lenticular, cD; galaxies : individual (NGC 4261, 3C 270); galaxies : nuclei; X-rays : galaxies ID HUBBLE-SPACE-TELESCOPE; DWARF SEYFERT NUCLEI; X-RAY-PROPERTIES; EARLY-TYPE GALAXIES; FIELD NORTH SURVEY; I RADIO GALAXIES; NEARBY GALAXIES; ACCRETION DISK; ASCA OBSERVATIONS; BLACK-HOLE AB We present results from a Chandra ACIS-S observation of the type 2 low-ionization nuclear emission-line region ( LINER) radio galaxy NGC 4261 (3C 270). The X-ray data show that this galaxy hosts a heavily obscured (N-H similar to 8 x 10(22) cm(-2)) active galactic nucleus (AGN) with an intrinsic luminosity of 2.4; 10(41) ergs s(-1), which dominates the energy output of the nucleus but is much less than the Eddington luminosity of its central massive black hole. The multiwavelength properties of this component are consistent with either radiatively inefficient accretion flows or emission from the inner part of a jet within 20 mas (3.4 pc) from the nucleus. A softer, unobscured power-law component, which we identify as synchrotron X-ray emission related to the unobscured part of the inner jet, produces similar to 10 % of the 0.1-10.0 keV emission from the nucleus and is likely to be associated with the arcsecond-scale optical/UV emission measured with the Hubble Space Telescope (HST). These results indicate that the energy source of some type 2 LINERs could be a heavily obscured AGN, when obscuration of the ionizing continuum might be responsible for the low ionization state of the line-emitting gas. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Bristol, Dept Phys, Bristol BS8 1TL, Avon, England. Univ Washington, Dept Phys, Seattle, WA 98195 USA. RP Zezas, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Peter, Annika/D-3698-2015; Zezas, Andreas/C-7543-2011; OI Zezas, Andreas/0000-0001-8952-676X; Peter, Annika/0000-0002-8040-6785 NR 81 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 JUL 10 PY 2005 VL 627 IS 2 BP 711 EP 720 DI 10.1086/430044 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 941CH UT WOS:000230191800010 ER PT J AU Greene, JE Ho, LC AF Greene, JE Ho, LC TI A comparison of stellar and gaseous kinematics in the nuclei of active galaxies SO ASTROPHYSICAL JOURNAL LA English DT Review DE galaxies : active; galaxies : kinematics and dynamics; galaxies : nuclei; galaxies : Seyfert ID DIGITAL SKY SURVEY; BLACK-HOLE MASS; NARROW-LINE REGION; TULLY-FISHER RELATION; DWARF SEYFERT NUCLEI; SURVEY PHOTOMETRIC SYSTEM; JET-INDUCED VELOCITIES; BH-SIGMA RELATION; GALACTIC NUCLEI; SPIRAL GALAXIES AB To investigate the relationship between black holes and their host galaxies, many groups have used the width of the [O (III)] lambda 5007 line as a substitute for the stellar velocity dispersion (sigma(*)) of galaxy bulges. We directly test this assumption with a large and homogeneous sample of narrow-line active galactic nuclei from the Sloan Digital Sky Survey. We consider multiple transitions ([O II] lambda 3727, [O III] lambda 5007, and [S II] lambda lambda 6716, 6731) and various techniques for quantifying the line width in order to obtain a calibration between the gas velocity dispersion, sigma(g), and sigma(*). We find that sigma(g) of the low-ionization lines traces sigma(*), as does sigma(g) for the core of [O iii] after its asymmetric blue wing is properly removed, although in all cases the correlation between sigma(g) and sigma(*) has considerable scatter. While the gas kinematics of the narrow- line region of active galaxies are primarily governed by the gravitational potential of the stars, the accretion rate, as traced by the Eddington luminosity ratio, seems to play an important secondary role. Departures from virial motions correlate systematically with accretion rate. We discuss the implications of these results for previous studies that use [O iii] line widths to infer stellar velocity dispersions in quasars and narrow- line Seyfert 1 galaxies. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Carnegie Inst Washington Observ, Pasadena, CA 91101 USA. RP Greene, JE (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 103 TC 151 Z9 152 U1 2 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 JUL 10 PY 2005 VL 627 IS 2 BP 721 EP 732 DI 10.1086/430590 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 941CH UT WOS:000230191800011 ER PT J AU Markevitch, M Govoni, F Brunetti, G Jerius, D AF Markevitch, M Govoni, F Brunetti, G Jerius, D TI Bow shock and radio halo in the merging cluster A520 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : clusters : individual ( A520); intergalactic medium; radio continuum : general; X-rays : galaxies : clusters ID COMA CLUSTER; GALAXY CLUSTERS; NONTHERMAL EMISSION; ACCELERATION; ELECTRONS; ORIGIN; MAPS AB Chandra observations of the merging galaxy cluster A520 reveal a prominent bow shock with M = 2.1(-0.3)(+0.4). This is only the second clear example of a substantially supersonic merger shock front in clusters. Comparison of the X-ray image with that of the previously known radio halo reveals a coincidence of the leading edge of the halo with the bow shock, offering an interesting experimental setup for determining the role of shocks in the radio halo generation. The halo in A520 apparently consists of two spatially distinct parts, the main turbulence-driven component and a cap-like forward structure related to the shock, where the latter may provide preenergized electrons for subsequent turbulent reacceleration. The radio edge may be caused by electron acceleration by the shock. If so, the synchrotron spectrum should have a slope of alpha similar or equal to 1.2 right behind the edge, with quick steepening farther away from the edge. Alternatively, if shocks are inefficient accelerators, the radio edge may be explained by an increase in the magnetic field and density of preexisting relativistic electrons due to gas compression. In the latter model, there should be radio emission in front of the shock with the same spectrum as that behind it, but 10-20 times fainter. If future sensitive radio measurements do not find such preshock emission, then the electrons are indeed accelerated ( or reaccelerated) by the shock, and one will be able to determine its acceleration efficiency. We also propose a method to estimate the magnetic field strength behind the shock, based on measuring the dependence of the radio spectral slope upon the distance from the shock. In addition, the radio edge provides a way to constrain the diffusion speed of the relativistic electrons. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Russian Acad Sci, Space Res Inst, Moscow 117997, Russia. CNR, Ist Radioastron, I-40129 Bologna, Italy. RP Markevitch, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM maxim@head.cfa.harvard.edu OI Govoni, Federica/0000-0003-3644-3084; Brunetti, Gianfranco/0000-0003-4195-8613 NR 35 TC 131 Z9 131 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 JUL 10 PY 2005 VL 627 IS 2 BP 733 EP 738 DI 10.1086/430695 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 941CH UT WOS:000230191800012 ER PT J AU Beuther, H Thorwirth, S Zhang, Q Hunter, TR Megeath, ST Walsh, AJ Menten, KM AF Beuther, H Thorwirth, S Zhang, Q Hunter, TR Megeath, ST Walsh, AJ Menten, KM TI High spatial resolution observations of NH3 and CH3OH toward the massive twin cores NGC 6334I and NGC 6334I(N) SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : individual (NGC6334I, NGC6334I(N)); line : profiles; masers; stars : early-type; stars : formation; techniques : interferometric ID H-II REGIONS; STAR-FORMATION; METHANOL MASERS; MOLECULAR CLOUD; AMMONIA OBSERVATIONS; YOUNG STAR; NGC-6334; EMISSION; OUTFLOWS; I(N) AB Molecular line observations of NH3 ( J, K) = ( 1; 1) and ( 2, 2) and CH3OH at 24.93 GHz taken with the Australian Telescope Compact Array (ATCA) toward the massive twin cores NGC 6334I and NGC 6334I(N) reveal significant variations in the line emission between the two massive cores. The UC H II region/ hot core NGC 6334I exhibits strong thermal NH3 and CH3OH emission adjacent to the UC H II region and coincident with two millimeter continuum peaks observed by T. R. Hunter et al. In contrast, we find neither compact NH3 nor thermal CH3OH line emission toward NGC 6334I( N). There the NH3 emission is distributed over a broad region (> 1') without a clear peak, and we find Class I CH3OH maser emission with peak brightness temperatures up to 7000 K. The maser emission peaks appear to be spatially associated with the interfaces between the molecular outflows and the ambient dense gas. Peak NH3 ( 1, 1) line brightness temperatures >= 70 K in both regions indicate gas temperatures on the same order. NH3 emission is also detected toward the outflow in NGC 6334I, resulting in an estimated rotational temperature of T-rot similar to 19 K. Furthermore, we observe CH3OH and NH3 absorption toward the UC H II region; the velocity structure is consistent with expanding molecular gas around the UC H II region. Thermal and kinematic effects possibly imposed from the UC H II region on the molecular core are also discussed. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ New S Wales, Sch Phys, Sydney, NSW 2052, Australia. Max Planck Inst Radioastron, D-53121 Bonn, Germany. RP Beuther, H (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM hbeuther@cfa.harvard.edu RI Thorwirth, Sven/C-6217-2011; Walsh, Andrew/B-5627-2013 OI Thorwirth, Sven/0000-0001-8200-6710; Walsh, Andrew/0000-0001-9506-0855 NR 43 TC 26 Z9 26 U1 1 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 JUL 10 PY 2005 VL 627 IS 2 BP 834 EP 844 DI 10.1086/430735 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 941CH UT WOS:000230191800020 ER PT J AU Krauss, MI Wang, ZX Dullighan, A Juett, AM Kaplan, DL Chakrabarty, D van Kerkwijk, MH Steeghs, D Jonker, PG Markwardt, CB AF Krauss, MI Wang, ZX Dullighan, A Juett, AM Kaplan, DL Chakrabarty, D van Kerkwijk, MH Steeghs, D Jonker, PG Markwardt, CB TI The X-ray position and optical counterpart of the accretion-powered millisecond pulsar XTE J1814-338 SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : close; pulsars : individual ( XTE J1814-338); stars : neutron; X-rays : binaries ID BINARY; OUTBURST; STARS; DISCOVERY; SPECTROSCOPY; CONSTRAINTS; EVOLUTION; MASS AB We report the precise optical and X-ray localization of the 3.2 ms accretion-powered X- ray pulsar XTE J1814-338 with data from the Chandra X- Ray Observatory as well as optical observations conducted during the 2003 June discovery outburst. Optical imaging of the field during the outburst of this soft X- ray transient reveals an R = 18 star at the X- ray position. This star is absent ( R > 20) from an archival 1989 image of the field and brightened during the 2003 outburst, and we therefore identify it as the optical counterpart of XTE J1814-338. The best source position derived from optical astrometry is R.A. = 18(h)13(m)39(s).04, decl: = -33 degrees 46'22."3 (J2000). The featureless X- ray spectrum of the pulsar in outburst is best fit by an absorbed power law ( with photon index gamma = 1: 41 +/- 0: 06) plus blackbody (with kT = 0: 95 +/- 0: 13 keV) model, where the blackbody component contributes approximately 10% of the source flux. The optical broadband spectrum shows evidence for an excess of infrared emission with respect to an X- ray heated accretion disk model, suggesting a significant contribution from the secondary or from a synchrotron-emitting region. A follow-up observation performed when XTE J1814-338 was in quiescence reveals no counterpart to a limiting magnitude of R = 23:3. This suggests that the secondary is an M3 V or later-type star and therefore very unlikely to be responsible for the soft excess, making synchrotron emission a more reasonable candidate. C1 MIT, Dept Phys, Cambridge, MA 02139 USA. MIT, Ctr Space Res, Cambridge, MA 02139 USA. Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H8, Canada. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Maryland, Dept Astron, College Pk, MD 20742 USA. NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. RP Krauss, MI (reprint author), MIT, Dept Phys, Cambridge, MA 02139 USA. EM miriam@space.mit.edu; wangzx@space.mit.edu; allyn@space.mit.edu; ajuett@space.mit.edu; dlk@space.mit.edu; deepto@space.mit.edu; mhvk@astro.utoronto.ca; dsteeghs@cfa.harvard.edu; p.jonker@sron.nl; craigm@milkyway.gsfc.nasa.gov RI Steeghs, Danny/C-5468-2009 OI Steeghs, Danny/0000-0003-0771-4746 NR 36 TC 25 Z9 25 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 JUL 10 PY 2005 VL 627 IS 2 BP 910 EP 914 DI 10.1086/430595 PN 1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 941CH UT WOS:000230191800028 ER PT J AU Drake, JJ Testa, P Hartmann, L AF Drake, JJ Testa, P Hartmann, L TI X-ray diagnostics of grain depletion in matter accreting onto T Tauri stars SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; stars : formation; stars : individual (BP Tauri, TW Hydrae); X-rays : stars ID PRE-MAIN-SEQUENCE; HYDRAE ASSOCIATION; CORONAL PLASMA; DISK ACCRETION; YOUNG STARS; INNER DISK; IUE ATLAS; BP-TAURI; ABUNDANCES; SOLAR AB Recent analysis of high-resolution Chandra X-ray spectra has shown that the Ne/O abundance ratio is remarkably constant in stellar coronae. Based on this result, we point out the utility of the Ne/O ratio as a discriminant for accretion-related X-rays from T Tauri stars and for probing the measure of grain depletion of the accreting material in the inner disk. We apply the Ne/O diagnostic to the classical T Tauri stars BP Tau and TW Hya - the two stars found to date whose X-ray emission appears to originate, at least in part, from accretion activity. We show that TW Hya appears to be accreting material that is significantly depleted in O relative to Ne. In contrast, BP Tau has an Ne/O abundance ratio consistent with that observed for post - T Tauri stars. We interpret this result in terms of the different ages and evolutionary states of the circumstellar disks of these stars. In the young BP Tau disk ( age similar to 0.6 Myr), dust is still present near the disk corotation radius and can be ionized and accreted, rereleasing elements depleted onto grains. In the more evolved TW Hya disk (age similar to 10 Myr), evidence points to ongoing coagulation of grains into much larger bodies, and possibly planets, that can resist the drag of inward-migrating gas, and the accreting gas is consequently depleted of grain-forming elements. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. RP Drake, JJ (reprint author), Smithsonian Astrophys Observ, MS-3,60 Garden St, Cambridge, MA 02138 USA. EM jdrake@cfa.harvard.edu NR 47 TC 27 Z9 27 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 JUL 10 PY 2005 VL 627 IS 2 BP L149 EP L152 DI 10.1086/432468 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 941CM UT WOS:000230192300017 ER PT J AU McGarry, MB Gaensler, BM Ransom, SM Kaspi, VM Veljkovik, S AF McGarry, MB Gaensler, BM Ransom, SM Kaspi, VM Veljkovik, S TI X-Ray timing, spectroscopy, and photometry of the anomalous X-ray pulsar candidate CXOU J010043.1-721134 SO ASTROPHYSICAL JOURNAL LA English DT Article DE pulsars : general; pulsars : individual ( CXOU J010043.1-721134); stars : neutron ID SMALL-MAGELLANIC-CLOUD; REPEATERS; DISCOVERY; MAGNETARS; EMISSION; BURSTS; FIELD AB We present new X-ray timing and spectral results on the 8.0 s X-ray pulsar CXOU J010043.1-721134 from a series of observations using the Chandra X-Ray Observatory. We found a spin period in 2004 January of 8.020392-0.000009 s. A comparison of this to the 2001 Chandra observations implies a period derivative P = (1.88 +/- 0.08) x 10(-11) s s(-1), leading to an inferred dipole surface magnetic field of 3.9 x 10(14) G. The spectrum is well fit to an absorbed blackbody of temperature kT = 0.38 +/- 0.02 keV with a power-law tail of photon index Gamma = 2.0 +/- 0.6. We find that the source has an unabsorbed X-ray flux (0.5-10 keV) of 4(-1)(+2) x 10(-13) ergs cm(-2) s(-1) and a corresponding X-ray luminosity of similar to 2 x 10(35) ergs s(-1) for a distance of 60 kpc. These properties support the classification of CXOU J010043.1-721134 as the seventh confirmed anomalous X-ray pulsar, the eleventh confirmed magnetar, and the first magnetar to be identified in the Small Magellanic Cloud. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. Harvard Univ, Cambridge, MA 02138 USA. RP McGarry, MB (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Gaensler, Bryan/F-8655-2010; OI Ransom, Scott/0000-0001-5799-9714; Gaensler, Bryan/0000-0002-3382-9558 NR 22 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 JUL 10 PY 2005 VL 627 IS 2 BP L137 EP L140 DI 10.1086/432441 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 941CM UT WOS:000230192300014 ER PT J AU Rusin, D Keeton, CR Winn, JN AF Rusin, D Keeton, CR Winn, JN TI Measuring supermassive black holes in distant galaxies with central lensed images SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; galaxies : nuclei; gravitational lensing ID ACTIVE GALACTIC NUCLEI; STRUCTURAL PARAMETERS; GRAVITATIONAL LENSES; VELOCITY DISPERSION; SEYFERT-GALAXIES; FERMAT PRINCIPLE; MASS PROFILES; QUASARS; EVOLUTION; MODELS AB The supermassive black hole at the center of a distant galaxy can be weighed, in rare but realistic cases, when the galaxy acts as a strong gravitational lens. The central image that should be produced by the lens is either destroyed or accompanied by a second central image, depending on the mass of the black hole. We demonstrate that when a central image pair is detected, the mass of the black hole can be determined with an accuracy of <= 0.1 dex, if the form of the smooth mass distribution near the galaxy core is known. Uncertainty in the central mass distribution introduces a systematic error in the black hole mass measurement. However, even with nearly complete ignorance of the inner mass distribution, the black hole mass can still be determined to within a factor of 10. Central image pairs should be readily observable with future radio interferometers, allowing this technique to be used for a census of supermassive black holes in inactive galaxies at significant redshift (0.2 less than or similar to z less than or similar to 1.0). C1 Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Rusin, D (reprint author), Univ Penn, Dept Phys & Astron, 209 S 33rd St, Philadelphia, PA 19104 USA. NR 37 TC 12 Z9 12 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 JUL 10 PY 2005 VL 627 IS 2 BP L93 EP L96 DI 10.1086/432439 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 941CM UT WOS:000230192300003 ER PT J AU Fabbiano, G AF Fabbiano, G TI The long search for black holes - Response SO SCIENCE LA English DT Letter ID X-RAY OBJECT; OPTICAL COUNTERPART; GALAXIES; X-1 C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Fabbiano, G (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 6, Cambridge, MA 02138 USA. NR 8 TC 0 Z9 0 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 JUL 8 PY 2005 VL 309 IS 5732 BP 245 EP 245 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 944SP UT WOS:000230449800020 ER PT J AU Golombek, MP Arvidson, RE Bell, JF Christensen, PR Crisp, JA Crumpler, LS Ehlmann, BL Fergason, RL Grant, JA Greeley, R Haldemann, AFC Kass, DM Parker, TJ Schofield, JT Squyres, SW Zurek, RW AF Golombek, MP Arvidson, RE Bell, JF Christensen, PR Crisp, JA Crumpler, LS Ehlmann, BL Fergason, RL Grant, JA Greeley, R Haldemann, AFC Kass, DM Parker, TJ Schofield, JT Squyres, SW Zurek, RW TI Assessment of Mars Exploration Rover landing site predictions SO NATURE LA English DT Article ID THERMAL EMISSION SPECTROMETER; GUSEV CRATER; MERIDIANI-PLANUM; SPIRIT ROVER; MICROSCOPIC IMAGER; LOCALIZATION; OPPORTUNITY; SELECTION; DEPOSITS; SURFACE AB Comprehensive analyses of remote sensing data during the three-year effort to select the Mars Exploration Rover landing sites at Gusev crater and at Meridiani Planum correctly predicted the atmospheric density profile during entry and descent and the safe and trafficable surfaces explored by the two rovers. The Gusev crater site was correctly predicted to be a low-relief surface that was less rocky than the Viking landing sites but comparably dusty. A dark, low-albedo, flat plain composed of basaltic sand and haematite with very few rocks was expected and found at Meridiani Planum. These results argue that future efforts to select safe landing sites based on existing and acquired remote sensing data will be successful. In contrast, geological interpretations of the sites based on remote sensing data were less certain and less successful, which emphasizes the inherent ambiguities in understanding surface geology from remotely sensed data and the uncertainty in predicting exactly what materials will be available for study at a landing site. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Washington Univ, St Louis, MO 63130 USA. Cornell Univ, Ithaca, NY 14853 USA. Arizona State Univ, Tempe, AZ 85287 USA. New Mexico Museum Nat Hist & Sci, Albuquerque, NM 87104 USA. Univ Oxford, Oxford OX1 3PG, England. Smithsonian Inst, Washington, DC 20560 USA. RP Golombek, MP (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM mgolombek@jpl.nasa.gov RI Crisp, Joy/H-8287-2016 OI Crisp, Joy/0000-0002-3202-4416 NR 38 TC 55 Z9 58 U1 0 U2 7 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD JUL 7 PY 2005 VL 436 IS 7047 BP 44 EP 48 DI 10.1038/nature03600 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 942QJ UT WOS:000230296600035 PM 16001058 ER PT J AU Haskin, LA Wang, A Jolliff, BL McSween, HY Clark, BC Des Marais, DJ McLennan, SM Tosca, NJ Hurowitz, JA Farmer, JD Yen, A Squyres, SW Arvidson, RE Klingelhofer, G Schroder, C de Souza, PA Ming, DW Gellert, R Zipfel, J Bruckner, J Bell, JF Herkenhoff, K Christensen, PR Ruff, S Blaney, D Gorevan, S Cabrol, NA Crumpler, L Grant, J Soderblom, L AF Haskin, LA Wang, A Jolliff, BL McSween, HY Clark, BC Des Marais, DJ McLennan, SM Tosca, NJ Hurowitz, JA Farmer, JD Yen, A Squyres, SW Arvidson, RE Klingelhofer, G Schroder, C de Souza, PA Ming, DW Gellert, R Zipfel, J Bruckner, J Bell, JF Herkenhoff, K Christensen, PR Ruff, S Blaney, D Gorevan, S Cabrol, NA Crumpler, L Grant, J Soderblom, L TI Water alteration of rocks and soils on Mars at the Spirit rover site in Gusev crater SO NATURE LA English DT Article ID MINERALOGY; SPECTROMETER; CHEMISTRY; DEPOSITS AB Gusev crater was selected as the landing site for the Spirit rover because of the possibility that it once held a lake. Thus one of the rover's tasks was to search for evidence of lake sediments(1). However, the plains at the landing site were found to be covered by a regolith composed of olivine-rich basaltic rock and windblown 'global' dust(2). The analyses of three rock interiors exposed by the rock abrasion tool showed that they are similar to one another, consistent with having originated from a common lava flow(3-8). Here we report the investigation of soils, rock coatings and rock interiors by the Spirit rover from sol (martian day) 1 to sol 156, from its landing site to the base of the Columbia hills. The physical and chemical characteristics of the materials analysed provide evidence for limited but unequivocal interaction between water and the volcanic rocks of the Gusev plains. This evidence includes the softness of rock interiors that contain anomalously high concentrations of sulphur, chlorine and bromine relative to terrestrial basalts and martian meteorites(9); sulphur, chlorine and ferric iron enrichments in multilayer coatings on the light-toned rock Mazatzal; high bromine concentration in filled vugs and veins within the plains basalts; positive correlations between magnesium, sulphur and other salt components in trench soils; and decoupling of sulphur, chlorine and bromine concentrations in trench soils compared to Gusev surface soils, indicating chemical mobility and separation. C1 Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA. Lockheed Martin Space Syst, Littleton, CO 80125 USA. NASA, Exobiol Branch, Ames Res Ctr, Moffett Field, CA 94035 USA. SUNY Stony Brook, Dept Geosci, Stony Brook, NY 11794 USA. Arizona State Univ, Dept Geol Sci, Tempe, AZ 85287 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Cornell Univ, Ithaca, NY 14853 USA. Johannes Gutenberg Univ Mainz, Inst Anorgan & Analyt Chem, D-55128 Mainz, Germany. Co Vale Rio Doce, BR-20030900 Rio De Janeiro, Brazil. NASA, Lyndon B Johnson Space Ctr, MC KR, Houston, TX 77058 USA. Max Planck Inst Chem, Abt Kosmochem, D-55128 Mainz, Germany. US Geol Survey, Flagstaff, AZ 86001 USA. Honeybee Robot, New York, NY 10012 USA. NASA, SETI Inst, Ames Res Ctr, Moffett Field, CA 94035 USA. NASA, Div Space Sci, Ames Res Ctr, Moffett Field, CA 94035 USA. New Mexico Museum Nat Hist & Sci, Albuquerque, NM 87104 USA. Smithsonian Inst, Washington, DC 20024 USA. RP Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. EM alianw@levee.wustl.edu RI Hurowitz, Joel/A-8862-2008; de Souza, Paulo/B-8961-2008; Schroder, Christian/B-3870-2009 OI de Souza, Paulo/0000-0002-0091-8925; Schroder, Christian/0000-0002-7935-6039 NR 27 TC 147 Z9 150 U1 3 U2 25 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 JUL 7 PY 2005 VL 436 IS 7047 BP 66 EP 69 DI 10.1038/nature03640 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 942QJ UT WOS:000230296600040 PM 16001063 ER PT J AU Smith, BD AF Smith, BD TI Reassessing Coxcatlan Cave and the early history of domesticated plants in Mesoamerica SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE archaeology; Mexico; cucurbits; agriculture ID ARCHAEOLOGICAL MAIZE; TEHUACAN; MEXICO; DATES; AGRICULTURE; AMERICA; ORIGIN; L. AB Reanalysis and direct accelerator mass spectrometry radiocarbon dating of the cucurbit assemblage from Coxcatlan Cave provide information on the timing and sequence of the initial appearance of three domesticated plants in the Tehuacan Valley (Puebla, Mexico) and allow reassessment of the overall temporal context of plant domestication in Mexico. Cucurbita pepo is the earliest documented domesticate in the cave, dating to 7,920 calibrated calendrical (cal) years B.P. The bottle gourd (Lagenaria siceraria) is dated at 7,200 cal years B.P. Cucurbita argyrosperma does not appear until 2,065 cal years B.P. The earlier identification of Cucurbita moschata specimens is not confirmed. Seventy-one radiocarbon dates, including 23 accelerator mass spectrometry dates on cucurbits, provide ample evidence of postdepositional vertical displacement of organic materials in the western half of Coxcatlan Cave, but they also indicate that the eastern half of the cave was largely undisturbed. C1 Smithsonian Inst, Archaeobiol Program, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Smith, BD (reprint author), Smithsonian Inst, Archaeobiol Program, Natl Museum Nat Hist, Washington, DC 20560 USA. EM smithb@si.edu NR 32 TC 36 Z9 38 U1 1 U2 13 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 JUL 5 PY 2005 VL 102 IS 27 BP 9438 EP 9445 DI 10.1073/pnas.0502847102 PG 8 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 944DN UT WOS:000230406000003 PM 15908505 ER PT J AU Touwaide, A De Santo, NG Aliotta, G AF Touwaide, A De Santo, NG Aliotta, G TI The origins of western herbal medicines for kidney diseases SO ADVANCES IN CHRONIC KIDNEY DISEASE LA English DT Article DE history of nephrology; herbals for kidney diseases; Hippocrates; Aristotle; Dioscorides AB This article gathers the data on the plants used for the treatment of pathologies of kidneys and the urinary tract from the most ancient medical texts of classical antiquity, the Corpus Hippocraticum, the Aristotelian Problems, and De Materia Medica by Dioscorides. If hippocratic information is scant and practical, aristotelian are of a more theoretical nature and propose an explanation of the action of drugs on the urinary tract. De Materia Medica, coming after a possible research activity in the Alexandrian School, reports the action of many drugs. The work had a deep influence on the subsequent centuries, up to the birth of modern pharmacochemistry. (c) 2005 by the National Kidney Foundation, Inc. C1 Natl Museum Nat Hist, Smithsonian Inst, Dept Bot, Washington, DC 20013 USA. Univ Naples, Dept Nephrol, Naples, Italy. Univ Naples, Dept Life Sci, Naples, Italy. RP Touwaide, A (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Dept Bot, MRC 166,POB 37012, Washington, DC 20013 USA. EM touwaida@si.edu NR 11 TC 6 Z9 6 U1 1 U2 2 PU W B SAUNDERS CO PI PHILADELPHIA PA INDEPENDENCE SQUARE WEST CURTIS CENTER, STE 300, PHILADELPHIA, PA 19106-3399 USA SN 1548-5595 J9 ADV CHRONIC KIDNEY D JI Adv. Chronic Kidney Dis. PD JUL PY 2005 VL 12 IS 3 BP 251 EP 260 DI 10.1053/j.ackd.2005.03.005 PG 10 WC Urology & Nephrology SC Urology & Nephrology GA 946XL UT WOS:000230606500003 PM 16010640 ER PT J AU Schiffer, MB AF Schiffer, MB TI The devil is in the details: The cascade model of invention processes SO AMERICAN ANTIQUITY LA English DT Review ID BEHAVIORAL ARCHAEOLOGY; ARTIFACT VARIABILITY; TECHNOLOGICAL-CHANGE; SOUTHWEST; STRATEGIES; FRAMEWORK; EVOLUTION; DESIGN AB I propose that archaeologists, in pursuing a renewed interest in studying technological change, construct general theories and models of invention processes. As an example, this paper presents the "cascade" model for investigating invention processes in the context of "complex technological systems." Building on the recognition that the vision of a new complex technological system is often obvious, the cascade model asserts that the hard work of invention takes place in a series of invention "cascades," as people strive to achieve acceptable values of a new technology's core or critical performance characteristics during life-history processes (i.e., fashioning a prototype, replication or manufacture, use, and maintenance). The cascade model is illustrated by means of the nineteenth-century electromagnetic telegraph, and implications are drawn for studying invention processes in the complex technological systems of small-scale societies. C1 Univ Arizona, Dept Anthropol, Tucson, AZ 85721 USA. Smithsonian Inst, Natl Museum Amer Hist, Lemelson Ctr, Washington, DC 20560 USA. RP Schiffer, MB (reprint author), Univ Arizona, Dept Anthropol, Tucson, AZ 85721 USA. EM Schiffer@u.arizona.edu NR 102 TC 31 Z9 31 U1 2 U2 9 PU SOC AMER ARCHAEOLOGY PI WASHINGTON PA 900 SECOND ST., NE STE 12, WASHINGTON, DC 20002-3557 USA SN 0002-7316 EI 2325-5064 J9 AM ANTIQUITY JI Am. Antiq. PD JUL PY 2005 VL 70 IS 3 BP 485 EP 502 PG 18 WC Anthropology; Archaeology SC Anthropology; Archaeology GA 952OC UT WOS:000231013300004 ER PT J AU Marriott, B Nicholson, CD Davis, C Manheimer, E AF Marriott, B. Nicholson, C. D. Davis, C. Manheimer, E. TI Plants eaten by rhesus monkeys (Macaca mulatta) in Nepal: Monkey life stage differences and nutrient content SO AMERICAN JOURNAL OF PRIMATOLOGY LA English DT Meeting Abstract C1 RTI Int, RTI, Res Triangle Pk, NC 27709 USA. Univ N Carolina, Chapel Hill, NC USA. Smithsonian Inst, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 1 PU WILEY-LISS PI HOBOKEN PA DIV JOHN WILEY & SONS INC, 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 0275-2565 J9 AM J PRIMATOL JI Am. J. Primatol. PD JUL PY 2005 VL 66 SU 1 MA 65 BP 89 EP 89 PG 1 WC Zoology SC Zoology GA V44GS UT WOS:000202991800066 ER PT J AU Warkentin, KM AF Warkentin, KM TI How do embryos assess risk? Vibrational cues in predator-induced hatching of red-eyed treefrogs SO ANIMAL BEHAVIOUR LA English DT Article ID SUBSOCIAL TREEHOPPER HEMIPTERA; LIFE-HISTORY; DIPODOMYS SPECTABILIS; UMBONIA-CRASSICORNIS; WANDERING SPIDER; SALAMANDER EGGS; KANGAROO RATS; COMMUNICATION; BEHAVIOR; AMPHIBIANS AB I examined the role of vibrations in predator-induced early hatching of red-eyed treefrogs, Agalychnis callidryas. The arboreal eggs of A. callidryas hatch up to 30% early if attacked by egg-eating snakes. This induced hatching is a behavioural response that occurs once snakes begin physically disturbing the clutch, and is sufficiently rapid to allow most embryos to escape. Other intense but benign disturbances, such as tropical storms, do not induce such hatching. I used a miniature accelerometer to record vibrations in egg clutches during snake attacks and rainstorms, and analysed the recordings to identify parameters that distinguished disturbance types. Snake-induced vibrations were on average longer, more widely spaced, and of lower frequency than rain-induced vibrations. I performed three sets of vibration playbacks to examine the hatching response of embryos to different vibration patterns. (1) Playbacks of recorded snake attacks elicited more hatching than did rain recordings. (2) 1 edited snake and rain recordings by moving periods of stillness to clump together rain vibrations and extend intervals, and divide snake vibrations into shorter, more tightly spaced bits. In playbacks, clumped rain elicited more, and divided snake vibrations less hatching than did the original recordings. (3) Bursts of white noise with a constant vibration-to-interval ratio but different cycle durations elicited different levels of hatching. Vibrations alone were sufficient to induce early hatching, without chemical or visual cues from predators. Embryos also clearly distinguished among different vibration patterns and used cues in the gross temporal pattern in making their hatching decision. (c) 2005 The Association for the Study of Animal Behaviour. Published by Elsevier Ltd. All rights reserved. C1 Boston Univ, Dept Biol, Boston, MA 02215 USA. Smithsonian Trop Res Inst, Balboa, Panama. RP Warkentin, KM (reprint author), Boston Univ, Dept Biol, 5 Cummington St, Boston, MA 02215 USA. EM kwarken@bu.edu NR 49 TC 53 Z9 56 U1 2 U2 22 PU ACADEMIC PRESS LTD ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0003-3472 J9 ANIM BEHAV JI Anim. Behav. PD JUL PY 2005 VL 70 BP 59 EP 71 DI 10.1016/j.anbehav.2004.09.019 PN 1 PG 13 WC Behavioral Sciences; Zoology SC Behavioral Sciences; Zoology GA 944QG UT WOS:000230443200007 ER PT J AU Sanson, G Brown, JL Farstad, W AF Sanson, G Brown, JL Farstad, W TI Non-invasive faecal steroid monitoring of ovarian and adrenal activity in farmed blue fox (Alopex lagopus) females during late pregnancy, parturition and lactation onset SO ANIMAL REPRODUCTION SCIENCE LA English DT Article DE fox; faecal steroids; oestrogens; progestagens; corticoids ID VULPES-VULPES; PLASMA PROGESTERONE; PERIPHERAL PLASMA; LUTEAL PHASE; PROLACTIN; CORTISOL; VIXENS; TESTOSTERONE; GESTATION; ESTRUS AB In the semi-domesticated blue fox, handling stress may influence reproductive performance and increase perinatal pup loss. Ovarian and adrenal steroids were analysed in faecal samples collected from mid-gestation through the first week of lactation in 40 female blue foxes to characterize hormone patterns during this important reproductive period. Daily faecal samples were collected from 40 foxes during 30 pregnancies, one late abortion and nine bred-matched non-pregnancies. Mean concentrations of faecal progestagens over the 10 days before birth were significantly higher in pregnant compared to non-pregnant females (51 +/- 1.50 mu g/g versus 36 +/- 3.72 mu g/g, respectively; P < 0.01). From 10 to 3 days before whelping, total faecal oestrogen concentrations also were higher (P < 0.01) in pregnant (1082 +/- 41.69 ng/g) than non-pregnant (628 +/- 72.43 ng/g) foxes, before declining to non-pregnant values (402 +/- 24.88 ng/g) after parturition. Overall mean faecal corticoid concentrations from 3 to 20 days before whelping differed between pregnant and non-pregnant foxes (128 +/- 3.11 ng/g versus 103 +/- 5.86 ng/g, respectively; P < 0.01). Furthermore, in pregnant foxes, corticoid excretion increased further from 2 days before to 3 days after whelping (216 +/- 13.71 ng/g; P < 0.01). Thereafter, corticoid concentrations were similar between pregnant and non-pregnant females (P > 0.05). In sum, the faecal steroid hormone patterns for oestrogens and progestagens were similar to those previously obtained by analyses of fox serum hormones, with both steroids being higher in pregnant than non-pregnant foxes at the end of gestation. The elevation in corticoid concentrations in pregnant females suggests that adrenal activation is involved in the initiation of parturition in the blue fox. Thus, faecal steroid analyses can be used to monitor ovarian activity during pregnancy and pseudopregnancy in farmed blue fox females. (c) 2004 Elsevier B.V. All rights reserved. C1 Norwegian Sch Vet Sci, Dept Prod Anim Clin Sci, NO-0033 Oslo, Norway. Smithsonian Inst, Conservat & Res Ctr, Front Royal, VA 22630 USA. RP Sanson, G (reprint author), Kurveien 38, N-0495 Oslo, Norway. EM gorm.sanson@veths.no NR 35 TC 10 Z9 11 U1 2 U2 10 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0378-4320 J9 ANIM REPROD SCI JI Anim. Reprod. Sci. PD JUL PY 2005 VL 87 IS 3-4 BP 309 EP 319 DI 10.1016/j.anireprosci.2004.12.001 PG 11 WC Agriculture, Dairy & Animal Science; Reproductive Biology SC Agriculture; Reproductive Biology GA 934LY UT WOS:000229711500012 PM 15911180 ER PT J AU Gingerich, O AF Gingerich, O TI Renaissance astrolabes and their makers. SO ANNALS OF SCIENCE LA English DT Book Review 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 1 TC 0 Z9 0 U1 0 U2 0 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 0003-3790 J9 ANN SCI JI Ann. Sci. PD JUL PY 2005 VL 62 IS 3 BP 400 EP 401 PG 2 WC History & Philosophy Of Science SC History & Philosophy of Science GA 946QM UT WOS:000230587200015 ER PT J AU Mathis, WN Zatwarnicki, T AF Mathis, WN Zatwarnicki, T TI Revision of new world species of shore fly genus Discomyza Meigen (Diptera : Ephydridae) SO ANNALS OF THE ENTOMOLOGICAL SOCIETY OF AMERICA LA English DT Article DE Diptera; Ephydridae; Discomyza; shore flies; malacophagy AB Two species of Discomyza Meigen occur in the New World, one, D. u-signata Cresson, naturally and the other, D. maculipennis (Wiedemann),apparently as an introduction. These species are revised and their malacophagous breeding habits are documented. The species treatments include the first detailed descriptions and illustrations of structures from the male terminalia, lectotype designations for Notiphila maculipennis Wiedemann and its New World synonym (D. balioptera Loew), as well as phylogenetic and biogeographic information, including maps. Although congeners, these two species are apparently not closely related, and their occurrence in the New World is independent of each other. D. maculipennis has a biogeographic connection with the Orient, and D. u-signata is linked with a group of Afrotropical species, D. eritrea Cresson specifically. C1 Smithsonian Inst, Dept Entomol, NHB 169, Washington, DC 20013 USA. Univ Opole, Dept Biosystemat, PL-45052 Opole, Poland. RP Mathis, WN (reprint author), Smithsonian Inst, Dept Entomol, NHB 169, POB 37012, Washington, DC 20013 USA. EM mathis.wayne@nmnh.si.edu; zatwar@uni.opole.pl OI Zatwarnicki, Tadeusz/0000-0003-2163-0143 NR 30 TC 5 Z9 6 U1 0 U2 0 PU ENTOMOL SOC AMER PI LANHAM PA 9301 ANNAPOLIS RD, LANHAM, MD 20706 USA SN 0013-8746 J9 ANN ENTOMOL SOC AM JI Ann. Entomol. Soc. Am. PD JUL PY 2005 VL 98 IS 4 BP 431 EP 443 DI 10.1603/0013-8746(2005)098[0431:RONWSO]2.0.CO;2 PG 13 WC Entomology SC Entomology GA 943NC UT WOS:000230359800002 ER PT J AU Bragg, AE Kenyon, SJ AF Bragg, AE Kenyon, SJ TI Structure and mass segregation in H and chi Persei SO ASTRONOMICAL JOURNAL LA English DT Article DE open clusters and associations; individual (NGC 869, NGC 884) ID DOUBLE CLUSTER-H; LARGE-MAGELLANIC-CLOUD; YOUNG OPEN CLUSTERS; RADIAL-VELOCITY MEASUREMENTS; COMPACT STAR-CLUSTERS; STELLAR CLUSTERS; PHOTOMETRY; EXTINCTION; EVOLUTION; TAURUS AB We use V magnitudes and spectral types to examine the density structure of h and chi Per. We describe an automatic method for deriving spectral types and compare classifications for observations made at two different facilities. With these data, we measure an extinction to the clusters of E( B - V) = 0.52 +/- 0.07, consistent with other authors. However, there appears to be a correlation between the spectral types of the stars used and the resulting value of the extinction. We compare extinction values measured by different authors using different numbers of stars and reproduce their values by imposing different cuts in the V magnitude. This variation in color excess versus spectral type suggests that the standard intrinsic colors for the earliest type stars are bluer than the stars in h and chi Per. We measure centers for h and chi Per at alpha( 2000) = 2(h)18(m)56.(s)4 +/- 3.(s)0, delta(2000) = 57 degrees 8'25 '' 23 '' and alpha( 2000) = 2(h)22(m)4.(s) 3 +/- 2.(s)9, delta( 2000) = 57 degrees 8'35 '' +/- 25 '', respectively. We fit the density structure of the clusters and find core radii of 1.9 and 2.4 pc, respectively. Integration of the Miller-Scalo initial mass function suggests overall cluster masses of 5500 and 4300 M-. and central densities of 27 and 50 M-. pc(-3), respectively. We find strong evidence of mass segregation in h Per but not in chi Per. Examination of the dynamical timescales, as well as comparisons between the two clusters, suggest that the mass segregation is partly primordial. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Bragg, AE (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM abragg@cfa.harvard.edu NR 33 TC 20 Z9 20 U1 3 U2 4 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 JUL PY 2005 VL 130 IS 1 BP 134 EP 147 DI 10.1086/430455 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 939PW UT WOS:000230085900012 ER PT J AU Mader, JA Torres, G Marschall, LA Rizvi, A AF Mader, JA Torres, G Marschall, LA Rizvi, A TI Optical photometry and spectroscopy of the suspected "cool Algol" AV Delphini: Determination of the physical properties SO ASTRONOMICAL JOURNAL LA English DT Article DE binaries : eclipsing; binaries : spectroscopic; stars : fundamental parameters; stars : individual (AV Delphini) ID BINARY STAR LIGHT; ECLIPSING BINARIES; AR-MONOCEROTIS; Y-2 ISOCHRONES; CURVES AB We present new spectroscopic and BVRI photometric observations of the double-lined eclipsing binary AV Del ( period = 3.85 days) conducted over six observing seasons. A detailed radial velocity and light-curve analysis of the optical data shows the system to be most likely semidetached, with the less massive and cooler star filling its Roche lobe. The system is probably a member of the rare class of "cool Algol'' systems, which are distinguished from the "classical'' Algol systems in that the mass-gaining component is also a late-type star rather than a B- or A-type star. By combining the spectroscopic and photometric analyses, we derive accurate absolute masses for the components of M-1 = 1.453 +/- 0.028 M-. and M-2 = 0.705 +/- 0.014 M-. and radii of R-1 = 2.632 +/- 0.030 R-. and R-2 = 4.233 +/- 0.060 R-., as well as effective temperatures of 6000 +/- 200 and 4275 +/- 150 K for the primary and secondary, respectively. There are no obvious signs of activity (spottedness) in the optical light curve of the binary. C1 WM Keck Observ, Kamuela, HI 96743 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Gettysburg Coll, Dept Phys, Gettysburg, PA 17325 USA. RP Mader, JA (reprint author), WM Keck Observ, 65-1120 Mamalahoa Highway, Kamuela, HI 96743 USA. EM jmader@keck.hawaii.edu; gtorres@cfa.harvard.edu; marschal@gettysburg.edu NR 42 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 0004-6256 J9 ASTRON J JI Astron. J. PD JUL PY 2005 VL 130 IS 1 BP 234 EP 245 DI 10.1086/430428 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 939PW UT WOS:000230085900021 ER PT J AU Kraus, S Schloerb, FP Traub, WA Carleton, NP Lacasse, M Pearlman, M Monnier, JD Millan-Gabet, R Berger, JP Haguenauer, P Perraut, K Kern, P Malbet, F Labeye, P AF Kraus, S Schloerb, FP Traub, WA Carleton, NP Lacasse, M Pearlman, M Monnier, JD Millan-Gabet, R Berger, JP Haguenauer, P Perraut, K Kern, P Malbet, F Labeye, P TI Infrared imaging of Capella with the IOTA closure phase interferometer SO ASTRONOMICAL JOURNAL LA English DT Article DE binaries : close; binaries : spectroscopic; methods : data analysis; stars : individual (Capella); techniques : interferometric ID SPECTROSCOPIC BINARIES; BEAM-COMBINATION; STARS AB We present infrared aperture synthesis maps produced with the upgraded Infrared Optical Telescope Array interferometer. Michelson interferograms on the close binary system Capella (alpha Aur) were obtained in the H band between 2002 November 12 and 16 using the IONIC3 beam combiner. With baselines of 15 m <= B <= 38 m, we were able to determine the relative position of the binary components with milliarcsecond precision and to track their movement along the approximate to 14 degrees arc covered by our observation run. We briefly describe the algorithms used for visibility and closure phase estimation. Three different hybrid mapping and bispectrum fitting techniques were implemented within one software framework and used to reconstruct the source brightness distribution. By dividing our data into subsets, the system could be mapped at three epochs, revealing the motion of the stars. The precise position of the binary components was also determined with model fits, which in addition revealed I-Aa/I-Ab = 1.49 +/- 0.10 and apparent stellar uniform-disk diameters of Theta(Aa) = 8.9 +/- 0.6 mas and Theta(Ab) = 5.8 +/- 0.8 mas. To improve the (u, v)-plane coverage, we compensated this orbital motion by applying a rotation-compensating coordinate transformation. The resulting model-independent map with a beam size of 5: 4 mas; 2: 6 mas allows the resolution of the stellar surfaces of the Capella giants themselves. C1 Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. Max Planck Inst Radioastron, D-53121 Bonn, Germany. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Michigan, Dept Astron, Ann Arbor, MI 48104 USA. CALTECH, Michelson Sci Ctr, Pasadena, CA 91125 USA. Lab Astrophys Grenoble, F-38041 Grenoble, France. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. CEA, LETI, Dept Microtechnol, F-38054 Grenoble, France. RP Kraus, S (reprint author), Univ Massachusetts, Dept Astron, LGRT-B 619E,710 N Pleasant St, Amherst, MA 01003 USA. EM skraus@mpifr-bonn.mpg.de NR 24 TC 26 Z9 26 U1 0 U2 2 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 JUL PY 2005 VL 130 IS 1 BP 246 EP 255 DI 10.1086/430456 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 939PW UT WOS:000230085900022 ER PT J AU Kenyon, SJ Bromley, BC AF Kenyon, SJ Bromley, BC TI Prospects for detection of catastrophic collisions in debris disks SO ASTRONOMICAL JOURNAL LA English DT Article DE circumstellar matter; planetary systems; solar system : formation; stars : formation ID TERRESTRIAL PLANET FORMATION; LATE HEAVY BOMBARDMENT; KUIPER-BELT OBJECTS; N-BODY SIMULATIONS; INNER SOLAR-SYSTEM; SIZE DISTRIBUTION; LUNAR CATACLYSM; KH 15D; GRAVITATIONAL REACCUMULATION; REFRACTORY INCLUSIONS AB We investigate the prospects for detecting dust from two-body collisions during the late stages of planet formation at 1 - 150 AU. We develop an analytic model to describe the formation of a dusty cloud of debris and use numerical coagulation and N-body calculations to predict observable signals from these events. In a minimum mass solar nebula, collisions of 100 - 1000 km objects at distances of 3 - 5 AU or less from the parent star are observable at mid-IR wavelengths as bright clumps or rings of dust. At 24 mu m, the clumps are similar to 0.1 - 1 mag brighter than emission from dust in the background debris disk. In edge-on systems, dusty clumps produce eclipses with depths of less than or similar to 1.0 mag that last for similar to 100 orbital periods. Large-scale surveys for transits from exosolar planets, using satellites such as Kepler, can plausibly detect these eclipses and provide important constraints on the terrestrial environment for ages of less than or similar to 100 - 300 Myr. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. Univ Utah, Dept Phys, Salt Lake City, UT 84112 USA. RP Kenyon, SJ (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM skenyon@cfa.harvard.edu; bromley@physics.utah.edu OI Kenyon, Scott/0000-0003-0214-609X NR 86 TC 87 Z9 87 U1 1 U2 2 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 JUL PY 2005 VL 130 IS 1 BP 269 EP 279 DI 10.1086/430461 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 939PW UT WOS:000230085900025 ER PT J AU Sadat, R Blanchard, A Vauclair, SC Lumb, DH Bartlett, J Romer, AK Bernard, JP Boer, M Marty, P Nevalainen, J Burke, DJ Collins, CA Nichol, RC AF Sadat, R Blanchard, A Vauclair, SC Lumb, DH Bartlett, J Romer, AK Bernard, JP Boer, M Marty, P Nevalainen, J Burke, DJ Collins, CA Nichol, RC TI The XMM-Newton Omega project - III. Gas mass fraction shape in high redshift clusters SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies : clusters : general; galaxies : intergalactic medium; cosmology : cosmological parameters; dark matter; X-rays : galaxies : clusters ID X-RAY-CLUSTERS; LUMINOSITY-TEMPERATURE RELATION; M-T RELATION; GALAXY CLUSTERS; COSMOLOGICAL IMPLICATIONS; INTRACLUSTER MEDIUM; BARYON CONTENT; EVOLUTION; ROSAT; PROFILES AB We study the gas mass fraction behavior in distant galaxy clusters observed within the XMM-Newton Omega project. The typical gas mass fraction f(gas) shape of high redshift galaxy clusters follows the global shape inferred at low redshift quite well, once scaled appropriately: the gas mass fraction increases with radius and flattens outward. This result is consistent with the simple picture in which clusters essentially form by gravitational collapse, leading to self similar structures for both the dark and baryonic matter. However, we find that the mean gas profile in distant clusters shows some differences to local ones, indicating a departure from strict scaling. Assuming an Einstein-de Sitter cosmology, we find a slight deficit of gas in the central part of high-z clusters. This result is consistent with the observed evolution in the luminosity-temperature relation. We quantitatively investigate this departure from scaling laws by comparing fgas from a sample of nearby galaxy clusters (Vikhlinin et al. 1999) to our eight high-z clusters. Within the local sample, a moderate but clear variation of the amplitude of the gas mass fraction with temperature is found, a trend that weakens in the outer regions. Taking into account these variations with radius and temperature, the apparent scaled gas mass fractions in our distant clusters still systematically differ from local clusters. This reveals that the gas fraction does not strictly follow a scaling law with redshift. This provides clues to understand the redshift evolution of the L-T relation whose origin is probably due to non-gravitational processes during cluster formation. An important implication of our results is that the gas fraction evolution, a test of the cosmological parameters, can lead to biased values when applied at radii smaller than the virial radius. From our XMM clusters, as well as Chandra clusters in the same redshift range, the apparent gas fraction at the virial radius obtained by extrapolation of the inner gas profile is consistent with a non-evolving universal value in a high matter density model while in a concordance model, high redshift clusters show an apparent higher f(gas) at the virial radius than local clusters. C1 UPS, CNRS, UMR 5572, OMP,Lab Astrophys Tarbes & Toulouse, F-31400 Toulouse, France. European Space Agcy, Estec, Adv Concepts & Sci Payloads Off, NL-2200 AG Noordwijk, Netherlands. Coll France, Lab Phys Corpusculaire & Cosmol, F-75231 Paris, France. Univ Sussex, Ctr Astron, Dept Phys & Astron, Brighton BN1 9QH, E Sussex, England. UPS, OMP, Ctr Etud Spatiale Rayonnements, F-31028 Toulouse, France. Observ Haute Provence, F-04870 St Michel, France. Univ Paris 11, Inst Astrophys Spatiale, F-91405 Orsay, France. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England. Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA. RP UPS, CNRS, UMR 5572, OMP,Lab Astrophys Tarbes & Toulouse, 14 Ave E Belin, F-31400 Toulouse, France. EM alain.blanchard@ast.obs-mip.fr NR 41 TC 16 Z9 16 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUL PY 2005 VL 437 IS 1 BP 31 EP 38 DI 10.1051/0004-6361:20041192 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 934XF UT WOS:000229742200009 ER PT J AU Jorgensen, JK Schoier, FL van Dishoeck, EF AF Jorgensen, JK Schoier, FL van Dishoeck, EF TI H2CO and CH3OH abundances in the envelopes around low-mass protostars SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars : formation; ISM : molecules; ISM : abundances; radiative transfer; astrochemistry ID IRAS 16293-2422; STAR-FORMATION; PROTOSTELLAR ENVELOPES; MOLECULAR CLOUDS; HOT CORE; OUTFLOW L1157; IRAS-16293-2422; FORMALDEHYDE; CHEMISTRY; METHANOL AB This paper presents the third in a series of single- dish studies of molecular abundances in the envelopes around a large sample of 18 low- mass pre- and protostellar objects. It focuses on typical grain mantle products and organic molecules, including H2CO, CH3OH and CH3CN. With a few exceptions, all H2CO lines can be fit by constant abundances of 7 x 10(-11)- 8 x 10(-9) throughout the envelopes if ortho- and para lines are considered independently. The current observational dataset does not require a large H2CO abundance enhancement in the inner warm regions, but this can also not be ruled out. Through comparison of the H2CO abundances of the entire sample, the H2CO ortho- para ratio is constrained to be 1.6 +/- 0.3 consistent with thermalization on grains at temperatures of 10- 15 K. The H2CO abundances can be related to the empirical chemical network established on the basis of our previously reported survey of other species and is found to be closely correlated with that of the nitrogen- bearing molecules. These correlations reflect the freeze- out of molecules at low temperatures and high densities, with the constant H2CO abundance being a measure of the size of the freeze- out zone. An improved fit to the data is obtained with a " drop" abundance structure in which the abundance is typically a few x 10(-10) when the temperature is lower than the evaporation temperature and the density high enough so that the timescale for depletion is less than the lifetime of the core. The location of the freeze- out zone is constrained from CO observations. Outside the freeze- out zone, the H2CO abundance is typically a few x 10(-9)- 10(-8). The observations show that the CH3OH lines are significantly broader than the H2CO lines, indicating that they probe kinematically distinct regions. CH3OH is moreover only detected toward a handful of sources and CH3CN toward only one, NGC 1333- IRAS2. For NGC 1333- IRAS2, CH3OH and CH3CN abundance enhancements of two- three orders of magnitude at temperatures higher than 90 K are derived. In contrast, the NGC 1333- IRAS4A and IRAS4B CH3OH data are fitted with a constant abundance and an abundance enhancement at a lower temperature of 30 K, respectively. This is consistent with a scenario where CH3OH probes the action of compact outflows on the envelopes, which is further supported by comparison to high frequency, high excitation CS J = 10- 9 and HDO line profiles which uniquely probe warm, dense gas. The extent to which the outflow dominates the abundance enhancements compared with the passively heated inner envelope depends on the filling factors of the two components in the observing beam. C1 Leiden Observ, NL-2300 RA Leiden, Netherlands. Stockholm Observ, AlbaNova, S-10691 Stockholm, Sweden. RP Jorgensen, JK (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St MS42, Cambridge, MA 02138 USA. EM jjorgensen@cfa.harvard.edu RI Jorgensen, Jes Kristian/L-7936-2014 OI Jorgensen, Jes Kristian/0000-0001-9133-8047 NR 35 TC 54 Z9 54 U1 0 U2 2 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 JUL PY 2005 VL 437 IS 2 BP 501 EP U17 DI 10.1051/0004-6361:20042060 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 938CV UT WOS:000229978400014 ER PT J AU Malbet, F Lachaume, R Berger, JP Colavita, MM Di Folco, E Eisner, JA Lane, BF Millan-Gabet, R Segransan, D Traub, WA AF Malbet, F Lachaume, R Berger, JP Colavita, MM Di Folco, E Eisner, JA Lane, BF Millan-Gabet, R Segransan, D Traub, WA TI New insights on the AU-scale circumstellar structure of FU Orionis SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars : pre-main-sequence; stars : individual : FU Ori; planetary systems : protoplanetary disks; infrared : stars; accretion, accretion disks; techniques : interferometric ID HERBIG AE/BE STARS; T-TAURI STARS; INFRARED INTERFEROMETRIC OBSERVATIONS; PALOMAR TESTBED INTERFEROMETER; COMMISSIONING INSTRUMENT; OPTICAL INTERFEROMETRY; STELLAR EVOLUTION; DISKS; OUTBURSTS; OBJECTS AB We report new near-infrared, long-baseline interferometric observations at the AU scale of the pre-main-sequence star FU Orionis with the PTI, IOTA and VLTI interferometers. This young stellar object has been observed on 42 nights over a period of 6 years from 1998 to 2003. We have obtained 287 independent measurements of the fringe visibility with 6 different baselines ranging from 20 to 110 m in length, in the H and K bands. Our data resolves FU Ori at the AU scale, and provides new constraints at shorter baselines and shorter wavelengths. Our extensive (u, v)- plane coverage, coupled with the published spectral energy distribution data, allows us to test the accretion disk scenario. We find that the most probable explanation for these observations is that FU Ori hosts an active accretion disk whose temperature law is consistent with standard models and with an accretion rate of. M = (6.3 +/- 0.6) x 10(-5) (M-* M-circle dot)(-1) M-circle dot yr(-1). We are able to constrain the geometry of the disk, including an inclination of 55(-7)(+5) deg and a position angle of 47(-11)(+7) deg. In addition, a 10 percent peak-to-peak oscillation is detected in the data ( at the two-sigma level) from the longest baselines, which we interpret as a possible disk hot-spot or companion. The still somewhat limited ( u, v) sampling and substantial measurement uncertainty prevent us from constraining the location of the spot with confidence, since many solutions yield a statistically acceptable fit. However, the oscillation in our best data set is best explained with an unresolved spot located at a projected distance of 10 +/- 1 AU at the 130 +/- 1 deg position angle and with a magnitude difference of Delta K approximate to 3.9 +/- 0.2 and Delta H approximate to 3.6 +/- 0.2 mag moving away from the center at a rate of 1.2 +/- 0.6 AU yr(-1). Although this bright spot on the surface of the disk could be tracing some thermal instabilities in the disk, we propose to interpret this spot as the signature of a companion of the central FU Ori system on an extremely eccentric orbit. We speculate that the close encounter of this putative companion and the central star could be the explanation of the initial photometric rise of the luminosity of this object. C1 UJF, Lab Astrophys Grenoble, CNRS, UMR 5571, F-38041 Grenoble, France. Max Planck Inst Radioastron, D-53121 Bonn, Germany. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. European So Observ, D-85748 Garching, Germany. CALTECH, Dept Astron, Pasadena, CA 91125 USA. MIT, Ctr Space Res, Cambridge, MA 02139 USA. CALTECH, Michelson Sci Ctr, Pasadena, CA 91125 USA. Observ Geneva, CH-1290 Sauverny, Switzerland. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Malbet, F (reprint author), UJF, Lab Astrophys Grenoble, CNRS, UMR 5571, BP 53, F-38041 Grenoble, France. EM Malbet@obs.ujf-grenoble.fr NR 51 TC 52 Z9 52 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 JUL PY 2005 VL 437 IS 2 BP 627 EP 636 DI 10.1051/0004-6361:20042556 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 938CV UT WOS:000229978400025 ER PT J AU Grappin, R Leorat, J Habbal, SR AF Grappin, R Leorat, J Habbal, SR TI Siphon flows and oscillations in long coronal loops due to Alfven waves SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE sun : corona; methods : numerical; magnetohydrodynamics (MHD) ID FINITE-DIFFERENCE SCHEMES; SOLAR CORONA; SIMULATIONS; STEADY AB Using an isothermal axisymmetric MHD model of the solar corona with transparent boundary conditions, we study how coronal loops with apex height between one third and two solar radii react to Alfven waves generated at the base of the corona. The first response is a steady increase of the density along the excited loops. Density oscillations are also observed, along the apex of the longest loops, that is, those along which waves are substantially damped. Both the steady and the oscillating component scale as the square of the Alfven wave amplitude, and accordingly, the frequency is double that of the mother wave. Siphon flows may also appear, along short or long loops, depending on whether both or a single foot-point of the loop system is excited. C1 Observ Paris, F-92195 Meudon, France. Univ Wales, Aberystwyth SY23 3BZ, Dyfed, Wales. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Grappin, R (reprint author), Observ Paris, 1 Pl J Janssen, F-92195 Meudon, France. EM roland.grappin@obspm.fr; jacques.leorat@obspm.fr; sdh@aber.ac.uk NR 17 TC 4 Z9 4 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 JUL PY 2005 VL 437 IS 3 BP 1081 EP 1092 DI 10.1051/0004-6361:20052745 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 941JC UT WOS:000230210100034 ER PT J AU Friedman, AS Bloom, JS AF Friedman, AS Bloom, JS TI Toward a more standardized candle using gamma-ray burst energetics and spectra SO ASTROPHYSICAL JOURNAL LA English DT Review DE cosmological parameters; cosmology : observations; gamma rays : bursts ID HUBBLE-SPACE-TELESCOPE; WIND-INTERACTION-MODELS; AFTERGLOW LIGHT CURVES; BROAD-BAND AFTERGLOW; HIGH COLUMN DENSITY; RICH GRB 981226; HOST GALAXY; OPTICAL AFTERGLOW; IA SUPERNOVAE; ENERGY RESERVOIR AB The use of gamma-ray burst (GRB) energetics for cosmography has long been advanced as a means to probe out to high redshifts, to the epoch of deceleration. However, although relatively immune to systematic biases from dust extinction, the prompt energy release in GRBs, even when corrected for jetting geometry, is far from being a standard candle. In this work we explore the cosmographic potential of a GRB standard candle based on the newly discovered relation by Ghirlanda and coworkers between the apparent geometry-corrected energies ( E(gamma)) and the peak in the rest-frame prompt-burst spectrum (E(p)). We present an explicit, self-consistent formalism for correcting GRB energies with a thorough accounting for observational uncertainties. In contrast to other work, we demonstrate that the current sample of 19 GRBs is not yet cosmographically competitive with results from Type Ia supernovae ( SNe Ia), large-scale structure, and the microwave background. Although the E(p)-E(gamma) relation is a highly significant correlation across a range of cosmologies [ 0 <= Omega(M), Omega(Lambda <=) 2], the goodness of fit of the data to a power law ( E(p) proportional to E(gamma)(eta)) depends strongly on input assumptions. The most important of these assumptions concern the unknown density ( and density profile) of the circumburst medium, the efficiency of converting explosion energy to gamma rays, data selection choices for individual bursts ( some of which were not included in similar work), and assumptions in the error analysis. Independent of assumptions, with very few low-z bursts, the current sample is most sensitive to Omega(M) but essentially insensitive to Omega(Lambda) ( let alone the dark energy equation of state w). The relation clearly represents a significant improvement in the search for an empirical GRB standard candle but is further hindered by an unknown physical basis for the relation, the lack of a low-z training set to calibrate the relation in a cosmology-independent way, and several major potential systematic uncertainties and selection effects. Until these concerns are addressed, a larger sample is acquired, and attempts are made to marginalize or perform Monte Carlo simulations over the unknown density distribution ( which itself may evolve with redshift), we urge caution concerning claims of the utility of GRBs for cosmography and especially attempts to combine the results from GRBs with those of SNe Ia. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Harvard Soc Fellows, Cambridge, MA 02138 USA. RP Friedman, AS (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM afriedman@cfa.harvard.edu; jbloom@cfa.harvard.edu RI Friedman, Andrew/I-4691-2013 OI Friedman, Andrew/0000-0003-1334-039X NR 199 TC 120 Z9 123 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 1 PY 2005 VL 627 IS 1 BP 1 EP 25 DI 10.1086/430292 PN 1 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 939PZ UT WOS:000230086200001 ER PT J AU Gibson, RR Marshall, HL Canizares, CR Lee, JC AF Gibson, RR Marshall, HL Canizares, CR Lee, JC TI The high-resolution X-ray spectrum of MR 2251-178 obtained with the Chandra HETGS SO ASTROPHYSICAL JOURNAL LA English DT Article DE quasars : emission lines; quasars : individual (MR 2251-178); X-rays : individual (MR 2251-178) ID ACTIVE GALACTIC NUCLEI; HUBBLE-SPACE-TELESCOPE; VELOCITY IONIZED OUTFLOW; DUSTY WARM ABSORBER; XMM-NEWTON; ABSORPTION-LINES; ULTRAVIOLET-ABSORPTION; GAS; MR-2251-178; EMISSION AB The QSO MR 2251-178 was observed with the Chandra High Energy Transmission Grating Spectrometer (HETGS) at a 2-10 keV luminosity of 2.41 x 10(44) ergs s(-1) ( using H-0 = 72 km s(-1) Mpc(-1)). We observe the source in a relatively low state. The light curve shows no evidence of variability. We present the zero-order image of MR 2251-178 and compare it to previous observations. We find evidence of a highly ionized, high-velocity outflow, which we detect in a resolved Fe XXVI Ly alpha absorption line. The outflow appears to have a large mass and kinetic energy flux compared to the estimated nuclear accretion rate and luminosity. We examine the possibility that other absorption features in the spectrum are associated with the high-velocity outflow. We detect a narrow Fe K alpha line and resolved forbidden line emission from Ne IX and O VII. Modeling the emitting material enables us to constrain its properties and conclude that it is not along our line of sight. C1 MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Gibson, RR (reprint author), MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA. EM rgibson@mit.edu; hermanm@space.mit.edu; crc@space.mit.edu; jclee@cfa.harvard.edu RI Lee, Julia/G-2381-2015 OI Lee, Julia/0000-0002-7336-3588 NR 56 TC 21 Z9 21 U1 1 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 JUL 1 PY 2005 VL 627 IS 1 BP 83 EP 96 DI 10.1086/430199 PN 1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 939PZ UT WOS:000230086200007 ER PT J AU Rigby, JR Rieke, GH Perez-Gonzalez, PG Donley, JL Alonso-Herrero, A Huang, JS Barmby, P Fazio, GG AF Rigby, JR Rieke, GH Perez-Gonzalez, PG Donley, JL Alonso-Herrero, A Huang, JS Barmby, P Fazio, GG TI Why optically faint AGNs are optically faint: The Spitzer perspective SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; infrared : galaxies; X-rays : galaxies ID DEEP FIELD-SOUTH; X-RAY SOURCES; MULTIBAND IMAGING PHOTOMETER; ENERGY-DISTRIBUTIONS; HELLAS2XMM SURVEY; SPACE-TELESCOPE; RADIO-SOURCES; NORTH SURVEY; LUMINOSITY; CATALOG AB Optically faint X-ray sources ( those with f(X)/f(R) > 10) constitute about 20% of X-ray sources in deep surveys and are potentially highly obscured and/or at high redshift. Their faint optical fluxes are generally beyond the reach of spectroscopy. For a sample of 20 optically faint sources in CDFS, we compile 0.4-24 mu m photometry, relying heavily on the Spitzer Space Telescope. We estimate photometric redshifts for 17 of these 20 sources. We find that these AGNs are optically faint, both because they lie at significantly higher redshifts (median z similar to 1.6) than most X-ray-selectedAGNs, and because their spectra are much redder than standard AGNs. They have 2-8 keV X-ray luminosities in the Seyfert range, unlike the QSO luminosities of optically faint AGNs found in shallow wide-field surveys. Their contribution to the X-ray Seyfert luminosity function is comparable to that of z > 1 optically bright AGNs. C1 Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. CSIC, Inst Estructura Mat, E-28006 Madrid, Spain. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Rigby, JR (reprint author), Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA. EM jrigby@as.arizona.edu; grieke@as.arizona.edu; pgperez@as.arizona.edu; jdonley@as.arizona.edu; aalonso@damir.iem.csic.es; jhuang@cfa.harvard.edu; pbarmby@cfa.harvard.edu; gfazio@cfa.harvard.edu RI Rigby, Jane/D-4588-2012; Barmby, Pauline/I-7194-2016; Perez-Gonzalez, Pablo/J-2871-2016; Alonso-Herrero, Almudena/H-1426-2015 OI Rigby, Jane/0000-0002-7627-6551; Barmby, Pauline/0000-0003-2767-0090; Perez-Gonzalez, Pablo/0000-0003-4528-5639; Alonso-Herrero, Almudena/0000-0001-6794-2519 NR 36 TC 17 Z9 17 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 JUL 1 PY 2005 VL 627 IS 1 BP 134 EP 139 DI 10.1086/430398 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 939PZ UT WOS:000230086200010 ER PT J AU Wake, DA Collins, CA Nichol, RC Jones, LR Burke, DJ AF Wake, DA Collins, CA Nichol, RC Jones, LR Burke, DJ TI The environmental dependence of galaxy colors in intermediate-redshift X-ray-selected clusters SO ASTROPHYSICAL JOURNAL LA English DT Review DE galaxies : clusters : general; galaxies : elliptical and lenticular, cD; galaxies : evolution; galaxies : fundamental parameters ID DIGITAL SKY SURVEY; ABSOLUTE MAGNITUDE RELATION; BUTCHER-OEMLER CLUSTERS; HUBBLE-SPACE-TELESCOPE; STAR-FORMATION RATE; DISTANT CLUSTERS; S0 GALAXIES; DISK GALAXIES; RICH CLUSTERS; PRECISION PHOTOMETRY AB We present a wide-field imaging study of the colors of bright galaxies (< M* + 2) in a sample of 12 X-ray-selected clusters and groups of galaxies at z similar to 0.3. The systems cover one of the largest ranges in X-ray luminosity ( L-X similar to 10(43)-10(45) ergs s(-1)), and hence mass, of any sample studied at this redshift. We find that the "red'' galaxies form a tight color-magnitude relation (CMR) and that neither the slope nor zero point of this relation changes significantly over the factor of 100 in X-ray luminosity covered by our sample. Using stellar population synthesis models, we find that our data allow a maximum possible change of 2 Gyr in the typical age of the "red'' galaxies on the CMR over the range of L-X of our sample. We also measure the fraction of blue galaxies (f(b)) relative to the CMR in our clusters and find a low value of f(b)similar to 0.1 consistent with other X-ray-selected cluster samples. We find that there is no correlation between fb and L-X over our large L-X range. However, we do find that both the CMR and fb depend significantly on cluster radius, with the zero point of the CMR shifting blueward in B-R by 0.10 +/- 0.036 mag out to a radius of 0.75 times the virial radius. This color change is equivalent to a luminosity-weighted age gradient of similar to 2.5 Gyr per log (radius) and is consistent with previous studies of the radial change in the zero point of the CMR. It thus appears that the global cluster environment, in the form of cluster mass (L-X), has little influence on the properties of the bright cluster galaxies, whereas the local environment, in the form of galaxy density ( radius), has a strong effect. The range of similar to 100 in L-X corresponds to a factor of similar to 40 in ram pressure efficiency, thus suggesting that ram pressure stripping or other mechanisms that depend on cluster mass, like tidal stripping or harassment, are unlikely to be solely responsible for changing the galaxy population from the "blue'' star-forming galaxies, which dominate low-density environments, to the "red'' passive galaxies, which dominate cluster cores. C1 Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 2EG, Hants, England. Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England. Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15217 USA. Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Wake, DA (reprint author), Univ Portsmouth, Inst Cosmol & Gravitat, Mercantile House,Hampshire Terrace, Portsmouth PO1 2EG, Hants, England. EM david.wake@port.ac.uk OI Burke, Douglas/0000-0003-4428-7835 NR 104 TC 42 Z9 42 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 JUL 1 PY 2005 VL 627 IS 1 BP 186 EP 202 DI 10.1086/430117 PN 1 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 939PZ UT WOS:000230086200015 ER PT J AU Gotthelf, EV Halpern, JP Seward, FD AF Gotthelf, EV Halpern, JP Seward, FD TI Discovery of a 105 ms X-ray pulsar in Kesteven 79: On the nature of compact central objects in supernova remnants SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : individual (Kesteven 79); pulsars : individual (CXOU J185238.6+004020, PSR J1852+0040); stars : neutron; supernova remnants ID ISOLATED NEUTRON-STAR; RADIATION PAIR FRONTS; RADIO PULSARS; XMM-NEWTON; SPIN-DOWN; EMISSION; SURFACE; 1E-1207.4-5209; LUMINOSITY; PSR-B1706-44 AB We report the discovery of 105 ms X-ray pulsations from the compact central object (CCO) in the supernova remnant Kes 79 using data acquired with the Newton X-Ray Multi-Mirror Mission (XMM-Newton). Two observations of the pulsar taken 6 days apart yield an upper limit on its spin-down rate of. P < 7 x 10(-14) s s(-1) and no evidence for binary orbital motion. The implied energy loss rate is. E < 2 x 10(36) ergs s(-1), the surface magnetic field strength is B-p < 3 x 10(12) G, and the spin-down age is tau > 24 kyr. The latter exceeds the remnant's estimated age, suggesting that the pulsar was born spinning near its current period. The X-ray spectrum of PSR J1852+ 0040 is best characterized by a blackbody model of temperature kT(BB) = 0: 44 +/- 0: 03 keV, radius R-BB approximate to 0.9 km, and L-bol = 3.7 x 10(33) ergs s(-1) at d = 7.1 kpc. The sinusoidal light curve is modulated with a pulsed fraction of > 45%, suggestive of a small hot spot on the surface of the rotating neutron star. The lack of a discernible pulsar wind nebula is consistent with an interpretation of PSR J1852+ 0040 as a rotation-powered pulsar whose spin- down luminosity falls below the empirical threshold for generating bright wind nebulae,. E-c approximate to 4 x 10(36) ergs s(-1). The age discrepancy implies that its. E has always been below. E-c, perhaps a distinguishing property of the CCOs. Alternatively, the X-ray spectrum of PSR J1852+ 0040 suggests a low-luminosity anomalous X-ray pulsar (AXP), but the weak inferred Bp field is incompatible with a magnetar theory of its X-ray luminosity. We cannot exclude accretion from a fallback disk. The ordinary spin parameters discovered from PSR J1852+ 0040 highlight the difficulty that existing theories of isolated neutron stars have in explaining the high luminosities and temperatures of CCO thermal X-ray spectra. C1 Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Gotthelf, EV (reprint author), Columbia Univ, Columbia Astrophys Lab, 550 W 120th St, New York, NY 10027 USA. EM eric@astro.columbia.edu; jules@astro.columbia.edu; fds@head.cfa.harvard.edu NR 46 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 JUL 1 PY 2005 VL 627 IS 1 BP 390 EP 396 DI 10.1086/430300 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 939PZ UT WOS:000230086200031 ER PT J AU Zane, S Cropper, M Turolla, R Zampieri, L Chieregato, M Drake, JJ Treves, A AF Zane, S Cropper, M Turolla, R Zampieri, L Chieregato, M Drake, JJ Treves, A TI XMM-Newton detection of pulsations and a spectral feature in the X-ray emission of the isolated neutron star 1RXS J214303.7+065419/RBS 1774 SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars : individual (1RXS J214303.7+065419, RBS 1774); stars : neutron; X-rays : stars ID RX J0720.4-3125; MAGNETIC-FIELD; PROPER MOTION; TIMING ANALYSIS; PULSAR; RX-J0720.4-3125; ATMOSPHERES; RX-J1856.5-3754; DISCOVERY; VARIABILITY AB We report on the results of a deep XMM-Newton observation of RBS 1774, the most recent dim isolated neutron star candidate found in the ROSAT archive data. Spectral and timing analysis of the high-quality pn and MOS data confirm the association of this source with an isolated neutron star. The spectrum is thermal and blackbody-like, and there is evidence at a significance level > 4 sigma that the source is an X-ray pulsar with a spin period of 9.437 s. Spectral fitting reveals the presence of an absorption feature at similar to 0.7 keV, but at this level data do not have enough resolution to allow us to discriminate between an absorption line or an edge. We compare the newly measured properties of RBS 1774 with those of other known dim isolated neutron stars and discuss possible interpretations for the absorption feature. C1 UCL, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. Univ Padua, Dept Phys, I-35131 Padua, Italy. Osserv Astron Padova, INAF, I-35122 Padua, Italy. Univ Insubria, Dept Math & Phys, I-22100 Como, Italy. Univ Zurich, Inst Theoret Phys, CH-8057 Zurich, Switzerland. Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Zane, S (reprint author), UCL, Mullard Space Sci Lab, Holmbury St Mary, Dorking RH5 6NT, Surrey, England. EM sz@mssl.ucl.ac.uk; turolla@pd.infn.it; zampieri@pd.astro.it; matteo.chieregato@pd.infn.it; jdrake@head-cfa.harvard.edu; treves@mib.infn.it RI Cropper, Mark/C-1574-2008; OI Zampieri, Luca/0000-0002-6516-1329 NR 46 TC 47 Z9 48 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 1 PY 2005 VL 627 IS 1 BP 397 EP 403 DI 10.1086/430138 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 939PZ UT WOS:000230086200032 ER PT J AU Boden, AF Torres, G Hummel, CA AF Boden, AF Torres, G Hummel, CA TI Testing stellar models with an improved physical orbit for 12 Bootis SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : spectroscopic; binaries : visual; stars : evolution; stars : individual (12 Bootis) ID PALOMAR TESTBED INTERFEROMETER; SOLAR-TYPE STARS; PROTOTYPE OPTICAL INTERFEROMETER; INTERMEDIATE-MASS STARS; FLUX METHOD IRFM; VISUAL ORBIT; EVOLUTIONARY TRACKS; ANGULAR DIAMETERS; Y-2 ISOCHRONES; EVOLVED STARS AB In a previous paper we reported on the binary system 12 Bootis and its evolutionary state. In particular, the 12 Boo primary component is in a rapid phase of evolution; hence accurate measurement of its physical parameters makes it an interesting test case for stellar evolution models. Here we report on a significantly improved determination of the physical orbit of the double-lined spectroscopic binary system 12 Boo. We have a 12 Boo interferometry data set spanning 6 yr with the Palomar Testbed Interferometer, a smaller amount of data from the Navy Prototype Optical Interferometer, and a radial velocity data set spanning 14 yr from the Harvard-Smithsonian Center for Astrophysics. We have updated the 12 Boo physical orbit model with our expanded interferometric and radial velocity data sets. The revised orbit is in good agreement with previous results, and the physical parameters implied by a combined fit to our visibility and radial velocity data result in precise component masses and luminosities. In particular, the orbital parallax of the system is determined to be 27: 72 +/- 0: 15 mas, and masses of the two components are determined to be 1.4160 +/- 0.0049 and 1.3740 +/- 0.0045 M circle dot, respectively. These mass determinations are more precise than those in the previous report by a factor of 4 - 5. As indicated in the previous publication, even though the two components are nearly equal in mass, the system exhibits a significant brightness difference between the components in the near-infrared and visible. We attribute this brightness difference to evolutionary differences between the two components in their transition between main-sequence and giant evolutionary phases, and based on theoretical models, we can estimate a system age of approximately 3.2 Gyr. Comparisons with stellar models suggest that the 12 Boo primary may be just entering the Hertzsprung gap, but that conclusion is highly dependent on details of the models. Such a dynamic evolutionary state makes the 12 Boo system a unique and important test for stellar models. C1 CALTECH, Michelson Sci Ctr, Pasadena, CA 91125 USA. Georgia State Univ, Dept Phys & Astron, Atlanta, GA 30303 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. European So Observ, Santiago 19, Chile. RP Boden, AF (reprint author), CALTECH, Michelson Sci Ctr, 770 S Wilson Ave, Pasadena, CA 91125 USA. EM bode@ipac.caltech.edu NR 51 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 JUL 1 PY 2005 VL 627 IS 1 BP 464 EP 476 DI 10.1086/430058 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 939PZ UT WOS:000230086200039 ER PT J AU Bergin, EA Melnick, GJ Gerakines, PA Neufeld, DA Whittet, DCB AF Bergin, EA Melnick, GJ Gerakines, PA Neufeld, DA Whittet, DCB TI Spitzer observations of CO2 ice toward field stars in the taurus molecular cloud SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrobiology; astrochemistry; ISM : lines and bands; ISM : molecules ID ATOMIC OXYGEN ABUNDANCE; SOLID CARBON-DIOXIDE; INFRARED SPECTROGRAPH; SPACE-TELESCOPE; DARK CLOUDS; HL-TAURI; SPECTROSCOPY; ABSORPTION; CHEMISTRY; GAS AB We present the first Spitzer Infrared Spectrograph observations of the 15.2 mu m bending mode of CO2 ice toward field stars behind a quiescent dark cloud. CO 2 ice is detected toward two field stars ( Elias 16 and Elias 3) and a single protostar (HL Tau) with an abundance of similar to 15% -20% relative to water ice. CO2 ice is not detected toward the source with lowest extinction in our sample, Tamura 17 ( A(v) = 3.9 mag). A comparison of the Elias 16 spectrum with laboratory data demonstrates that the majority of CO2 ice is embedded in a polar, H2O-rich ice component, with similar to 15% of CO2 residing in an apolar, H2O-poor mantle. This is the first detection of apolar CO2 toward a field star. We find that the CO2 extinction threshold is Av = 4 +/- 1 mag, comparable to the threshold for water ice, but significantly less than the threshold for CO ice, the likely precursor of CO2. Our results confirm that CO2 ice forms in tandem with H2O ice along quiescent lines of sight. This argues for CO2 ice formation by means of a mechanism similar to that responsible for H2O ice formation, viz., simple catalytic reactions on grain surfaces. C1 Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Alabama, Dept Phys, Astro & Solar Syst Phys Program, Birmingham, AL 35294 USA. Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. Rensselaer Polytech Inst, New York Ctr Studies Origins Life, Troy, NY 12180 USA. Univ Michigan, Dept Phys Appl Phys & Astron, Ann Arbor, MI 48109 USA. RP Bergin, EA (reprint author), Univ Michigan, Dept Astron, 825 Dennison Bldg,500 Church St, Ann Arbor, MI 48109 USA. EM ebergin@umich.edu RI Gerakines, Perry/B-9705-2009; Gerakines, Perry/D-2226-2012; OI Gerakines, Perry/0000-0002-9667-5904; Whittet, Douglas/0000-0001-8539-3891 NR 38 TC 59 Z9 59 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 JUL 1 PY 2005 VL 627 IS 1 BP L33 EP L36 DI 10.1086/431932 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 939QC UT WOS:000230086500009 ER PT J AU Bronson, CL Grubb, TC Sattler, GD Braun, MJ AF Bronson, CL Grubb, TC Sattler, GD Braun, MJ TI Reproductive success across the black-capped Chickadee (Poecile atricapillus) and Carolina Chickadee (P-Carolinensis) hybrid zone in Ohio SO AUK LA English DT Article DE black-capped Chickadee; Carolina Chickadee; genetic indices; hybrid zone; Poecile atricapillus; Poecile carolinensis; reproductive success ID PARUS-ATRICAPILLUS; SEX-CHROMOSOMES; CONTACT ZONE; HUMAN DNA; SPECIATION; EVOLUTIONARY; PATTERNS; MALES; RULE AB Black-capped Chickadees (Poecile atricapillus) and Carolina Chickadees (P. carolinensis) hybridize in an east-west band from New Jersey to Kansas. Within the past century, the Ohio portion of this hybrid zone and the Carolina Chickadee range to the south have been moving northward, whereas the Black-capped Chickadee range has retracted. In Ohio, we characterized the genetic composition of the hybrid zone using five diagnostic molecular loci. Although there was no evidence of assortative mating in the center of the hybrid zone, we found a relative paucity of genetically intermediate breeding females as compared with breeding males. That suggests viability selection against female hybrids, in line with Haldane's rule. On the basis of reproductive variables (number of nestlings, reproductive success), we found a decrease in productivity of breeding pairs in the hybrid zone that is significantly and positively related to their probability of producing homozygous offspring at each autosomal or sex-linked locus. We also found that the decrease in productivity was significantly and positively related to the genetic composition of the male of the pair (i.e. pure male chickadees more productive). These data strongly suggest that hybrids are at a selective disadvantage. Because the zone of reduced reproductive success was considerably narrower than the zone of introgression, our results demonstrate that genetic introgression is occurring in the face of substantial selection against hybrids. C1 Ohio State Univ, Div Immunol, Dept Internal Med, Dept Ecol Evolut & Organismal Biol, Columbus, OH 43210 USA. Liberty Univ, Dept Biol & Chem, Lynchburg, VA 24502 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Suitland, MD 20746 USA. RP Bronson, CL (reprint author), Ohio State Univ, Div Immunol, Dept Internal Med, Dept Ecol Evolut & Organismal Biol, 473 W 12th Ave, Columbus, OH 43210 USA. EM bronson.5@osu.edu NR 55 TC 22 Z9 23 U1 0 U2 16 PU AMER ORNITHOLOGISTS UNION PI LAWRENCE PA ORNITHOLOGICAL SOC NORTH AMER PO BOX 1897, LAWRENCE, KS 66044-8897 USA SN 0004-8038 J9 AUK JI AUK PD JUL PY 2005 VL 122 IS 3 BP 759 EP 772 DI 10.1642/0004-8038(2005)122[0759:RSATBC]2.0.CO;2 PG 14 WC Ornithology SC Zoology GA 952EG UT WOS:000230984600003 ER PT J AU Dechmann, DKN Kalko, EKV Konig, B Kerth, G AF Dechmann, DKN Kalko, EKV Konig, B Kerth, G TI Mating system of a Neotropical roost-making bat: the white-throated, round-eared bat, Lophostoma silvicolum (Chiroptera : Phyllostomidae) SO BEHAVIORAL ECOLOGY AND SOCIOBIOLOGY LA English DT Article DE reproductive cycle; reproductive success; resource-defense polygyny; Lophostoma silvicolum; post-partum estrus ID CYNOPTERUS SPHINX CHIROPTERA; ARTIBEUS-JAMAICENSIS CHIROPTERA; INDIAN FRUIT BAT; SOCIAL-ORGANIZATION; PATERNITY INFERENCE; TONATIA-SILVICOLA; HAREM MAINTENANCE; SEXUAL-DIMORPHISM; PTEROPODIDAE; ECOLOGY AB The vast majority of bats strongly depend on, but do not make, shelters or roosts. We investigated Lophostoma silvicolum, which roosts in active termite nests excavated by the bats themselves, to study the relationship between roost choice and mating systems. Due to the hardness of the termite nests, roost-making is probably costly in terms of time and energy for these bats. Video-observations and capture data showed that single males excavate nests. Only males in good physical condition attracted females to the resulting roosts. Almost all groups captured from excavated nests were single male-multifemale associations, suggesting a harem structure. Paternity assignments based on ten polymorphic microsatellites, revealed a high reproductive success of 46% by nest-holding males. We suggest that the mating system of L. silvicolum is based on a resource-defense polygyny. The temperatures in the excavated nests are warm and stable, and might provide a suitable shelter for reproductive females. Reproductive success achieved by harem males appears to justify the time and effort required to excavate the nests. Reproductive success may thus have selected on an external male phenotype, the excavated nests, and have contributed to the evolution of an otherwise rare behavior in bats. C1 Univ Zurich, Inst Zool, CH-8057 Zurich, Switzerland. Univ Ulm, D-89069 Ulm, Germany. Smithsonian Trop Res Inst, Balboa, Panama. RP Dechmann, DKN (reprint author), Univ Zurich, Inst Zool, Winterthurerstr 190, CH-8057 Zurich, Switzerland. EM dechmann@zool.unizh.ch RI Dechmann, Dina/A-1827-2010 NR 59 TC 29 Z9 31 U1 0 U2 10 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013 USA SN 0340-5443 J9 BEHAV ECOL SOCIOBIOL JI Behav. Ecol. Sociobiol. PD JUL PY 2005 VL 58 IS 3 BP 316 EP 325 DI 10.1007/s00265-005-0913-y PG 10 WC Behavioral Sciences; Ecology; Zoology SC Behavioral Sciences; Environmental Sciences & Ecology; Zoology GA 933FS UT WOS:000229614900012 ER PT J AU Torchin, ME Hechinger, RF Huspeni, TC Whitney, KL Lafferty, KD AF Torchin, ME Hechinger, RF Huspeni, TC Whitney, KL Lafferty, KD TI The introduced ribbed mussel (Geukensia demissa) in Estero de Punta Banda, Mexico: interactions with the native cord grass, Spartina foliosa SO BIOLOGICAL INVASIONS LA English DT Article DE Baja California; biomass; bivalve; clapper rail; Estero de Punta Banda; Geukensia demissa; introduced species; Mexico ID ENGLAND SALT-MARSH; SOUTHERN CALIFORNIA; SHORE LEVEL; RECRUITMENT; DILLWYN AB Introduced populations of Guekensia demissa occur on the west coast of North America. They have been reported in San Francisco Bay, four southern California wetlands, and in Estero de Punta Banda (EPB), Baja California Norte, Mexico. We randomly sampled benthic invertebrates in four habitat types within EPB: marsh, channel, mudflat and pan. Geukensia demissa was the most abundant bivalve in the wetland at EPB. It was significantly associated with the native cordgrass, Spartina foliosa, and occurred at higher average densities in vegetated marsh sites (24/m(2)) and Spartina-dominated tidal channels (35/m(2)), compared to mudflat (0/m(2)), and pan (0/m(2)) sites. We estimated that the total biomass of this invader was over four times that of the next most abundant bivalve, Tagelus spp., in EPB. We examined G. demissa for parasites and found that only a few native parasites colonized this introduced host at very low prevalences and intensities. We performed bird surveys to determine the habitat overlap and potential impact of this mussel on the EPB population of light-footed clapper rails (Rallus longirostrus levipes), an endangered species in the United States. The high abundance of G. demissa in EPB, its presence in clapper rail habitat, and its known effects on salt marsh habitat in it's native range, warrant further investigations of the impact of this invader in EPB and elsewhere. C1 Univ Calif Santa Barbara, Inst Marine Sci, Santa Barbara, CA 93106 USA. Univ Calif Santa Barbara, Dept Ecol Evolut & Marine Biol, Santa Barbara, CA 93106 USA. US Geol Survey, Western Ecol Res Ctr, Santa Barbara, CA 93106 USA. RP Torchin, ME (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Ancon, Panama. EM torchinm@si.edu RI Lafferty, Kevin/B-3888-2009; Hechinger, Ryan/F-6754-2010 OI Lafferty, Kevin/0000-0001-7583-4593; NR 26 TC 3 Z9 4 U1 2 U2 14 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 1387-3547 J9 BIOL INVASIONS JI Biol. Invasions PD JUL PY 2005 VL 7 IS 4 BP 607 EP 614 DI 10.1007/s10530-004-5851-5 PG 8 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 963KZ UT WOS:000231804500006 ER PT J AU Warren, BH Bermingham, E Prys-Jones, RP Thebaud, C AF Warren, BH Bermingham, E Prys-Jones, RP Thebaud, C TI Tracking island colonization history and phenotypic shifts in Indian Ocean bulbuls (Hypsipetes : Pycnonotidae) SO BIOLOGICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Article DE convergent evolution; homoplasy; Madagascar; molecular clock; parallel evolution; phylogeography ID BODY-SIZE; EVOLUTION; DNA; LIZARDS; DIVERSIFICATION; SUBSTITUTION; CONVERGENCE; EXPLANATION; DIVERGENCE; PASSERINE AB Molecular phylogenies of island organisms provide useful systems for testing hypotheses of convergent or parallel evolution, since selectively neutral molecular characters are likely to be independent of phenotype, and the existence of similar environments on multiple isolated islands provides numerous opportunities for populations to evolve independently under the same constraints. Here we construct a phylogenetic hypothesis for Hypsipetes bulbuls of the western Indian Ocean, and use this to test hypotheses of colonization pattern and phenotypic change among islands of the region. Mitochondrial sequence data were collected from all extant taxa of the region, combined with sequence data from relevant lineages in Asia. Data are consistent with a single Hypsipetes colonization of the western Indian Ocean from Asia within the last 2.6 Myr. The expansion of Hypsipetes appears to have occurred rapidly, with descendants found across the breadth of its western Indian Ocean range. The data suggest that a more recent expansion of Hypsipetes madagascariensis from Madagascar led to the colonization of Aldabra and a secondary colonization of the Comoros. Groupings of western Indian Ocean Hypsipetes according to phenotypic similarities do not correspond to mtDNA lineages, suggesting that these similarities have evolved by convergence or parallelism. The direction of phenotypic change cannot be inferred with confidence, since the primary expansion occurred rapidly relative to the rate of mtDNA substitution, and the colonization sequence remains uncertain. However, evidence from biogeography and comparison of independent colonization events are consistent with the persistence of a small grey continental bulbul in India and Madagascar, and multiple independent origins of large size and green plumage in insular island populations of the Comoros, Mascarenes and Seychelles. (c) 2005 The Linnean Society of London. C1 Univ E Anglia, Sch Biol Sci, Norwich NR4 7TJ, Norfolk, England. Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. Nat Hist Museum, Dept Zool, Bird Grp, Tring HP23 6AP, Herts, England. Univ Toulouse 3, UMR 5174 CNRS, Lab Evolut & Diversite Biol, F-31062 Toulouse, France. RP Warren, BH (reprint author), Univ Reading, Sch Plant Sci, Reading RG6 6AS, Berks, England. EM b.warren@reading.ac.uk RI Thebaud, Christophe/N-3916-2016 OI Thebaud, Christophe/0000-0002-8586-1234 NR 48 TC 40 Z9 41 U1 1 U2 10 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0024-4066 J9 BIOL J LINN SOC JI Biol. J. Linnean Soc. PD JUL PY 2005 VL 85 IS 3 BP 271 EP 287 DI 10.1111/j.1095-8312.2005.00492.x PG 17 WC Evolutionary Biology SC Evolutionary Biology GA 945YJ UT WOS:000230538600002 ER PT J AU Loew, SS Williams, DF Ralls, K Pilgrim, K Fleischer, RC AF Loew, SS Williams, DF Ralls, K Pilgrim, K Fleischer, RC TI Population structure and genetic variation in the endangered Giant Kangaroo Rat (Dipodomys ingens) SO CONSERVATION GENETICS LA English DT Article DE Dipodomys ingens; endangered species; gene flow; genetic variation; microsatellite primers; population fragmentation ID MICROSATELLITE DATA; SUBDIVISION; DIVERSITY; DIFFERENTIATION; CONSEQUENCES; EXTINCTION; DISPERSAL; LOCI; RECOLONIZATION; CONSERVATION AB Populations of the endangered giant kangaroo rat, Dipodomys ingens (Heteromyidae), have suffered increasing fragmentation and isolation over the recent past, and the distribution of this unique rodent has become restricted to 3% of its historical range. Such changes in population structure can significantly affect effective population size and dispersal, and ultimately increase the risk of extinction for endangered species. To assess the fine-scale population structure, gene flow, and genetic diversity of remnant populations of Dipodomys ingens, we examined variation at six microsatellite DNA loci in 95 animals from six populations. Genetic subdivision was significant for both the northern and southern part of the kangaroo rat's range although there was considerable gene flow among southern populations. While regional gene diversity was relatively high for this endangered species, hierarchical F-statistics of northern populations in Fresno and San Benito counties suggested non-random mating and genetic drift within subpopulations. We conclude that effective dispersal, and therefore genetic distances between populations, is better predicted by ecological conditions and topography of the environment than linear geographic distance between populations. Our results are consistent with and complimentary to previous findings based on mtDNA variation of giant kangaroo rats. We suggest that management plans for this endangered rodent focus on protection of suitable habitat, maintenance of connectivity, and enhancement of effective dispersal between populations either through suitable dispersal corridors or translocations. C1 Illinois State Univ, Dept Biol Sci, Behav Ecol Evolut & Systemat Sect, Normal, IL 61790 USA. Calif State Univ Stanislaus, Endangered Species Recovery Program, Turlock, CA 95382 USA. Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, Washington, DC 20008 USA. Smithsonian Inst, Natl Museum Nat Hist, Genet Program, Washington, DC 20008 USA. Rocky Mt Res Stn, Carnivore Conservat Genet Lab, Missoula, MT 59807 USA. RP Loew, SS (reprint author), Illinois State Univ, Dept Biol Sci, Behav Ecol Evolut & Systemat Sect, 210 Julian Hall, Normal, IL 61790 USA. EM ssloew@ilstu.edu NR 64 TC 13 Z9 13 U1 1 U2 31 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 1566-0621 J9 CONSERV GENET JI Conserv. Genet. PD JUL PY 2005 VL 6 IS 4 BP 495 EP 510 DI 10.1007/s10592-005-9005-9 PG 16 WC Biodiversity Conservation; Genetics & Heredity SC Biodiversity & Conservation; Genetics & Heredity GA 000FH UT WOS:000234445800002 ER PT J AU Mora, C Robertson, DR AF Mora, C Robertson, DR TI Causes of latitudinal gradients in species richness: A test with fishes of the Tropical Eastern Pacific SO ECOLOGY LA English DT Article DE diversity; energy/habitat/stability effects; fishes; geographic range; mid-domain effect; Rapoport's rule; spatial scale ID CLIMATE-CHANGE; RAPOPORTS RULE; CORAL-REEFS; RANGE-SIZE; EL-NINO; PATTERNS; DIVERSITY; BIODIVERSITY; SCALE; OCEAN AB Recent advances in analytical methods and exploration of regional diversity patterns in greater depth than simple whole-fauna patterns may change our understanding of the determinants of latitudinal gradients in species richness. Using a comprehensive database on the geographical distributions of the large fauna of endemic shorefishes from the Tropical Eastern Pacific (TEP), we delineated latitudinal diversity gradients (LDGs) of species with different range sizes and assessed how the mid-domain effect, energy supply, environmental variability, and habitat availability predicted the various LDGs. We used statistical methods that account for spatial autocorrelation within each variable and consider collinearity among them. We found marked variation in LDGs among species with different range sizes: species with large ranges contributed the most to the convex form of the entire-fauna LDG while species with small ranges generated most deviations from that form. The mid-domain effect was the strongest determinant for the entire-fauna LDG, largely due to the strength of its effect on widespread species. Habitat variables were the best predictors for LDGs of small-range species but had no significant effects on the entire-fauna pattern. We found that any relationship between energy supply and LDGs likely is spurious and arises from statistical effects of (1) the marked spatial autocorrelation of the residuals in those relationships and (2) strong covariation between energy supply and the mid-domain effect, two factors that have never been analyzed together in marine studies (and seldom in terrestrial studies). There was no indication that environmental stability was an important LDG determinant at any level within the fauna. We found that latitudinal (Rapoport) trends in range size in this fauna arise as corollaries of the mid-domain effect. The disparate contributions of species with different range sizes to diversity patterns demonstrate the failure of traditional, whole-fauna LDGs to adequately represent all faunal components and their determinants, particularly those of small-range (and more threatened) species. We argue that, just as analyses of whole-fauna patterns within a region obscure variation in determinants among faunal components, analyses of patterns at transoceanic (multiregional) scales are likely to conceal important regional variation in determinants of diversity gradients. 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 59 TC 64 Z9 68 U1 2 U2 28 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 JUL PY 2005 VL 86 IS 7 BP 1771 EP 1782 DI 10.1890/04-0883 PG 12 WC Ecology SC Environmental Sciences & Ecology GA 941YH UT WOS:000230249600014 ER PT J AU Helmuth, L AF Helmuth, L TI Ageing research in the media - How the demands of newspaper and magazine publishing influence what people read about ageing SO EMBO REPORTS LA English DT Editorial Material ID SCIENTIFIC COMMUNITY C1 Smithsonian Magazine, Washington, DC 20001 USA. RP Helmuth, L (reprint author), Smithsonian Magazine, Washington, DC 20001 USA. EM helmuth@nasw.org NR 8 TC 0 Z9 0 U1 0 U2 2 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 1469-221X J9 EMBO REP JI EMBO Rep. PD JUL PY 2005 VL 6 SI SI BP S81 EP S83 DI 10.1038/sj.embor.7400434 PG 3 WC Biochemistry & Molecular Biology; Cell Biology SC Biochemistry & Molecular Biology; Cell Biology GA 953NI UT WOS:000231082800018 PM 15995670 ER PT J AU Leimgruber, P Christen, CA Laborderie, A AF Leimgruber, P Christen, CA Laborderie, A TI The impact of Landsat satellite monitoring on conservation biology SO ENVIRONMENTAL MONITORING AND ASSESSMENT LA English DT Article DE conservation biology; Earth resource monitoring; global change; Landsat; Landsat history; satellite monitoring ID HABITAT FRAGMENTATION; DEFORESTATION; BIODIVERSITY; EVOLUTION; FORESTS/; PROGRAM; SCIENCE; FUTURE; FIRE AB Landsat 7's recent malfunctioning will result in significant gaps in long-term satellite monitoring of Earth, affecting not only the research of the Earth science community but also conservation users of these data. To determine whether or how important Landsat monitoring is for conservation and natural resource management, we reviewed the Landsat program's history with special emphasis on the development of user groups. We also conducted a bibliographic search to determine the extent to which conservation research has been based on Landsat data. Conservation biologists were not an early user group of Landsat data because a) biologists lacked technical capacity - computers and software - to analyze these data; b) Landsat's 1980s commercialization rendered images too costly for biologists' budgets; and c) the broad-scale disciplines of conservation biology and landscape ecology did not develop until the mid-to-late 1980s. All these conditions had changed by the 1990s and Landsat imagery became an important tool for conservation biology. Satellite monitoring and Landsat continuity are mandated by the Land Remote Sensing Act of 1992. This legislation leaves open commercial options. However, past experiments with commercial operations were neither viable nor economical, and severely reduced the quality of monitoring, archiving and data access for academia and the public. Future satellite monitoring programs are essential for conservation and natural resource management, must provide continuity with Landsat, and should be government operated. C1 Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, Front Royal, VA 22630 USA. Univ Kent, Durrell Inst Conservat & Ecol, Canterbury CT2 7NZ, Kent, England. RP Christen, CA (reprint author), Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, 1500 Remount Rd, Front Royal, VA 22630 USA. EM christenc@si.edu RI Leimgruber, Peter/O-1304-2015 OI Leimgruber, Peter/0000-0002-3682-0153 NR 49 TC 29 Z9 30 U1 3 U2 23 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0167-6369 J9 ENVIRON MONIT ASSESS JI Environ. Monit. Assess. PD JUL PY 2005 VL 106 IS 1-3 BP 81 EP 101 DI 10.1007/s10661-005-0763-0 PG 21 WC Environmental Sciences SC Environmental Sciences & Ecology GA 939RV UT WOS:000230091000006 PM 16001713 ER PT J AU Grenier, JL Greenberg, R AF Grenier, JL Greenberg, R TI A biogeographic pattern in sparrow bill morphology: Parallel adaptation to tidal marshes SO EVOLUTION LA English DT Article DE bill morphology; biogeographic rule; convergence; ecological speciation; Emberizidae; tidal marsh; trophic adaptation ID MITOCHONDRIAL-DNA VARIATION; NATURAL-SELECTION; SONG SPARROWS; SWAMP SPARROW; EVOLUTION; BIRDS; POPULATION; FINCHES; DIFFERENTIATION; DIVERGENCE AB The study of ecological convergence, the evolution of similar traits on multiple occasions in response to similar conditions, is a powerful method for developing and testing adaptive hypotheses. However, despite the great attention paid to geographic variation and the foraging ecology of birds, surprisingly few cases of convergent or parallel feeding adaptations have been adequately documented. In this study, we document a biogeographic pattern of parallel bill morphology across 10 sparrow taxa endemic to tidal marshes. All North American tidal marsh sparrows display parallel differentiation from close relatives in other habitats, suggesting that selection on bill morphology is strong. Relative to their body mass, tidal marsh sparrows have longer, thinner bills than their non-tidal marsh counterparts, which is likely an adaptation for consuming more invertebrates and fewer seeds, as well as for probing in sediment crevices to capture prey. Published data on tidal marsh food resources and diet of the relevant taxa support this hypothesis. This morphological differentiation is most pronounced between sister taxa with the greatest estimated divergence times, but is found even in taxa that show little or no structure in molecular genetic markers. We, therefore, speculate that tidal marsh ecosystems are likely settings for ecological speciation. C1 Univ Calif Berkeley, Dept Environm Sci Policy & Management, Berkeley, CA 94720 USA. Natl Zool Pk, Smithsonian Migratory Bird Ctr, Washington, DC 20008 USA. RP Grenier, JL (reprint author), San Francisco Estuary Inst, 7770 Pardee Lane, Oakland, CA 94621 USA. EM letitia@sfei.org; antbird@erols.com NR 70 TC 24 Z9 25 U1 3 U2 17 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0014-3820 EI 1558-5646 J9 EVOLUTION JI Evolution PD JUL PY 2005 VL 59 IS 7 BP 1588 EP 1595 PG 8 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 952BE UT WOS:000230975600020 PM 16153044 ER PT J AU Vick, T AF Vick, T TI Duk and cover (Korean cinema, Kim Kuk) SO FILM COMMENT LA English DT Letter C1 Smithsonian Inst, Washington, DC 20560 USA. RP Vick, T (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU FILM SOC LINCOLN CENTER PI NEW YORK PA 70 LINCOLN CENTER PLAZA, NEW YORK, NY 10023-6595 USA SN 0015-119X J9 FILM COMMENT JI Film Comment PD JUL-AUG PY 2005 VL 41 IS 4 BP 11 EP 11 PG 1 WC Film, Radio, Television SC Film, Radio & Television GA 943OE UT WOS:000230362700004 ER PT J AU Mulhern, DM AF Mulhern, DM TI A probable case of Gigantism in a fifth dynasty skeleton from the western cemetery at Giza, Egypt SO INTERNATIONAL JOURNAL OF OSTEOARCHAEOLOGY LA English DT Article DE gigantism; acromegaly; pituitary; Giza; Egypt; skeletal ID CAPITAL FEMORAL EPIPHYSIS; PITUITARY GIGANTISM; MANIFESTATIONS; HYPOGONADISM; ENDOCRINE; STATURE; BONES; DEATH AB Pituitary gigantism is a rare endocrine disorder caused by excess secretion of growth hormone during childhood. Individuals with this condition exhibit unusually tall stature due to prolonged growth as well as associated degenerative changes. Continued secretion of excess growth hormone during adulthood results in acromegaly, a related condition that results in bony overgrowth of the skull, hands and feet. The remains of a large adult male, probably in his late 20s or early 30s, from a Fifth Dynasty tomb (2494-2345 BC) were excavated in 2001 from Cemetery 2500 in the Western Cemetery at Giza, Egypt, as part of the Howard University Giza Cemetery Project, This individual exhibits characteristics of pituitary gigantism, including tall but normally-proportioned stature, delayed epiphyseal union, a large sella turcica, advanced arthritis and a transepiphyseal fracture of the left femoral head. Additional pathological features, including osteopenia and thinness of the parietal bones, suggest that this individual may also have been hypogonadal. Craniometric comparisons with other ancient Egyptian groups as well as modern normal and acromegalic patients show some tendency toward acromegalic skull morphology. Differential diagnosis includes eunuchoid gigantism, Sotos syndrome, Beckwith-Wiedemann syndrome, Marfan syndrome, homocystinuria, Weaver syndrome and Klinefelter syndrome. In conclusion, the pathological features associated with this skeleton are more consistent with pituitary gigantism than any of the other syndromes that result in skeletal overgrowth. Copyright (c) 2004 John Wiley & Sons, Ltd. C1 Smithsonian Inst, Dept Anthropol, NMNH, MRC 138, Washington, DC 20013 USA. RP Mulhern, DM (reprint author), Smithsonian Inst, Dept Anthropol, NMNH, MRC 138, POB 37012, Washington, DC 20013 USA. EM mulhern.dawn@nmnh.si.edu NR 44 TC 6 Z9 6 U1 1 U2 1 PU JOHN WILEY & SONS LTD PI CHICHESTER PA THE ATRIUM, SOUTHERN GATE, CHICHESTER PO19 8SQ, W SUSSEX, ENGLAND SN 1047-482X J9 INT J OSTEOARCHAEOL JI Int. J. Osteoarchaeol. PD JUL-AUG PY 2005 VL 15 IS 4 BP 261 EP 275 DI 10.1002/oa.781 PG 15 WC Anthropology; Archaeology SC Anthropology; Archaeology GA 957JR UT WOS:000231366600003 ER PT J AU Capper, A Tibbetts, IR O'Neil, JM Shaw, GR AF Capper, A Tibbetts, IR O'Neil, JM Shaw, GR TI The fate of Lyngbya majuscula toxins in three potential consumers SO JOURNAL OF CHEMICAL ECOLOGY LA English DT Article DE Stylocheilus striatus; Bursatella leachii; Diniatys dentifer; lyngbyatoxin-a; debromoaplysiatoxin; bioaccumulation; Opisthobranchia; secondary metabolites ID HARE STYLOCHEILUS-LONGICAUDA; SECONDARY METABOLITES; SEA HARE; BURSATELLA-LEACHII; NATURAL-PRODUCTS; GAIMARD 1824; OPISTHOBRANCHIA; GASTROPODA; DIET; QUOY AB Blooms of Lyngbya majuscula have been reported with increasing frequency and severity in the last decade in Moreton Bay, Australia. A number of grazers have been observed feeding upon this toxic cyanobacterium. Differences in sequestration of toxic compounds from L. majuscula were investigated in two anaspideans, Stylocheilus striatus, Bursatella leachii, and the cephalaspidean Diniatys dentifer. Species fed a monospecific diet of L. majuscula had different toxin distribution in their tissues and excretions. A high concentration of lyngbyatoxin-a was observed in the body of S. striatus (3.94 mg/kg(-1)) compared to bodily secretions (ink 0.12 mg/kg- 1; fecal matter 0.56 mg/kg(-1); eggs 0.05 mg/kg(-1)). In contrast, B. leachii secreted greater concentrations of lyngbyatoxin-a (ink 5.41 mg/kg(-1); fecal matter 6.71 mg/kg(-1)) than that stored in the body (2.24 mg/kg(-1)). The major internal repository of lyngbyatoxin-a and debromoaplysiatoxin was the digestive gland for both S. striatus (6.31 +/- 0.31 mg/kg(-1)) and B. leachii (156.39 +/- 46.92 mg/kg(-1)). D. dentifer showed high variability in the distribution of sequestered compounds. Lyngbyatoxin-a was detected in the digestive gland (3.56 +/- 3.56 mg/kg(-1)) but not in the head and foot, while debromoaplysiatoxin was detected in the head and foot (133.73 +/- 129.82 mg/kg(-1)) but not in the digestive gland. The concentrations of sequestered secondary metabolites in these animals did not correspond to the concentrations found in L. majuscula used as food for these experiments, suggesting it may have been from previous dietary exposure. Trophic transfer of debromoaplysiatoxin from L. majuscula into S. striatus is well established; however, a lack of knowledge exists for other grazers. The high levels of secondary metabolites observed in both the anaspidean and the cephalapsidean species suggest that these toxins may bioaccumulate through marine food chains. C1 Smithsonian Marine Stn, Ft Pierce, FL 34949 USA. Univ Queensland, Sch Life Sci, Ctr Marine Studies, Brisbane, Qld 4072, Australia. Univ Maryland, Ctr Environm Sci, Cambridge, MD 21673 USA. Univ Queensland, Natl Ctr Environm Toxicol EnTox, Coopers Plains, Qld, Australia. RP Capper, A (reprint author), Smithsonian Marine Stn, 701 Seaway Dr, Ft Pierce, FL 34949 USA. EM capper@sms.si.edu RI Capper, Angela/B-4403-2012; Tibbetts, Ian/K-6191-2013; O'Neil, Judith/F-9024-2013; OI Tibbetts, Ian/0000-0002-1481-238X; O'Neil, Judith/0000-0002-7697-5299; Capper, Angela/0000-0002-4922-0253 NR 23 TC 32 Z9 32 U1 3 U2 19 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0098-0331 J9 J CHEM ECOL JI J. Chem. Ecol. PD JUL PY 2005 VL 31 IS 7 BP 1595 EP 1606 DI 10.1007/S10886-005-5800-5 PG 12 WC Biochemistry & Molecular Biology; Ecology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology GA 952FN UT WOS:000230989500010 PM 16222795 ER PT J AU Buzas-Stephens, P Buzas, MA AF Buzas-Stephens, P Buzas, MA TI Population dynamics and dissolution of foraminifera in Nueces Bay, Texas SO JOURNAL OF FORAMINIFERAL RESEARCH LA English DT Article ID SCALE SPATIAL VARIATION; BENTHIC FORAMINIFERA; POLLUTION SOURCES; TEST DEFORMATION; HEAVY-METALS; TESTS; RIVER AB Foraminifers are important lower trophic-level members of oceans and estuaries, and study of their populations provides information about the health of an ecosystem. Replicate cores were taken at five stations in Nueces Bay, Texas, to evaluate living foraminifers in this heavily impacted estuary. A shallow secondary bay, Nueces Bay is naturally stressed and receives point-source and non-point-source effluents from the Nueces River and various industries. Most of the industries are clustered on the south shore of the bay, which also has a power plant and a shipping channel. The north shore, in contrast, is nearly devoid of industry and habitation. Since salinities in the bay vary due to freshwater influence, foraminiferal populations were sampled mid-bay, and spaced on a north-south transect where conditions are most constant. Results show that living densities and species richness are much higher at the south shore, probably due to the proximity of river inflow. In addition, foraminiferal communities are different at the northern and southern shores, as shown by statistical analyses. A high percentage of living foraminifers, almost exclusively Ammonia, have damaged shells, with a few chambers to entire whorls missing. This shell loss is attributed to dissolution. Framboidal pyrite found in living tests in oxygenated sediments is a stress response to heavy metal contamination, and pyritization may contribute to acidic conditions responsible for dissolution. Such dissolution is usually associated with diagenesis, but apparently can occur extensively in living individuals. The study cautions against assuming that lower densities, species richness, and shell dissolution along a transect are due solely to anthropogenic rather than natural causes. C1 Midwestern State Univ, Dept Biol, Wichita Falls, TX 76310 USA. Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA. RP Buzas-Stephens, P (reprint author), Midwestern State Univ, Dept Biol, 3410 Taft Blvd, Wichita Falls, TX 76310 USA. EM pamela.stephens@mwsu.edu NR 49 TC 30 Z9 30 U1 1 U2 5 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 JUL PY 2005 VL 35 IS 3 BP 248 EP 258 DI 10.2113/35.3.248 PG 11 WC Paleontology SC Paleontology GA 946PD UT WOS:000230583500005 ER PT J AU Ashenberg, J AF Ashenberg, J TI Proposed method for modeling the gravitational interaction between finite bodies SO JOURNAL OF GUIDANCE CONTROL AND DYNAMICS LA English DT Article ID ORDER AB A new computational approach to the problem of the mutual gravitational attraction between finite-size bodies is presented. In this case, the gravitational force acting on each body consists of contributions from the mutual interactions between all particles comprising all bodies. The current approach is mostly suitable for high-precision modeling of the gravitational perturbations acting on a satellite in the vicinity of large and irregular objects. This approach is preferable in problems such as a satellite in the vicinity of an asteroid or near a planetary ring. If the shape of the asteroid is irregular, the traditional Legendre polynomials method does not give a good approximation. The series expansion of the potential in the planetary ring problem has a convergence problem because the distance between the satellite and the ring center of mass can be small compared with the size of the ring. These difficulties are overcome by defining new integrals over the attracting body. The operations on these integrals for the purpose of methodical computation are also presented. The potential via radial basis functions is modeled, and the gradients based on these smooth functions are derived. C1 Harvard Smithsonian Ctr Astrophys, Radio & Geoastron Div, Cambridge, MA 02138 USA. RP Ashenberg, J (reprint author), Harvard Smithsonian Ctr Astrophys, Radio & Geoastron Div, MS 80,60 Garden St, Cambridge, MA 02138 USA. EM jashenberg@cfa.harvard.edu NR 13 TC 3 Z9 3 U1 1 U2 2 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 JUL-AUG PY 2005 VL 28 IS 4 BP 768 EP 774 DI 10.2514/1.9201 PG 7 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA 944OI UT WOS:000230438000022 ER PT J AU Neufeld, MJ AF Neufeld, MJ TI The end of the Army Space Program: Interservice rivalry and the transfer of the von Braun Group to NASA, 1958-1959 SO JOURNAL OF MILITARY HISTORY LA English DT Article AB The Army-Air Force struggle over ballistic missiles and space policy in the late 1950s was one of the worst episodes of U.S. inter-service strife during the Cold War. The papers of General J. B. Medaris provide an important new window onto the process by which the Army avoided transferring its ballistic missile and space capability to the National Aeronautics and Space Administration (NASA) in 1958, and then reluctantly did so in 1959, in part to prevent the Air Force from obtaining it. Medaris's papers illustrate how interservice rivalry shaped the actions of the Secretary of the Army and the leadership of Army Ordnance. C1 Smithsonian Inst, Natl Air & Space Museum, Space Hist Div, Washington, DC 20560 USA. RP Neufeld, MJ (reprint author), Smithsonian Inst, Natl Air & Space Museum, Space Hist Div, Washington, DC 20560 USA. NR 51 TC 1 Z9 1 U1 0 U2 1 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 JUL PY 2005 VL 69 IS 3 BP 737 EP 757 DI 10.1353/jmh.2005.0178 PG 21 WC History SC History GA 943RU UT WOS:000230372800004 ER PT J AU Choi, KH Kimmerer, W Smith, G Ruiz, GM Lion, K AF Choi, KH Kimmerer, W Smith, G Ruiz, GM Lion, K TI Post-exchange zooplankton in ballast water of ships entering the San Francisco Estuary SO JOURNAL OF PLANKTON RESEARCH LA English DT Article ID INVASION; CALIFORNIA; COPEPODS; PACIFIC; BAY AB The San Francisco Estuary in California (CA), USA, has been heavily altered by invasions of nonnative zooplankton and benthic organisms, presumably by the discharge of ships' ballast water. Since 2000, ships entering CA have been required to exchange ballast water with oceanic water during the voyage to decrease the number of organisms discharged into the Estuary that had previously been taken aboard at foreign ports. We examined abundance of zooplankton in ballast water of 18 container ships and 48 bulk carriers. Asia dominated the sources of ballast water, which contained multiple nonnative zooplankton including species that have invaded and since become common residents in the Estuary. The abundance of zooplankton was significantly lower in ballast water that had been emptied and refilled with oceanic water than those that had continuously been flushed with oceanic water (about three times the volume of ballast water), suggesting that empty-refill is more effective in removing exotic zooplankton. C1 San Francisco State Univ, Romberg Tiburon Ctr, Tiburon, CA 94920 USA. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Choi, KH (reprint author), San Francisco State Univ, Romberg Tiburon Ctr, 3152 Paradise Dr, Tiburon, CA 94920 USA. EM khchoi@sfsu.edu OI Ruiz, Gregory/0000-0003-2499-441X NR 25 TC 26 Z9 29 U1 0 U2 7 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0142-7873 J9 J PLANKTON RES JI J. Plankton Res. PD JUL PY 2005 VL 27 IS 7 BP 707 EP 714 DI 10.1093/plankt/fbi044 PG 8 WC Marine & Freshwater Biology; Oceanography SC Marine & Freshwater Biology; Oceanography GA 961WA UT WOS:000231691300008 ER PT J AU Fernandez-Marin, H Wcislo, WT AF Fernandez-Marin, H Wcislo, WT TI Production of minima workers by gynes of Atta colombica Guerin-Meneville (Hymenoptera : Formicidae : Attini) that lack a fungal pellet SO JOURNAL OF THE KANSAS ENTOMOLOGICAL SOCIETY LA English DT Article DE fungal acquisition; foundresses; fungus growing ants ID GROWING ANTS HYMENOPTERA AB Early studies of Atta nest founding showed that gynes exhibit claustral nest foundation, cultivate fungal gardens with fecal secretions, and nourish their larvae with eggs. These studies also showed that gynes sometimes lose their fungal pellets, or the fungal garden fails before workers emerge, apparently dooming the incipient colony. Here we report that Atta colombica foundresses maintained in the laboratory can produce workers even though they lack fungal pellets to initiate gardens. If such behavior occurs in nature, it raises the possibility that workers might re-acquire a fungal symbiont after nest establishment, and potentially rescue failing colonies. C1 Univ Puerto Rico, Dept Biol, San Juan, PR 00931 USA. Smithsonian Trop Res Inst, Balboa, Panama. RP Fernandez-Marin, H (reprint author), Univ Puerto Rico, Dept Biol, POB 23360, San Juan, PR 00931 USA. EM ic972735@rrpac.upr.clu.edu; WcisloW@si.edu NR 11 TC 7 Z9 7 U1 0 U2 6 PU KANSAS ENTOMOLOGICAL SOC PI LAWRENCE PA PO BOX 368, LAWRENCE, KS 66044 USA SN 0022-8567 J9 J KANSAS ENTOMOL SOC JI J. Kans. Entomol. Soc. PD JUL PY 2005 VL 78 IS 3 BP 290 EP 292 DI 10.2317/0402.19.1 PG 3 WC Entomology SC Entomology GA 982AA UT WOS:000233127900010 ER PT J AU Troyer, JL Pecon-Slattery, J Roelke, ME Johnson, W VandeWoude, S Vazquez-Salat, N Brown, M Frank, L Woodroffe, R Winterbach, C Winterbach, H Hemson, G Bush, M Alexander, KA Revilla, E O'Brien, SJ AF Troyer, JL Pecon-Slattery, J Roelke, ME Johnson, W VandeWoude, S Vazquez-Salat, N Brown, M Frank, L Woodroffe, R Winterbach, C Winterbach, H Hemson, G Bush, M Alexander, KA Revilla, E O'Brien, SJ TI Seroprevalence and genomic divergence of circulating strains of Feline immunodeficiency virus among Felidae and Hyaenidae species SO JOURNAL OF VIROLOGY LA English DT Article ID LIONS PANTHERA-LEO; FREE-RANGING LIONS; DOMESTIC CAT; PHYLOGENETIC ASPECTS; GENETIC DIVERSITY; MANDRILLUS-SPHINX; SEQUENCE-ANALYSIS; VIRAL-INFECTIONS; AFRICAN LIONS; LENTIVIRUS AB Feline immunodeficiency virus (FIV) infects numerous wild and domestic feline species and is closely related to human immunodeficiency virus (HIV) and simian immunodeficiency virus (SIV). Species-specific strains of FIV have been described for domestic cat (Felis catus), puma (Puma concolor), lion (Panthera leo), leopard (Panthera pardus), and Pallas' cat (Otocolobus manul). Here, we employ a three-antigen Western blot screening (domestic cat, puma, and lion FIV antigens) and PCR analysis to survey worldwide prevalence, distribution, and genomic differentiation of FIV based on 3,055 specimens from 35 Felidae and 3 Hyaenidae species. Although FIV infects a wide variety of host species, it is confirmed to be endemic in free-ranging populations of nine Felidae and one Hyaenidae species. These include the large African carnivores (lion, leopard, cheetah, and spotted hyena), where FIV is widely distributed in multiple populations; most of the South American felids (puma, jaguar, ocelot, margay, Geoffroy's cat, and tigrina), which maintain a lower FIV-positive level throughout their range; and two Asian species, the Pallas' cat, which has a species-specific strain of FIV, and the leopard cat, which has a domestic cat FIV strain in one population. Phylogenetic analysis of FIV proviral sequence demonstrates that most species for which FIV is endemic harbor monophyletic, genetically distinct species-specific FIV strains, suggesting that FIV transfer between cat species has occurred in the past but is quite infrequent today. C1 Natl Canc Inst, Lab Genom Divers, Ft Detrick, MD 21702 USA. Colorado State Univ, Dept Microbiol Immunol & Pathol, Ft Collins, CO 80523 USA. SAIC, ISRP Program, Ft Detrick, MD 21702 USA. Univ Calif Berkeley, Museum Vertebrate Zool, Laikipia Predator Project, Berkeley, CA 94720 USA. Univ Calif Davis, Dept Wildlife Fish & Conservat Biol, Davis, CA 95616 USA. Tau Consultants Pty Ltd, Maun, Botswana. Univ Oxford, Dept Zool, Wildlife Conservat Res Unit, Oxford OX1 2JD, England. Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, Front Royal, VA 22630 USA. Ctr Conservat African Resources Anim Communities, Kasane, Botswana. CSIC, Dept Appl Biol, Estac Biol Donana, E-41080 Seville, Spain. RP O'Brien, SJ (reprint author), Natl Canc Inst, Lab Genom Divers, Ft Detrick, MD 21702 USA. EM obrien@ncifcrf.gov RI Revilla, Eloy/B-5100-2008; Alexander, Kathleen/A-9765-2010; Troyer, Jennifer/B-8415-2012; Johnson, Warren/D-4149-2016; CSIC, EBD Donana/C-4157-2011 OI Revilla, Eloy/0000-0001-5534-5581; Alexander, Kathleen/0000-0001-7338-5341; Johnson, Warren/0000-0002-5954-186X; CSIC, EBD Donana/0000-0003-4318-6602 FU NCI NIH HHS [N01-CO-12400, N01CO12400] NR 38 TC 86 Z9 88 U1 3 U2 13 PU AMER SOC MICROBIOLOGY PI WASHINGTON PA 1752 N ST NW, WASHINGTON, DC 20036-2904 USA SN 0022-538X J9 J VIROL JI J. Virol. PD JUL PY 2005 VL 79 IS 13 BP 8282 EP 8294 DI 10.1128/JVI.79.13.8282-8294.2005 PG 13 WC Virology SC Virology GA 936PA UT WOS:000229866700034 PM 15956574 ER PT J AU Hutchinson, A AF Hutchinson, A TI Encyclopedia of cryptozoology: A global guide to hidden animals and their pursuers. SO LIBRARY JOURNAL LA English DT Book Review C1 Smithsonian Inst Lib, Washington, DC 20560 USA. RP Hutchinson, A (reprint author), Smithsonian Inst Lib, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 2 U2 4 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 JUL PY 2005 VL 130 IS 12 BP 125 EP 125 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 943CG UT WOS:000230328900365 ER PT J AU Aleon, J Krot, AN McKeegan, KD MacPherson, GJ Ulyanov, AA AF Aleon, J Krot, AN McKeegan, KD MacPherson, GJ Ulyanov, AA TI Fine-grained, spinel-rich inclusions from the reduced CV chondrite Efremovka: II. Oxygen isotopic compositions SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID RARE-EARTH ELEMENTS; EARLY SOLAR NEBULA; CARBONACEOUS CHONDRITES; ALLENDE METEORITE; REFRACTORY INCLUSIONS; FUN INCLUSION; CALCIUM; CAI; ANOMALIES; SYSTEM AB Oxygen isotopes have been measured by ion microprobe in individual minerals (spinel, Al-Ti-diopside, melilite, and anorthite) within four relatively unaltered, fine-grained, spinel-rich Ca-Al-rich inclusions (CAIs) from the reduced CV chondrite Efremovka. Spinel is uniformly O-16-rich (Delta(17)O <= -20 parts per thousand) in all four CAIs; Al-Ti-diopside is similarly O-16-rich in all but one CAT, where it has smaller 160 excesses (-15 parts per thousand <= Delta(17)O <= -10 parts per thousand). Anorthite and melilite vary widely in composition from O-16-rich to O-16-poor (-22 parts per thousand <= Delta(17)O <= -5 parts per thousand). Two of the CAIs are known to have group II volatility-fractionated rare-earth-element patterns, which is typical of this variety of CAI and which suggests formation by condensation. The association of such trace element patterns with O-16-enrichment in these CAIs suggests that they formed by gas-solid condensation from an O-16-rich gas. They subsequently experienced thermal processing in an O-16-poor reservoir, resulting in partial oxygen isotope exchange. Within each inclusion, oxygen isotope variations from mineral to mineral are consistent with solid-state oxygen self-diffusion at the grain-to-grain scale, but such a model is not consistent with isotopic variations at a larger scale in two of the CAIs. The spatial association of 160 depletions with both elevated Fe contents in spinel and the presence of nepheline suggests that late-stage iron-alkali metasomatism played some role in modifying the isotopic patterns in some CAIs. One of the CAIs is a compound object consisting of a coarse-grained, melilite-rich (type A) lithology joined to a fine-grained, spinel-rich one. Melilite and anorthite in the fine-grained portion are mainly O-16-rich, whereas melilite in the type A portion ranges from O-16-rich to O-16-poor, suggesting that oxygen isotope exchange predated the joining together of the two parts and that both O-16-rich and O-16-poor gaseous reservoirs existed simultaneously in the early solar nebula. C1 Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA. CNRS, UPR 2300, Ctr Rech Petrog & Geochim, F-54501 Vandoeuvre Les Nancy, France. Univ Hawaii, Sch Ocean & Earth Sci & Technol, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA. Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. Moscow MV Lomonosov State Univ, Moscow 119992, Russia. RP Aleon, J (reprint author), Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA. EM aleon@crpg.cnrs-nancy.fr RI McKeegan, Kevin/A-4107-2008; UCLA, SIMS/A-1459-2011 OI McKeegan, Kevin/0000-0002-1827-729X; NR 57 TC 13 Z9 13 U1 2 U2 7 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 JUL PY 2005 VL 40 IS 7 BP 1043 EP 1058 PG 16 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 969TK UT WOS:000232257500007 ER PT J AU Kathriarachchi, H Hoffmann, P Samuel, R Wurdack, KJ Chase, MW AF Kathriarachchi, H Hoffmann, P Samuel, R Wurdack, KJ Chase, MW TI Molecular phylogenetics of Phyllanthaceae inferred from five genes (plastid atpB, matK, 3 ' ndhF, rbcL, and nuclear PHYC) SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article DE atpB; matK; ndhF; PHYC; Dicoelia; Lingelsheimia; Malpighiales; molecular phylogenctics; Phyllanthaceae ID OBLIGATE POLLINATION MUTUALISM; EPICEPHALA-MOTHS GRACILLARIIDAE; SYSTEMATIC FOLIAR MORPHOLOGY; DNA-SEQUENCES; PHYLLANTHOIDEAE EUPHORBIACEAE; ACALYPHOIDEAE EUPHORBIACEAE; SUBFAMILY PHYLLANTHOIDEAE; CLADISTIC-ANALYSIS; POLLEN MORPHOLOGY; FLOWERING PLANTS AB Phyllanthaceae are a pantropical family of c. 2000 species for which circumscription is believed to be coincident with subfamily Phyllanthoideae of Euphorbiaceae sensu lato (Malpighiales) excluding Putranjivaceae. A phylogenetic study of the family using DNA sequence data has delivered largely congruent results from the plastid atpB, matK, ndhF, rbcL, and the nuclear PHYC. Our analyses include sampling from 54 of 59 genera, representing all tribes and subtribes of Phyllanthoideae. The family falls into two major clades characterized by inflorescence and leaf anatomical features. Several traditional taxonomic groupings were retrieved with minor modifications, but most clades recovered are considerably different from previous non-molecular based ideas of relationships. The enigmatic genus Dicoelia and the geographically disjunct genus Lingelsheimia are shown to be embedded in Phyllanthaceae. The taxonomic status of Leptopus diplospermus (= Chorisandrachne) and the debated placement of Andrachne ovalis have been clarified, and Protomegabaria and Richeriella are newly placed. Paraphyly of Cleistanthus and Phyllanthus is confirmed, having three and four other genera embedded, respectively. Petalodiscus is also paraphyletic, including all other Malagassian Wielandieae. © 2005 Elsevier Inc. All rights reserved. C1 Univ Vienna, Inst Bot, Dept Higher Plant Systemat & Evolut, 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. Royal Bot Gardens, Jodrell Lab, Richmond TW9 3DS, Surrey, England. RP Samuel, R (reprint author), Univ Vienna, Inst Bot, Dept Higher Plant Systemat & Evolut, Rennweg 14, A-1030 Vienna, Austria. EM mary.rosabella.samuel@univie.ac.at RI Chase, Mark /A-6642-2011 NR 98 TC 45 Z9 57 U1 1 U2 5 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 1055-7903 J9 MOL PHYLOGENET EVOL JI Mol. Phylogenet. Evol. PD JUL PY 2005 VL 36 IS 1 BP 112 EP 134 DI 10.1016/j.ympev.2004.12.002 PG 23 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 932RO UT WOS:000229571300009 PM 15904861 ER PT J AU Zdziarski, AA Gierlinski, M Rao, AR Vadawale, SV Mikolajewska, J AF Zdziarski, AA Gierlinski, M Rao, AR Vadawale, SV Mikolajewska, J TI GRS 1915+105: the distance, radiative processes and energy-dependent variability SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; black hole physics; radiation mechanisms : non-thermal; binaries : general; stars : individual; GRS 1915+105; X-rays : stars ID ACCRETING BLACK-HOLES; X-RAY VARIABILITY; GRS 1915+105; CYGNUS X-1; SPECTRAL STATES; SUPERLUMINAL SOURCE; SCALE STRUCTURE; HARD STATE; GAMMA-RAYS; SOFT STATE AB We present an exhaustive analysis of five broad-band observations of GRS 1915+105 in two variability states,. and., observed simultaneously by the Proportional Counter Array (PCA) and High-Energy X-ray Timing Experiment (HEXTE) detectors aboard the Rossi X-ray Timing Explorer, and the Oriented Scintillation Spectrometer Experiment (OSSE) detector aboard the Compton Gamma-ray Observatory. We find all the spectra well fitted by Comptonization of disc blackbody photons, with very strong evidence for the presence of a non-thermal electron component in the Comptonizing plasma. Both the energy and the power spectra in the. state are typical of the very high/intermediate state of black hole binaries. The spectrum of the. state is characterized by a strong blackbody component Comptonized by thermal electrons and a weak non-thermal tail. We then calculate rms spectra ( fractional variability as functions of energy) for the PCA data. We accurately model the rms spectra by coherent superposition of variability in the components implied by the spectral fits, namely a less variable blackbody and more variable Comptonization. The latter dominates at high energies, resulting in a flattening of the rms at high energies in most of the data. This is also the case for the spectra of the quasi-periodic oscillations present in the. state. Then, some of our data require a radial dependence of the rms of the disc blackbody. We also study the distance to the source, and find d similar or equal to 11 kpc as the most likely value, contrary to a recent claim of a much lower value. C1 Ctr Astron M Kopernika, PL-00716 Warsaw, Poland. Univ Durham, Dept Phys, Durham DH1 3LE, England. Jagiellonian Univ, Astron Observ, PL-30244 Krakow, Poland. Tata Inst Fundamental Res, Bombay 400005, Maharashtra, India. Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Zdziarski, AA (reprint author), Ctr Astron M Kopernika, Bartycka 18, PL-00716 Warsaw, Poland. EM aaz@camk.edu.pl; Marek.Gierlinski@durham.ac.uk OI Gierlinski, Marek/0000-0001-9149-3514 NR 64 TC 44 Z9 44 U1 1 U2 2 PU BLACKWELL PUBLISHING 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 JUL 1 PY 2005 VL 360 IS 3 BP 825 EP 838 DI 10.1111/j.1365-2966.2005.09112.x PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 935KY UT WOS:000229782400003 ER PT J AU Jonker, PG Mendez, M van der Klis, M AF Jonker, PG Mendez, M van der Klis, M TI Sidebands to the lower kilohertz quasi-periodic oscillation in 4U 1636-53 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; binaries : general; stars : individual; 4U 1636-53; stars : neutron; X-rays : binaries ID X-RAY BINARY; 4U 1636-53; MILLISECOND PULSAR; NONLINEAR RESONANCE; ACCRETION DISK; DISCOVERY; FREQUENCY AB In this paper we report on further observations of the third and fourth kilohertz quasi-periodic oscillations (QPOs) in the power spectrum of the low-mass X-ray binary( LMXB) 4U 1636-53. These kilohertz QPOs are sidebands to the lower kilohertz QPO. The upper sideband has a frequency 55.5 +/- 1.7 Hz larger than that of the contemporaneously measured lower kilohertz QPO. Such a sideband has now been measured at a significance > 6 sigma in the power spectra of three neutron-star LMXBs (4U 1636-53, 1728-34 and 1608-52). We also confirm the presence of a sideband at a frequency similar to 55 Hz less than the frequency of the lower kilohertz QPO. The lower sideband is detected at a 3.5 sigma level only when the lower kilohertz QPO frequency is between 800 and 850 Hz. In that frequency interval, the sidebands are consistent with being symmetric around the lower kilohertz QPO frequency. The upper limit to the rms amplitude of the lower sideband is significantly lower than that of the upper sideband for lower kilohertz QPO frequencies > 850 Hz. Symmetric sidebands are unique to 4U 1636-53. This might be explained by the fact that lower kilohertz QPO frequencies as high as 800-850 Hz are rare for 4U 1728-34 and 1608-52. Finally, we also measured a low-frequency QPO at a frequency of similar to 43 Hz when the lower kilohertz QPO frequency is between 700 and 850 Hz. A similar low-frequency QPO is present in the power spectra of the other two systems for which a sideband has been observed. We briefly discuss the possibility that the sideband is caused by Lense-Thirring precession. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. SRON, Natl Inst Space Res, NL-3584 CA Utrecht, Netherlands. Univ Utrecht, Astron Inst, NL-3508 TA Utrecht, Netherlands. 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 Mendez, Mariano/C-8011-2012 OI Mendez, Mariano/0000-0003-2187-2708 NR 20 TC 14 Z9 14 U1 0 U2 0 PU BLACKWELL PUBLISHING 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 JUL 1 PY 2005 VL 360 IS 3 BP 921 EP 925 DI 10.1111/j.1365-2966.2005.09075.x PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 935KY UT WOS:000229782400011 ER PT J AU Perez-Torres, MA Alberdi, A Marcaide, JM Guerrero, MA Lundqvist, P Shapiro, II Ros, E Lara, L Guirado, JC Weiler, KW Stockdale, CJ AF Perez-Torres, MA Alberdi, A Marcaide, JM Guerrero, MA Lundqvist, P Shapiro, II Ros, E Lara, L Guirado, JC Weiler, KW Stockdale, CJ TI High-resolution observations of SN 2001gd in NGC 5033 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE supernovae : individual : SN 2001gd; galaxies : individual : NGC5033; radio continuum : stars; X-rays : individual SN 2001gd ID RADIO-EMISSION; CIRCUMSTELLAR INTERACTION; 1993J; ABSORPTION; SUPERNOVAE; SHELL; UV AB We report on 8.4-GHz very-long-baseline interferometry (VLBI) observations of SN 2001gd in the spiral galaxy NGC 5033 made on 2002 June 26 (2002.48) and 2003 April 8 (2003.27). We used the interferometric visibility data to estimate angular diameter sizes for the supernova by model fitting. Our data nominally suggest a relatively strong deceleration for the expansion of SN 2001gd, but we cannot dismiss the possibility of a free supernova expansion. From our VLBI observations on 2003 April 8, we inferred a minimum total energy in relativistic particles and magnetic fields in the supernova shell of E-min = (0.3-14) x 1047 erg, and a corresponding equipartition average magnetic field of B-min = 50-350 mG. We also present multiwavelength Very Large Array (VLA) measurements of SN 2001gd made at our second VLBI epoch at frequencies of 1.4, 4.9, 8.4, 15.0, 22.5 and 43.3 GHz. The VLA data are well fitted by an optically thin, synchrotron spectrum (alpha = -1.0 +/- 0.1; S-v proportional to v(a)), partially absorbed by thermal plasma. We obtain a supernova flux density of 1.02 +/- 0.05 mJy at the observing frequency of 8.4 GHz for the second epoch, which results in an isotropic radio luminosity of (6.0 +/- 0.3) x 10(36) erg s(-1) between 1.4 and 43.3 GHz, at an adopted distance of 13.1 Mpc. Finally, we report on an XMM-Newton X-ray detection of SN 2001gd on 2002 December 18. The supernova X-ray spectrum is consistent with optically thin emission from a soft component ( associated with emission from the reverse shock) at a temperature of around 1 keV. The observed flux corresponds to an isotropic X-ray luminosity of L-X = (1.4 +/- 0.4) x 10(39) erg s(-1) in the 0.3-5 keV band. We suggest that both radio and X-ray observations of SN 2001gd indicate that a circumstellar interaction similar to that displayed by SN 1993J in M 81 is taking place. C1 CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain. Univ Valencia, Dept Astron & Astrofis, E-46100 Burjassot, Spain. Stockholm Observ, SE-10691 Stockholm, Sweden. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Max Planck Inst Radioastron, D-53121 Bonn, Germany. Univ Granada, Dept Fis Teor & Comos, E-18071 Granada, Spain. USN, Res Lab, Washington, DC 20375 USA. RP Perez-Torres, MA (reprint author), CSIC, Inst Astrofis Andalucia, Apdo Correos 3004, E-18080 Granada, Spain. EM torres@iaa.es OI Guerrero, Martin/0000-0002-7759-106X; Ros, Eduardo/0000-0001-9503-4892 NR 30 TC 18 Z9 18 U1 0 U2 4 PU BLACKWELL PUBLISHING 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 JUL 1 PY 2005 VL 360 IS 3 BP 1055 EP 1062 DI 10.1111/j.1365-2966.2005.09102.x PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 935KY UT WOS:000229782400023 ER PT J AU Yuan, YF Heyl, JS AF Yuan, YF Heyl, JS TI Rotational evolution of protoneutron stars with hyperons: spin up or not? SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE dense matter; stars : evolution; stars : neutron; stars : rotation ID PROTO-NEUTRON STARS; COLLAPSE SUPERNOVA EXPLOSIONS; GENERAL RELATIVISTIC STARS; MEAN-FIELD THEORY; CORE-COLLAPSE; PHASE-TRANSITIONS; NUMERICAL-METHOD; MASSIVE STARS; NUCLEAR; MATTER AB We study the evolution of a rigidly rotating protoneutron star (PNS) with hyperons and nucleons or solely nucleons in its core due to the escape of trapped neutrinos. As the neutrinos escape, the core nucleonic neutron star (NS) expands and the stellar rotation slows. After the neutrinos escape, the range of the spin periods is narrower than the initial one, but the distribution is still nearly uniform. A PNS with hyperons, at the late stage of its evolution, keeps shrinking and spinning up until all the trapped neutrinos escape. Consequently, the distribution of the stellar initial spin periods is skewed towards shorter periods. If the hyperonic star is metastable, its rotational frequency accelerates distinguishedly before it collapses to a black hole. C1 Univ Sci & Technol China, Ctr Astrophys, Hefei 230026, Peoples R China. Harvard Univ, Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. RP Univ Sci & Technol China, Ctr Astrophys, Hefei 230026, Peoples R China. EM yfyuan@ustc.edu.cn; heyl@physics.ubc.ca NR 59 TC 4 Z9 4 U1 1 U2 2 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUL PY 2005 VL 360 IS 4 BP 1493 EP 1505 DI 10.1111/j.1365-2966.2005.09142.x PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 942SY UT WOS:000230303900025 ER PT J AU Lovelock, CE Ewel, JJ AF Lovelock, CE Ewel, JJ TI Links between tree species, symbiotic fungal diversity and ecosystem functioning in simplified tropical ecosystems SO NEW PHYTOLOGIST LA English DT Article DE Acaulospora morrowiae; Acaulospora scrobiculata; Acaulospora spinosa; arbuscular mycorrihzas; Cedrela odorata; Cordia alliodora; Hyeronima alchorneoides; tropical trees ID ARBUSCULAR MYCORRHIZAL FUNGI; PLANT COMMUNITY STRUCTURE; HYACINTHOIDES NON-SCRIPTA; NUTRIENT-USE EFFICIENCY; GROWTH-RESPONSES; FOREST; PRODUCTIVITY; MODEL; SEEDLINGS; PATTERNS AB We studied the relationships among plant and arbuscular mycorrhizal (AM) fungal diversity, and their effects on ecosystem function, in a series of replicate tropical forestry plots in the La Selva Biological Station, Costa Rica. Forestry plots were 12 yr old and were either monocultures of three tree species, or polycultures of the tree species with two additional understory species. Relationships among the AM fungal spore community, host species, plant community diversity and ecosystem phosphorus-use efficiency (PUE) and net primary productivity (NPP) were assessed. Analysis of the relative abundance of AM fungal spores found that host tree species had a significant effect on the AM fungal community, as did host plant community diversity (monocultures vs polycultures). The Shannon diversity index of the AM fungal spore community differed significantly among the three host tree species, but was not significantly different between monoculture and polyculture plots. Over all the plots, significant positive relationships were found between AM fungal diversity and ecosystem NPP, and between AM fungal community evenness and PUE. Relative abundance of two of the dominant AM fungal species also showed significant correlations with NPP and PUE. We conclude that the AM fungal community composition in tropical forests is sensitive to host species, and provide evidence supporting the hypothesis that the diversity of AM fungi in tropical forests and ecosystem NPP covaries. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Univ Queensland, Sch Integrat Biol, St Lucia, Qld 4072, Australia. US Forest Serv, Pacific SW Res Stn, Inst Pacific Isl Forestry, Honolulu, HI 96813 USA. RP Lovelock, CE (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM c.lovelock@uq.edu.au RI Lovelock, Catherine/G-7370-2012 OI Lovelock, Catherine/0000-0002-2219-6855 NR 55 TC 29 Z9 32 U1 8 U2 26 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0028-646X J9 NEW PHYTOL JI New Phytol. PD JUL PY 2005 VL 167 IS 1 BP 219 EP 228 DI 10.1111/j.1469-8137.2005.01402.x PG 10 WC Plant Sciences SC Plant Sciences GA 932VF UT WOS:000229581600022 PM 15948844 ER PT J AU Friedman, AS Bloom, JS AF Friedman, AS Bloom, JS TI Present and future prospects for GRB standard candles SO NUOVO CIMENTO DELLA SOCIETA ITALIANA DI FISICA C-GEOPHYSICS AND SPACE PHYSICS LA English DT Article; Proceedings Paper CT 4th Workshop on Gamma-Ray Bursts in the Afterglow Era CY OCT 18-22, 2004 CL Rome, ITALY ID GAMMA-RAY BURSTS; DARK ENERGY; DECELERATION; AFTERGLOWS; ENERGETICS; SUPERNOVA; UNIVERSE; SPECTRA AB Following our previous work, we conclude that a CRB standard candle constructed from the Ghirlanda et al. power-law relation between the geometry corrected energy (E-gamma) and the peak of the rest-frame prompt burst spectrum (E-p) is not yet cosmographically useful, despite holding some potential advantages over SNe Ia. This is due largely to the small sample of similar to 20 GRBs with the required measured redshifts, jet-breaks, and peak energies, and to the strong sensitivity of the goodness-of-fit of the power-law to input assumptions. The most important such finding concerns the sensitivity to the generally unknown density (and density profile), of the circumburst medium. Although the E-p-E-gamma relation is a highly significant correlation over many cosmologies, until the sample expands to include many low-z events, it will be most sensitive to Omega(M) but essentially insensitive to Omega(Lambda) and w, with some hope of constraining dw/dt with high-z GRB data alone. The relation clearly represents a significant improvement in the search for an empirical GRB standard candle, but is further hindered by an unknown physical basis for the relation, the lack of a low-z training set to calibrate the relation in a cosmology-independent way, and several major potential systematic uncertainties and selection effects. Until these concerns are addressed, a larger sample is acquired, and attempts are made to marginalize or perform Monte Carlo simulations over the unknown density distribution, we urge caution concerning claims of the utility of GRBs for cosmography and especially the attempts to combine GRBs with SNe Ia. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. RP Friedman, AS (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Friedman, Andrew/I-4691-2013 OI Friedman, Andrew/0000-0003-1334-039X NR 30 TC 1 Z9 1 U1 0 U2 0 PU SOCIETA ITALIANA DI FISICA PI BOLOGNA PA VIA SARAGOZZA, 12, I-40123 BOLOGNA, ITALY SN 1124-1896 J9 NUOVO CIMENTO C JI Nuovo Cimento Soc. Ital. Fis. C-Geophys. Space Phys. PD JUL-OCT PY 2005 VL 28 IS 4-5 BP 669 EP 672 DI 10.1393/ncc/i2005-10125-2 PG 4 GA 997RW UT WOS:000234266300038 ER PT J AU Vasconcelos, HL Laurance, WF AF Vasconcelos, HL Laurance, WF TI Influence of habitat, litter type, and soil invertebrates on leaf-litter decomposition in a fragmented Amazonian landscape SO OECOLOGIA LA English DT Article DE Amazon; edge effects; habitat fragmentation; secondary-forest succession; nutrient cycling ID FOREST DISTURBANCE; TROPICAL FOREST; SECONDARY FOREST; RAIN-FOREST; FAUNA; TREES; RATES; COMMUNITIES; HERBIVORY; EDGES AB Amazonian forest fragments and second-growth forests often differ substantially from undisturbed forests in their microclimate, plant-species composition, and soil fauna. To determine if these changes could affect litter decomposition, we quantified the mass loss of two contrasting leaf-litter mixtures, in the presence or absence of soil macroinvertebrates, and in three forest habitats. Leaf-litter decomposition rates in second-growth forests (> 10 years old) and in fragment edges (< 100 m from the edge) did not differ from that in the forest interior (> 250 in from the edges of primary forests). In all three habitats, experimental exclusion of soil invertebrates resulted in slower decomposition rates. Faunal-exclosure effects were stronger for litter of the primary forest, composed mostly of leaves of old-growth trees, than for litter of second-growth forests, which was dominated by leaves of successional species. The latter had a significantly lower initial concentration of N, higher C:N and lignin:N ratios, and decomposed at a slower rate than did litter from forest interiors. Our results indicate that land-cover changes in Amazonia affect decomposition mainly through changes in plant species composition, which in turn affect litter quality. Similar effects may occur on fragment edges, particularly on very disturbed edges, where successional trees become dominant. The drier microclimatic conditions in fragment edges and second-growth forests (>10 years old) did not appear to inhibit decomposition. Finally, although soil invertebrates play a key role in leaf-litter decomposition, we found no evidence that differences in the abundance, species richness, or species composition of invertebrates between disturbed and undisturbed forests significantly altered decomposition rates. C1 Univ Fed Uberlandia, Inst Biol, BR-38400902 Uberlandia, MG, Brazil. Smithsonian Trop Res Inst, Balboa, Panama. INPA, Biol Dynam Forest Fragments Project, BR-69011970 Manaus, Amazonas, Brazil. RP Vasconcelos, HL (reprint author), Univ Fed Uberlandia, Inst Biol, CP 593, BR-38400902 Uberlandia, MG, Brazil. EM heraldo@umuarama.ufu.br RI Laurance, William/B-2709-2012; Vasconcelos, Heraldo/C-3353-2013 OI Vasconcelos, Heraldo/0000-0001-6969-7131 NR 43 TC 66 Z9 77 U1 7 U2 69 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013 USA SN 0029-8549 J9 OECOLOGIA JI Oecologia PD JUL PY 2005 VL 144 IS 3 BP 456 EP 462 DI 10.1007/s00442-005-0117-1 PG 7 WC Ecology SC Environmental Sciences & Ecology GA 955SL UT WOS:000231247800013 PM 15942762 ER PT J AU Franklin, LA Neale, PJ Jeffrey, WH Philips-Kress, JD AF Franklin, L. A. Neale, P. J. Jeffrey, W. H. Philips-Kress, J. D. TI UV RADIATION INHIBITS CARBON UPTAKE AND ALLOCATION IN A ROSS SEA PHYTOPLANKTON BLOOM SO PHYCOLOGIA LA English DT Meeting Abstract C1 [Franklin, L. A.; Neale, P. J.; Philips-Kress, J. D.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Jeffrey, W. H.] Univ W Florida, Pensacola, FL 32514 USA. EM franklinl@si.edu RI Neale, Patrick/A-3683-2012 NR 0 TC 0 Z9 0 U1 0 U2 3 PU INT PHYCOLOGICAL SOC PI LAWRENCE PA NEW BUSINESS OFFICE, PO BOX 1897, LAWRENCE, KS 66044-8897 USA SN 0031-8884 J9 PHYCOLOGIA JI Phycologia PD JUL PY 2005 VL 44 IS 4 MA 79 BP 33 EP 34 PG 2 WC Plant Sciences; Marine & Freshwater Biology SC Plant Sciences; Marine & Freshwater Biology GA V81JZ UT WOS:000205501500080 ER PT J AU Fredericq, S Freshwater, DW Lopez-Bautista, JM Gavio, B Norris, JN Hommersand, MH AF Fredericq, S. Freshwater, D. W. Lopez-Bautista, J. M. Gavio, B. Norris, J. N. Hommersand, M. H. TI A REVISED CLASSIFICATION OF THE RED ALGAE CENTERED AROUND KYLIN'S GIGARTINALES AND CRYPTONEMIALES SO PHYCOLOGIA LA English DT Meeting Abstract C1 [Fredericq, S.] Univ Louisiana Lafayette, Dept Biol, Lafayette, LA 70504 USA. [Freshwater, D. W.] Univ N Carolina, Ctr Marine Sci, Wilmington, NC 28409 USA. [Lopez-Bautista, J. M.] Univ Alabama, Dept Biol Sci, Tuscaloosa, AL 35487 USA. [Gavio, B.] Univ Magdalena, Dept Biol, Santa Marta, Colombia. [Norris, J. N.] Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, Washington, DC 20013 USA. [Hommersand, M. H.] Univ N Carolina, Dept Biol, Chapel Hill, NC 27599 USA. EM slf9209@louisiana.edu NR 0 TC 0 Z9 0 U1 0 U2 1 PU INT PHYCOLOGICAL SOC PI LAWRENCE PA NEW BUSINESS OFFICE, PO BOX 1897, LAWRENCE, KS 66044-8897 USA SN 0031-8884 J9 PHYCOLOGIA JI Phycologia PD JUL PY 2005 VL 44 IS 4 MA 80 BP 34 EP 34 PG 1 WC Plant Sciences; Marine & Freshwater Biology SC Plant Sciences; Marine & Freshwater Biology GA V81JZ UT WOS:000205501500081 ER PT J AU Zibrov, S Novikova, I Phillips, DF Taichenachev, AV Yudin, VI Walsworth, RL Zibrov, AS AF Zibrov, S Novikova, I Phillips, DF Taichenachev, AV Yudin, VI Walsworth, RL Zibrov, AS TI Three-photon-absorption resonance for all-optical atomic clocks SO PHYSICAL REVIEW A LA English DT Article ID POPULATION-TRAPPING RESONANCES; FREQUENCY STANDARDS; VAPOR; 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. We present measurements of the N-resonance contrast, width and light shift for the D-1 line of Rb-87 with varying buffer gases, and find good agreement with an analytical model of this resonance. The results suggest that N resonances are promising for atomic clock applications. C1 Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. Moscow State Engn Phys Inst, Moscow 115409, Russia. PN Lebedev Phys Inst, Moscow 117924, Russia. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Russian Acad Sci, Inst Laser Phys, SB, Novosibirsk 630090, Russia. Novosibirsk State Univ, Novosibirsk 630090, Russia. RP Zibrov, S (reprint author), Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. RI Novikova, Irina/B-9041-2008; Taichenachev, Aleksei/K-7065-2015; Zibrov, Sergei/M-6400-2015; Zibrov, Alexander/G-7419-2014 OI Taichenachev, Aleksei/0000-0003-2273-0066; NR 17 TC 24 Z9 25 U1 0 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 JUL PY 2005 VL 72 IS 1 AR 011801 DI 10.1103/PhysRevA.72.011801 PG 4 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 950VU UT WOS:000230887300012 ER PT J AU Geshnizjani, G Chung, DJH Afshordi, N AF Geshnizjani, G Chung, DJH Afshordi, N TI Do large-scale inhomogeneities explain away dark energy? SO PHYSICAL REVIEW D LA English DT Article ID GENERAL-RELATIVITY; COSMOLOGICAL PERTURBATIONS; APPROXIMATION SCHEME; UNIVERSE AB Recently, new arguments [E. Barausse, S. Matarrese, and A. Riotto, Phys. Rev. D 71, 063537 (2005).][E. W. Kolb, S. Matarrese, A. Notari, and A. Riotto, hep-th/0503117 [Phys. Rev. Lett. (to be published)].] for how corrections from super-Hubble modes can explain the present-day acceleration of the universe have appeared in the literature. However, in this paper, we argue that, to second order in spatial gradients, these corrections only amount to a renormalization of local spatial curvature, and thus cannot account for the negative deceleration. Moreover, cosmological observations already put severe bounds on such corrections, at the level of a few percent, while in the context of inflationary models, these corrections are typically limited to similar to 10(-5). Currently there is no general constraint on the possible correction from higher order gradient terms, but we argue that such corrections are even more constrained in the context of inflationary models. C1 Univ Wisconsin, Dept Phys, Madison, WI 53706 USA. Harvard Univ, Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. RP Geshnizjani, G (reprint author), Univ Wisconsin, Dept Phys, Madison, WI 53706 USA. EM ghazal@physics.wisc.edu; Danielchung@wisc.edu; nafshordi@cfa.harvard.edu NR 24 TC 42 Z9 42 U1 0 U2 0 PU AMERICAN PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1550-7998 J9 PHYS REV D JI Phys. Rev. D PD JUL PY 2005 VL 72 IS 2 AR 023517 DI 10.1103/PhysRevD.72.023517 PG 4 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 950WO UT WOS:000230889600027 ER PT J AU Kirby, K Houle, F AF Kirby, K Houle, F TI Albert Einstein to Michele Bessol - Reply SO PHYSICS TODAY LA English DT Letter C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. IBM Corp, Almaden Res Ctr, San Jose, CA USA. RP Kirby, K (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM kkirby@cfa.harvard.edu; houle@almaden.ibm.com NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0031-9228 J9 PHYS TODAY JI Phys. Today PD JUL PY 2005 VL 58 IS 7 BP 16 EP 16 PG 1 WC Physics, Multidisciplinary SC Physics GA 942AC UT WOS:000230254300009 ER PT J AU Noren, SR Iverson, SJ Boness, DJ AF Noren, SR Iverson, SJ Boness, DJ TI Development of the blood and muscle oxygen stores in gray seals (Halichoerus grypus): Implications for juvenile diving capacity and the necessity of a terrestrial postweaning fast SO PHYSIOLOGICAL AND BIOCHEMICAL ZOOLOGY LA English DT Article ID AEROBIC DIVE LIMITS; STORAGE CAPACITY; GREY SEALS; MIROUNGA-ANGUSTIROSTRIS; ONDATRA-ZIBETHICUS; VOLUME MEASUREMENT; NITROGEN TENSIONS; SEASONAL-CHANGES; WEDDELL SEALS; HARBOR SEALS AB To successfully transition from nursing to foraging, phocid seal pups must develop adequate diving physiology within the limited time between birth and their first independent foraging trip to sea. We studied the postpartum development of oxygen stores in gray seals (Halichoerus grypus, n = 40) to better understand the ontogeny of diving capacity in phocids. Hemoglobin (Hb), hematocrit (Hct), blood volume (BV), and myoglobin (Mb) levels in newborn (3 d postpartum [DPP]) and newly weaned (DPP) pups were among the lowest 17 +/- 0.4 measured across age classes. During the pups' terrestrial postweaning fast (PWF), Hb, Hct, mass-specific BV, and Mb increased by 28%, 21%, 13%, and 29%, respectively, resulting in a 35% increase in total body mass-specific oxygen stores and a 23% increase in calculated aerobic dive limit (CADL). Although Hb and Hct levels at the end of the PWF were nearly identical to those of yearlings, total body mass-specific oxygen stores and CADL of weaned pups departing for sea were only 66% - 67% and 32% - 62%, respectively, of those for yearlings and adult females. The PWF represents an integral component of the physiological development of diving capacity in phocids; however, newly independent phocids still appear to have limited diving capabilities at the onset of foraging. C1 Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, Washington, DC 20008 USA. Dalhousie Univ, Dept Biol, Halifax, NS B3H 4J1, Canada. RP Noren, SR (reprint author), Natl Marine Fisheries Serv, SW Fisheries Sci Ctr, 8604 La Jolla Shores Dr, La Jolla, CA 92038 USA. EM shawn.noren@noaa.gov NR 53 TC 59 Z9 59 U1 1 U2 14 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 1522-2152 EI 1537-5293 J9 PHYSIOL BIOCHEM ZOOL JI Physiol. Biochem. Zool. PD JUL-AUG PY 2005 VL 78 IS 4 BP 482 EP 490 DI 10.1086/430228 PG 9 WC Physiology; Zoology SC Physiology; Zoology GA 938DE UT WOS:000229979300002 PM 15957103 ER PT J AU Robbins, RK AF Robbins, RK TI Phylogenetic relationships among the species of Panthiades Hubner (Lycaenidae : Theclinae : Eumaeini) SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE hairstreaks; false head hypothesis; Cycnus AB A species level phylogenetic analysis of Panthiades Hubner was performed using twelve characters of wing pattern, androconia, and male and female genitalia. The purposes were to determine whether Panthiades is monophyletic without Cycnus Hubner and to provide a cladogram for a project on the evolution of "false head" wing patterns. Parsimony analysis with all characters unordered yielded two trees. One was the strict consensus of the two trees, and the other was the only most parsimonious tree when one of the multi-state characters was ordered. Panthiades is characterized by five hypothesized synapomorphies. If Cycnus is recognized, Panthiades is not monophyletic on either of the most parsimonious cladograms. The "classic" false head wing patterns in Panthiades appear to have evolved once. C1 Smithsonian Inst, Dept Entomol, Washington, DC 20013 USA. RP Robbins, RK (reprint author), Smithsonian Inst, Dept Entomol, POB 37012,NHB Stop 127, Washington, DC 20013 USA. EM RobbinsR@SI.edu NR 18 TC 1 Z9 3 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 JUL PY 2005 VL 107 IS 3 BP 501 EP 509 PG 9 WC Entomology SC Entomology GA 942JC UT WOS:000230277700003 ER PT J AU Huang, YM AF Huang, YM TI Cornetius, a new subigenus of Aedes, and a redescription of Aedes (Cornetius) Cozi Cornet (Diptera : Culicidae) SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Cornetius; new subgenus; Aedes cozi; characteristics; systematics; Culicidae; Senegal AB Cornetius, a new subgenus of Aedes Meigen is characterized and diagnosed. Aedes cozi Cornet is removed from the subgenus Stegomyia Theobald and placed in the new monotypic subgenus Cornetius on the basis of a critical study of all known stages. The adult of both sexes, the pupa, and the larva of Ae. (Cornetius) cozi are described and illustrated. Its affinity to other subgenera of the genus Aedes is discussed. Information on type data, distribution, bionomics, and medical importance, and a taxonomic discussion of this species are presented. C1 Smithsonian Inst, Dept Entomol, Washington, DC 20013 USA. RP Huang, YM (reprint author), Smithsonian Inst, Dept Entomol, MRC 534,POB 37012, Washington, DC 20013 USA. EM huang.yiau-min@nmnh.si.edu NR 16 TC 4 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 JUL PY 2005 VL 107 IS 3 BP 517 EP 529 PG 13 WC Entomology SC Entomology GA 942JC UT WOS:000230277700005 ER PT J AU Smith, DR Stocks, IC AF Smith, DR Stocks, IC TI A new trigonalid wasp (Hymenoptera : Trigonalidae) from eastern north America SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE hyperparasitoid; parasitoid; wasp; Trigonalyidae AB Orthogonalys bella, n. sp., is described from Great Smoky Mountains National Park, Tennessee. It is the second species of Orthogonalys Schulz and the fifth species of Nearctic Trigonalidae. Characters separating it from Orthogonalys pulchella (Cresson) are given. C1 Smithsonian Inst, Natl Museum Nat Hist, USDA, PSI,Systemat Entomol Lab, Washington, DC 20013 USA. Clemson Univ, Dept Entomol Soils & Plant Sci, Clemson, SC 29634 USA. RP Smith, DR (reprint author), Smithsonian Inst, Natl Museum Nat Hist, USDA, PSI,Systemat Entomol Lab, POB 37012,MRC 168, Washington, DC 20013 USA. EM dsmith@sel.barc.usda.gov; istocks@clemson.edu NR 9 TC 3 Z9 4 U1 1 U2 3 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD JUL PY 2005 VL 107 IS 3 BP 530 EP 535 PG 6 WC Entomology SC Entomology GA 942JC UT WOS:000230277700006 ER PT J AU Jennings, JT Smith, DR AF Jennings, JT Smith, DR TI The taxonomic placement of several New World and Oriental gasteruptiid wasps (Hymenoptera : Gasteruptiidae) SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Hymenoptera; Gasteruptiidae; Gasteruptiinae; Gasteruption; Pseudofoenus ID HYPTIOGASTRINE WASPS; KIEFFER HYMENOPTERA; REVISION AB The generic placement of several New World and Oriental gasteruptiid wasps is reviewed. Based on a number of character states, including non-overlapping mandibles (when at rest), the presence of a trochantellus (prefemur) and an exserted ovipositor, and the pattern of the veins in the forewing, five species currently in Pseudofoenus are transferred to Gasteruption L.; namely G. longiceps (Kieffer 1910), n. comb., G. ceylonensis (Enderlein 1912), n. comb., G. maculicorne Cameron 1887, revised comb., G. sericeum Cameron 1887, revised comb., and G. tenuicolle Schletterer 1885, revised comb. In addition, G. longiceps (Kieffer 1910) is a junior secondary homonym of G. longiceps Kieffer 1904 and is renamed G. austini, n. name, and Pseudofoenus neotropicus Schrottky 1906 is placed as incertae sedis. C1 Univ Adelaide, Ctr Evolutionary Biol & Biodoversity, Glen Osmond, SA 5064, Australia. Univ Adelaide, Sch Agr & Wine, Glen Osmond, SA 5064, Australia. Smithsonian Inst, Natl Museum Nat Hist, USDA, Systemat Entonol Lab,PSI,Agr Res Serv, Washington, DC 20013 USA. RP Jennings, JT (reprint author), Univ Adelaide, Ctr Evolutionary Biol & Biodoversity, Waite Campus, Glen Osmond, SA 5064, Australia. EM john.jennings@adelaide.edu.au; dsmith@sel.barc.usda.gov NR 26 TC 3 Z9 4 U1 1 U2 9 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 JUL PY 2005 VL 107 IS 3 BP 686 EP 692 PG 7 WC Entomology SC Entomology GA 942JC UT WOS:000230277700023 ER PT J AU Barrows, EM McIntyre, AM Flint, OS AF Barrows, EM McIntyre, AM Flint, OS TI Alderfly (Neuroptera : Sialidae) flight periods, sex ratios, and habitat use in a Virginia freshwater tidal marsh, low forest, and their ecotones SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Neuroptera; Sialidae; alderflies; flight periods; sex ratios; freshwater marsh; low forest ID NORTH-AMERICA; LIFE-HISTORY; MEGALOPTERA AB Six Malaise traps, run from April 1998 through December 1999, obtained 3306 adult Sialis iola Ross (34% females) and one male S. mohri Ross in Dyke Marsh Preserve (DMP), Virginia. They flew from early April through early June. The abundance of S. iola significantly varied among a low forest, freshwater tidal marsh, and the forest-marsh ecotone, sometimes being significantly more common in the ecotone than other habitats. Malaise traps can be used efficiently to survey and monitor sialids in DMP and similar places. A thorough monitoring effort in the Preserve should include at least two traps in the three habitats and monitoring throughout sialid flight periods and the Preserve. C1 Georgetown Univ, Dept Biol, Lab Entomol & Biodivers, Washington, DC 20057 USA. Smithsonian Inst, Dept Entomol, Washington, DC 20013 USA. RP Barrows, EM (reprint author), Georgetown Univ, Dept Biol, Lab Entomol & Biodivers, Reiss Bldg Suite 406,Box 571229, Washington, DC 20057 USA. EM barrowse@georgetown.edu; flinto@si.edu NR 17 TC 3 Z9 4 U1 0 U2 1 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD JUL PY 2005 VL 107 IS 3 BP 693 EP 699 PG 7 WC Entomology SC Entomology GA 942JC UT WOS:000230277700024 ER PT J AU Woodley, NE AF Woodley, NE TI Distributional notes on Bertamyia notata (Loew), including the first report of the family Platypezidae from the Caribbean (Diptera : Platypezidae) SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article C1 Smithsonian Inst, USDA, ARS, Systemat Entomol Lab, Washington, DC 20013 USA. RP Woodley, NE (reprint author), Smithsonian Inst, USDA, ARS, Systemat Entomol Lab, NHB-168,POB 37012, Washington, DC 20013 USA. RI Woodley, Norman/M-6160-2014 NR 5 TC 1 Z9 1 U1 0 U2 3 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD JUL PY 2005 VL 107 IS 3 BP 731 EP 732 PG 2 WC Entomology SC Entomology GA 942JC UT WOS:000230277700027 ER PT J AU Henry, TJ Ferreira, PSF AF Henry, TJ Ferreira, PSF TI Froeschneropsidea, a replacement name for the preoccupied genus Froeschnerisca (Hemiptera : Heteroptera : Miridae : Deraeocorinae : hyaliodini) SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article C1 Smithsonian Inst, Natl Museum Nat Hist, USDA, Agr Res Serv,Plant Sci Inst,Systemat Entomol Lab, Washington, DC 20013 USA. Univ Fed Vicosa, Dept Biol Anim, BR-36571000 Vicosa, MG, Brazil. RP Henry, TJ (reprint author), Smithsonian Inst, Natl Museum Nat Hist, USDA, Agr Res Serv,Plant Sci Inst,Systemat Entomol Lab, POB 37012, Washington, DC 20013 USA. EM thenry@sel.barc.usda.gov; pfiuza@ufv.br NR 4 TC 0 Z9 0 U1 0 U2 0 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD JUL PY 2005 VL 107 IS 3 BP 735 EP 735 PG 1 WC Entomology SC Entomology GA 942JC UT WOS:000230277700029 ER PT J AU Clarke, GKC Leverington, DW Teller, JT Dyke, AS Marshall, SJ AF Clarke, GKC Leverington, DW Teller, JT Dyke, AS Marshall, SJ TI Fresh arguments against the Shaw megaflood hypothesis. A reply to comments by David Sharpe on "Paleohydraulics of the last outburst flood from glacial Lake Agassiz and the 8200 BP cold event" SO QUATERNARY SCIENCE REVIEWS LA English DT Letter ID LAURENTIDE ICE-SHEET; CONTINUUM MIXTURE MODEL; SUBGLACIAL BEDFORMS; GREENLAND ICE; DRUMLINS; STREAM; THERMOMECHANICS; PALEOHYDROLOGY; EVOLUTION; MISSOULA C1 Univ British Columbia, Vancouver, BC V6T 1Z4, Canada. Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. Univ Manitoba, Dept Geol Sci, Winnipeg, MB R3T 2N2, Canada. Geol Survey Canada, Terrain Sci Div, Ottawa, ON K1A 0E8, Canada. Univ Calgary, Dept Geog, Calgary, AB T2N 1N4, Canada. RP Clarke, GKC (reprint author), Univ British Columbia, 6339 Stores Rd, Vancouver, BC V6T 1Z4, Canada. EM clarke@eos.ubc.ca; LeveringtonD@nasm.si.edu; tellerjt@ms.umanitoba.ca; ADyke@NRCan.gc.ca; marshals@ucalgary.ca NR 48 TC 38 Z9 38 U1 4 U2 21 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0277-3791 J9 QUATERNARY SCI REV JI Quat. Sci. Rev. PD JUL PY 2005 VL 24 IS 12-13 BP 1533 EP 1541 DI 10.1016/j.quascirev.2004.12.003 PG 9 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA 933PZ UT WOS:000229646700015 ER PT J AU Parenti, LR Lim, KKP AF Parenti, LR Lim, KKP TI Fishes of the Rajang basin, Sarawak, Malaysia SO RAFFLES BULLETIN OF ZOOLOGY LA English DT Review DE Fish diversity; species checklist; new records; Rajang basin; Sarawak; Borneo ID CYPRINID FISH; SYSTEMATIC REVISION; WEST KALIMANTAN; SOUTHEAST-ASIA; TELEOSTEI; BORNEO; CATFISH; PERCIFORMES; COBITIDAE; BLEEKER AB An annotated checklist of the fishes recorded from the Rajang basin in Sarawak, Malaysian Borneo, from its headwaters to the brackish waters near its mouth, is presented. At least 164 species are recorded, collected mainly by several recent expeditions to Belaga and the Balui River, Kapit and the Batch River, and around Sibu. Sixty-four fish species are recorded for the first time in the Rajang basin, two of which (Pangio piperata and Macrognathus circumcinctus) are new records for Borneo. The list should be treated as preliminary as many areas in the Rajang system have not been sampled. The list fills a critical gap in our knowledge of the fishes of Sarawak and includes the first report on fishes of the Batang Balui, a headwater tributary of the Rajang. C1 Smithsonian Inst, Natl Museum Nat Hist, Div Fishes, Dept Vertebrate Zool, Washington, DC 20560 USA. Natl Univ Singapore, Raffles Museum Biodivers REs, Dept Biol Sci, Singapore 119260, Singapore. RP Parenti, LR (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Div Fishes, Dept Vertebrate Zool, Washington, DC 20560 USA. EM parenti.lynne@nmnh.si.edu; dbslimkp@nus.edu.sg NR 189 TC 5 Z9 7 U1 1 U2 5 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 JUL 1 PY 2005 SU 13 BP 175 EP 208 PG 34 WC Zoology SC Zoology GA 955WE UT WOS:000231257500012 ER PT J AU Spangler, PJ Steiner, WE AF Spangler, PJ Steiner, WE TI A new aquatic beetle family, Meruidae, from Venezuela (Coleoptera : Adephaga) SO SYSTEMATIC ENTOMOLOGY LA English DT Article ID 18S RIBOSOMAL-RNA; SYSTEMATIC POSITION; HALIPLIDAE-COLEOPTERA; MORPHOLOGY; GYRINIDAE; PHYLOGENY; EVOLUTION; INSECTA AB An unknown beetle collected in the Territorio Federal Amazonas, Venezuela, and designated as belonging to a new family, is described (as Meru phyllisaegen.n., sp.n.) and illustrated by line drawings and scanning electron micrographs. The new family, Meruidae, is diagnosed and assigned to the suborder Adephaga with a discussion of some characters and likely phylogenetic affinities. With a body length of 0.85-0.9 mm, M. phyllisae is the smallest known member of aquatic Adephaga. Based on the observed skeletal and behavioural characters to date, the taxon appears to represent the sister clade to the remaining families of Dytiscoidea, but also has features suggesting a close relationship among Noteridae and/or Haliplidae. A description and photographs of the habitat are included, with a list of other associated water beetle taxa. Some observations on the behaviour of captive beetles are given. The minute 'comb-clawed cascade beetles' are known only from the type locality, El Tobogan, where streams flow among exposed areas of bedrock in the geologically ancient Guyana Shield region. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20560 USA. RP Steiner, WE (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, NHB-187, Washington, DC 20560 USA. EM steinerw@si.edu NR 33 TC 33 Z9 35 U1 1 U2 5 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0307-6970 J9 SYST ENTOMOL JI Syst. Entomol. PD JUL PY 2005 VL 30 IS 3 BP 339 EP 357 DI 10.1111/j.1365-3113.2005.00288.x PG 19 WC Evolutionary Biology; Entomology SC Evolutionary Biology; Entomology GA 942LX UT WOS:000230285000001 ER PT J AU Brown, JK AF Brown, JK TI Photography on the color line: W. E. B. DuBois, race, and visual culture. SO TECHNOLOGY AND CULTURE LA English DT Book Review C1 Smithsonian Inst, Amer Museum Nat Hist, Washington, DC 20560 USA. RP Brown, JK (reprint author), Smithsonian Inst, Amer Museum Nat Hist, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 1 U2 1 PU JOHNS HOPKINS UNIV PRESS PI BALTIMORE PA JOURNALS PUBLISHING DIVISION, 2715 NORTH CHARLES ST, BALTIMORE, MD 21218-4363 USA SN 0040-165X J9 TECHNOL CULT JI Technol. Cult. PD JUL PY 2005 VL 46 IS 3 BP 687 EP 688 DI 10.1353/tech.2005.0115 PG 2 WC History & Philosophy Of Science SC History & Philosophy of Science GA 961LB UT WOS:000231662800046 ER PT J AU Agnarsson, I AF Agnarsson, I TI Revision and phylogenetic analysis of American ethicus and rupununi groups of Anelosimus (Araneae, Theridiidae) SO ZOOLOGICA SCRIPTA LA English DT Article ID SUBSOCIAL SPIDER; SOCIAL SPIDERS; MISSING DATA; SEX-RATIO; BEHAVIOR; LIMITS AB Two species groups of the social spider genus Anelosimus are revised. The ethicus group contains six species found in South America, in an area ranging from the Guianas to southern Brazil and Argentina. Of these, A. rabus Levi, 1963, A. ethicus (Keyserling, 1884), and A. nigrescens (Keyserling, 1884) are redescribed, while A. nigrescens is removed from synonymy with A. ethicus. Three new species are described: A. misiones sp. nov., A. sumisolena sp. nov. and A. inhandava sp. nov. Anelosimus ethicus is reportedly either subsocial or solitary, while the behaviour of the other species in the group is unknown. The rupununi group contains two quasisocial species, A. rupununi Levi, 1956 and A. lorenzo Fowler & Levi, 1979, from the Caribbean and tropical South America. Both are redescribed here. A parsimony analysis of morphological characters provides support for the monophyly of both groups. In the phylogeny, subsociality optimizes to the base of Anelosimus, indicating that the common ancestor of the ethicus group was subsocial. Its members can thus be predicted to be subsocial, or secondarily solitary. Quasisociality arose de novo in the rupununi group, representing one of 6-7 independent origins in theridiids. Study of the biology of Anelosimus is important to advance our understanding of the evolution of sociality in spiders. C1 Smithsonian Inst, Washington, DC 20013 USA. George Washington Univ, Dept Biol Sci, Washington, DC 20052 USA. RP Agnarsson, I (reprint author), Univ British Columbia, Dept Bot, 3529-6270 Univ Blvd, Vancouver, BC V6T 1Z4, Canada. EM ingi@zoology.ubc.ca NR 39 TC 26 Z9 28 U1 0 U2 7 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0300-3256 J9 ZOOL SCR JI Zool. Scr. PD JUL PY 2005 VL 34 IS 4 BP 389 EP 413 DI 10.1111/j.1463-6409.2005.00189.x PG 25 WC Evolutionary Biology; Zoology SC Evolutionary Biology; Zoology GA 938ZA UT WOS:000230040700004 ER PT J AU Reynolds, DR Gilbert, GS AF Reynolds, DR Gilbert, GS TI Epifoliar fungi from Queensland, Australia SO AUSTRALIAN SYSTEMATIC BOTANY LA English DT Review ID SOOTY MOLDS; MORPHOLOGY; REVISION; LEPTOXYPHIUM; SEURATIACEAE; TAXONOMY AB Collections of epifoliar ascomycete fungi from leaf surfaces in the tropical rain forests of Queensland, Australia, yielded 42 genera and 50 species, including one new genus (Dubujiana), three new species (Dennisiela asetosa, Dubujiana glandulifera, Microxiphium pleomorphum), three new combinations (Polychaeton purpuraefaciens, Seuratia australiensis, Stomiopeltis gautheriae), lectotypi. cation of Micropeltis biseptata, various emended descriptions, and new species records. Each species is described and compared with similar taxa, and the new species are illustrated. C1 Los Angeles Cty Museum Nat Hist, Res & Collect, LAC, Los Angeles, CA 90007 USA. Univ Calif Santa Cruz, Santa Cruz, CA 95064 USA. Smithsonian Trop Res Inst, Balboa, Panama. RP Reynolds, DR (reprint author), Los Angeles Cty Museum Nat Hist, Res & Collect, LAC, 900 Exposit Blvd, Los Angeles, CA 90007 USA. EM dreynold@nhm.org NR 144 TC 19 Z9 21 U1 0 U2 2 PU C S I R O PUBLISHING PI COLLINGWOOD PA 150 OXFORD ST, PO BOX 1139, COLLINGWOOD, VICTORIA 3066, AUSTRALIA SN 1030-1887 J9 AUST SYST BOT JI Aust. Syst. Bot. PD JUN 30 PY 2005 VL 18 IS 3 BP 265 EP 289 DI 10.1071/SB04030 PG 25 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA 940KR UT WOS:000230143900003 ER PT J AU Ardila, NE Fauchald, K Lattig, P AF Ardila, NE Fauchald, K Lattig, P TI Eunice colombia (Eunicidae : Polychaeta), a new species from the southern Caribbean SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article AB Eunice colombia, a new species collected on the northern Caribbean coast of Colombia at depths of 300 and 500 in in soft bottoms, is described. The shape of the posterior ventral cirri, the position of the branchiae, and their length in relation to that of the notopodial cirri are the main differences from congeneric species. C1 INVEMAR, Museo Hist Nat Marina, Inst Invest Marinas, Santa Marta 1016, Colombia. Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. Univ Autonoma Madrid, Dept Biol Zool, E-28049 Madrid, Spain. RP Ardila, NE (reprint author), INVEMAR, Museo Hist Nat Marina, Inst Invest Marinas, Santa Marta 1016, Colombia. EM neardila@yahoo.com; Fauchaldk@si.edu; patricia.lattig@uam.es NR 8 TC 2 Z9 2 U1 0 U2 3 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD JUN 29 PY 2005 VL 118 IS 2 BP 259 EP 263 DI 10.2988/0006-324X(2005)118[259:ECEPAN]2.0.CO;2 PG 5 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 941OF UT WOS:000230223400003 ER PT J AU Ardila, NE Harasewych, MG AF Ardila, NE Harasewych, MG TI Cocculinid and pseudococculinid limpets (Gastropoda : Cocculiniformia) from off the Caribbean coast of Colombia SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article ID MOLLUSCA; ARCHAEOGASTROPODA; SYSTEMATICS; PHYLOGENY; BRAZIL AB The present paper reports on the occurrence of six species of Cocculinidae and three species of Pseudococculinidae off the Caribbean coast of Colombia. Cocculina messingi McLean & Harasewych, 1995, Cocculina emsoni McLean & Harasewych, 1995 Notocrater houbricki McLean & Harasewych, 1995 and Notocrater youngi McLean & Harasewych, 1995 were not previously known to occur within the of the Caribbean Sea, while Fedikovella beanii (Dall, 1882) had been reported only from the western margins of the Atlantic Ocean, including the lesser Antilles. New data are presented on the external anatomy and radular morphology of Coccocrater portoricensis (Dall & Simpson, 1901) that supports its placement in the genus Coccocrater. Cocculina fenestrata n. sp. (Cocculinidae) and Copulabyssia colombia n. sp. (Pseudococculinidae) are described from the upper continental slope of Caribbean Colombia. C1 INVEMAR, Museo Hist Nat Marina Colombia, Inst Invest Marinas, Santa Marta 1016, Colombia. Natl Museum Nat Hist, Dept Invertebrate Zool, Smithsonian Inst, Washington, DC 20013 USA. RP Ardila, NE (reprint author), INVEMAR, Museo Hist Nat Marina Colombia, Inst Invest Marinas, Santa Marta 1016, Colombia. EM neardila@yahoo.com; Harasewych@si.edu NR 32 TC 4 Z9 6 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 JUN 29 PY 2005 VL 118 IS 2 BP 344 EP 366 DI 10.2988/0006-324X(2005)118[344:CAPLGC]2.0.CO;2 PG 23 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 941OF UT WOS:000230223400012 ER PT J AU Orrell, TM Weigt, L AF Orrell, TM Weigt, L TI The northern snakehead Channa argus (Anabantomorpha : Channidae), a non-indigenous fish species in the Potomac River, USA SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article ID DNA AB Mitochondrial sequence variation was examined in the northern snakehead, Channa argus (Cantor, 1842), a species of fish native to Asia and recently collected in the eastern United States. There are seven unique haplotypes in 29 specimens studied, with no haplotype shared between areas of introduction. One haplotype was shared by 15 individuals from the Potomac River system (both males and females < 480 mm total length), indicating possible breeding within the system. A single large adult male from the Potomac River system has a unique haplotype. All Crofton, Maryland, specimens had one haplotype. Two haplotypes were found in Meadow Lake, FDR Park, Philadelphia, Pennsylvania. Unique haplotypes were found in Wheaton, Maryland, and Shrewsbury, Massachusetts. These results support the conclusion that there were several independent introductions of the northern snakehead into these waters, and that no two introductions came from the same maternal source. C1 Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20013 USA. Smithsonian Inst, Labs Analyt Biol, Suitland, MD 20746 USA. RP Orrell, TM (reprint author), Natl Museum Nat Hist, Smithsonian Inst, POB 37012, Washington, DC 20013 USA. EM orrellt@si.edu; lweigt@lab.si.edu NR 15 TC 11 Z9 13 U1 3 U2 36 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 JUN 29 PY 2005 VL 118 IS 2 BP 407 EP 415 DI 10.2988/0006-324X(2005)118[407:TNSCAA]2.0.CO;2 PG 9 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 941OF UT WOS:000230223400014 ER PT J AU Scully, SWJ Aguilar, A Emmons, ED Phaneuf, RA Halka, M Leitner, D Levin, JC Lubell, MS Puttner, R Schlachter, AS Covington, AM Schippers, S Muller, A McLaughlin, BM AF Scully, SWJ Aguilar, A Emmons, ED Phaneuf, RA Halka, M Leitner, D Levin, JC Lubell, MS Puttner, R Schlachter, AS Covington, AM Schippers, S Muller, A McLaughlin, BM TI K-shell photoionization of Be-like carbon ions: experiment and theory for C2+ SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS LA English DT Article ID CROSS-SECTIONS; ISOELECTRONIC SEQUENCE; C-III; AUGER; IONIZATION; BERYLLIUM; RECOMBINATION; FLUORESCENCE; SPECTROSCOPY; SCATTERING AB Absolute cross-section measurements for K-shell photoionization of Be-like C2+ ions have been performed in the photon energy range 292-325 eV. These measurements have been made using the photon-ion merged-beam endstation at the Advanced Light Source, Lawrence Berkeley National Laboratory. Absolute measurements compared with theoretical results from the R-matrix method indicate that the primary C2+ ion beam consisted of 62% groundstate (1s(2)2S(2) S-1) and 38% metastable state (1s(2)2s(2)p (3)p(o)) ions. Reasonable agreement is seen between theory and experiment for absolute photoionization cross sections, resonance energies and autoionization linewidths of K-shell-vacancy Auger states. C1 Univ Nevada, Dept Phys, Reno, NV 89557 USA. Lawrence Berkeley Lab, Berkeley, CA 94720 USA. Embry Riddle Aeronaut Univ, Prescott, AZ 86329 USA. Univ Tennessee, Dept Phys & Astron, Knoxville, TN 37996 USA. CUNY City Coll, Phys Dept, New York, NY 10031 USA. Free Univ Berlin, Inst Experimentalphys d, D-14195 Berlin, Germany. Univ Giessen, Inst Atom & Molekulphys, D-35392 Giessen, Germany. Harvard Univ, Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. RP Scully, SWJ (reprint author), Univ Nevada, Dept Phys, MS 220, Reno, NV 89557 USA. EM s.scully@qub.ac.uk; b.mclaughlin@qub.ac.uk RI Muller, Alfred/A-3548-2009; Schippers, Stefan/A-7786-2008 OI Muller, Alfred/0000-0002-0030-6929; Schippers, Stefan/0000-0002-6166-7138 NR 46 TC 29 Z9 29 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 JUN 28 PY 2005 VL 38 IS 12 BP 1967 EP 1975 DI 10.1088/0953-4075/38/12/011 PG 9 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 959JF UT WOS:000231513300013 ER PT J AU Diaz, MC Van Soest, RWM Rutzler, K Guzman, HM AF Diaz, MC Van Soest, RWM Rutzler, K Guzman, HM TI Aplysina chiriquiensis, a new pedunculate sponge from the Gulf of Chiriqui, Panama, Eastern Pacific (Aplysinidae, Verongida) SO ZOOTAXA LA English DT Article DE Aplysina; taxonomy; new species; Porifera; Eastern Pacific Ocean AB A new pedunculate aplysinid sponge, Aplysina chiriquiensis, is described from shallow waters (1.5 - 35 m) in the Gulf of Chiriqui, western Panama, Eastern Pacific. The species chiriquiensis is a common component of coral reefs and soft coral reefs in that region. After examining the systematic status of related taxa we conclude that there are only two valid taxa of stalked Aplysina, A. bathyphila Maldonado and Young from the Caribbean, and our new species from the eastern Pacific. A. chiriquiensis a yellow to purplish, stalked and branching sponge with oscules arranged in one or more rows along the branches. The branches can be cylindrical with smooth tapering ends, or stubby and laterally compressed. A. chiriquiensis is the first Aplysina species described from Panama and its distribution elsewhere in tropical and subtropical Eastern Pacific has yet to be evaluated. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Zool, Washington, DC 20560 USA. Museo Marino Margarita, Nueva Esparta, Venezuela. Univ Amsterdam, Museum Zool, NL-1090 GT Amsterdam, Netherlands. Smithsonian Trop Res Inst, Balboa, Panama. RP Diaz, MC (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Zool, Washington, DC 20560 USA. EM crisdiaz@ix.netcom.com; guzmanh@naos.si.edu NR 20 TC 3 Z9 4 U1 1 U2 1 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD JUN 28 PY 2005 IS 1012 BP 1 EP 12 PG 12 WC Zoology SC Zoology GA 940MX UT WOS:000230149700001 ER PT J AU Woodley, NE AF Woodley, NE TI Dacochile microsoma Poinar & Brown, not a tanyderid but a bruchomyiine psychodid (Diptera : Psychodidae, Tanyderidae) SO ZOOTAXA LA English DT Article DE Diptera; Tanyderidae; Psychodidae; Bruchomyiinae; fossil; Burmese amber ID BURMESE AMBER AB A review of the characters used by Poinar & Brown (2004) to place their new fossil fly from Burmese amber, Dacochile microsoma, in the family Tanyderidae conclusively demonstrates that the fly actually belongs to the subfamily Bruchomyiinae in the family Psychodidae. C1 USDA ARS, Smithsonian Institut, Systemat Entomol Lab, Washington, DC 20560 USA. RP Woodley, NE (reprint author), USDA ARS, Smithsonian Institut, Systemat Entomol Lab, NHB-168, Washington, DC 20560 USA. EM nwoodley@sel.barc.usda.gov RI Woodley, Norman/M-6160-2014 NR 22 TC 10 Z9 11 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 JUN 28 PY 2005 IS 1012 BP 53 EP 60 PG 8 WC Zoology SC Zoology GA 940MX UT WOS:000230149700006 ER PT J AU Narita, N Suto, Y Winn, JN Turner, EL Aoki, W Leigh, CJ Sato, B Tamura, M Yamada, T AF Narita, N Suto, Y Winn, JN Turner, EL Aoki, W Leigh, CJ Sato, B Tamura, M Yamada, T TI Subaru HDS transmission spectroscopy of the transiting extrasolar planet HD 209458b SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN LA English DT Article DE stars : planetary systems : individual (HD 209458b); techniques : spectroscopic ID GRAVITATIONAL LENSING EXPERIMENT; LUMINOSITY OBJECT TRANSITS; GALACTIC DISK; 2001 CAMPAIGN; SEARCH; ATMOSPHERE; ABSORPTION; EXOSPHERE; SPECTRUM; PHOTOMETRY AB We have searched for absorption in several common atomic species due to the atmosphere or exosphere of the transiting extrasolar planet HD 209458b, using high precision optical spectra obtained with the Subaru High Dispersion Spectrograph (HDS). Previously we reported an Lipper limit on Ha absorption of 0.1% (3 sigma) within a 5.1 angstrom band. Using the same procedure, we now report upper limits on absorption due to the optical transitions of Na D, Li. H alpha, H beta, H gamma, Fe, and Ca. The 3 sigma upper limit for each transition is approximately 1% within a 0.3 angstrom band (the core of the line), and a few tenths of a per cent within a 2 angstrom band (the full line width). The wide-band results are close to the expected limit due to photon-counting (Poisson) statistics, although in the narrow-band case we have encountered unexplained systematic errors at a few times the Poisson level. These results are consistent with all previously reported detections and upper limits, but are significantly more sensitive. C1 Univ Tokyo, Sch Sci, Dept Phys, Tokyo 1130033, Japan. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Princeton Univ Observ, Princeton, NJ 08544 USA. Natl Astron Observ, Mitaka, Tokyo 1818588, Japan. Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England. Kobe Univ, Grad Sch Sci & Technol, Nada Ku, Kobe, Hyogo 6578501, Japan. RP Univ Tokyo, Sch Sci, Dept Phys, Tokyo 1130033, Japan. EM narita@utap.phys.s.u-tokyo.ac.jp; suto@phys.s.u-tokyo.ac.jp; jwinn@cfa.harvard.edu; elt@astro.princeton.edu; aoki.wako@nao.ac.jp; cjl@astro.livjm.ac.uk; satobn@kobe-u.ac.jp; tamurant@cc.nao.ac.jp; yamada@optik.mtk.nao.ac.jp RI Turner, Edwin/A-4295-2011 NR 32 TC 39 Z9 39 U1 1 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0004-6264 EI 2053-051X J9 PUBL ASTRON SOC JPN JI Publ. Astron. Soc. Jpn. PD JUN 25 PY 2005 VL 57 IS 3 BP 471 EP 480 DI 10.1093/pasj/57.3.471 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 946BQ UT WOS:000230547400010 ER PT J AU Verling, E Ruiz, GM Smith, LD Galil, B Miller, AW Murphy, KR AF Verling, E Ruiz, GM Smith, LD Galil, B Miller, AW Murphy, KR TI Supply-side invasion ecology: characterizing propagule pressure in coastal ecosystems SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE biological invasion; ballast water; propagule supply; survivorship; shipping patterns ID BALLAST WATER; BIOLOGICAL INVASIONS; MARINE ORGANISMS; INVADERS; INTRODUCTIONS; INVASIBILITY; PATTERNS; HISTORY; SHIPS AB The observed rates and deleterious impacts of biological invasions have caused significant alarm in recent years, driving efforts to reduce the risk (establishment) of new introductions. Characterizing the supply of propagules is key to understanding invasion risk and developing effective management strategies. In coastal ecosystems, ships' ballast water is an important transfer mechanism (vector) for marine and freshwater species. Commercial ships exhibit a high degree of variation in ballast water operations that affect both the quantity and quality of propagule supply, and thereby invasion risk. The per-ship inoculation size from ballast water depends upon both the volume discharged and the organism density. Moreover, propagule quality will vary among source regions (ports) and voyage routes, due to differences in species composition and transport conditions, respectively. We show that significant differences exist in (i) the frequency and volume of ballast water discharge among vessel types, (ii) the frequency of vessel types and routes (source regions) among recipient ports, and (iii) the transit success (survivorship) of zooplankton in ballast tanks among voyage routes. Thus, propagule supply is not a simple function of total ship arrivals. For ships, as well as other vectors, variation in propagule quantity and quality must be explicitly considered to estimate invasion risk and advance predictive ability. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Smith Coll, Dept Biol Sci & Environm Sci, Northampton, MA 01063 USA. Israel Oceanog & Limnol Res, IL-31080 Haifa, Israel. RP Verling, E (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM verlinge@si.edu RI Murphy, Kathleen/B-8217-2009; OI Murphy, Kathleen/0000-0001-5715-3604; Ruiz, Gregory/0000-0003-2499-441X; Miller, Whitman/0000-0003-0484-182X NR 33 TC 82 Z9 89 U1 1 U2 29 PU ROYAL SOCIETY PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8452 J9 P ROY SOC B-BIOL SCI JI Proc. R. Soc. Lond. Ser. B-Biol. Sci. PD JUN 22 PY 2005 VL 272 IS 1569 BP 1249 EP 1256 DI 10.1098/rspb.2005.3090 PG 8 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 946HO UT WOS:000230563200008 PM 16024389 ER PT J AU Rossi, S Homan, J Miller, JM Belloni, T AF Rossi, S Homan, J Miller, JM Belloni, T TI Iron-line and continuum flux variations in the RXTE spectra of the black hole candidate XTE J1650-500 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; black hole physics; relativity; X-rays : individual : XTE J1650-500; X-rays : stars ID X-RAY REFLECTION; ACTIVE GALACTIC NUCLEI; ALPHA EMISSION-LINE; TIMING EXPLORER; TRANSIENT XTE-J1650-500; GALAXY MCG-6-30-15; ACCRETION DISK; XMM-NEWTON; OUTBURST; PERFORMANCE AB We present the results of spectral fits made to 57 pointed observations of the Galactic black hole candidate and X-ray transient XTE J1650-500, made with the Rossi X-ray Timing Explorer (RXTE) in 2001 when the source was in a transition from the hard state to the soft state. A strong and variable Fe K alpha emission line is detected in these spectra. The line flux varies in a non-linear way with the hard X-ray flux, in apparent contradiction to the predictions of simple disc reflection models. We observe a change in the overall trend that coincides with changes in the continuum X-ray spectrum and the fast X-ray variability. The Fe-line flux versus hard X-ray flux variations are consistent with the predictions of reflection models that consider high disc-ionization states and with a model that considers gravitational light-bending effects. Indications for an anticorrelation between the Fe-line flux and the hard X-ray flux in the spectrally hardest observations and weak variations in the Fe-line energy (as observed with XMM-Newton and BeppoSAX) slightly favour the light-bending interpretation. C1 Osserv Astron Brera, Merate, Italy. Univ Milano Bicocca, I-20126 Milan, Italy. MIT, Ctr Space Res, Cambridge, MA 02139 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Rossi, S (reprint author), Osserv Astron Brera, Via E Bianchi 46, Merate, Italy. EM srossi@merate.mi.astro.it; jeroen@space.mit.edu NR 38 TC 42 Z9 42 U1 0 U2 0 PU BLACKWELL PUBLISHING 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 JUN 21 PY 2005 VL 360 IS 2 BP 763 EP 768 DI 10.1111/j.1365-2966.2005.09069.x PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 933OM UT WOS:000229642800033 ER PT J AU Silver, E Austin, G Beeman, J Goulding, F Haller, EE Landis, D Madden, N AF Silver, E Austin, G Beeman, J Goulding, F Haller, EE Landis, D Madden, N TI An NTD germanium-based microcalorimeter with 3.1 eV energy resolution at 6 keV SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT LA English DT Article DE microcalorimeter; X-ray spectroscopy ID X-RAY; SPECTROMETERS AB This paper reports recent advances in our microcalorimeter spectrometer that result in an energy resolution of 3.1 eV FWHM for 6keV X-rays. We have developed a detailed model that indicates that further minor improvements will realize 2eV FWHM at 6keV and well under 2eV at I keV. The results demonstrate the value of the microcalorimeter for many applications where a premium exists for very fine resolution in the 0.2-10 keV energy band. (c) 2005 Elsevier B.V. All rights reserved. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. Lawrence Berkeley Lab, Berkeley, CA 94720 USA. Univ Calif Berkeley, Dept Mat Sci & Engn, Berkeley, CA 94720 USA. Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. RP Silver, E (reprint author), Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. EM esilver@cfa.harvard.edu NR 8 TC 15 Z9 15 U1 0 U2 1 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0168-9002 J9 NUCL INSTRUM METH A JI Nucl. Instrum. Methods Phys. Res. Sect. A-Accel. Spectrom. Dect. Assoc. Equip. PD JUN 21 PY 2005 VL 545 IS 3 BP 683 EP 689 DI 10.1016/j.nima.2005.02.024 PG 7 WC Instruments & Instrumentation; Nuclear Science & Technology; Physics, Nuclear; Physics, Particles & Fields SC Instruments & Instrumentation; Nuclear Science & Technology; Physics GA 942FJ UT WOS:000230268000014 ER PT J AU Wilf, P Labandeira, CC Johnson, KR Cuneo, NR AF Wilf, P Labandeira, CC Johnson, KR Cuneo, NR TI Richness of plant-insect associations in eocene patagonia: A legacy for south American biodiversity SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE paleobotany; Argentina; herbivory; Laguna del Hunco; paleoecology ID SPECIES RICHNESS; AMAZONIAN FORESTS; RIVER FORMATION; DIVERSITY; COEVOLUTION; HERBIVORY; LEPIDOPTERA; COMMUNITIES; BUTTERFLIES; ARGENTINA AB South America has some of the most diverse floras and insect faunas that are known, but its Cenozoic fossil record of insects and insect herbivory is sparse. We quantified insect feeding on 3,599 leaves from the speciose Laguna del Hunco flora (Chubut, Argentina), which dates to the early Eocene climatic optimum (52 million years ago) and compared the results with three well preserved, rich, and identically analyzed early- and middle-Eocene floras from the following sites in North America: Republic, WA; Green River, LIT; and Sourdough, WY. We found significantly more damage diversity at Laguna del Hunco than in the North American floras, whether measured on bulk collections or on individual plant species, for both damage morphotypes and feeding groups. An ancient history of rich, specialized plant-insect associations on diverse plant lineages in warm climates may be a major factor contributing to the current biodiversity of South America. C1 Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. Smithsonian Inst, Dept Paleobiol, Washington, DC 20013 USA. Univ Maryland, Dept Entomol, College Pk, MD 20742 USA. Denver Museum Nat & Sci, Dept Earth Sci, Denver, CO 80205 USA. Museo Paleontol Egidio Feruglio, RA-9100 Chubut, Argentina. RP Wilf, P (reprint author), Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. EM pvvilf@psu.edu NR 64 TC 57 Z9 61 U1 0 U2 10 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 JUN 21 PY 2005 VL 102 IS 25 BP 8944 EP 8948 DI 10.1073/pnas.0500516102 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 939CI UT WOS:000230049500030 PM 15956213 ER PT J AU Shapley, AE Steidel, CC Erb, DK Reddy, NA Adelberger, KL Pettini, M Barmby, P Huang, JS AF Shapley, AE Steidel, CC Erb, DK Reddy, NA Adelberger, KL Pettini, M Barmby, P Huang, JS TI Ultraviolet to mid-infrared observations of star-forming galaxies at z similar to 2: Stellar masses and stellar populations SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : observations; galaxies : evolution; galaxies : high-redshift; galaxies : starburst; stars : formation ID LYMAN BREAK GALAXIES; HUBBLE DEEP FIELD; HIGH-REDSHIFT GALAXIES; GOODS-NORTH FIELD; MASSIVE GALAXIES; PHOTOMETRIC REDSHIFTS; SPACE-TELESCOPE; FORMATION EPOCH; RED GALAXIES; TO 2.5 AB We present the broadband UV through mid-infrared spectral energy distributions (SEDs) of a sample of 72 spectroscopically confirmed star-forming galaxies at z = 2.30 +/- 0.3. Located in a 72 arcmin(2) field centered on the bright background QSO, HS 1700+643, these galaxies were preselected to lie at z similar to 2 solely on the basis of their rest-frame UV colors and luminosities and should be representative of UV-selected samples at high redshift. In addition to deep ground-based photometry spanning from 0.35 to 2.15 mu m, we make use of Spitzer IRAC data, which probe the rest-frame near-IR at z similar to 2. The range of stellar populations present in the sample is investigated with simple, single-component stellar population synthesis models. The inability to constrain the form of the star formation history limits our ability to determine the parameters of extinction, age, and star formation rate without using external multiwavelength information. Emphasizing stellar mass estimates, which are much less affected by these uncertainties, we find < logM(*)/M-circle dot> = 10.32 +/- 0.51 for the sample. The addition of Spitzer IRAC data as a long-wavelength baseline reduces stellar mass uncertainties by a factor of 1.5-2 relative to estimates based on optical-K-s photometry alone. However, the total stellar mass estimated for the sample is remarkably insensitive to the inclusion of IRAC data. We find correlations between stellar mass and rest-frame R band (observed K-s) and rest-frame 1.4 mu m ( observed 4.5 mu m) luminosities, although with significant scatter. Even at rest-frame 1.4 mu m, the mass-to-light ratio varies by a factor of 15 indicating that even the rest-frame near-IR, when taken alone, is a poor indicator of stellar mass in star-forming galaxies at z similar to 2. Allowing for the possibility of episodic star formation, we find that typical galaxies in our sample could contain up to 3 times more stellar mass in an old underlying burst than what was inferred from single-component modeling. In contrast, mass estimates for the most massive galaxies in the sample (M-* > 10(11) M-circle dot) are fairly insensitive to the method used to model the stellar population. Galaxies in this massive tail, which are also the oldest objects in the sample, could plausibly evolve into the passive galaxies discovered at z similar to 1.7 with near-IR selection techniques. In the general framework of hierarchical galaxy formation and mergers, which implies episodic star formation histories, galaxies at high redshift may pass in and out of UV-selected and near-IR color-selected samples as they evolve from phases of active star formation to quiescence and back again. C1 Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. CALTECH, Pasadena, CA 91125 USA. Carnegie Inst Washington Observ, Pasadena, CA 91101 USA. Inst Astron, Cambridge CB3 0HA, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Shapley, AE (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. RI Barmby, Pauline/I-7194-2016 OI Barmby, Pauline/0000-0003-2767-0090 NR 51 TC 264 Z9 264 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 JUN 20 PY 2005 VL 626 IS 2 BP 698 EP 722 DI 10.1086/429990 PN 1 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 935PU UT WOS:000229795000007 ER PT J AU Brand, K Dey, A Brown, MJI Watson, CR Jannuzi, BT Najita, JR Kochanek, CS Shields, JC Fazio, GG Forman, WR Green, PJ Jones, CJ Kenter, AT McNamara, BR Murray, SS Rieke, M Vikhlinin, A AF Brand, K Dey, A Brown, MJI Watson, CR Jannuzi, BT Najita, JR Kochanek, CS Shields, JC Fazio, GG Forman, WR Green, PJ Jones, CJ Kenter, AT McNamara, BR Murray, SS Rieke, M Vikhlinin, A TI Tracing the nuclear accretion history of the red galaxy population SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : observations; galaxies : active; galaxies : elliptical and lenticular; cD galaxies : evolution ID X-RAY-EMISSION; STAR-FORMATION RATE; ADVECTION-DOMINATED ACCRETION; SUPERMASSIVE BLACK-HOLES; ACTIVE GALACTIC NUCLEI; HUBBLE-SPACE-TELESCOPE; LYMAN BREAK GALAXIES; FIELD-NORTH SURVEY; ELLIPTIC GALAXIES; HOST GALAXIES AB We investigate the evolution of the hard X-ray luminosity of the red galaxy population using a large sample of 3316 red galaxies selected over a wide range in redshift (0.3 < z < 0.9) from a 1.4 deg(2) region in the Bootes field of the NOAO Deep Wide-Field Survey (NDWFS). The red galaxies are early-type, bulge-dominated galaxies and are selected to have the same evolution-corrected, absolute R-band magnitude distribution as a function of redshift to ensure that we are tracing the evolution in the X-ray properties of a comparable optical population. Using a stacking analysis of 5 ks Chandra/ACIS observations within this field to study the X-ray emission from these red galaxies in three redshift bins, we find that the mean X-ray luminosity increases as a function of redshift. The large mean X-ray luminosity and the hardness of the mean X-ray spectrum suggest that the X-ray emission is largely dominated by active galactic nuclei (AGNs) rather than stellar sources. The hardness ratio can be reproduced by either an absorbed (N-H approximate to 2 x 10(22) cm(-2)) Gamma = 1.7 power-law source, consistent with that of a population of moderately obscured Seyfert-like AGNs, or an unabsorbed Gamma = 0: 7 source, suggesting a radiatively inefficient accretion flow ( e. g., an advection-dominated accretion flow). We also find that the emission from this sample of red galaxies constitutes at least 5% of the hard X-ray background. These results suggest a global decline in the mean AGN activity of normal early-type galaxies from z similar to 1 to the present, which indicates that we are witnessing the tailing off of the accretion activity onto supermassive black holes in early-type galaxies since the quasar epoch. C1 Natl Opt Astron Observ, Tucson, AZ 85726 USA. Princeton Univ, Princeton, NJ 08544 USA. Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. Ohio Univ, Dept Phys & Astron, Athens, OH 45701 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. RP Brand, K (reprint author), Natl Opt Astron Observ, Tucson, AZ 85726 USA. RI Brown, Michael/B-1181-2015; OI Brown, Michael/0000-0002-1207-9137; Forman, William/0000-0002-9478-1682 NR 63 TC 23 Z9 23 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 JUN 20 PY 2005 VL 626 IS 2 BP 723 EP 732 DI 10.1086/430124 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 935PU UT WOS:000229795000008 ER PT J AU Croston, JH Hardcastle, MJ Harris, DE Belsole, E Birkinshaw, M Worrall, DM AF Croston, JH Hardcastle, MJ Harris, DE Belsole, E Birkinshaw, M Worrall, DM TI An X-ray study of magnetic field strengths and particle content in the lobes of FR II radio sources SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; quasars : general; radiation mechanisms : nonthermal; X-rays : galaxies ID ACTIVE GALACTIC NUCLEI; HOT-SPOTS; CHANDRA DETECTION; COMPLETE SAMPLE; GALAXY 3C-265; CYGNUS-A; EMISSION; JETS; ENVIRONMENTS; QUASARS AB We present a Chandra and XMM-Newton study of X-ray emission from the lobes of 33 classical double radio galaxies and quasars. We report new detections of lobe-related X-ray emission in 11 sources. Together with previous detections, we find that X-ray emission is detected from at least one radio lobe in similar to 75% of the sample. For all of the lobe detections, we find that the measured X-ray flux can be attributed to inverse Compton scattering of the cosmic microwave background radiation, with magnetic field strengths in the lobes between 0.3 B-eq and 1.3 B-eq, where the value Beq corresponds to equipartition between the electrons and magnetic field, assuming a filling factor of unity. There is a strong peak in the magnetic field strength distribution at B similar to 0.7 B-eq. We find that more than 70% of the radio lobes are either at equipartition or electron dominated by a small factor. The distribution of measured magnetic field strengths differs for narrow- and broad-line objects, in the sense that broad-line radio galaxies and quasars appear to be further from equipartition; however, this is likely to be due to a combination of projection effects and worse systematic uncertainty in the X-ray analysis for those objects. Our results suggest that the lobes of classical double radio sources do not contain an energetically dominant proton population, because this would require the magnetic field energy density to be similar to the electron energy density rather than the overall energy density in relativistic particles. C1 CEA Saclay, Serv Astrophys, F-91191 Gif Sur Yvette, France. Univ Bristol, Dept Phys, Bristol BS8 1TL, Avon, England. Univ Hertfordshire, Sch Phys Astron & Math, Hatfield AL10 9AB, Herts, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Croston, JH (reprint author), CEA Saclay, Serv Astrophys, L Orme Merisiers, F-91191 Gif Sur Yvette, France. EM jcroston@discovery.saclay.cea.fr RI Hardcastle, Martin/E-2264-2012 OI Hardcastle, Martin/0000-0003-4223-1117 NR 52 TC 168 Z9 168 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 JUN 20 PY 2005 VL 626 IS 2 BP 733 EP 747 DI 10.1086/430170 PN 1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 935PU UT WOS:000229795000009 ER PT J AU Young, A Rudnick, L Katz, D Delaney, T Kassim, NE Makishima, K AF Young, A Rudnick, L Katz, D Delaney, T Kassim, NE Makishima, K TI Canonical particle acceleration in FR I radio galaxies SO ASTROPHYSICAL JOURNAL LA English DT Review DE acceleration of particles; galaxies : active; galaxies : jets; radio continuum : galaxies; techniques : image processing ID ACTIVE GALACTIC NUCLEI; RILEY TYPE-I; COMPTON X-RAYS; SHOCK ACCELERATION; RELATIVISTIC JETS; MAGNETIC-FIELDS; HOT-SPOTS; 3C 66B; ELECTRON ACCELERATION; SYNCHROTRON RADIATION AB Matched-resolution multifrequency VLA observations of four radio galaxies are used to derive the asymptotic low-energy slope of the relativistic electron distribution. When available, low-energy slopes are also determined for other sources in the literature. They provide information on the acceleration physics independent of radiative and other losses, which confuse measurements of the synchrotron spectra in most radio, optical, and X-ray studies. We find a narrow range of inferred low-energy electron energy slopes n(E) proportional to E-2.1 for the currently small sample of lower luminosity sources classified as FR I (not classical doubles). This distribution is close to, but apparently inconsistent with, the test particle limit of n(E) proportional to E-2.0 expected from strong diffusive shock acceleration in the nonrelativistic limit. Relativistic shocks or those modified by the back-pressure of efficiently accelerated cosmic rays are two alternatives to produce somewhat steeper spectra. We note for further study the possibility of acceleration through shocks, turbulence, or shear in the flaring and brightening regions in FR I jets as they move away from the nucleus. Jets on parsec scales and the collimated jets and hot spots of FR II (classical double) sources would be governed by different acceleration sites and mechanisms; they appear to show a much wider range of spectra than those for FR I sources. C1 Univ Minnesota, Dept Astron, Minneapolis, MN 55455 USA. Kutztown State Univ, Dept Phys Sci, Kutztown, PA 19530 USA. USN Acad, Annapolis, MD 21402 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. USN, Res Lab, Remote Sensing Div, Washington, DC 20375 USA. Univ Tokyo, Sch Sci, Dept Phys, Bunkyo Ku, Tokyo 1130033, Japan. RP Univ Minnesota, Dept Astron, 116 Church St SE, Minneapolis, MN 55455 USA. NR 117 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 JUN 20 PY 2005 VL 626 IS 2 BP 748 EP 766 DI 10.1086/430107 PN 1 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 935PU UT WOS:000229795000010 ER PT J AU Kavars, DW Dickey, JM McClure-Griffiths, NM Gaensler, BM Green, AJ AF Kavars, DW Dickey, JM McClure-Griffiths, NM Gaensler, BM Green, AJ TI "Missing link'' clouds in the Southern Galactic Plane Survey SO ASTROPHYSICAL JOURNAL LA English DT Article DE Galaxy : structure; ISM : atoms; ISM : clouds; radio lines : ISM ID HYDROGEN SELF-ABSORPTION; COLD ATOMIC-HYDROGEN; H-II-REGIONS; MOLECULAR CLOUDS; MILKY-WAY; NEUTRAL HYDROGEN; INTERSTELLAR CLOUDS; OUTER GALAXY; DUST CLOUDS; TRANSITION AB We present an automated routine to search for H I self- absorption features within the Southern Galactic Plane Survey ( SGPS). The data were taken with the Australia Telescope Compact Array ( ATCA) and the Parkes Radio Telescope and encompass 3 degrees x 105 degrees of sky in the Galactic plane. We apply our routine to this entire region and derive spin temperatures and column densities for 70 of the larger HISA complexes, finding spin temperatures ranging from 6 to 41 K with H I number densities of a few cm(-3). These "missing link" clouds fill in the spin temperature and density gaps between dense molecular clouds and diffuse atomic clouds. We compare the H I emission with (CO)-C-12 emission and find that similar to 60% of detected H I self- absorption is correlated in space and in velocity with a molecular counterpart. This is potentially due to a molecular/ atomic gas transition. We also compare H I self- absorption with Galactic spiral arms and discuss the possibility of using it as a spiral arm tracer. C1 Univ Minnesota, Dept Astron, Minneapolis, MN 55455 USA. Univ Tasmania, Sch Math & Phys, Hobart, Tas 7001, Australia. Australia Telescope Natl Facil, CSIRO, Shimla 171001, Himachal Prades, India. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Sydney, Sch Phys, Dept Astrophys, Sydney, NSW 2006, Australia. RP Kavars, DW (reprint author), Univ Minnesota, Dept Astron, 116 Church St SE, Minneapolis, MN 55455 USA. EM dkavars@astro.umn.edu; john.dickey@utas.edu.au; naomi.mcclure-griffiths@atnf.csiro.au; bgaensler@cfa.harvard.edu; agreen@physics.usyd.edu.au RI Gaensler, Bryan/F-8655-2010; Dickey, John/C-6156-2013; OI McClure-Griffiths, Naomi/0000-0003-2730-957X; Dickey, John/0000-0002-6300-7459; Gaensler, Bryan/0000-0002-3382-9558 NR 51 TC 25 Z9 25 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 JUN 20 PY 2005 VL 626 IS 2 BP 887 EP 899 DI 10.1086/430296 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 935PU UT WOS:000229795000021 ER PT J AU Vanderbei, RJ Traub, WA AF Vanderbei, RJ Traub, WA TI Pupil mapping in two dimensions for high-contrast imaging SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; techniques : high angular resolution ID TERRESTRIAL PLANETS; VISIBLE-LIGHT; APODIZATION; CORONAGRAPH; MASKS; TELESCOPE AB Pupil mapping is a technique whereby a uniformly illuminated input pupil, such as from starlight, can be mapped into a nonuniformly illuminated exit pupil, such that the image formed from this pupil will have suppressed sidelobes, many orders of magnitude weaker than classical Airy ring intensities. Pupil mapping is therefore a candidate technique for coronagraphic imaging of extrasolar planets around nearby stars. The pupil mapping technique is lossless and preserves the full angular resolution of the collecting telescope, so it could possibly give the highest signal-to-noise ratio of any proposed single-telescope system for detecting extrasolar planets. A planet fainter than 10(-10) times its parent star and as close as about 2 lambda/D should be detectable. We derive the two-dimensional equations of pupil mapping for both two-mirror and two-lens systems. We give examples for both cases. We derive analytical estimates of aberration in a two-mirror system and show that the aberrations are essentially corrected with an added reversed set of mirrors. C1 Princeton Univ, Princeton, NJ 08544 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Vanderbei, RJ (reprint author), Princeton Univ, Engn Quadrangle, Princeton, NJ 08544 USA. EM rvdb@princeton.edu; wtraub@cfa.harvard.edu RI Vanderbei, Robert/A-9779-2009 NR 21 TC 38 Z9 38 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 JUN 20 PY 2005 VL 626 IS 2 BP 1079 EP 1090 DI 10.1086/429909 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 935PU UT WOS:000229795000040 ER PT J AU Wilner, DJ D'Alessio, P Calvet, N Claussen, MJ Hartmann, L AF Wilner, DJ D'Alessio, P Calvet, N Claussen, MJ Hartmann, L TI Toward planetesimals in the disk around TW hydrae: 3.5 centimeter dust emission SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; planetary systems : protoplanetary disks; stars : individual (TW Hydrae) ID YOUNG STELLAR OBJECTS; TAURI STARS; CIRCUMSTELLAR DISKS; X-RAY; PROTOPLANETARY DISKS; VLA OBSERVATIONS; ACCRETION DISKS; RADIO-EMISSION; SPECTROSCOPY; SEARCH AB We present Very Large Array observations at lambda = 3.5 cm of the nearby young star TW Hya that show the emission is constant in time over weeks, months, and years, and spatially resolved with peak brightness temperature similar to 10 K at similar to 0.25 (15 AU) resolution. These features are naturally explained if the emission mechanism at this wavelength is thermal emission from dust particles in the disk surrounding the star. To account quantitatively for the observations, we construct a self-consistent accretion disk model that incorporates a population of centmetersize particles that matches the long-wavelength spectrum and spatial distribution. A substantal mass fraction of orbiting particles in the TW Hya disk must have agglomerated to centmeter size. These data provide the first clear indication that dust emission from protoplanetary disks may be observed at centmeter wavelengths, and that changes in the spectral slope of the dust emission may be detected, providing constraints on dust evolution and the planet formation process. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Nacl Autonoma Mexico, Astron Inst, Morelia 58089, Michoacan, Mexico. Natl Radio Astron Observ, Socorro, NM 87801 USA. RP Wilner, DJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM dwilner@cfa.harvard.edu NR 38 TC 94 Z9 94 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 JUN 20 PY 2005 VL 626 IS 2 BP L109 EP L112 DI 10.1086/431757 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 935PW UT WOS:000229795200010 ER PT J AU Jackson, JBC Ogden, JC Pandolfi, JM Baron, N Bradbury, RH Guzman, HM Hughes, TP Kappel, CV Micheli, F Possingham, HP Sala, E AF Jackson, JBC Ogden, JC Pandolfi, JM Baron, N Bradbury, RH Guzman, HM Hughes, TP Kappel, CV Micheli, F Possingham, HP Sala, E TI Reassessing US coral reefs - Response SO SCIENCE LA English DT Letter C1 Univ Calif San Diego, Scripps Inst Oceanog, Ctr Marine Biodivers & Conservat, La Jolla, CA 92093 USA. Smithsonian Trop Res Inst, Balboa, Panama. Florida Inst Oceanog, St Petersburg, FL 33701 USA. Univ Queensland, Dept Math, St Lucia, Qld 4072, Australia. Univ Queensland, Sch Life Sci, St Lucia, Qld 4072, Australia. Univ Queensland, Ctr Marine Studies, St Lucia, Qld 4072, Australia. Univ Queensland, Dept Earth Sci, St Lucia, Qld 4072, Australia. Natl Ctr Ecol Anal & Synth, Santa Barbara, CA 93101 USA. Australian Natl Univ, Canberra, ACT 0200, Australia. James Cook Univ N Queensland, Ctr Coral Reef Biodivers, Sch Marine Biol, Townsville, Qld 4811, Australia. Stanford Univ, Hopkins Marine Stn, Pacific Grove, CA 93950 USA. RP Jackson, JBC (reprint author), Univ Calif San Diego, Scripps Inst Oceanog, Ctr Marine Biodivers & Conservat, La Jolla, CA 92093 USA. RI Possingham, Hugh/B-1337-2008; Kappel, Carrie/B-9534-2009; Pandolfi, John/A-3121-2009; Hughes, Terry/L-4721-2013 OI Possingham, Hugh/0000-0001-7755-996X; Pandolfi, John/0000-0003-3047-6694; Hughes, Terry/0000-0002-5257-5063 NR 14 TC 0 Z9 0 U1 0 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 JUN 17 PY 2005 VL 308 IS 5729 BP 1741 EP 1742 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 937LY UT WOS:000229926800024 ER PT J AU Rung, A Mathis, WN Papp, L AF Rung, A Mathis, WN Papp, L TI Curiosimusca, gen nov, and three new species in the family Aulacigastridae from the Oriental Region (Diptera : Opomyzoidea) SO ZOOTAXA LA English DT Article DE Aulacigastridae; Diptera; systematics; Oriental region ID CLASSIFICATION AB A new genus, Curiosimusca, and three new species (C. khooi, C. orientalis, C. maefangensis) are described from specimens collected in the Oriental Region (Malaysia, Thailand). Curiosimusca is postulated to be the sister group of Aulacigaster Macquart and for the present is the only other genus included in the family Aulacigastridae (Opomyzoidea). Morphological evidence is presented to document our preliminary hypothesis of phylogenetic relationships. C1 Univ Maryland, Dept Entomol, College Pk, MD 20742 USA. Smithsonian Inst, Dept Entomol, Washington, DC 20013 USA. Hungarian Nat Hist Museum, Dept Zool, H-1431 Budapest, Hungary. RP Rung, A (reprint author), Univ Maryland, Dept Entomol, 4112 Plant Sci Bldg, College Pk, MD 20742 USA. EM baptist@wam.umd.edu; mathisw@si.edu; lpapp@zoo.zoo.nhmus.hu NR 30 TC 2 Z9 3 U1 0 U2 0 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD JUN 17 PY 2005 IS 1009 BP 21 EP 36 PG 16 WC Zoology SC Zoology GA 936OH UT WOS:000229864800003 ER PT J AU MacPherson, GJ Huss, GR AF MacPherson, GJ Huss, GR TI Petrogenesis of Al-rich chondrules: Evidence from bulk compositions and phase equilibria SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article ID UNEQUILIBRATED ORDINARY CHONDRITES; TRACE-ELEMENT ABUNDANCES; CHEMICAL MASS-TRANSFER; REDUCED-CV CHONDRITES; CARBONACEOUS CHONDRITES; SOLAR NEBULA; FERROMAGNESIAN CHONDRULES; ALLENDE METEORITE; REFRACTORY INCLUSIONS; OLIVINE INCLUSIONS AB We measured major, minor, and trace-element compositions for eleven M-rich chondrules from unequilibrated ordinary chondrites to investigate the relationships between Al-rich chondrules, ferromagnesian chondrules, Ca-, Al-rich inclusions (CAIs), and amoeboid olivine aggregates (AOAs). Phase equilibrium considerations show that, for the most part, mineral assemblages in Al-rich chondrules are those expected from melts of the observed compositions. The diversity of mineral assemblages and Al-rich chondrule types arises mainly from the fact that the array of compositions spans both the spinel-saturated anorthite-forsterite reaction curve and a thermal divide defined by where the anorthite-forsterite join crosses the reaction curve. The reaction curve accounts for the two principal varieties of M-rich chondrule, plagioclase-phyric and olivine-phyric, with or without altuminous spinel. The thermal divide influences the subsequent evolution of each variety. A third variety of Al-rich chondrule contains abundant sodium-rich glass; trace-element fractionation patterns suggest that these glassy Al-rich chondrules could have been derived from the other two by extensive alteration of plagioclase to nepheline followed by remelting. The bulk compositions of Al-rich chondrules (except sodium-rich ones) are intermediate in a volatility sense between ferromagnesian chondrules and type C CAIs. The combined trend of bulk compositions for CAIs, Al-rich chondrules, and ferromagnesian chondrules mirrors, but does not exactly match, the trend predicted from equilibrium condensation at P-T similar to 10(-3) atm; the observed trend does not match the trend found for evaporation from a liquid of chondritic composition. We thus infer that the bulk compositions of the precursors to CAIs, Al-rich chondrules, were ferromagnesian chondrules were controlled primarily by vapor-solid reactions (condensation or sublimation) in the solar nebula. Some M-rich chondrules are consistent with an origin by melting of a compound CAI-ferromagnesian chondrule hybrid; others cannot be so explained. Any hybrid model is restricted by the constraint that the CAI precursor consisted dominantly of pyroxene + plagioclase + spinel; melilite cannot have been a significant component. Amoeboid olivine aggregates also have the inferred mineralogical characteristics of Al-rich chondrule precursors-they are mixtures of olivine with plagioclase-spinel-pyroxene-rich CAIs-but the few measured bulk compositions are more olivine-rich than those of Al-rich chondrules. Copyright (c) 2005 Elsevier Ltd. C1 Smithsonian Inst, Museum Natl Hist Nat, Dept Mineral Sci, Washington, DC 20560 USA. Arizona State Univ, Dept Geol, Tempe, AZ 85287 USA. Arizona State Univ, Ctr Meteorite Sci, Tempe, AZ 85287 USA. RP MacPherson, GJ (reprint author), Smithsonian Inst, Museum Natl Hist Nat, Dept Mineral Sci, POB 37012, Washington, DC 20560 USA. EM glenn@volcano.si.edu NR 81 TC 44 Z9 45 U1 0 U2 2 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUN 15 PY 2005 VL 69 IS 12 BP 3099 EP 3127 DI 10.1016/j.gca.2004.12.022 PG 29 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 940PO UT WOS:000230156600012 ER PT J AU Sajeev, Y Santra, R Pal, S AF Sajeev, Y Santra, R Pal, S TI Analytically continued Fock space multireference coupled-cluster theory: Application to the (2)Pi(g) shape resonance in e-N-2 scattering SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID ELECTRON-MOLECULE SCATTERING; COMPLEX ABSORBING POTENTIALS; SELF-CONSISTENT-FIELD; VIBRATIONAL-EXCITATION; QUANTUM-CHEMISTRY; TEMPORARY ANIONS; EFFECTIVE-HAMILTONIANS; STABILIZATION METHOD; GENERAL FORMALISM; PROPAGATOR THEORY AB The technique of Fock space multireference coupled-cluster (FSMRCC) is applied for the first time to the correlated calculation of the energy and width of a shape resonance in an electron-molecule collision. The procedure is based upon combining a complex absorbing potential with FSMRCC theory. Accurate resonance parameters are obtained by solving a small non-Hermitian eigenvalue problem. The potential-energy curve of the (2)Pi(g) state of N-2(-) is calculated using the FSMRCC and multireference configuration-interaction (MRCI) level of theories. Comparison with the single-determinant Hartree-Fock theory indicates that correlation effects are important in determining the behavior of the resonance state. (C) 2005 American Institute of Physics. C1 Natl Chem Lab, Div Phys Chem, Theory Grp, Pune 411008, Maharashtra, India. Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom Mol & Opt Phys, Cambridge, MA 02138 USA. RP Natl Chem Lab, Div Phys Chem, Theory Grp, Pune 411008, Maharashtra, India. EM pal@ems.ncl.res.in RI Santra, Robin/E-8332-2014 OI Santra, Robin/0000-0002-1442-9815 NR 72 TC 24 Z9 24 U1 1 U2 2 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 JUN 15 PY 2005 VL 122 IS 23 AR 234320 DI 10.1063/1.1938887 PG 10 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 939RZ UT WOS:000230091400031 PM 16008454 ER PT J AU Riley, S AF Riley, S TI The Washingtonienne. SO LIBRARY JOURNAL LA English DT Book Review C1 Smithsonian Inst, Lib, Washington, DC 20560 USA. RP Riley, S (reprint author), Smithsonian Inst, Lib, Washington, DC 20560 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 JUN 15 PY 2005 VL 130 IS 11 BP 57 EP 57 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 936VY UT WOS:000229884700018 ER PT J AU Yoo, J Kochanek, CS Falco, EE McLeod, BA AF Yoo, J Kochanek, CS Falco, EE McLeod, BA TI The lens galaxy in PG 1115+080 is an ellipse SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : observations; dark matter; gravitational lensing ID DARK-MATTER SUBSTRUCTURE; GRAVITATIONAL LENSES; GALACTIC SATELLITES; PG 1115+080; MODELS; DEGENERACIES; SYSTEMS; RADIO; HALOS; PROBE AB We use the structure of the Einstein ring image of the quasar host galaxy in the four-image quasar lens PG 1115+080 to determine the angular structure of the gravitational potential of the lens galaxy. We find that it is well described as an ellipsoid and that the best-fit nonellipsoidal models are consistent with the ellipsoidal model. We find upper limits on the standard parameters for the deviation from an ellipse of &VERBAR; a(3)(B)/a(0)&VERBAR; < 0.035 and &VERBAR;α(B)(4)/a(0)&VERBAR; < 0.064. We also find that the position of the center of mass is consistent with the center of light, with an upper limit of &VERBAR;&UDelta; x&VERBAR; < 0".005 on the offset between them. Neither the ellipsoidal nor the nonellipsoidal models can reproduce the observed image flux ratios while simultaneously maintaining a reasonable fit to the Einstein ring, so the anomalous flux ratio of the A(1) and A(2) quasar images must be due to substructure in the gravitational potential such as compact satellite galaxies or stellar microlenses rather than odd angular structure in the lens galaxy. C1 Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Yoo, J (reprint author), Ohio State Univ, Dept Astron, 140 W 18th Ave, Columbus, OH 43210 USA. EM jaiyul@astronomy.ohio-state.edu; ckochanek@astronomy.ohio-state.edu; efalco@cfa.harvard.edu; bmcleod@cfa.harvard.edu NR 45 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 JUN 10 PY 2005 VL 626 IS 1 BP 51 EP 57 DI 10.1086/429959 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 932CQ UT WOS:000229532200005 ER PT J AU Modjaz, M Moran, JM Kondratko, PT Greenhill, LJ AF Modjaz, M Moran, JM Kondratko, PT Greenhill, LJ TI Probing the magnetic field at subparsec radii in the accretion disk of NGC 4258 SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; galaxies : individual ( NGC 4258); galaxies : magnetic fields; galaxies : nuclei; masers; polarization ID ACTIVE GALACTIC NUCLEI; ASTROPHYSICAL WATER MASERS; SPECTRAL-LINE PROFILES; DWARF SEYFERT NUCLEI; NGC 4258; CIRCULAR-POLARIZATION; BLACK-HOLES; H2O MASERS; MAGNETOHYDRODYNAMIC SIMULATIONS; ARRAY OBSERVATIONS AB We present an analysis of polarimetric observations at 22 GHz of the water vapor masers in NGC 4258 obtained with the VLA and the GBT. We do not detect any circular polarization in the spectrum indicative of Zeeman-induced splitting of the maser lines of water, a non-paramagnetic molecule. We have improved the 1 σ 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 to 90 mG. We have developed a new method for the analysis of spectra with blended features and derive a 1 σ 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 &SIM; 10(-3.7) M-&ODOT; yr(-1) for a total magnetic field of less than 130 mG. We discuss the ramifications of our results on current maser models proposed to explain the observed maser emission structure and the consequences for current accretion theories. We find from our magnetic field limits that the thin-disk model and the jet-disk model are better candidates for accounting for the extremely low luminosity nature of NGC 4258 than models that include advection-dominated accretion flows. 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. EM mmodjaz@cfa.harvard.edu OI Moran, James/0000-0002-3882-4414 NR 97 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 JUN 10 PY 2005 VL 626 IS 1 BP 104 EP 119 DI 10.1086/429559 PN 1 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 932CQ UT WOS:000229532200010 ER PT J AU Stawarz, X Siemiginowska, A Ostrowski, M Sikora, M AF Stawarz, X Siemiginowska, A Ostrowski, M Sikora, M TI On the magnetic field in the kiloparsec-scale jet of radio galaxy M87 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : individual ( M87); galaxies : jets; galaxies : magnetic fields; radiation mechanisms : nonthermal ID X-RAY JET; SPACE-TELESCOPE OBSERVATIONS; ACTIVE GALACTIC NUCLEI; TURBULENT GENERATION; ASTROPHYSICAL JETS; COMPTON-SCATTERING; HIGH-RESOLUTION; GAMMA-RAYS; EMISSION; SPECTRUM AB Several low-power kiloparsec-scale jets in nearby radio galaxies are known for their synchrotron radiation extending up to optical and X-ray photon energies. Here we comment on high-energy gamma-ray emission of one particular object of this kind, i.e., the kiloparsec-scale jet of the M87 radio galaxy, resulting from Comptonization of the starlight photon field of the host galaxy by the synchrotron-emitting jet electrons. In our analysis, we include the relativistic bulk velocity of the jet, as well as the Klein-Nishina effects. We show that upper limits to the kiloparsec-scale jet inverse Compton radiation imposed by the HESS and HEGRA Cerenkov Telescopes-which detected a variable source of very high energy gamma-ray emission within 0 degrees.1 (similar to 30 kpc) of the M87 central region-give us an important constraint on the magnetic field strength in this object, namely, that the magnetic field cannot be smaller than the equipartition value ( referring solely to the radiating electrons) in the brightest knot of the jet, and most likely, is even stronger. In this context, we point out a need for the amplification of the magnetic energy flux along the M87 jet from the subparsec to kiloparsec scales, suggesting the turbulent dynamo as a plausible process responsible for the aforementioned amplification. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Jagiellonian Univ, Astron Observ, PL-30244 Krakow, Poland. Nicolaus Copernicus Astron Ctr, PL-00716 Warsaw, Poland. RP Stawarz, X (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM stawarz@oa.uj.edu.pl; asiemiginowska@cfa.harvard.edu; mio@oa.uj.edu.pl; sikora@camk.edu.pl NR 61 TC 31 Z9 31 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 JUN 10 PY 2005 VL 626 IS 1 BP 120 EP 127 DI 10.1086/430087 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 932CQ UT WOS:000229532200011 ER PT J AU Vrtilek, SD Raymond, JC Boroson, B McCray, R AF Vrtilek, SD Raymond, JC Boroson, B McCray, R TI Photoionized lines in X-ray spectra of SMC X-1 SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; binaries : close; pulsars : individual (SMC X-1); X rays : stars ID HUBBLE-SPACE-TELESCOPE; COMPTON HEATED WINDS; ACCRETION DISKS; STELLAR WIND; BINARY-SYSTEMS; EMISSION-LINE; LMC X-4; DYNAMICS; SPECTROSCOPY; SMC-X-1 AB We present a detailed spectral analysis of Chandra ACIS- S continuous clocking ( CC) mode observations of the massive X-ray binary system SMC X-1. The system was observed during both the high and low X-ray states of the roughly 60 day superorbital period. The continuum spectra during both states are well represented by a power law with photon index α = 0.9 and a blackbody of kT = 0.15 keV. The high-state spectra are dominated by the continuum and independent of orbital phase, whereas the low-state spectra show a strong orbital dependence as well as line emission from O, Ne, Mg, Fe, and Si. This is consistent with the states attributed to disk precession: during the high state, X-ray emission is dominated by the compact source, which is abruptly eclipsed; during the low state, the compact object is hidden by the disk, and a larger, less luminous scattering region is responsible for the X-ray emission. A prominent Ne IX feature places a stringent limit ( logξ = 2.0-2.5) on the ionization parameter, which constrains the wind dynamics of the system. The Fe line fluxes are related linearly to the blackbody fluxes, indicating that both originate in the same region or are excited by the same mechanism. There is evidence for structure in the Fe line that cannot be fully resolved by the current observations. The pulse period measured during our observations, 0.7057147 &PLUSMN; 0.00000027 s, shows that the uninterrupted spin-up trend of SMC X-1 continues. We discuss the implications of our results for models of SMC X-1. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Bowling Green State Univ, Bowling Green, OH 43403 USA. Univ Colorado, JILA, Boulder, CO 80309 USA. RP Vrtilek, SD (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM svrtilek@cfa.harvard.edu NR 49 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 JUN 10 PY 2005 VL 626 IS 1 BP 307 EP 316 DI 10.1086/429718 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 932CQ UT WOS:000229532200027 ER PT J AU Bock, DCJ Gaensler, BM AF Bock, DCJ Gaensler, BM TI Measurement of spectral breaks in pulsar wind nebulae with millimeter-wave interferometry SO ASTROPHYSICAL JOURNAL LA English DT Article DE pulsars : individual (PSR J1846-0258); radio continuum : ISM; supernovae : individual (G11.2-0.3, G16.7+0.1, G29.7-0.3); supernova remnants ID RADIO-CONTINUUM OBSERVATIONS; SUPERNOVA REMNANT G11.2-0.3; CRAB-NEBULA; EVOLUTION; PLERIONS AB We have observed pulsar wind nebulae (PWNe) in the three supernova remnants G11.2-0.3, G16.7+0.1, and G29.7-0.3 at 89 GHz with the Berkeley-Illinois-Maryland Association array, measuring total flux densities of two of them for comparison with archival data at other frequencies. In G16.7+0.1, we find a break in the spectrum of the PWN at &SIM; 26 GHz. In G29.7-0.3, our data suggest a break in the integrated spectrum of the central nebula at &SIM; 55 GHz, lower than previously estimated. However, we have found spatial structure in the spectrum of this nebula. The emission to the north of pulsar J1846-0258 has a broken spectrum with break frequency &LSIM; 100 GHz, consistent with a conventional pulsar-powered nebula. The emission to the south of the pulsar has a nearly power-law spectrum from radio to X-rays: this component may be unrelated to the PWN, or it may be evidence of asymmetries and/or time evolution in the pulsar's energy output. We present 89 GHz images of each remnant. C1 Univ Calif Berkeley, Radio Astron Lab, Berkeley, CA 94720 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Bock, DCJ (reprint author), CARMA, POB 968, Big Pine, CA 93513 USA. EM dbock@astro.berkeley.edu; bgaensler@cfa.harvard.edu RI Gaensler, Bryan/F-8655-2010; OI Gaensler, Bryan/0000-0002-3382-9558 NR 33 TC 13 Z9 13 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 JUN 10 PY 2005 VL 626 IS 1 BP 343 EP 349 DI 10.1086/429789 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 932CQ UT WOS:000229532200030 ER PT J AU Lipscy, SJ Jura, M Reid, MJ AF Lipscy, SJ Jura, M Reid, MJ TI Radio photosphere and mass-loss envelope of VY canis majoris SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared : stars; radio continuum : stars; stars : atmospheres; stars : individual ( VY Canis Majoris); stars : mass loss; supergiants ID LATE-TYPE STARS; CIRCUMSTELLAR DUST SHELLS; ALPHA-ORIONIS; EXTENDED CHROMOSPHERE; SUPERNOVA EXPLOSIONS; TIME VARIATIONS; EVOLVED STARS; EMISSION; SUBMILLIMETER; SUPERGIANTS AB We have used the VLA to detect emission from the supergiant VY CMa at radio wavelengths and have constructed 3000-4500 K isothermal outer atmospheres constrained by the data. These models produce a radio photosphere at 1.5-2 R*. An extrapolation of the model can account for the observed total mass-loss rate of the star. We also present mid-infrared imaging of the supergiant which suggests that warm dust is extended in the same direction as the near-infrared reflection nebula around VY CMa. The origin of the asymmetries in the outflow remains an unsolved problem. C1 Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Lipscy, SJ (reprint author), Ball Aerosp & Technol Corp, 1600 Commerce St,M-S TT-2, Boulder, CO 80301 USA. EM slipscy@ball.com NR 43 TC 7 Z9 7 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 JUN 10 PY 2005 VL 626 IS 1 BP 439 EP 445 DI 10.1086/429900 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 932CQ UT WOS:000229532200039 ER PT J AU Mohanty, S Jayawardhana, R Basri, G AF Mohanty, S Jayawardhana, R Basri, G TI The T tauri phase down to nearly planetary masses: Echelle spectra of 82 very low mass stars and brown dwarfs SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; planetary systems; stars : formation; stars : low-mass, brown dwarfs; stars : pre-main-sequence; techniques : spectroscopic ID SCORPIUS OB ASSOCIATION; MAIN-SEQUENCE STARS; X-RAY SOURCES; MEASURING FUNDAMENTAL PARAMETERS; EMISSION-LINE DIAGNOSTICS; AURIGA MOLECULAR CLOUD; FORMING REGION; DISK ACCRETION; RHO-OPHIUCHI; EVOLUTIONARY MODELS AB Using the largest high-resolution spectroscopic sample to date of young, very low mass stars and brown dwarfs, we investigate disk accretion in objects ranging from just above the hydrogen-burning limit all the way to nearly planetary masses. Our 82 targets span spectral types from M5 to M9.5, or masses from 0.15 M-&ODOT; down to about 15 jupiters. They are confirmed members of the ρ Ophiuchus, Taurus, Chamaeleon I, IC 348, R Coronae Australis, Upper Scorpius, and TW Hydrae star-forming regions and young clusters, with ages from < 1 to &SIM; 10 Myr. The sample contains 41 brown dwarfs (spectral types &GE; M6.5). We have previously presented high-resolution optical spectra for roughly half the sample; the rest are new. This is a close to complete survey of all confirmed brown dwarfs known so far in the regions examined, except in ρ Oph and IC 348 (where we are limited by a combination of extinction and distance). We find that (1) classical T Tauri-like disk accretion persists in the substellar domain down to nearly the deuterium-burning limit; (2) while an Hα 10% width &GE; 200 km s(-1) is our prime accretion diagnostic (following our previous work), permitted emission lines of Ca II, O I, and He I are also good accretion indicators, just as in classical T Tauri stars (we caution against a blind use of Hα width alone, since inclination and rotation effects on the line are especially important at the low accretion rates in very low mass objects); (3) the Ca II λ 8662 line flux is an excellent quantitative measure of the accretion rate in very low mass stars and brown dwarfs (as in higher mass classical T Tauri Stars), correlating remarkably well with the. M obtained from veiling and Hα modeling; (4) the accretion rate diminishes rapidly with mass - our measurements support previous suggestions that M &PROP; M-*(2) (albeit with considerable scatter) and extend this correlation to the entire range of substellar masses; (5) the fraction of very low mass stellar and substellar accretors decreases substantially with age, as in higher mass stars; (6) at any given age, the fraction of very low mass stellar and substellar accretors is comparable to the accretor fraction in higher mass stars; and (7) a number of our sources with infrared excesses arising from dusty disks do not evince measurable accretion signatures, with the incidence of such a mismatch increasing with age: this implies that disks in the low-mass regime can persist beyond the main accretion phase and parallels the transition from the classical to post-T Tauri stage in more massive stars. These strong similarities at young ages, between higher mass stars on the one hand and low-mass bodies close to and below the hydrogen-burning limit on the other, are consistent with a common formation mechanism in the two mass regimes. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H8, Canada. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. RP Mohanty, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM smohanty@cfa.harvard.edu; rayjay@astro.utoronto.ca; basri@soleil.berkeley.edu NR 79 TC 218 Z9 218 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 JUN 10 PY 2005 VL 626 IS 1 BP 498 EP 522 DI 10.1086/429794 PN 1 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 932CQ UT WOS:000229532200043 ER PT J AU Charbonneau, D Allen, LE Megeath, ST Torres, G Alonso, R Brown, TM Gilliland, RL Latham, DW Mandushev, G O'Donovan, FT Sozzetti, A AF Charbonneau, D Allen, LE Megeath, ST Torres, G Alonso, R Brown, TM Gilliland, RL Latham, DW Mandushev, G O'Donovan, FT Sozzetti, A TI Detection of thermal emission from an extrasolar planet SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : eclipsing; infrared : stars; planetary systems; stars : individual (TrES-1); techniques : photometric ID GRAVITATIONAL LENSING EXPERIMENT; LUMINOSITY OBJECT TRANSITS; GIANT PLANETS; HD 209458B; GALACTIC DISK; INFRARED OBSERVATIONS; IRRADIATED PLANETS; SECONDARY ECLIPSE; SPACE-TELESCOPE; BROWN DWARFS AB We present Spitzer Space Telescope infrared photometric time series of the transiting extrasolar planet system TrES-1. The data span a predicted time of secondary eclipse, corresponding to the passage of the planet behind the star. In both bands of our observations, we detect a flux decrement with a timing, amplitude, and duration as predicted by published parameters of the system. This signal represents the first direct detection of (i.e., the observation of photons emitted by) a planet orbiting another star. The observed eclipse depths (in units of relative flux) are 0.00066 &PLUSMN; 0.00013 at 4.5 μ m and 0.00225 &PLUSMN; 0.00036 at 8.0 μ m. These estimates provide the first observational constraints on models of the thermal emission of hot Jupiters. Assuming that the planet emits as a blackbody, we estimate an effective temperature of T-p = 1060 &PLUSMN; 50 K. Under the additional assumptions that the planet is in thermal equilibrium with the radiation from the star and emits isotropically, we find a Bond albedo of A = 0.31 &PLUSMN; 0.14. This would imply that the planet absorbs the majority of stellar radiation incident upon it, a conclusion of significant impact to atmospheric models of these objects. We also compare our data to a previously published model of the planetary thermal emission, which predicts prominent spectral features in our observational bands due to water and carbon monoxide. This model adequately reproduces the observed planet-to-star flux ratio at 8.0 μ m; however, it significantly overpredicts the ratio at 4.5 μ m. We also present an estimate of the timing of the secondary eclipse, which we use to place a strong constraint on the expression e cos ω, where e is the orbital eccentricity and ω is the longitude of periastron. The resulting upper limit on e is sufficiently small that we conclude that tidal dissipation is unlikely to provide a significant source of energy interior to the planet. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Inst Astrofis Canarias, Tenerife 38200, Spain. Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Lowell Observ, Flagstaff, AZ 86001 USA. CALTECH, Pasadena, CA 91125 USA. Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA. RP Charbonneau, D (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM dcharbonneau@cfa.harvard.edu RI Alonso, Roi/D-8799-2014; O'Donovan, Francis/I-2423-2014; OI Alonso, Roi/0000-0001-8462-8126; Sozzetti, Alessandro/0000-0002-7504-365X; O'Donovan, Francis/0000-0002-4858-6106; Charbonneau, David/0000-0002-9003-484X NR 54 TC 447 Z9 451 U1 3 U2 38 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 JUN 10 PY 2005 VL 626 IS 1 BP 523 EP 529 DI 10.1086/429991 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 932CQ UT WOS:000229532200044 ER PT J AU Korzennik, SG AF Korzennik, SG TI A mode-fitting methodology optimized for very long helioseismic time series SO ASTROPHYSICAL JOURNAL LA English DT Article DE methods : statistical; Sun : oscillations ID SOLAR P-MODES; CYCLE; PARAMETERS; SPECTRA; IMAGER; GONG; FREQUENCIES; EXCITATION; NETWORK; GOLF AB I describe and present the results of a newly developed fitting methodology optimized for very long time series. The development of this new methodology was motivated by the fact that we now have more than half a decade of nearly uninterrupted observations by the Global Oscillation Network Group (GONG) and the Michelson Doppler Imager (MDI), with fill factors as high as 82.2% and 89.8%, respectively. It was recently prompted by the availability of a 2088 day long time series of spherical harmonic coefficients produced by the MDI team. The fitting procedure uses an optimal sine multitaper spectral estimator, with the number of tapers based on the mode line width, the complete leakage matrix (i.e., horizontal as well as vertical components), and an asymmetric mode profile to fit simultaneously all the azimuthal orders with individually parameterized profiles. This method was applied to 2088 day long time series of MDI and GONG observations, as well as 728 day long subsets, and for spherical harmonic degrees between 1 and 25. The values resulting from these fits are intercompared (MDI vs. GONG) and compared to equivalent estimates from the MDI team and the GONG project. I also compare the results from fitting the 728 day subsets to the result of the 2088 day time series. This comparison shows the well-known change of frequencies with solar activity and how it scales with a nearly constant pattern in frequency and m/l. This comparison also shows some changes in the mode line width and the constancy of the mode asymmetry. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Korzennik, SG (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 30 TC 32 Z9 32 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 JUN 10 PY 2005 VL 626 IS 1 BP 585 EP 615 DI 10.1086/429748 PN 1 PG 31 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 932CQ UT WOS:000229532200051 ER PT J AU Stanek, KZ Garnavich, PM Nutzman, PA Hartman, JD Garg, A Adelberger, K Berlind, P Bonanos, AZ Calkins, ML Challis, P Gaudi, BS Holman, MJ Kirshner, RP McLeod, BA Osip, D Pimenova, T Reiprich, TH Romanishin, W Spahr, T Tegler, SC Zhao, X AF Stanek, KZ Garnavich, PM Nutzman, PA Hartman, JD Garg, A Adelberger, K Berlind, P Bonanos, AZ Calkins, ML Challis, P Gaudi, BS Holman, MJ Kirshner, RP McLeod, BA Osip, D Pimenova, T Reiprich, TH Romanishin, W Spahr, T Tegler, SC Zhao, X TI Deep photometry of GRB 041006 afterglow: Hypernova bump at redshift z=0.716 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : distances and redshifts; gamma rays : bursts; supernovae : general ID GAMMA-RAY BURST; OPTICAL AFTERGLOW; SUPERNOVA 2003DH; LIGHT-CURVE; GRB-030329; DISCOVERY; SPECTRUM; GRB-011121 AB We present deep optical photometry of the afterglow of gamma-ray burst (GRB) 041006 and its associated hypernova obtained over 65 days after detection (55 R-band epochs on 10 different nights). Our early data (t < days) joined with published GCN data indicate a steepening decay, approaching F(v) proportional to t(-0.6) at early times (t << day) and at late times. The break at days is the earliest reported jet break among all GRB afterglows. During our first night, we obtained 39 exposures spanning 2.15 hr from 0.62 to 0.71 days after the burst that reveal a smooth afterglow, with an rms deviation of 0.024 mag from the local power-law fit, consistent with photometric errors. After days, the decay slows considerably, and the light curve remains approximately flat at mag t similar to 4 R similar to 24 for a month before decaying by another magnitude to reach mag 2 months after the burst. This "bump" is R similar to 25 well fit by a k-corrected light curve of supernova SN 1998bw, but only if stretched by a factor of 1.38 in time. In comparison with the other GRB-related SN bumps, GRB 041006 stakes out new parameter space for GRBs/SNe, with a very bright and significantly stretched late-time SN light curve. Within a small sample of fairly well observed GRB/SN bumps, we see a hint of a possible correlation between their peak luminosity and their "stretch factor," broadly similar to the well-studied Phillips relation for the Type Ia supernovae. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. Carnegie Observ, Pasadena, CA 91101 USA. FL Whipple Observ, Amado, AZ 85645 USA. Carnegie Inst Washington, Campanas Observ, La Serena, Chile. Univ Bonn, Inst Astrophys & Extraterr Forsch, D-53121 Bonn, Germany. Univ Oklahoma, Dept Phys & Astron, Norman, OK 73019 USA. No Arizona Univ, Dept Phys & Astron, Flagstaff, AZ 86011 USA. RP Stanek, KZ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM kstanek@cfa.harvard.edu RI Gaudi, Bernard/I-7732-2012; Bonanos, Alceste/K-5392-2013 OI Bonanos, Alceste/0000-0003-2851-1905 NR 45 TC 47 Z9 47 U1 1 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2005 VL 626 IS 1 BP L5 EP L9 DI 10.1086/431361 PN 2 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 932CT UT WOS:000229532500002 ER PT J AU Kress, WJ Wurdack, KJ Zimmer, EA Weigt, LA Janzen, DH AF Kress, WJ Wurdack, KJ Zimmer, EA Weigt, LA Janzen, DH TI Use of DNA barcodes to identify flowering plants SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE angiosperm; internal transcribed spacer; Plummers island; species identification; trnH-psbA ID CHLOROPLAST DNA; PHYLOGENETIC-RELATIONSHIPS; MOLECULAR PHYLOGENY; SEQUENCES; EVOLUTION; BIOGEOGRAPHY; NUCLEOTIDE; GENUS; CPDNA; SAXIFRAGACEAE AB Methods for identifying species by using short orthologous DNA sequences, known as "DNA barcodes," have been proposed and initiated to facilitate biodiversity studies, identify juveniles, associate sexes, and enhance forensic analyses. The cytochrome c oxidase 1 sequence, which has been found to be widely applicable in animal barcoding, is not appropriate for most species of plants because of a much slower rate of cytochrome c oxidase 1 gene evolution in higher plants than in animals. We therefore propose the nuclear internal transcribed spacer region and the plastid trnH-psbA intergenic spacer as potentially usable DNA regions for applying barcoding to flowering plants. The internal transcribed spacer is the most commonly sequenced locus used in plant phylogenetic investigations at the species level and shows high levels of interspecific divergence. The trnH-psbA spacer, although short (approximate to 450-bp), is the most variable plastid region in angiosperms and is easily amplified across a broad range of land plants. Comparison of the total plastid genomes of tobacco and deadly nightshade enhanced with trials on widely divergent angiosperm taxa, including closely related species in seven plant families and a group of species sampled from a local flora encompassing 50 plant families (for a total of 99 species, 80 genera, and 53 families), suggest that the sequences in this pair of loci have the potential to discriminate among the largest number of plant species for barcoding purposes. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA. Smithsonian Inst, Natl Museum Nat Hist, Lab Analyt Biol, Washington, DC 20013 USA. Univ Penn, Dept Biol, Philadelphia, PA 19104 USA. RP Kress, WJ (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, POB 37012, Washington, DC 20013 USA. EM kressj@si.edu RI Zimmer, Elizabeth/G-3890-2011 NR 54 TC 731 Z9 911 U1 27 U2 244 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 JUN 7 PY 2005 VL 102 IS 23 BP 8369 EP 8374 DI 10.1073/pnas.0503123102 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 933RL UT WOS:000229650500053 PM 15928076 ER PT J AU Novotny, V Basset, Y AF Novotny, V Basset, Y TI Review - Host specificity of insect herbivores in tropical forests SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Review DE food web; herbivore guild; host plant range; insect sampling; rainforest; species richness ID PAPUA-NEW-GUINEA; LEAF-CHEWING INSECTS; LOWLAND RAIN-FOREST; SPECIES RICHNESS; BEETLES COLEOPTERA; PHYTOPHAGOUS BEETLES; PARASITOID COMMUNITY; PALAME COLEOPTERA; DECIDUOUS FOREST; PLANT DIVERSITY AB Studies of host specificity in tropical insect herbivores are evolving from a focus on insect distribution data obtained by canopy fogging and other mass collecting methods, to a focus on obtaining data on insect rearing and experimentally verified feeding patterns. We review this transition and identify persisting methodological problems. Replicated quantitative surveys of plant-herbivore food webs, based on sampling efforts of an order of magnitude greater than is customary at present, may be cost-effectively achieved by small research teams supported by local assistants. Survey designs that separate historical and ecological determinants of host specificity by studying herbivores feeding on the same plant species exposed to different environmental or experimental conditions are rare. Further, we advocate the use of host-specificity measures based on plant phylogeny. Existing data suggest that a minority of species in herbivore communities feed on a single plant species when alternative congeneric hosts are available. Thus, host plant range limits tend to coincide with those of plant genera, rather than species or suprageneric taxa. Host specificity among tropical herbivore guilds decreases in the sequence: granivore > leaf-miners > fructivores > leaf-chewers=sap-suckers > xylophages > root-feeders, thus paralleling patterns observed in temperate forests. Differences in host specificity between temperate and tropical forests are difficult to assess since data on tropical herbivores originate from recent field studies, whereas their temperate counterparts derive from regional host species lists, assembled over many years. No major increase in host specificity from temperate to tropical communities is evident. This conclusion, together with the recent downward revisions of extremely high estimates of tropical species richness, suggest that tropical ecosystems may not be as biodiverse as previously thought. C1 Univ S Bohemia, Acad Sci Czech Republ, Inst Entomol, Ceske Budejovice 37005, Czech Republic. Univ S Bohemia, Fac Biol, Ceske Budejovice 37005, Czech Republic. Smithsonian Trop Res Inst, Ancon, Panama. RP Novotny, V (reprint author), Univ S Bohemia, Acad Sci Czech Republ, Inst Entomol, Branisovska 31, Ceske Budejovice 37005, Czech Republic. EM novotny@entu.cas.cz RI Basset, Yves/B-6642-2014; Novotny, Vojtech/G-9434-2014 OI Novotny, Vojtech/0000-0001-7918-8023 NR 81 TC 161 Z9 166 U1 9 U2 75 PU ROYAL SOCIETY PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8452 J9 P ROY SOC B-BIOL SCI JI Proc. R. Soc. Lond. Ser. B-Biol. Sci. PD JUN 7 PY 2005 VL 272 IS 1568 BP 1083 EP 1090 DI 10.1098/rspb.2004.3023 PG 8 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 946HN UT WOS:000230563100001 PM 16024368 ER PT J AU Ward, PD Buick, R Erwin, DH AF Ward, PD Buick, R Erwin, DH TI Response to comment on "Abrupt and gradual extinction among late Permian land vertebrates in the Karoo basin, South Africa" SO SCIENCE LA English DT Editorial Material C1 Univ Washington, Dept Biol, Seattle, WA 98195 USA. Univ Washington, Dept Earth & Space Sci, Seattle, WA 98195 USA. 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 NR 6 TC 0 Z9 0 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 JUN 3 PY 2005 VL 308 IS 5727 DI 10.1126/science.1110538 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 933HK UT WOS:000229619300028 ER PT J AU Cronk, QCB Kiehn, M Wagner, WL Smith, JE AF Cronk, QCB Kiehn, M Wagner, WL Smith, JE TI Evolution of Cyrtandra (Gesneriaceae) in the Pacific Ocean: The origin of a supertramp clade SO AMERICAN JOURNAL OF BOTANY LA English DT Article ID INTERNAL TRANSCRIBED SPACER; NUCLEAR RIBOSOMAL DNA; HAWAIIAN-ISLANDS; SEQUENCE DATA; ASIAN TAXA; COLONIZATION; BIOGEOGRAPHY; PHYLOGENY; DISPERSAL; ASTERACEAE AB Cyrtandra comprises at least 600 species distributed throughout Malesia, where it is known for many local endemics and in Polynesia and Micronesia, where it is present on most island groups, and is among the most successfully dispersing genera of the Pacific. To ascertain the origin of the oceanic Pacific island species of Cyrtandra, we sequenced the internal transcribed spacers of nuclear ribosomal DNA of samples from throughout its geographical range. Because all oceanic Pacific island species form a well-supported clade, these species apparently result from a single initial colonization into the Pacific, possibly by a species from the eastern rim of SE Asia via a NW-to-SE stepping stone migration. Hawaiian species form a monophyletic group, probably as a result of a single colonization. The Pacific island clade of Cyrtandra dispersed across huge distances, in contrast to the apparent localization of the SE Asian clades. Although highly vagile, the Pacific clade is restricted to oceanic islands. Individual species are often endemic to a single island, characteristic of the "supertramp" life form sensu Diamond (1974, Science 184: 803-806). The evolution of fleshy fruit within Cyrtandra provided an adaptation for colonization throughout the oceanic Pacific via bird dispersal from a single common ancestor. C1 Boise State Univ, Dept Biol, Boise, ID 83725 USA. Univ British Columbia, Bot Garden, Vancouver, BC V6T 1Z4, Canada. Univ British Columbia, Ctr Plant Res, Vancouver, BC V6T 1Z4, Canada. Univ Vienna, Dept Systemat & Evolutionary Bot, A-1030 Vienna, Austria. Smithsonian Inst, Dept Bot, Washington, DC 20013 USA. RP Smith, JE (reprint author), Boise State Univ, Dept Biol, 1910 Univ Dr, Boise, ID 83725 USA. EM jfsmith@boisestate.edu NR 73 TC 43 Z9 50 U1 2 U2 10 PU BOTANICAL SOC AMER INC PI ST LOUIS PA PO BOX 299, ST LOUIS, MO 63166-0299 USA SN 0002-9122 J9 AM J BOT JI Am. J. Bot. PD JUN PY 2005 VL 92 IS 6 BP 1017 EP 1024 DI 10.3732/ajb.92.6.1017 PG 8 WC Plant Sciences SC Plant Sciences GA 931BV UT WOS:000229461700014 PM 21652486 ER PT J AU Liu, X Sioris, CE Chance, K Kurosu, TP Newchurch, MJ Martin, RV Palmer, PI AF Liu, X Sioris, CE Chance, K Kurosu, TP Newchurch, MJ Martin, RV Palmer, PI TI Mapping tropospheric ozone profiles from an airborne ultraviolet-visible spectrometer SO APPLIED OPTICS LA English DT Article ID ATMOSPHERIC ABSORPTION-MEASUREMENTS; ARCTIC STRATOSPHERIC EXPEDITION; SATELLITE MEASUREMENTS; COLUMN ABUNDANCES; FEBRUARY 1989; TOMS MEASUREMENTS; SOUTH-AMERICA; NO2; JANUARY; MODEL AB We present a novel technique for retrieving ozone (O-3) profiles and especially tropospheric O-3 from airborne UV/visible spectrometer measurements. This technique utilizes radiance spectra from one down-looking and two up-looking (85 degrees and 75 degrees) directions, taking advantage of the O-3 absorption structure in the Huggins (300-340-nm) and Chappuis (530-650-nm) bands. This technique is especially sensitive to tropospheric O-3 below and : S km above the aircraft with a vertical resolution of 2-6 km and is sensitive to lower and middle stratospheric O-3 with a vertical resolution of 8-15 km. It can measure tropospheric O-3 at spatial resolutions of 2 km x 2 km or higher and is therefore well suited for regional air-quality studies and validation of satellite measurements. (c) 2005 Optical Society of America. C1 Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA. Univ Alabama, Dept Atmospher Sci, Huntsville, AL 35805 USA. Harvard Univ, Div Engn & Appl Sci, Cambridge, MA 02138 USA. Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 3J5, Canada. RP Liu, X (reprint author), Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, 60 Garden St, Cambridge, MA 02138 USA. EM xliu@cfa.harvard.edu RI Martin, Randall/A-2051-2008; Palmer, Paul/F-7008-2010; Martin, Randall/C-1205-2014; Liu, Xiong/P-7186-2014; OI Martin, Randall/0000-0003-2632-8402; Liu, Xiong/0000-0003-2939-574X; Chance, Kelly/0000-0002-7339-7577; Sioris, Christopher/0000-0003-1168-8755 NR 43 TC 9 Z9 9 U1 0 U2 3 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 1559-128X EI 2155-3165 J9 APPL OPTICS JI Appl. Optics PD JUN 1 PY 2005 VL 44 IS 16 BP 3312 EP 3319 DI 10.1364/AO.44.003312 PG 8 WC Optics SC Optics GA 934QT UT WOS:000229724000023 PM 15943268 ER PT J AU Williams, BF AF Williams, BF TI Variable star candidates in an advanced camera for surveys field of M31 SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies : individual (M31); galaxies : stellar content; stars : variables : other ID DETACHED ECLIPSING BINARIES; RR LYRAE STARS; LONG-PERIOD VARIABLES; POINT-AGAPE SURVEY; DIRECT DISTANCES; MICROLENSING CANDIDATES; ANDROMEDA GALAXY; POPULATION-II; CEPHEIDS; M-31 AB A search for variable stars is performed using two epochs of Hubble Space Telescope Advanced Camera for Surveys imaging data for a 9.28 arcmin(2) portion of M31. This data set reveals 254 sources that vary by at least 4 sigma between epochs. The positions and two-epoch B-band ( equivalent) photometry of these sources are presented. The photometry suggests that this catalog includes most of the RR Lyrae population of this portion of M31. 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 NR 48 TC 2 Z9 2 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 JUN PY 2005 VL 129 IS 6 BP 2663 EP 2669 DI 10.1086/429735 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 931FY UT WOS:000229472400013 ER PT J AU Covey, KR Greene, TP Doppmann, GW Lada, CJ AF Covey, KR Greene, TP Doppmann, GW Lada, CJ TI The angular momentum content and evolution of Class I and flat-spectrum protostars SO ASTRONOMICAL JOURNAL LA English DT Article DE accretion, accretion disks; infrared : stars; stars : formation; stars : pre-main-sequence; stars : rotation ID T-TAURI STARS; LOW-MASS STARS; MAIN-SEQUENCE STARS; ORION-NEBULA CLUSTER; NEAR-INFRARED SPECTRA; RHO-OPHIUCHI CLOUD; YOUNG STELLAR POPULATION; AURIGA MOLECULAR CLOUD; ROTATIONAL VELOCITIES; ALPHA-PERSEI AB We report on the angular momentum content of heavily embedded protostars on the basis of our analysis of the projected rotation velocities ( v sin I) of 38 Class I / flat- spectrum young stellar objects recently presented by Doppmann and others. After correcting for projection effects, we find that infrared-selected Class I/flat-spectrum objects rotate significantly more quickly ( median equatorial rotation velocity similar to 38 km s(-1)) than classical T Tauri stars (CTTSs; median equatorial rotation velocity similar to 18 km s(-1)) in the rho Ophiuchi and Taurus-Aurigae regions. Projected rotation velocity ( v sin i) is weakly correlated with T-eff in our sample but does not seem to correlate with Br gamma emission ( a common accretion tracer), the amount of excess continuum veiling (r(k)), or the slope of the spectral energy distribution between the near- and mid-IR (alpha). The detected difference in rotation speeds between Class I/flat-spectrum sources and CTTSs proves difficult to explain without some mechanism that transfers angular momentum out of the protostar between the two phases. Assuming that Class I / flat- spectrum sources possess physical characteristics ( M-*, R-*, and B-*) typical of pre-main-sequence stars, fully disk-locked Class I objects should have corotation radii within their protostellar disks that match well ( within 30%) with predicted magnetic coupling radii. The factor of 2 difference in rotation rates between Class I / flat- spectrum and CTTS sources when interpreted in the context of disk-locking models also implies a factor of 5 or greater difference in mass accretion rate between the two phases. A lower limit of. (M) over dot similar to 10(-8) M-. yr(-1) for objects transitioning from the Class I / flat- spectrum stage to CTTSs is required to account for the difference in rotation rates of the two classes by angular momentum extraction through a viscous disk via magnetic coupling. C1 Univ Washington, Dept Astron, Seattle, WA 98195 USA. NASA, Ames Res Ctr, Moffett Field, CA USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Covey, KR (reprint author), Univ Washington, Dept Astron, Box 351580, Seattle, WA 98195 USA. EM covey@astro.washington.edu; thomas.p.greene@nasa.gov; doppmann@gemini.edu; clada@cfa.harvard.edu OI Covey, Kevin/0000-0001-6914-7797 NR 84 TC 21 Z9 21 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 JUN PY 2005 VL 129 IS 6 BP 2765 EP 2776 DI 10.1086/429736 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 931FY UT WOS:000229472400021 ER PT J AU Williamon, RM Van Hamme, W Torres, G Sowell, JR Ponce, VC AF Williamon, RM Van Hamme, W Torres, G Sowell, JR Ponce, VC TI The eclipsing binary system AR Monocerotis SO ASTRONOMICAL JOURNAL LA English DT Article DE binaries : close; binaries : eclipsing; binaries : spectroscopic; stars : individual (AR Monocerotis); stars : variables : other ID LINED SPECTROSCOPIC BINARIES; RADIAL-VELOCITIES; LIGHT CURVES; COOL ALGOLS; STAR LIGHT; ACCURACY; TODCOR; CYGNI; ORBIT AB New differential UBV photoelectric photometry and echelle spectroscopy for the eclipsing binary AR Mon are presented. A total of 46 radial velocities for each component are obtained using the TODCOR procedure. We solve the new and previously published multicolor light curves simultaneously with the new radial velocities using the latest version of the Wilson-Devinney program. We confirm that AR Mon is a semidetached binary consisting of two evolved giant stars and is a member of the rare class of "cool Algols.'' The size of the primary, more massive component is about 1/3 that of its limiting lobe, and the secondary star is a lobe filler. We present two solutions, one without third light, the other including amounts of third light of 8% in V, 6% in B, and 5% in U. We determine magnitudes and colors for AR Mon's two components, as well as for the third star. If real, the latter is estimated to be a dwarf foreground star. The mass and radius of the primary (2.480 +/- 0.014 M-., 8.002 +/- 0.089 R-.) place the star very close to the evolutionary track of a 2.5 M-. single star of solar chemical composition, indicating that the star may have adjusted its structure to mass gained from its companion. Synchronous rotation rates for both stars are in excellent agreement with v sin i values determined from line profiles. C1 Emory Univ, Dept Phys, Atlanta, GA 30322 USA. Florida Int Univ, Dept Phys, Miami, FL 33199 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA. Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA. RP Williamon, RM (reprint author), Emory Univ, Dept Phys, Atlanta, GA 30322 USA. EM rwilliamon@physics.emory.edu; vanhamme@fiu.edu; gtorres@cfa.harvard.edu; jim.sowell@physics.gatech.edu NR 32 TC 8 Z9 8 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD JUN PY 2005 VL 129 IS 6 BP 2798 EP 2805 DI 10.1086/430215 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 931FY UT WOS:000229472400024 ER PT J AU Mochejska, BJ Stanek, KZ Sasselov, DD Szentgyorgyi, AH Bakos, GA Devor, J Hradecky, V Marrone, DP Winn, JN Zaldarriaga, M AF Mochejska, BJ Stanek, KZ Sasselov, DD Szentgyorgyi, AH Bakos, GA Devor, J Hradecky, V Marrone, DP Winn, JN Zaldarriaga, M TI Planets in stellar clusters extensive search. III. A search for transiting planets in the metal-rich open cluster NGC 6791 SO ASTRONOMICAL JOURNAL LA English DT Article DE binaries : eclipsing; novae, cataclysmic variables; planetary systems; stars : variables : other ID GRAVITATIONAL LENSING EXPERIMENT; LUMINOSITY OBJECT TRANSITS; IMAGE SUBTRACTION PHOTOMETRY; GIANT PLANETS; EXTRASOLAR PLANET; GALACTIC DISK; 2001 CAMPAIGN; STARS; FIELD; OLD AB We have undertaken a long-term project, Planets in Stellar Clusters Extensive Search (PISCES), to search for transiting planets in open clusters. In this paper we present the results for NGC 6791, a very old, populous, metal-rich cluster. We have monitored the cluster for over 300 hr, spread over 84 nights. We have not detected any good transiting planet candidates. Given the photometric precision and temporal coverage of our observations and the current best estimates for the frequency and radii of short-period planets, the expected number of detectable transiting planets in our sample is 1.5. We have discovered 14 new variable stars in the cluster, most of which are eclipsing binaries, and present high-precision light curves spanning 2 years for these new variables and also the previously known variables. C1 Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Hungarian Acad Sci, Konkoly Observ, H-1525 Budapest, Hungary. RP Mochejska, BJ (reprint author), Purdue Univ, Dept Phys, 525 NW Ave, W Lafayette, IN 47907 USA. EM bmochejs@cfa.harvard.edu; kstanek@cfa.harvard.edu; sasselov@cfa.harvard.edu; saint@cfa.harvard.edu; gbakos@cfa.harvard.edu; jdevor@cfa.harvard.edu; vhradecky@cfa.harvard.edu; dmarrone@cfa.harvard.edu; jwinn@cfa.harvard.edu; mzaldarriaga@cfa.harvard.edu OI Marrone, Daniel/0000-0002-2367-1080 NR 46 TC 42 Z9 42 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 JUN PY 2005 VL 129 IS 6 BP 2856 EP 2868 DI 10.1086/430219 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 931FY UT WOS:000229472400030 ER PT J AU Henkel, C Peck, AB Tarchi, A Nagar, NM Braatz, JA Castangia, P Moscadelli, L AF Henkel, C Peck, AB Tarchi, A Nagar, NM Braatz, JA Castangia, P Moscadelli, L TI New H2O masers in Seyfert and FIR bright galaxies SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE masers; galaxies : active; galaxies : jets; galaxies : Seyfert; galaxies : starburst; radio lines : galaxies ID ACTIVE GALACTIC NUCLEI; WATER-VAPOR MASER; NARROW-LINE REGION; PARSEC-SCALE JET; ARP 299; IRAS GALAXIES; LUMINOSITY FUNCTIONS; MEGAMASER EMISSION; VLA OBSERVATIONS; RADIO STRUCTURES AB Using the Effelsberg 100-m telescope, detections of four extragalactic water vapor masers are reported. Isotropic luminosities are similar to 50, 1000, 1 and 230 L-circle dot for Mrk 1066 ( UGC 2456), Mrk 34, NGC 3556 and Arp 299, respectively. Mrk 34 contains by far the most distant and one of the most luminous water vapor megamasers so far reported in a Seyfert galaxy. The interacting system Arp 299 appears to show two maser hotspots separated by approximately 20''. With these new results and even more recent data from Braatz et al. ( 2004, ApJ, 617, L29), the detection rate in our sample of Seyferts with known jet-Narrow Line Region interactions becomes 50% ( 7/14), while in star forming galaxies with high ( S-100 mu m > 50 Jy) far infrared fluxes the detection rate is 22% (10/45). The jet-NLR interaction sample may not only contain "jet-masers" but also a significant number of accretion "disk-masers" like those seen in NGC4258. A statistical analysis of 53 extragalactic H2O sources ( excluding the Galaxy and the Magellanic Clouds) indicates ( 1) that the correlation between IRAS Point Source and H2O luminosities, established for individual star forming regions in the galactic disk, also holds for AGN-dominated megamaser galaxies; ( 2) that maser luminosities are not correlated with 60 mu m/100 mu m color temperatures; and ( 3) that only a small fraction of the luminous megamasers ( L-H2O > 100 L-circle dot) detectable with 100-m sized telescopes have so far been identified. The H2O luminosity function (LF) suggests that the number of galaxies with 1L(circle dot) < L-H2O < 10L(circle dot), the transition range between " kilomasers" ( mostly star formation) and " megamasers" ( active galactic nuclei), is small. The overall slope of the LF, similar to-1.5, indicates that the number of detectable masers is almost independent of their luminosity. If the LF is not steepening at very high maser luminosities and if it is possible to find suitable candidate sources, H2O megamasers at significant redshifts should be detectable even with present day state-of-the-art facilities. C1 Max Planck Inst Radioastron, D-53121 Bonn, Germany. Harvard Smithsonian Ctr Astrophys, SAO, SMA Project, Hilo, HI 96720 USA. CNR, Ist Radioastron, I-40129 Bologna, Italy. Osservatorio Astron Cagliari, INAF, I-09012 Capoterra, CO, Italy. Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy. Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. Univ Concepcion, Dept Fis, Astron Grp, Concepcion, Chile. Natl Radio Astron Observ, Green Bank, WV 24944 USA. Citta Univ, Dipartimento Fis, Univ Cagliari, I-09012 Capoterra, CA, Italy. RP Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. EM chenkel@mpifr-bonn.mpg.de OI Castangia, Paola/0000-0002-2318-8531; Moscadelli, Luca/0000-0002-8517-8881; Tarchi, Andrea/0000-0001-8540-3500 NR 98 TC 54 Z9 56 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUN PY 2005 VL 436 IS 1 BP 75 EP 90 DI 10.1051/0004-6361:20042175 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 928IR UT WOS:000229265500011 ER PT J AU Perrin, G Ridgway, ST Verhoelst, T Schuller, PA du Foresto, VC Traub, WA Millan-Gabet, R Lacasse, MG AF Perrin, G Ridgway, ST Verhoelst, T Schuller, PA du Foresto, VC Traub, WA Millan-Gabet, R Lacasse, MG TI Study of molecular layers in the atmosphere of the supergiant star mu Cep by interferometry in the K band SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE techniques : interferometric; stars : fundamental parameters; stars : mass-loss; infrared : stars; stars : individual : mu Cep ID WATER-VAPOR ENVELOPE; APPARENT SIZE; ALPHA-ORIONIS; OPTICAL INTERFEROMETER; MILKY-WAY; VISIBILITIES; GIANTS; MODEL; CALIBRATION; EXTINCTION AB Infrared interferometry of supergiant and Mira stars has recently been reinterpreted as revealing the presence of deep molecular layers. Empirical models for a photosphere surrounded by a simple molecular layer or envelope have led to a consistent interpretation of previously inconsistent data. The stellar photospheres are found to be smaller than previously understood, and the molecular layer is much higher and denser than predicted by hydrostatic equilibrium. However, the analysis was based on spatial observations with medium-band optical filters, which mixed the visibilities of different spatial structures. This paper reports spatial interferometry with narrow spectral bands, isolating near-continuum and strong molecular features, obtained for the supergiant mu Cep. The measurements confirm strong variation of apparent diameter across the K-band. A layer model shows that a stellar photosphere of angular diameter 14.11 +/- 0.60 mas is surrounded by a molecular layer of diameter 18.56 +/- 0.26 mas, with an optical thickness varying from nearly zero at 2.15 mu m to > 1 at 2.39 mu m. Although mu Cep and alpha Ori have a similar spectral type, interferometry shows that they differ in their radiative properties. Comparison with previous broad-band measurements shows the importance of narrow spectral bands. The molecular layer or envelope appears to be a common feature of cool supergiants. C1 Observ Paris, LESIA, UMR 8109, F-92190 Meudon, France. Natl Opt Astron Observ, Tucson, AZ 85726 USA. Katholieke Univ Leuven, Inst Sterrenkunde, Louvain, Belgium. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CALTECH, Michelson Sci Ctr, Pasadena, CA 91125 USA. RP Observ Paris, LESIA, UMR 8109, F-92190 Meudon, France. EM guy.perrin@obspm.fr NR 35 TC 23 Z9 23 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 JUN PY 2005 VL 436 IS 1 BP 317 EP 324 DI 10.1051/0004-6361:20042313 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 928IR UT WOS:000229265500029 ER PT J AU Maccarone, TJ Jonker, PG Sills, AI AF Maccarone, TJ Jonker, PG Sills, AI TI Lithium enhancement in X-ray binaries due to stellar rotation SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars : abundances; binaries : close; X-rays : binaries ID ACCRETION-INDUCED COLLAPSE; GLOBULAR-CLUSTERS; NEUTRON-STARS; BLACK-HOLES; COMPANIONS; MASS; ABUNDANCES; EVOLUTION; SOFT; TRANSIENTS AB We discuss the high lithium abundances in the secondary stars of X-ray binaries. We show that no lithium production in these stars is necessary, and that the abundances can be explained simply due to the tidally locked rotation of the stars, which lead naturally to slower lithium destruction rates. The differences in abundances of CVs' secondaries from those of LMXBs had previously been put forth as evidence that the compact object was related to the lithium abundance, but this scenario also accounts for the lower lithium abundances in the secondary stars in cataclysmic variable systems (CVs) than in low mass X-ray binaries (LMXBs), since these stars have typically lived much longer before becoming tidally locked short period systems. We point out that if this scenario is correct, then the globular cluster X-ray binaries' donor stars should, as a class, show less lithium enhancement relative to other stars of the same spectral type in the clusters than the field X-ray binaries donor stars show. C1 Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02139 USA. McMaster Univ, Dept Phys & Astron, Hamilton, ON L8S 4M1, Canada. SRON, Natl Inst Space Res, NL-3584 CA Utrecht, Netherlands. RP Maccarone, TJ (reprint author), Univ Amsterdam, Astron Inst Anton Pannekoek, Kruislaan 403, NL-1098 SJ Amsterdam, Netherlands. EM tjm@science.uva.nl NR 29 TC 5 Z9 5 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 JUN PY 2005 VL 436 IS 2 BP 671 EP 675 DI 10.1051/0004-6361:20052791 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 931HE UT WOS:000229475600035 ER PT J AU Kravtsov, AV Nagai, D Vikhlinin, AA AF Kravtsov, AV Nagai, D Vikhlinin, AA TI Effects of cooling and star formation on the baryon fractions in clusters SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : theory; galaxies : formation; methods : numerical ID X-RAY-CLUSTERS; DARK-MATTER HALOS; NEARBY GALAXY CLUSTERS; GAS MASS FRACTION; K-BAND PROPERTIES; INTRACLUSTER MEDIUM; COSMOLOGICAL SIMULATIONS; INTERGALACTIC GAS; SCALING RELATIONS; CONSTRAINTS AB We study the effects of radiative cooling and galaxy formation on the baryon fractions in clusters using high-resolution cosmological simulations that resolve formation of cluster galaxies. The simulations of nine individual clusters spanning a decade in mass are performed with the shock-capturing Eulerian adaptive mesh refinement N-body+gasdynamical Adaptive Refinement Tree code. For each cluster the simulations were done in the adiabatic regime ( without dissipation) and with radiative cooling and several physical processes critical to various aspects of galaxy formation: star formation, metal enrichment, and stellar feedback. We show that radiative cooling of gas and associated star formation increase the total baryon fractions within radii as large as the virial radius. The effect is strongest within cluster cores, where the simulations with cooling have baryon fractions larger than the universal value, in contrast to the adiabatic simulations in which the fraction of baryons is substantially smaller than the universal value. At larger radii ( r greater than or similar to r(500)) the cumulative baryon fractions in simulations with cooling are close to the universal value. The gas fractions in simulations with dissipation are reduced by approximate to 20% - 40% at r < 0.3r(vir) and approximate to 10% at larger radii compared to the adiabatic runs, because a fraction of gas is converted into stars. There is an indication that gas fractions within different radii increase with increasing cluster mass as f(gas) proportional to M-vir(0.2). We find that the total baryon fraction within the cluster virial radius does not evolve with time in both adiabatic simulations and in simulations with cooling. The gas fractions in the latter decrease slightly from z = 1 to 0 due to ongoing star formation. Finally, to evaluate systematic uncertainties in the baryon fraction in cosmological simulations we present a comparison of gas fractions in our adiabatic simulations to resimulations of the same objects with the entropy-conserving smoothed particle hydrodynamics (SPH) code Gadget. The cumulative gas fraction profiles in the two sets of simulations on average agree to better than approximate to 3% outside the cluster core ( r/r(vir) greater than or similar to 0.2) but differ by up to 10% at small radii. The differences are smaller than those found in previous comparisons of Eulerian and SPH simulations. Nevertheless, they are systematic and have to be kept in mind when using gas fractions from cosmological simulations. C1 Univ Chicago, Kavli Inst Cosmol Phys, Dept Astron & Astrophys, Chicago, IL 60637 USA. Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Space Res Inst, Moscow 117997, Russia. RP Kravtsov, AV (reprint author), Univ Chicago, Kavli Inst Cosmol Phys, Dept Astron & Astrophys, 5640 S Ellis Ave, Chicago, IL 60637 USA. EM andrey@oddjob.uchicago.edu; daisuke@oddjob.uchicago.edu NR 63 TC 143 Z9 145 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 JUN 1 PY 2005 VL 625 IS 2 BP 588 EP 598 DI 10.1086/429796 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 930SJ UT WOS:000229436900002 ER PT J AU Kraft, RP Nolan, LA Ponman, TJ Jones, C Raychaudhury, S AF Kraft, RP Nolan, LA Ponman, TJ Jones, C Raychaudhury, S TI A Chandra observation of the nearby lenticular galaxy NGC 5102: Where are the X-ray binaries? SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : individual (NGC 5102); galaxies : ISM; X-rays : binaries; X-rays : galaxies ID STAR-FORMATION RATE; GLOBULAR CLUSTER CONNECTION; INTERSTELLAR-MEDIUM; ELLIPTIC GALAXIES; GALACTIC NUCLEI; EMISSION MECHANISMS; SPECTRAL PROPERTIES; NGC 5128; EVOLUTION; POPULATION AB We present results from a 34 ks Chandra ACIS-S observation of the low-mass X-ray binary (LMXB) population and the hot interstellar medium (ISM) in the nearby (d = 3: 1 Mpc) lenticular galaxy NGC 5102, previously shown to have an unusually low X-ray luminosity. We detect 11 X-ray point sources within the D-25 optical boundary of the galaxy (93% of the light), one-third to one-half of which are likely to be background active galactic nuclei (AGNs). One of the X-ray sources is coincident with the optical nucleus and may be a low-luminosity AGN. Only two sources with an X-ray luminosity greater than 10(37) ergs s(-1) in the 0.5-5.0 keV band were detected, one of which is statistically likely to be a background AGN. We expected to detect seven or five such luminous sources if the X-ray binary (XRB) population scales linearly with the B-band or J-band magnitudes, respectively, of the host galaxy. By this measure, NGC 5102 has an unusually low number of XRBs. The deficit of LMXBs is even more striking, because some of these sources may in fact be high- mass X-ray binaries (HMXBs). NGC 5102 is unusually blue for its morphological type and has undergone at least two recent bursts of star formation only similar to 1.5; 10(7) and similar to 3 x 10(8) yr ago. We present the results of optical/UV spectral synthesis analysis and demonstrate that a significant fraction (> 50%) of the stars in this galaxy are comparatively young (< 3; 10(9) yr old). We discuss the relationship between the XRB population, the globular cluster ( GC) population, and the relative youth of the majority of stars in this galaxy. If the lack of X-ray binaries is related to the relative youth of most of the stars, this would support models of LMXB formation and evolution that require wide binaries to shed angular momentum on a timescale of Gyr. We have also analyzed archival Hubble Space Telescope ( HST) images of NGC 5102 and find that it has an unusually low specific frequency of GCs (S-N similar to 0: 4). The lack of LMXBs could also be explained by the small number of GCs. We have also detected diffuse X-ray emission in the central similar to 1 kpc of the galaxy with an X-ray luminosity of 4: 1; 10(37) ergs s - 1 in the 0.1-2.0 keV band. This hot gas is most likely a superbubble created by multiple supernovae of massive stars born during the most recent star burst and is driving the shock into the ISM, which was inferred from previous [OIII] lambda 5007 and H alpha observations. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. RP Kraft, RP (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-67, Cambridge, MA 02138 USA. NR 58 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 JUN 1 PY 2005 VL 625 IS 2 BP 785 EP 795 DI 10.1086/429982 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 930SJ UT WOS:000229436900019 ER PT J AU Heinke, CO Grindlay, JE Edmonds, PD Cohn, HN Lugger, PM Camilo, F Bogdanov, S Freire, PC AF Heinke, CO Grindlay, JE Edmonds, PD Cohn, HN Lugger, PM Camilo, F Bogdanov, S Freire, PC TI A deep Chandra survey of the globular cluster 47 tucanae: Catalog of point sources SO ASTROPHYSICAL JOURNAL LA English DT Review DE globular clusters : individual (NGC 104); novae, cataclysmic variables; pulsars : general; stars : neutron; X-rays : binaries ID X-RAY SOURCES; HUBBLE-SPACE-TELESCOPE; CLUSTER 47 TUCANAE; ALL-SKY SURVEY; MAGNETIC CATACLYSMIC VARIABLES; GALACTIC GLOBULAR-CLUSTERS; XMM-NEWTON OBSERVATION; FAR-ULTRAVIOLET SURVEY; ACTIVE BINARY CORONAE; HELIUM WHITE-DWARF AB We have detected 300 X-ray sources within the half-mass radius (2.'79) of the globular cluster 47 Tucanae in a deep (281 ks) Chandra exposure. We perform photometry and simple spectral fitting for our detected sources and construct luminosity functions, X-ray color-magnitude, and color-color diagrams. Eighty-seven X-ray sources show variability on timescales from hours to years. Thirty-one of the new X-ray sources are identified with chromospherically active binaries from the catalogs of Albrow and coworkers. The radial distributions of detected sources imply that roughly 70 are background sources of some kind. The radial distribution of the known millisecond pulsar ( MSP) systems is consistent with that expected from mass segregation, if the average neutron star mass is 1: 39 +/- 0: 19 M(circle dot). Most source spectra are well fitted by thermal plasma models, except for quiescent low-mass X-ray binaries (qLMXBs; containing accreting neutron stars) and MSPs. We identify three new candidate qLMXBs with relatively low X-ray luminosities. One of the brightest cataclysmic variables (CVs; X10) shows evidence (a 4.7 hr period pulsation and strong soft X-ray emission) for a magnetically dominated accretion flow as in AM Her systems. Most of the bright CVs require intrinsic N(H) columns of order 10(21) cm(-2), suggesting a possible DQ Her nature. A group of X-ray sources associated with bright ( sub) giant stars also requires intrinsic absorption. By comparing the X-ray colors, luminosities, variability, and quality of spectral fits of the detected MSPs to those of unidentified sources, we estimate that a total of similar to 25 MSPs exist in 47 Tuc (< 60 at 95% confidence), regardless of their radio beaming fraction. We estimate that the total number of neutron stars in 47 Tuc is of order 300, reducing the discrepancy between theoretical neutron star retention rates and observed neutron star populations in globular clusters. Comprehensive tables of source properties and simple spectral fits are provided electronically. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA. Indiana Univ, Dept Astron, Bloomington, IN 47405 USA. Columbia Univ, Astrophys Lab, New York, NY 10027 USA. Arecibo Observ, Natl Astron & Ionosphere Ctr, Arecibo, PR 00612 USA. RP Heinke, CO (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM cheinke@cfa.harvard.edu; josh@cfa.harvard.edu; pedmonds@cfa.harvard.edu; cohn@indiana.edu; lugger@indiana.edu; fernando@astro.columbia.edu; sbogdanov@cfa.harvard.edu; pfreire@naic.edu OI Bogdanov, Slavko/0000-0002-9870-2742; Heinke, Craig/0000-0003-3944-6109 NR 127 TC 115 Z9 116 U1 1 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 2005 VL 625 IS 2 BP 796 EP 824 DI 10.1086/429899 PN 1 PG 29 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 930SJ UT WOS:000229436900020 ER PT J AU Zhang, QZ Hunter, TR Brand, J Sridharan, TK Cesaroni, R Molinari, S Wang, J Kramer, M AF Zhang, QZ Hunter, TR Brand, J Sridharan, TK Cesaroni, R Molinari, S Wang, J Kramer, M TI Search for CO outflows toward a sample of 69 high-mass protostellar candidates. II. Outflow properties SO ASTROPHYSICAL JOURNAL LA English DT Article DE HII regions; ISM : clouds; ISM : jets and outflows; ISM : kinematics and dynamics; stars : formation ID ULTRACOMPACT HII-REGIONS; LUMINOUS IRAS SOURCES; FAR-INFRARED SOURCES; BIPOLAR MOLECULAR OUTFLOWS; YOUNG STELLAR OBJECTS; STAR-FORMATION; LINE EMISSION; H2O MASERS; CLOUDS; JET AB We present a study of molecular outflows toward a sample of 69 luminous IRAS point sources. The sample is associated with dense molecular gas and has far-infrared luminosities ranging from 10(2) to 10(5) L-circle dot, indicating these objects as regions likely forming high-mass stars. Mapping in the CO = J 2-1 line shows that molecular outflows are ubiquitous in these regions. Most of the outflows have masses of tens of M (circle dot). The typical dynamical timescale of the flow, without correcting for inclination of the flow axis, is a few times 10(4) yr. The typical energy in the outflows is 10(46) ergs, comparable to the turbulent energy in the core. Nearly half of the outflows show spatially resolved bipolar lobes. This indicates that low-mass young stars that coexist in the region are not responsible for the bipolar outflows observed. It is the more massive stars that drive the outflow. The large detection rate of outflows in the region favors an accretion process in the formation of massive stars. The maximum mass-loss rate in the wind is about 10(-4)M (circle dot) yr(-1). If these outflows are driven via accretion, the accretion rate should be as high as a few times 10(-4)M(circle dot)yr(-1). We compare CO outflows with images at near-infrared wavelengths from the Two Micron All Sky Survey (2MASS) archive and find that some outflows are associated with extended emission in the K band, which may be partly due to vibrationally excited H-2 emission at 2.12 mu m. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CNR, Ist Radioastron, I-40129 Bologna, Italy. Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy. CNR, Ist Fis Spazio Interplanetario, I-00133 Rome, Italy. Peking Univ, Dept Astron, Beijing 100871, Peoples R China. Oberlin Coll, Oberlin, OH 44074 USA. RP Zhang, QZ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Molinari, Sergio/O-4095-2016; OI Molinari, Sergio/0000-0002-9826-7525; Brand, Jan/0000-0003-1615-9043; Cesaroni, Riccardo/0000-0002-2430-5103; Hunter, Todd/0000-0001-6492-0090; Zhang, Qizhou/0000-0003-2384-6589 NR 69 TC 133 Z9 134 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 JUN 1 PY 2005 VL 625 IS 2 BP 864 EP 882 DI 10.1086/429660 PN 1 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 930SJ UT WOS:000229436900026 ER PT J AU Bourke, TL Hyland, AR Robinson, G AF Bourke, TL Hyland, AR Robinson, G TI On the identification of high-mass star forming regions using IRAS: Contamination by low-mass protostars SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; ISM : clouds; masers; stars : formation ID H-II REGIONS; ULTRACOMPACT HII-REGIONS; YOUNG STELLAR OBJECTS; SOUTHERN GALACTIC PLANE; POINT-SOURCE-CATALOG; GHZ METHANOL MASERS; SMALL DARK CLOUDS; MOLECULAR CLOUDS; PROTOSTELLAR CANDIDATES; HIGH-RESOLUTION AB We present the results of a survey of a small sample (14) of low-mass protostars (L-IR < 10(3) L-circle dot) for 6.7 GHz methanol maser emission performed using the ATNF Parkes radio telescope. No new masers were discovered. We find that the lower luminosity limit for maser emission is near 10(3) L-circle dot by comparison of the sources in our sample with previously detected methanol maser sources. We examine the IRAS properties of our sample and compare them with sources previously observed for methanol maser emission, almost all of which satisfy the Wood & Churchwell criterion for selecting candidate UC H-II regions. We find that about half of our sample satisfy this criterion, and in addition, almost all of this subgroup have integrated fluxes between 25 and 60 mu m that are similar to sources with detectable methanol maser emission. By identifying a number of low-mass protostars in this work and from the literature that satisfy the Wood & Churchwell criterion for candidate UC H (II) regions, we show conclusively for the first time that the fainter flux end of their sample is contaminated by lower mass nonionizing sources, confirming the suggestion by van der Walt and Ramesh & Sridharan. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. James Cook Univ N Queensland, Deputy Vicechancellors Off, Townsville, Qld 4811, Australia. Australian Def Force Acad, UNSW ADFA, Sch Phys Environm & Math Sci, Canberra, ACT 2600, Australia. RP Bourke, TL (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM tbourke@cfa.harvard.edu NR 83 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 JUN 1 PY 2005 VL 625 IS 2 BP 883 EP 890 DI 10.1086/429818 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 930SJ UT WOS:000229436900027 ER PT J AU Muzerolle, J Luhman, KL Briceno, C Hartmann, L Calvet, N AF Muzerolle, J Luhman, KL Briceno, C Hartmann, L Calvet, N TI Measuring accretion in young substellar objects: Approaching the planetary mass regime SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; circumstellar matter; stars : emission-line, Be; stars : low-mass, brown dwarfs; stars : pre-main sequence ID T-TAURI STARS; BROWN DWARFS; DISK ACCRETION; FORMING REGION; EVOLUTIONARY MODELS; EMISSION; CENSUS; RATES AB We present observations of H alpha emission-line profiles taken at Magellan Observatory for a sample of 39 young low-mass stars and brown dwarfs in the Taurus and Chamaeleon I star-forming regions. We have identified 11 new substellar accretors, more than tripling the number of known brown dwarfs with measurable accretion activity. These include the lowest-mass objects yet seen with accretion, with masses down to similar to 0.015 M-circle dot. Using models of H alpha emission produced in magnetospheric accretion flows, the most widely applicable primary calibrator now available, we determine the first estimates of mass accretion rates for objects at such extremely low masses. For the six objects with masses less than or similar to 0.03M(circle dot), we find accretion rates of similar to 5 x 10(-12) M(circle dot)yr(-1), among the smallest yet measured. These new results continue the trend of decreasing mass accretion rate with decreasing (sub) stellar mass that we have noted previously for samples of more massive objects; the overall correlation is. M proportional to M-2.1, and it now extends over a mass range of over 2 orders of magnitude. Finally, the absence of a discontinuity in the distribution of accretion rates with mass tends to suggest that stars and brown dwarfs share similar formation histories. C1 Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Ctr Invest Astron, Merida 5101A, Venezuela. RP Muzerolle, J (reprint author), Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA. NR 37 TC 184 Z9 184 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 JUN 1 PY 2005 VL 625 IS 2 BP 906 EP 912 DI 10.1086/429483 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 930SJ UT WOS:000229436900029 ER PT J AU Drake, JJ Werner, K AF Drake, JJ Werner, K TI Deposing the cool corona of KPD 0005+5106 SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars : activity; stars : coronae; stars : mass loss; white dwarfs; X-rays : stars ID PHOTOIONIZATION CROSS-SECTIONS; WHITE-DWARF KPD-0005+5106; HUBBLE-SPACE-TELESCOPE; X-RAY-EMISSION; HOT; SPECTROSCOPY; STARS; ATOMS; FUSE; IONS AB The ROSAT PSPC pulse-height spectrum of the peculiar He-rich hot white dwarf KPD 0005+5106 provided a great surprise when first analyzed by Fleming, Werner,& Barstow. It defied the best non-LTE modeling attempts in terms of photospheric emission from He-dominated atmospheres including C, N, and O and was instead interpreted as the first evidence for a coronal plasma around a white dwarf. We show here that a recent high-resolution Chandra LETGS spectrum has more structure than expected from a thermal bremsstrahlung continuum and lacks the narrow lines of H- like and He-like C expected from a coronal plasma. Moreover, a coronal model requires a total luminosity more than 2 orders of magnitude larger than that of the star itself. Instead, the observed 20-80 angstrom flux is consistent with photospheric models containing trace amounts of heavier elements such as Fe. The soft X-ray flux is highly sensitive to the adopted metal abundance and provides a metal abundance diagnostic. The weak X-ray emission at 1 keV announced by O'Dwyer and coworkers instead cannot arise from the photosphere and requires alternative explanations. We echo earlier speculation that such emission arises in a shocked wind. Despite the presence of UV-optical O VIII lines from transitions between levels n = 7 and 10, no X-ray O VIII Ly alpha flux is detected. We show that O VIII Lyman photons can be trapped by resonant scattering within the emitting plasma and destroyed by photoelectric absorption. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. Inst Astron & Astrophys, D-72076 Tubingen, Germany. RP Drake, JJ (reprint author), Smithsonian Astrophys Observ, MS-3,60 Garden St, Cambridge, MA 02138 USA. EM jdrake@cfa.harvard.edu; werner@astro.uni-tuebingen.de NR 26 TC 7 Z9 7 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 JUN 1 PY 2005 VL 625 IS 2 BP 973 EP 977 DI 10.1086/429661 PN 1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 930SJ UT WOS:000229436900036 ER PT J AU Creevey, OL Benedict, GF Brown, TM Alonso, R Cargile, P Mandushev, G Charbonneau, D McArthur, BE Cochran, W O'Donovan, FT Jimenez-Reyes, SJ Belmonte, JA Kolinski, D AF Creevey, OL Benedict, GF Brown, TM Alonso, R Cargile, P Mandushev, G Charbonneau, D McArthur, BE Cochran, W O'Donovan, FT Jimenez-Reyes, SJ Belmonte, JA Kolinski, D TI A new detached m dwarf eclipsing binary SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : close; binaries : eclipsing; stars : individual ( TrES-Her0-07621); stars : late-type ID COLOR-MAGNITUDE DIAGRAMS; HUBBLE-SPACE-TELESCOPE; HOBBY-EBERLY TELESCOPE; LOW-MASS STARS; ABSOLUTE DIMENSIONS; EVOLUTIONARY MODELS; YY-GEMINORUM; MAIN-SEQUENCE; CM DRACONIS; SYSTEM AB We describe a newly discovered detached M dwarf eclipsing binary system. This system was first observed by the TrES network during a long-term photometry campaign of 54 nights. Analysis of the folded light curve indicates two very similar components orbiting each other with a period of 1.12079 +/- 0.00001 days. Spectroscopic observations with the Hobby-Eberly Telescope show the system to consist of two M3e dwarfs in a near-circular orbit. Double-line radial velocity amplitudes, combined with the orbital inclination derived from light-curve fitting, yield M-total = 0.983 +/- 0.007 M-circle dot with component masses of M-1 = 0.493 +/- 0.003 M-circle dot and M-2 = The light-curve fit yields component radii of R-1 = 0.489 +/- 0.003 R-circle dot and R-2 = 0.452 +/- 0.050 R-circle dot. Although a precise parallax is lacking, broadband VJHK colors and spectral typing suggest component 0.050 absolute magnitudes of and. M (1) = 11.18 +/- 0.30 M (2) = 11.28 +/- 0.30. C1 Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA. Univ La Laguna, E-38206 San Cristobal la Laguna, Tenerife, Spain. Inst Astrofis Canarias, E-38200 San Cristobal la Laguna, Tenerife, Spain. Univ Texas, McDonald Observ, Austin, TX 78712 USA. Lowell Observ, Flagstaff, AZ 86001 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CALTECH, Pasadena, CA 91125 USA. RP Creevey, OL (reprint author), Natl Ctr Atmospher Res, High Altitude Observ, 3450 Mitchel Lane, Boulder, CO 80307 USA. EM creevey@hao.ucar.edu; fritz@astro.as.utexas.edu; timbrown@hao.ucar.edu; ras@iac.es; p.cargile@mail.utexas.edu; gmand@lowell.edu; dcharbonneau@cfa.harvard.edu; mca@barney.as.utexas.edu; wdc@shiraz.as.utexas.edu; francis@caltech.edu; sjimenez@iac.es; jba@iac.es; kolinski@hao.ucar.edu RI Alonso, Roi/D-8799-2014; O'Donovan, Francis/I-2423-2014 OI Alonso, Roi/0000-0001-8462-8126; Jimenez Reyes, Sebastian/0000-0002-0317-4247; O'Donovan, Francis/0000-0002-4858-6106 NR 29 TC 35 Z9 36 U1 1 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 JUN 1 PY 2005 VL 625 IS 2 BP L127 EP L130 DI 10.1086/431278 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 930SK UT WOS:000229437000015 ER PT J AU Dupree, AK Brickhouse, NS Smith, GH Strader, J AF Dupree, AK Brickhouse, NS Smith, GH Strader, J TI A hot wind from the classical T tauri stars: TW hydrae and T tauri SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared : stars; stars : individual ( TW Hydrae, T Tauri); stars : pre-main-sequence stars : winds, outflows; ultraviolet : stars ID MAIN-SEQUENCE STARS; LUMINOUS COOL STARS; ECHELLE SPECTROGRAPH; ULTRAVIOLET-SPECTRA; H-2 FLUORESCENCE; YOUNG STARS; DG-TAURI; ACCRETION; EMISSION; SPECTROSCOPY AB Spectroscopy of the infrared He (I) (10830 angstrom) line with NIRSPEC on Keck and CSHELL at the IRTF, and of the ultraviolet C (III) ( 977) and O (VI) (1032 angstrom) emission with FUSE, reveals that the classical T Tauri star TW Hydrae exhibits P Cygni profiles, line asymmetries, and absorption indicative of a continuous, fast (similar to 400 km s(-1)), hot (similar to 300,000 K) accelerating outflow with a mass-loss rate similar to 10(-11) to 10(-12) M-circle dot yr(-1) or larger. Spectra of T Tau N appear consistent with such a wind. The source of the emission and outflow seems restricted to the stars themselves. Although the mass accretion rate is an order of magnitude less for TW Hya than for T Tau, the outflow reaches higher velocities at chromospheric temperatures in TW Hya. Winds from young stellar objects may be substantially hotter and faster than previously thought. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Calif Santa Cruz, Dept Astron & Astrophys, UCO Lick Observ, Santa Cruz, CA 95064 USA. RP Dupree, AK (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM adupree@cfa.harvard.edu OI Brickhouse, Nancy/0000-0002-8704-4473 NR 38 TC 67 Z9 67 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 JUN 1 PY 2005 VL 625 IS 2 BP L131 EP L134 DI 10.1086/431323 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 930SK UT WOS:000229437000016 ER PT J AU Hopkins, PF Hernquist, L Martini, P Cox, TJ Robertson, B Di Matteo, T Springel, V AF Hopkins, PF Hernquist, L Martini, P Cox, TJ Robertson, B Di Matteo, T Springel, V TI A physical model for the origin of quasar lifetimes SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : theory; galaxies : active; galaxies : evolution; galaxies : nuclei quasars : general ID DIGITAL SKY SURVEY; PARTICLE HYDRODYNAMICS SIMULATIONS; SUPERMASSIVE BLACK-HOLES; ACTIVE GALACTIC NUCLEUS; DARK-MATTER UNIVERSE; GALAXIES; GROWTH; LUMINOSITY; EVOLUTION; REDSHIFT AB We propose a model of quasar lifetimes in which longer periods of rapid black hole accretion are distinguished from observationally inferred lifetimes of quasars owing to gas and dust obscuration. In our picture, quasars are powered by gas funneled to galaxy centers, fueling starbursts and feeding black hole growth, but are "buried" until feedback from the accretion disperses the obscuring material, creating a window in which the black hole is observable as an optical quasar. Eventually, the activity ceases when the accretion rate drops below that required to maintain quasar luminosities. We study this process by simulating galaxy mergers, using the gas density to infer the bolometric luminosity of the black hole and the gas metallicity and column density to determine the B-band attenuation along arbitrary lines of sight. Defining the visible quasar lifetime as the total time with an observed B-band luminosity greater than some lower limit L-B,L-min, we find lifetimes similar to 10-20 Myr for L-B,L-min = 10(11) L-circle dot (M-B approximate to -23), in good agreement with observations, but significantly shorter than the "intrinsic" lifetime similar to 100 L-circle dot Myr obtained if attenuation is neglected. The ratio of observed to intrinsic lifetimes is also a strong function of both the limiting luminosity and observed frequency range. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Max Planck Inst Astrophys, D-85740 Garching, Germany. RP Hopkins, PF (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Di Matteo, Tiziana/O-4762-2014 OI Di Matteo, Tiziana/0000-0002-6462-5734 NR 42 TC 216 Z9 216 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 JUN 1 PY 2005 VL 625 IS 2 BP L71 EP L74 DI 10.1086/431146 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 930SK UT WOS:000229437000001 ER PT J AU McClure-Griffiths, NM Dickey, JM Gaensler, BM Green, AJ Haverkorn, M Strasser, S AF McClure-Griffiths, NM Dickey, JM Gaensler, BM Green, AJ Haverkorn, M Strasser, S TI The Southern Galactic Plane Survey: HI observations and analysis SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE Galaxy : structure; ISM : structure; radio lines : ISM; surveys ID INNER GALAXY; ABSORPTION; SHELLS; CALIBRATION; WARM; ARM AB We describe the H I component of the Southern Galactic Plane Survey (SGPS). The SGPS is a large-scale project to image at arcminute resolution the H I spectral line and 21 cm continuum emission in parts of the plane of the Milky Way. The survey covers Galactic longitudes 253 degrees <= l <= 358 degrees and latitudes \b\ <= 1.degrees 5 (SGPS I), plus a first quadrant extension covering 5 degrees <= l <= 20 degrees and \b\ <= 1.degrees 5 ( SGPS II). The survey combines data from the Australia Telescope Compact Array and the Parkes Radio Telescope for sensitivity to angular scales ranging from 20 to several degrees. The combined data cover 325 deg(2) and have an rms sensitivity of 1.6 K. Here we describe the H I observations and data reduction in detail and present examples from the final data products. The complete data set is publicly available through the Australia Telescope National Facility's H I Surveys archive. This data set provides an unprecedented view of the neutral component of interstellar hydrogen in the inner Milky Way. C1 CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. Univ Minnesota, Dept Astron, Minneapolis, MN 55455 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Sydney, Sch Phys, Sydney, NSW 2006, Australia. RP McClure-Griffiths, NM (reprint author), CSIRO, Australia Telescope Natl Facil, POB 76, Epping, NSW 1710, Australia. EM naomi.mcclure-griffiths@csiro.au; john@astro.umn.edu; bgaensler@cfa.harvard.edu; agreen@physics.usyd.edu.au; mhaverkorn@cfa.harvard.edu; strasser@astro.umn.edu RI Gaensler, Bryan/F-8655-2010; Dickey, John/C-6156-2013; OI McClure-Griffiths, Naomi/0000-0003-2730-957X; Dickey, John/0000-0002-6300-7459 NR 30 TC 205 Z9 206 U1 0 U2 3 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 JUN PY 2005 VL 158 IS 2 BP 178 EP 187 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 930SM UT WOS:000229437300003 ER PT J AU Cunningham, A Frank, A Varniere, P Poludnenko, A Mitran, S Hartmann, L AF Cunningham, A Frank, A Varniere, P Poludnenko, A Mitran, S Hartmann, L TI Evolution and fragmentation of wide-angle wind driven molecular outflows SO ASTROPHYSICS AND SPACE SCIENCE LA English DT Article; Proceedings Paper CT 5th International Conference on High Energy Density Laboratory Astrophysics CY MAR 10-13, 2004 CL Tucson, AZ DE protostellar outflow; HH object; molecular outflow; wide-angle wind; fragmentation ID INTER-STELLAR SHOCKS; INFRARED-EMISSION; DISSOCIATION; EXCITATION; HYDROGEN; IONIZATION; ATOMS AB We present two dimensional cylindrically symmetric hydrodynamic simulations and synthetic emission maps of a stellar wind propagating into an infalling, rotating environment. The resulting outflow morphology, collimation and stability observed in these simulations have relevance to the study of young stellar objects, Herbig-Haro jets and molecular outflows. Our code follows hydrogen gas with molecular, atomic and ionic components tracking the associated time dependent molecular chemistry and ionization dynamics with radiative cooling appropriate for a dense molecular gas. We present tests of the code as well as new simulations which indicate the presence of instabilities in the wind-blown bubbles swept-up shell. C1 Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. Univ N Carolina, Chapel Hill, NC USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Cunningham, A (reprint author), Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. RI Mitran, Sorin/G-4682-2011 NR 20 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 JUN PY 2005 VL 298 IS 1-2 BP 317 EP 322 DI 10.1007/s10509-005-3961-x PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 934MK UT WOS:000229712700047 ER PT J AU Sanchez, CR Murray, SZ AF Sanchez, CR Murray, SZ TI Diagnosis and successful treatment of a presumptive case of aspergillosis in a Micronesian kingfisher (Halcyon cinnamomina cinnamomina) SO AVIAN DISEASES LA English DT Article DE aspergillosis; itraconazole; electrophoresis; Micronesian kingfisher ID PROTEIN ELECTROPHORESIS AB A 4-yr-old male Micronesian kingfisher was suspected of having an aspergillus infection. The infection was thought to be related to stress associated with movement to a new enclosure/exhibit and cage-mate aggression. The diagnosis was based on an elevated white cell count, positive antibody and antigen aspergillus titers, and abnormal plasma protein electrophoresis characterized by a moderate elevation of alpha 2 and severe elevation on the beta protein Fractions. The bird was treated with antifungal medication administered systemically and by nebulization for 10 wk. Response to treatment was monitored by serial white cell counts and plasma electrophoresis. Clinical improvement in this bird was correlated with a return of the white blood cell count to normal levels and what was considered a normal protein electrophoresis distribution. C1 Smithsonian Inst, Natl Zool Pk, Dept Anim Hlth, Washington, DC 20008 USA. RP Sanchez, CR (reprint author), Smithsonian Inst, Natl Zool Pk, Dept Anim Hlth, 3001 Connecticut Ave NW, Washington, DC 20008 USA. NR 23 TC 2 Z9 3 U1 2 U2 2 PU AMER ASSOC AVIAN PATHOLOGISTS PI ATHENS PA 953 COLLEGE STATION RD, ATHENS, GA 30602-4875 USA SN 0005-2086 J9 AVIAN DIS JI Avian Dis. PD JUN PY 2005 VL 49 IS 2 BP 309 EP 312 DI 10.1637/7336-020105R PG 4 WC Veterinary Sciences SC Veterinary Sciences GA 937TV UT WOS:000229949500024 PM 16094842 ER PT J AU Villanueva-G, R Roubik, DW Colli-Ucan, W AF Villanueva-G, R Roubik, DW Colli-Ucan, W TI Extinction of Melipona beecheii and traditional beekeeping in the Yucatan peninsula SO BEE WORLD LA English DT Article ID MEXICO; HONEY; BEES AB Rearing of the 'xunan-kab' bee (Melipona beecheii) had been practised widely by the Mayans of the Yucatan peninsula long before arrival of the Spanish in the New World, and had been a culturally and economically important activity that region. Melipona beecheii kept almost exclusively in traditional log hives. Beekeepers using this bee, from the Mayan zone in Quintana Roo state, Mexico, testify to a 93% decrease in hives during the past one-quarter century. Despite concern that stingless bee keeping is going extinct, there were scant data to examine direct impact of competition from feral African Apis mellifera, deforestation, hurricane damage and lack of instruction and incentive for new stingless bee keepers. We therefore made a survey of beekeepers constituting 20% of the largest traditional beekeeping group in the Americas. These data combined with our field studies, taken over 24 years, suggest that bees are threatened both by environmental changes and by inappropriate management and conservation efforts. Overharvest and failure to transfer colonies to hives or divide them are serious impediments. The major tactics to confront these problems are presented. C1 El Colegio Frontera Sur, Chetumal 77900, Quintana Roo, Mexico. Smithsonian Trop Res Inst, APO, AA 34002 USA. RP Villanueva-G, R (reprint author), El Colegio Frontera Sur, Av Centenario Km 5-5,Apdo Postal 424, Chetumal 77900, Quintana Roo, Mexico. EM rogel@ecosur-qroo.mx NR 46 TC 18 Z9 20 U1 2 U2 12 PU INT BEE RESEARCH ASSOC PI CARDIFF PA JOURNALS LIBRARIAN, 18 NORTH RD, CARDIFF CF1 3DY, WALES SN 0005-772X J9 BEE WORLD JI Bee World PD JUN PY 2005 VL 86 IS 2 BP 35 EP 41 PG 7 WC Entomology SC Entomology GA 938JL UT WOS:000229995700003 ER PT J AU Collins, AG Daly, M AF Collins, AG Daly, M TI A new deepwater species of Stauromedusae, Lucernaria janetae (Cnidaria, Staurozoa, Lucernariidae), and a preliminary investigation of stauromedusan phylogeny based on nuclear and mitochondrial rDNA data SO BIOLOGICAL BULLETIN LA English DT Article ID EVOLUTION; MEDUSOZOA; PHYLUM; LIFE AB The deepwater stauromedusan Lucernaria janetae n. sp is described from adult and juvenile specimens collected from the East Pacific Rise. Lucernaria janetae is the first species in the genus recorded from the Pacific Ocean, and differs from its congeners in size and morphology . Mitochondrial (16S) and nuclear (SSU) ribosomal gene sequences from L. janetae were analyzed with those of representative stauromedusan taxa to evaluate stauromedusan monophyly. Both genes recovered a strongly monophyletic Stauromedusae that is the sister group to all other medusozoans. Support of these hypotheses is robust to method of phylogenetic reconstruction and to outgroup, selection. buttressing the argument that Stauromedusae should be recognized as the class Staurozoa. The molecular markers used here favor the same topology of relationships among our samples and clearly distinguished between two species. Haliclystus sanjuanensis and H. octoradiatus, that have been considered synonymous by many workers. A stable systematic framework for Stauromedusae appears achievable through comprehensive study of both morpholooical and sequence data. C1 Smithsonian Inst, Natl Museum Nat Hist, Natl Systemat Lab, NMFS, Washington, DC 20013 USA. Ohio State Univ, Dept Ecol Evolut & Organismal Biol, Columbus, OH 43210 USA. RP Collins, AG (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Natl Systemat Lab, NMFS, MRC-153,POB 37012, Washington, DC 20013 USA. EM Collinsa@si.edu RI Collins, Allen/A-7944-2008; Daly, Marymegan/F-9178-2011 OI Collins, Allen/0000-0002-3664-9691; NR 56 TC 30 Z9 32 U1 0 U2 6 PU MARINE BIOLOGICAL LABORATORY PI WOODS HOLE PA 7 MBL ST, WOODS HOLE, MA 02543 USA SN 0006-3185 J9 BIOL BULL-US JI Biol. Bull. PD JUN PY 2005 VL 208 IS 3 BP 221 EP 230 DI 10.2307/3593154 PG 10 WC Biology; Marine & Freshwater Biology SC Life Sciences & Biomedicine - Other Topics; Marine & Freshwater Biology GA 937IY UT WOS:000229919000008 PM 15965127 ER PT J AU Laurance, WF Oliveira, AA Laurance, SG Condit, R Dick, CW Andrade, A Nascimento, HEM Lovejoy, TE Ribeiro, JELS AF Laurance, WF Oliveira, AA Laurance, SG Condit, R Dick, CW Andrade, A Nascimento, HEM Lovejoy, TE Ribeiro, JELS TI Altered tree communities in undisturbed Amazonian forests: A consequence of global change? SO BIOTROPICA LA English DT Editorial Material DE Amazon; Brazil; carbon dioxide; climatic change; disturbance; drought; fire; floods; rainforest; tree communities ID RAIN-FOREST; TROPICAL FORESTS; CO2; RESPONSES; SEEDLINGS; GROWTH C1 Smithsonian Trop Res Inst, Balboa, Panama. Univ Sao Paulo, Dept Biol, BR-14040901 Sao Paulo, Brazil. Natl Inst Amazonian Res, INPA, Biol Dynam & Forest Fragments Project, BR-69011970 Manaus, Amazonas, Brazil. Natl Inst Amazonian Res, INPA, Dept Bot, BR-69011970 Manaus, Amazonas, Brazil. RP Laurance, WF (reprint author), Smithsonian Trop Res Inst, Apartado 2072, Balboa, Panama. EM laurancew@tivoli.si.edu RI Dick, Christopher/A-8744-2008; Laurance, William/B-2709-2012; Nascimento, Henrique/F-8612-2012; Oliveira, Alexandre/G-8830-2012; Laurance, Susan/G-6021-2011; Lahoz da Silva Ribeiro, Jose Eduardo/A-8574-2013 OI Oliveira, Alexandre/0000-0001-5526-8109; Laurance, Susan/0000-0002-2831-2933; Lahoz da Silva Ribeiro, Jose Eduardo/0000-0002-2389-5631 NR 23 TC 13 Z9 13 U1 1 U2 6 PU BLACKWELL PUBLISHING INC PI MALDEN PA 350 MAIN ST, MALDEN, MA 02148 USA SN 0006-3606 J9 BIOTROPICA JI Biotropica PD JUN PY 2005 VL 37 IS 2 BP 160 EP 162 DI 10.1111/j.1744-7429.2005.00022.x PG 3 WC Ecology SC Environmental Sciences & Ecology GA 929ON UT WOS:000229355500002 ER PT J AU La Marca, E Lips, KR Lotters, S Puschendorf, R Ibanez, R Rueda-Almonacid, JV Schulte, R Marty, C Castro, F Manzanilla-Puppo, J Garcia-Perez, JE Bolanos, F Chaves, G Pounds, JA Toral, E Young, BE AF La Marca, E Lips, KR Lotters, S Puschendorf, R Ibanez, R Rueda-Almonacid, JV Schulte, R Marty, C Castro, F Manzanilla-Puppo, J Garcia-Perez, JE Bolanos, F Chaves, G Pounds, JA Toral, E Young, BE TI Catastrophic population declines and extinctions in neotropical harlequin frogs (Bufonidae : Atelopus) SO BIOTROPICA LA English DT Article DE amphibians; Atelopus; climate change; declines; disease; extinction; Neotropics; population; trade ID BULLFROGS RANA-CATESBEIANA; GLOBAL AMPHIBIAN DECLINES; CLIMATE-CHANGE; FISH INTRODUCTIONS; TROPICAL MOUNTAIN; CENTRAL-AMERICA; CHYTRIDIOMYCOSIS; MORTALITY; TOAD; VENEZUELA AB We surveyed the population status of the Neotropical toad genus Atelopus, and document recent catastrophic declines that are more severe than previously reported for any amphibian genus. Of 113 species that have been described or are candidates for description, data indicate that in 42 species, population sizes have been reduced by at least half and only ten species have stable populations. The status of the remaining taxa is unknown. At least 30 species have been missing from all known localities for at least 8 yr and are feared extinct. Most of these species were last seen between 1984 and 1996. All species restricted to elevations of above 1000 m have declined and 75 percent have disappeared, while 58 percent of lowland species have declined and 38 percent have disappeared. Habitat loss was not related to declines once we controlled for the effects of elevation. In fact, 22 species that occur in protected areas have disappeared. The fungal disease Batrachochytrium dendrobatidis has been documented from nine species that have declined, and may explain declines in higher elevation species that occur in undisturbed habitats. Climate change may also play a role, but other potential factors such as environmental contamination, trade, and introduced species are unlikely to have affected more than a handful of species. Widespread declines and extinctions in Atelopus may reflect population changes in other Neotropical amphibians that are more difficult to survey, and the loss of this trophic group may have cascading effects on other species in tropical ecosystems. C1 Univ Los Andes, Fac Ciencias Forestales & Ambientales, Escuela Geog, Lab Biogeog, Merida 5101A, Venezuela. So Illinois Univ, Dept Zool, Carbondale, IL 62901 USA. Univ Mainz, Dept Ecol, Inst Zool, D-55099 Mainz, Germany. Univ Costa Rica, Escuela Biol, San Pedro, Costa Rica. Univ Panama, Dept Zool, Panama City, Panama. Smithsonian Trop Res Inst, Balboa, Ancon, Panama. Conservac Int, Programa Especies Amenazadas, Bogota, Colombia. Inst Invest Biol Cordilleras Orientales, INIBICO, Tarapoto, Peru. Impasse Jean Galot, Montjoly 097354, Guyana. Univ Valle, Dept Biol, Fac Ciencias, Secc Zool,Lab Herpetol, Cali, Colombia. Museo Nacl Ciencias Nat, Madrid, Spain. Cent Univ Venezuela, Museo Inst Zool Agr, Maracay, Venezuela. UNELLEZ, Vice Rectorado Prod Agr, Programa Recursos Nat Renovables, Museo Zool, Guanare, Estado Portugue, Venezuela. Monteverde Cloud Forest Preserve & Trop Sci Ctr, Golden Toad Lab Conservat, Santa Elena 565573, Puntarenas, Costa Rica. NatureServe, Monteverde 5655, Puntarenas, Costa Rica. RP La Marca, E (reprint author), Univ Los Andes, Fac Ciencias Forestales & Ambientales, Escuela Geog, Lab Biogeog, Apartado Postal 116, Merida 5101A, Venezuela. RI Puschendorf, Robert/B-6280-2011; OI Puschendorf, Robert/0000-0002-8105-171X; Chaves, Gerardo/0000-0002-4301-6569; Lips, Karen/0000-0002-2719-1551 NR 72 TC 166 Z9 186 U1 7 U2 68 PU BLACKWELL PUBLISHING INC PI MALDEN PA 350 MAIN ST, MALDEN, MA 02148 USA SN 0006-3606 J9 BIOTROPICA JI Biotropica PD JUN PY 2005 VL 37 IS 2 BP 190 EP 201 DI 10.1111/j.1744-7429.2005.00026.x PG 12 WC Ecology SC Environmental Sciences & Ecology GA 929ON UT WOS:000229355500006 ER PT J AU Evans, C Abrams, E Reitsma, R Roux, K Salmonsen, L Marra, PP AF Evans, C Abrams, E Reitsma, R Roux, K Salmonsen, L Marra, PP TI The Neighborhood Nestwatch program: Participant outcomes of a citizen-science ecological research project SO CONSERVATION BIOLOGY LA English DT Editorial Material ID CONSERVATION EDUCATION C1 Paul Smiths Coll, Paul Smiths, NY 12970 USA. Univ New Hampshire, Vice Presidents Off Res & Publ Serv, Durham, NH 03824 USA. Smithsonian Environm Res Ctr, Avian Ecol Lab, Edgewater, MD 21037 USA. Larry Box Conservat Ctr, Brooksville, MS 39739 USA. RP Evans, C (reprint author), Paul Smiths Coll, Routes 86 & 30, Paul Smiths, NY 12970 USA. EM evansc@paulsmiths.edu NR 13 TC 84 Z9 86 U1 10 U2 75 PU BLACKWELL PUBLISHING INC PI MALDEN PA 350 MAIN ST, MALDEN, MA 02148 USA SN 0888-8892 J9 CONSERV BIOL JI Conserv. Biol. PD JUN PY 2005 VL 19 IS 3 BP 589 EP 594 DI 10.1111/j.1523-1739.2005.00s01.x PG 6 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 930WP UT WOS:000229448100002 ER PT J AU Toscano, MA Macintyre, IG AF Toscano, MA Macintyre, IG TI Blanchon P, Comment on Toscano MA and Macintyre IG (2003): Corrected western Atlantic sea-level curve for the last 11,000 years based on calibrated C-14 dates from Acropora palmata framework and intertidal mangrove peat. SO CORAL REEFS LA English DT Editorial Material ID RADIOCARBON AGE CALIBRATION; HOLOCENE DEVELOPMENT; FLORIDA MARGIN; REEFS; CORALS; RECORD; BELIZE C1 Natl Museum Nat Hist, Dept Paleobiol, Smithsonian Inst, MRC 121, Washington, DC 20013 USA. RP Toscano, MA (reprint author), Natl Museum Nat Hist, Dept Paleobiol, Smithsonian Inst, MRC 121, POB 37012, Washington, DC 20013 USA. EM TOSCANOM@si.edu NR 25 TC 11 Z9 11 U1 0 U2 6 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013 USA SN 0722-4028 J9 CORAL REEFS JI Coral Reefs PD JUN PY 2005 VL 24 IS 2 BP 187 EP 190 DI 10.1007/s00338-005-0481-7 PG 4 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 936RI UT WOS:000229872700002 ER PT J AU Macintyre, IG Glynn, PW Hinds, F AF Macintyre, IG Glynn, PW Hinds, F TI Evidence of the role of Diadema antillarum in the promotion of coral settlement and survivorship SO CORAL REEFS LA English DT Editorial Material C1 Smithsonian Inst, NMNH MRC 121, Washington, DC 20013 USA. Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, MBF, Miami, FL 33149 USA. Coastal Zone Management Unit, St Michael, Barbados. RP Macintyre, IG (reprint author), Smithsonian Inst, NMNH MRC 121, POB 37012, Washington, DC 20013 USA. EM macintyre.ian@nmnh.si.edu NR 3 TC 9 Z9 10 U1 0 U2 2 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013 USA SN 0722-4028 J9 CORAL REEFS JI Coral Reefs PD JUN PY 2005 VL 24 IS 2 BP 273 EP 273 DI 10.1007/s00338-005-0492-4 PG 1 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 936RI UT WOS:000229872700018 ER PT J AU Forsman, ZH Guzman, HM Chen, CA Fox, GE Wellington, GM AF Forsman, ZH Guzman, HM Chen, CA Fox, GE Wellington, GM TI An ITS region phylogeny of Siderastrea (Cnidaria : Anthozoa): is S-glynni endangered or introduced? SO CORAL REEFS LA English DT Article DE Siderastrea glynni; ITS region; endangered coral; coral species phylogeny; Panama Canal; introduced species ID INTERNAL TRANSCRIBED SPACERS; SPECIES BOUNDARIES; EASTERN PACIFIC; SCLERACTINIA; EVOLUTION; SEQUENCES; CORALS; RDNA; UTILITY; ITS2 AB The genus Siderastrea contains only five extant species, including Siderastrea glynni, which is one of the few recognized species of endangered stony coral. Cloned sequences of the internal transcribed spacer (ITS) region had low levels of intragenomic nucleotide diversity, and few alignment ambiguities, which allowed for the first species-level phylogenetic analysis of the genus. Results indicated an unexpected deep divergence between the Western-Pacific and Atlantic species. ITS region sequences indicated that S. glynni is not derived from S. savignyana, as previously thought. Instead, S. glynni shared identical sequence types with S. siderea in the Caribbean. Given a range of previously published evolutionary rates for the ITS region, it is unlikely that S. glynni represents the remnants of a population that was divided by the closure of the Central American Seaway (approximately 3-3.8 MYA). It is more likely that S. glynni originated by a breach of the Isthmus (approximately 2 MYA), or a contemporary introduction by ship. C1 Univ Hawaii, Dept Biol, Honolulu, HI 96822 USA. Smithsonian Trop Res Inst, Balboa, Panama. Acad Sinica, Res Ctr Biodivers, Taipei 115, Taiwan. Univ Houston, Dept Biol & Biochem, Houston, TX 77204 USA. RP Forsman, ZH (reprint author), Univ Hawaii, Dept Biol, Honolulu, HI 96822 USA. EM zac@hawaii.edu RI Forsman, Zac/F-1266-2015 OI Forsman, Zac/0000-0002-5837-3614 NR 32 TC 21 Z9 23 U1 1 U2 6 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013 USA SN 0722-4028 J9 CORAL REEFS JI Coral Reefs PD JUN PY 2005 VL 24 IS 2 BP 343 EP 347 DI 10.1007/s00338-005-0497-z PG 5 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 936RI UT WOS:000229872700027 ER PT J AU Lemaitre, R AF Lemaitre, R TI Remarks on the life and works of Fenner A. Chace, Jr. (1908-2004), with a list of his taxa and complete bibliography SO CRUSTACEANA LA English DT Biographical-Item C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20013 USA. RP Lemaitre, R (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, MRC 163,POB 37012, Washington, DC 20013 USA. EM LEMAITRR@si.edu NR 1 TC 1 Z9 1 U1 0 U2 0 PU BRILL ACADEMIC PUBLISHERS PI LEIDEN PA PLANTIJNSTRAAT 2, P O BOX 9000, 2300 PA LEIDEN, NETHERLANDS SN 0011-216X J9 CRUSTACEANA JI Crustaceana PD JUN PY 2005 VL 78 BP 621 EP 639 DI 10.1163/156854005774318141 PN 5 PG 19 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 972JN UT WOS:000232450200008 ER PT J AU De Santo, NG Bisaccia, C De Santo, RM Cirillo, M Touwaide, A AF De Santo, NG Bisaccia, C De Santo, RM Cirillo, M Touwaide, A TI Pre-Vesalilan anatomy: The kidney of Berengario da Carpi SO DIALYSIS & TRANSPLANTATION LA English DT Article C1 Univ Naples 2, Ist Mazzini, Naples, Italy. Smithsonian Inst, Washington, DC 20560 USA. RP De Santo, NG (reprint author), Univ Naples 2, Ist Mazzini, Naples, Italy. NR 7 TC 0 Z9 0 U1 0 U2 2 PU CREATIVE AGE PUBL PI VAN NUYS PA 7628 DENSMORE AVE, VAN NUYS, CA 91406-2088 USA SN 0090-2934 J9 DIALYSIS TRANSPLANT JI Dial. Transplant. PD JUN PY 2005 VL 34 IS 6 BP 388 EP + PG 3 WC Engineering, Biomedical; Transplantation; Urology & Nephrology SC Engineering; Transplantation; Urology & Nephrology GA 930VC UT WOS:000229444200007 ER PT J AU Linares, OF AF Linares, OF TI Isle of fire: The political ecology of landscape burning in Madagascar. SO GEOGRAPHICAL JOURNAL LA English DT Book Review C1 Smithsonian Trop Res Inst, Balboa, Panama. RP Linares, OF (reprint author), Smithsonian Trop Res Inst, Balboa, Panama. NR 1 TC 0 Z9 0 U1 0 U2 0 PU ROYAL GEOGRAPHICAL SOC PI LONDON PA 1 KENSINGTON GORE, LONDON SW7 2AR, ENGLAND SN 0016-7398 J9 GEOGR J JI Geogr. J. PD JUN PY 2005 VL 171 BP 180 EP 181 PN 2 PG 2 WC Geography SC Geography GA 946DT UT WOS:000230553200009 ER PT J AU MacLeod, KG Huber, BT Isaza-Londono, C AF MacLeod, KG Huber, BT Isaza-Londono, C TI North Atlantic warming during global cooling at the end of the Cretaceous SO GEOLOGY LA English DT Article DE Maastrichtian; foraminifera; stable isotopes; paleoclimate; Ocean Drilling Program; greenhouse climate ID SEA-SURFACE TEMPERATURES; THERMAL MAXIMUM; CLIMATE; TERRESTRIAL; EXTINCTION; DIAGENESIS; HOTHOUSE AB Differences in regional responses to climate fluctuations are well documented on short time scales (e.g., El Nino-Southern Oscillation), but with the exception of latitudinal temperature gradients, regional patterns are seldom considered in discussions of ancient greenhouse climates. Contrary to the expectation of global warming or global cooling implicit in most treatments of climate evolution over millions of years, this paper shows that the North Atlantic warmed by as much as 6 degrees C (1.5 parts per thousand decrease in delta(18)O values of planktic foraminifera) during the Maastrichtian global cooling interval. We suggest that warming was the result of the importation of heat from the South Atlantic. Decreasing North Atlantic delta(18)O values are also associated with increasing gradients in planktic delta(13)C values, suggesting increasing surface-water stratification and a correlated strengthening of the North Atlantic Polar Front. If correct, this conclusion predicts arctic cooling during the late Maastrichtian. Beyond implications for the Maastrichtian, these data demonstrate that climate does not behave as if there is a simple global thermostat, even on geologic time scales. C1 Univ Missouri, Dept Geol Sci, Columbia, MO 65211 USA. Smithsonian Inst, Dept Paleobiol, Washington, DC 20013 USA. RP MacLeod, KG (reprint author), Univ Missouri, Dept Geol Sci, Columbia, MO 65211 USA. EM macleodk@missouri.edu RI MacLeod, Kenneth/C-4042-2017 OI MacLeod, Kenneth/0000-0002-6016-0837 NR 36 TC 38 Z9 40 U1 0 U2 8 PU GEOLOGICAL SOC AMER, INC PI BOULDER PA PO BOX 9140, BOULDER, CO 80301-9140 USA SN 0091-7613 J9 GEOLOGY JI Geology PD JUN PY 2005 VL 33 IS 6 BP 437 EP 440 DI 10.1130/G21466.1 PG 4 WC Geology SC Geology GA 930ZE UT WOS:000229454800002 ER PT J AU Irwin, RP Craddock, RA Howard, AD AF Irwin, RP Craddock, RA Howard, AD TI Interior channels in Martian valley networks: Discharge and runoff production SO GEOLOGY LA English DT Article DE Mars; channels; discharge; runoff; Noachian Period ID EARLY MARS; AQUEOUS SEDIMENTATION; MARGARITIFER SINUS; DEGRADATION; SABAEUS; ORIGIN AB The highland valley networks are perhaps the most compelling evidence for widespread fluvial activity on Mars > 3.5 Ga. However, determining the hydrology of these features has been difficult owing to poor image resolution and the lack of available topographic data. New orbital imaging reveals 21 late-stage channels within valley networks, which we use to estimate formative discharges and to evaluate water supply mechanisms. We find that channel width and associated formative discharge are comparable to terrestrial valley networks of similar area and relief. For 15 narrow channels in basin-filling networks, likely episodic runoff production rates up to centimeters per day and first-order formative discharges of similar to 300-3000 m(3)/s are similar to terrestrial floods supplied by precipitation. Geothermal melting of ground ice would produce discharges similar to 100 times smaller per unit area and would require pulsed outbursts to form the channels. In four large valleys with few tributaries, wider channels may represent large subsurface outflows or paleolake overflows, as these four channels originate at breached basin divides and/or near source regions for the catastrophic outflow channels. C1 Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20013 USA. Univ Virginia, Dept Environm Sci, Charlottesville, VA 22904 USA. RP Irwin, RP (reprint author), Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, 6th St & Independence Ave SW, Washington, DC 20013 USA. RI Craddock, Robert/B-3884-2013; OI Howard, Alan/0000-0002-5423-1600 NR 34 TC 80 Z9 80 U1 0 U2 6 PU GEOLOGICAL SOC AMERICA, INC PI BOULDER PA PO BOX 9140, BOULDER, CO 80301-9140 USA SN 0091-7613 J9 GEOLOGY JI Geology PD JUN PY 2005 VL 33 IS 6 BP 489 EP 492 DI 10.1130/G21333.1 PG 4 WC Geology SC Geology GA 930ZE UT WOS:000229454800015 ER PT J AU Viola, HJ AF Viola, HJ TI Indian views of the Custer fight: a source book. SO GREAT PLAINS QUARTERLY LA English DT Book Review C1 Smithsonian Inst, Washington, DC 20560 USA. RP Viola, HJ (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU CENT GREAT PLAINS STUD PI LINCOLN PA UNIV NEBRASKA-LINCOLN 1214 OLDFATHER HALL, LINCOLN, NE 68588-0313 USA SN 0275-7664 J9 GREAT PLAINS QUART JI Gt. Plains Q. PD SUM PY 2005 VL 25 IS 3 BP 192 EP 193 PG 2 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA 953IE UT WOS:000231069000011 ER PT J AU Loudkov, D Tong, CYE Blundell, R Kaurova, N Grishina, E Voronov, B Gol'tsman, G AF Loudkov, D Tong, CYE Blundell, R Kaurova, N Grishina, E Voronov, B Gol'tsman, G TI An investigation of the performance of the superconducting HEB mixer as a function of its RF embedding impedance SO IEEE TRANSACTIONS ON APPLIED SUPERCONDUCTIVITY LA English DT Article; Proceedings Paper CT 2004 Applied Superconductivity Conference CY OCT 03-08, 2004 CL Jacksonville, FL DE embedding impedance; fixed-tuned waveguide receiver; hot-electron bolometer mixer ID RECEIVER AB We have conducted an investigation of the optimal embedding impedance for a waveguide superconducting hot-electron bolometric (HEB) mixer. Three mixer chip. designs for 800 GHz, offering nominal embedding resistances of 70 Omega, 35 Omega, and 15 Omega, have been developed. We used both High Frequency Structure Simulator (HFSS) software and scale model impedance measurements in the design process. We subsequently fabricated HEB mixers to these designs using 3-4 nm thick NbN thin film. Receiver noise temperature measurements and Fourier Transform Spectrometer (FTS) scans were performed to determine the optimal combination of embedding impedance and normal-state resistance for a 50 Ohm IF load impedance. A receiver noise temperature of 440 K was measured at a local oscillator frequency 850 GHz for a mixer with normal state resistance of 62 Omega incorporated into a circuit offering a nominal embedding impedance of 70 M We conclude from our data that, for low noise operation, the normal state resistance of the HEB mixer element should be close to the embedding impedance of the mixer mount. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Moscow State Pedag Univ, Moscow 119992, Russia. RP Loudkov, D (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM dkoudkov@cfa.harvard.edu; etong@cfa.harvard.edu; rblundell@cfa.harvard.edu; nkaurova@mail.ru; Grishina@front.ru; bmvoronov@mail.ru; goltsman00@mail.ru OI Tong, Edward/0000-0002-7736-4203 NR 12 TC 1 Z9 1 U1 1 U2 3 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 1051-8223 J9 IEEE T APPL SUPERCON JI IEEE Trans. Appl. Supercond. PD JUN PY 2005 VL 15 IS 2 BP 472 EP 475 DI 10.1109/TASC.2005.849879 PN 1 PG 4 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA 935FO UT WOS:000229765300099 ER PT J AU Loudkov, D Tong, CYE Blundell, R Megerian, KG Stern, JA AF Loudkov, D Tong, CYE Blundell, R Megerian, KG Stern, JA TI Performance of the NbTiN hot electron bolometer mixer with AlN buffer layer at terahertz frequency range SO IEEE TRANSACTIONS ON APPLIED SUPERCONDUCTIVITY LA English DT Article; Proceedings Paper CT 2004 Applied Superconductivity Conference CY OCT 03-08, 2004 CL Jacksonville, FL DE hot electron bolometric mixer; NbTiN superconducting film; waveguide terahertz receiver ID RECEIVER AB We present recent measurements of receiver noise temperature and intermediate frequency (IF) bandwidth in the frequency range 0.8-1.3 THz for waveguide NbTiN HEB mixers of various dimensions. These devices are fabricated from an NbTiN film deposited on crystalline quartz substrates with AIN buffer layer. The lengths of the mixer elements vary from 0.3 to 0.5 mu m and their widths vary from 3 to 10 mu m. Critical temperatures are typically at 8.5 K, and the measured normal state resistance of the devices is about 1000 ohms per square. All the device DC parameters demonstrate a high degree of uniformity. A double side band noise temperature at 0.8 THz as low as 550 K has been measured at an IF frequency of 1.8 GHz, with a conversion loss of around 14 dB. At an IF of 3 GHz, the noise temperature increases to 750 K. We have also made extensive measurements of the IF bandwidth as a function of bias voltages and currents. At the optimal low-noise operation point, a 3-dB IF bandwidth of 1.2 GHz is obtained for a wide variety of device dimensions and bath temperature. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Loudkov, D (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM dloudkov@cfa.harvard.edu; etong@cfa.harvard.edu; rblundell@cfa.harvard.edu; Koko.G.Megerian@jpl.nasa.gov; Jeffrey.A.Stern@jpl.nasa.gov OI Tong, Edward/0000-0002-7736-4203 NR 10 TC 10 Z9 10 U1 0 U2 2 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 1051-8223 J9 IEEE T APPL SUPERCON JI IEEE Trans. Appl. Supercond. PD JUN PY 2005 VL 15 IS 2 BP 476 EP 479 DI 10.1109/TASC.2005.849881 PN 1 PG 4 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA 935FO UT WOS:000229765300100 ER PT J AU Tong, CYE Blundell, R Megerian, KG Stern, JA Pan, SK Pospieszalski, M AF Tong, CYE Blundell, R Megerian, KG Stern, JA Pan, SK Pospieszalski, M TI A distributed lumped-element SIS mixer with very wide instantaneous bandwidth SO IEEE TRANSACTIONS ON APPLIED SUPERCONDUCTIVITY LA English DT Article; Proceedings Paper CT 2004 Applied Superconductivity Conference CY OCT 03-08, 2004 CL Jacksonville, FL DE distributed mixing; intermediate frequency bandwidth; submillimeter waves; superconductor-insulator-superconductor mixers ID SUBMILLIMETER WAVELENGTHS; RECEIVER; DESIGN; OPERATION AB A novel type of distributed superconducting mixer with very low output capacitance has been designed for a 330-420 GHz waveguide mixer. In this design, a pair of lumped element Superconductor-Insulator-Superconductor junctions is connected in series to form the unit cell of a composite transmission line. The mixer utilizes two cascaded cells. Using an intermediate frequency (IF) of 5 GHz, we have measured Double-side-band (DSB) receiver noise temperatures of 90-120 K between 360 and 410 GHz. This mixer design offers very wide instantaneous bandwidth. The measured IF bandwidth is in excess of 18 GHz. At a Local Oscillator frequency of 384 GHz, the Y-factor measured at an IF frequency of 18 GHz is 2.1, compared to a Y-factor of 2.2 measured at an IF of 5 GHz. The mixer also has a high dynamic range. The 1-dB input compression point is only reached with an input black body load of 30,000 K. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91107 USA. Natl Radio Astron Observ, Charlottesville, VA 22903 USA. RP Tong, CYE (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM etong@cfa.harvard.edu; rblundell@cfa.harvard.edu; Koko.G.Megerian@jpl.nasa.gov; Jeffrey.A.Stern@jpl.nasa.gov; span2@nrao.edu; mpospies@nrao.edu OI Tong, Edward/0000-0002-7736-4203 NR 14 TC 10 Z9 10 U1 0 U2 2 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 1051-8223 J9 IEEE T APPL SUPERCON JI IEEE Trans. Appl. Supercond. PD JUN PY 2005 VL 15 IS 2 BP 490 EP 494 DI 10.1109/TASC.2005.849885 PN 1 PG 5 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA 935FO UT WOS:000229765300103 ER PT J AU Miura, O Kuris, AM Torchin, ME Hechinger, RF Dunham, EJ Chiba, S AF Miura, O Kuris, AM Torchin, ME Hechinger, RF Dunham, EJ Chiba, S TI Molecular-genetic analyses reveal cryptic species of trernatodes in the intertidal gastropod, Batillaria cumingi (Crosse) SO INTERNATIONAL JOURNAL FOR PARASITOLOGY LA English DT Article DE cryptic species; Batillaria cumingi; Cercaria batillariae; restriction fragment-length polymorphism; cytochrome oxidase subunit 1; internal transcribed spacer 1 ID PHYLOGENY; TREMATODA; PARASITES; DIGENEA; SPECIFICITY; RICHNESS; NUCLEAR; SEA AB Cryptic species of the digeneans, Cercaria batillariae (Heterophyidae) and an undescribed philophthalmid, were detected using polymerase chain reaction-based restriction fragment-length polymorphism methodology and sequence analyses. These digeneans were all collected from the same species of gastropod first intermediate host, Batillaria cumingi (=Batillaria attramentaria). The mitochondrial cytochrome oxidase subunit I gene (approximately 800 bp) and nuclear internal transcribed spacer I gene (approximately 400 bp) were used for species level discrimination. Restriction fragment-length polymorphism analyses of cytochrome oxidase subunit I gene showed that C. batillariae included 10 distinguishable fragment patterns, and the philophthalmid included five patterns. On the basis of subsequent sequence analyses, the restriction fragment length polymorphism patterns of C. batillariae were grouped into eight phylogenetically distinct lineages and those of the philophthalmid into three phylogenetically distinct lineages. There was no evidence of gene flow among the different lineages due to the lack of heterozygosity within the observed internal transcribed spacer I gene fragment patterns. This suggests that all of these lineages are different species. Most of these species were widespread, but some exhibited restricted geographic distributions. We discuss the implications of these findings for host specificity of these trematodes. These results demonstrate the utility of genetic analysis to distinguish species of morphologically similar trematodes. Hence, trematode species diversity may often be underestimated when species identifications are limited to morphological features. (c) 2005 Australian Society for Parasitology Inc. Published by Elsevier Ltd. All rights reserved. C1 Tohoku Univ, Grad Sch Life Sci, Dept Ecol & Evolutionary Biol, Sendai, Miyagi 9808578, Japan. Univ Calif Santa Barbara, Inst Marine Sci, Santa Barbara, CA 93106 USA. Univ Calif Santa Barbara, Dept Ecol Evolut & Marine Biol, Santa Barbara, CA 93106 USA. Smithsonian Trop Res Inst, Ancon, Panama. RP Miura, O (reprint author), Tohoku Univ, Grad Sch Life Sci, Dept Ecol & Evolutionary Biol, Sendai, Miyagi 9808578, Japan. EM 3-ura@biology.tohoku.ac.jp RI Hechinger, Ryan/F-6754-2010 NR 46 TC 61 Z9 64 U1 2 U2 19 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0020-7519 J9 INT J PARASITOL JI Int. J. Parasit. PD JUN PY 2005 VL 35 IS 7 BP 793 EP 801 DI 10.1016/j.ijpara.2005.02.014 PG 9 WC Parasitology SC Parasitology GA 940XE UT WOS:000230178400012 PM 15925598 ER PT J AU DeVorkin, D AF DeVorkin, D TI Robert Phillip Multhaue, 1919-2004 SO ISIS LA English DT Biographical-Item C1 Smithsonian Inst, Washington, DC 20560 USA. RP DeVorkin, D (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0021-1753 J9 ISIS JI Isis PD JUN PY 2005 VL 96 IS 2 BP 252 EP 257 DI 10.1086/431537 PG 6 WC History & Philosophy Of Science SC History & Philosophy of Science GA 950JY UT WOS:000230854600007 ER PT J AU Bedini, SA AF Bedini, SA TI Drawing the line: How Mason and Dixon surveyed the most famous border in America. SO ISIS LA English DT Book Review C1 Smithsonian Inst, Washington, DC 20560 USA. RP Bedini, SA (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0021-1753 J9 ISIS JI Isis PD JUN PY 2005 VL 96 IS 2 BP 279 EP 279 DI 10.1086/491502 PG 1 WC History & Philosophy Of Science SC History & Philosophy of Science GA 950JY UT WOS:000230854600030 ER PT J AU Santos-Granero, F AF Santos-Granero, F TI My cocaine museum. SO JOURNAL OF ANTHROPOLOGICAL RESEARCH LA English DT Book Review C1 Smithsonian Trop Res Inst, Balboa, Panama. RP Santos-Granero, F (reprint author), Smithsonian Trop Res Inst, Balboa, Panama. NR 2 TC 0 Z9 0 U1 0 U2 0 PU UNIV NEW MEXICO PI ALBUQUERQUE PA DEPT ANTHROPOLOGY, ALBUQUERQUE, NM 87131-1561 USA SN 0091-7710 J9 J ANTHROPOL RES JI J. Anthropol. Res. PD SUM PY 2005 VL 61 IS 2 BP 232 EP 233 PG 2 WC Anthropology SC Anthropology GA 935VX UT WOS:000229812600013 ER PT J AU Nietfeld, PL AF Nietfeld, PL TI Magnificent objects from the University of Pennsylvania Museum of Archaeology and Anthropology. SO JOURNAL OF ANTHROPOLOGICAL RESEARCH LA English DT Book Review C1 Smithsonian Inst, Natl Museum Amer Indian, Washington, DC 20560 USA. RP Nietfeld, PL (reprint author), Smithsonian Inst, Natl Museum Amer Indian, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU UNIV NEW MEXICO PI ALBUQUERQUE PA DEPT ANTHROPOLOGY, ALBUQUERQUE, NM 87131-1561 USA SN 0091-7710 J9 J ANTHROPOL RES JI J. Anthropol. Res. PD SUM PY 2005 VL 61 IS 2 BP 260 EP 261 PG 2 WC Anthropology SC Anthropology GA 935VX UT WOS:000229812600029 ER PT J AU Cooke, R AF Cooke, R TI Prehistory of native Americans on the Central American land bridge: Colonization, dispersal, and divergence SO JOURNAL OF ARCHAEOLOGICAL RESEARCH LA English DT Review DE Central American land bridge; continuity; Precolumbian agriculture; exchange; chiefdom ID COSTA-RICA; FOREST DISTURBANCE; MANIHOT-ESCULENTA; TROPICAL FOREST; CUCURBITA CUCURBITACEAE; MAIZE EVOLUTION; WESTERN PANAMA; YOUNGER DRYAS; POLLEN RECORD; STARCH GRAINS AB The Central American land bridge has served as a passageway for animals and humans moving between North and South America. Nevertheless, after the first waves of human immigration at the end of the Pleistocene, contact between the native peoples who remained on this isthmus and other peoples living in continental areas where civilization ultimately developed, is characterized, according to the field record, by the transfer of crops, technologies, and goods, until ca. 1400 BP when speakers of Mesoamerican languages occupied the northwestern edge (Gran Nicoya). The ancestors of modern-day speakers of Chibchan and Chocoan languages underwent social and cultural diversification mostly within the confines of the land bridge. Some Precolumbian residents altered vegetation immediately after first arrival at least 11,000 years ago, and began to add domesticated crops to their subsistence inventory between 9000 and 7000 BE Maize and manioc (or cassava), domesticated outside the land bridge, were introduced in Preceramic times, early in the period between 7000 and 4500 BP, and gradually dominated regional agriculture as they became more productive, and as human populations increased and spread into virgin areas. Diversity in material culture is visible ca. 6000 BP, and becomes more apparent after the introduction of pottery ca. 4500 BE By 2000 BP culture areas with distinctive artifact inventories are discernible. Between 2500 and 1300 BP hierarchies among regions, sites, social groups, and individuals point to the establishment of chiefdoms whose elite members came to demand large numbers of costume and sumptuary goods. A few special centers with stone sculptures and low-scale architecture served a social universe larger than the chiefdom, such as clusters of recently fissioned social groups with memories of a common heritage. Social interactions on the land bridge, endowed with productive bottomlands, highland valleys, and coastal habitats, appear always to have been strongest among neighboring groups. C1 Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. RP Cooke, R (reprint author), Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. EM cooker@naos.si.edu NR 421 TC 28 Z9 30 U1 3 U2 21 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1059-0161 J9 J ARCHAEOL RES JI J. Archaeol. Res. PD JUN PY 2005 VL 13 IS 2 BP 129 EP 187 DI 10.1007/s10804-005-2486-4 PG 59 WC Anthropology; Archaeology SC Anthropology; Archaeology GA 927NI UT WOS:000229200200002 ER PT J AU Schlachter, AS Scully, SWJ Phaneuf, RA Emmons, ED Aguilar, A Leitner, D Lubell, MS Covington, AM Puettner, R Mueller, A Halka, M Levin, JC McLaughlin, BM AF Schlachter, AS Scully, SWJ Phaneuf, RA Emmons, ED Aguilar, A Leitner, D Lubell, MS Covington, AM Puettner, R Mueller, A Halka, M Levin, JC McLaughlin, BM TI K-shell photoionization of C2+ ions: experiment and theory SO JOURNAL OF ELECTRON SPECTROSCOPY AND RELATED PHENOMENA LA English DT Article; Proceedings Paper CT 14th International Conference on Vacuum Ultraviolet Radiation Physics CY JUL 19-23, 2004 CL Cairns, AUSTRALIA DE K-shell; photoionization; C2+ ions AB Cross-sections for inner-shell photoionization processes in beryllium-like carbon ions are determined both theoretically and experimentally for photon impact energies in the region of the carbon K edge. Measurements of absolute cross-sections, resonance energies, and life-time/linewidths measured using the merged-beam technique at the Advanced Light Source are in good agreement with R-matrix calculations. Published by Elsevier B.V. C1 Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. Univ Nevada, Reno, NV 89557 USA. CUNY City Coll, New York, NY 10031 USA. Free Univ Berlin, D-1000 Berlin, Germany. Univ Giessen, Inst Atom & Mol Phys, Giessen, Germany. Embry Riddle Aeronaut Univ, Prescott, AZ USA. Univ Tennessee, Knoxville, TN USA. Queens Univ Belfast, Belfast, Antrim, North Ireland. Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. RP Schlachter, AS (reprint author), Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. EM fsschlachter@lbl.gov RI Muller, Alfred/A-3548-2009 OI Muller, Alfred/0000-0002-0030-6929 NR 3 TC 0 Z9 0 U1 0 U2 0 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0368-2048 J9 J ELECTRON SPECTROSC JI J. Electron Spectrosc. Relat. Phenom. PD JUN PY 2005 VL 144 SI SI BP 53 EP 54 DI 10.1016/j.elspec.2005.01.291 PG 2 WC Spectroscopy SC Spectroscopy GA 933TZ UT WOS:000229657100014 ER PT J AU Carver, AM Wolcott, TG Wolcott, DL Hines, AH AF Carver, AM Wolcott, TG Wolcott, DL Hines, AH TI Unnatural selection: Effects of a male-focused size-selective fishery on reproductive potential of a blue crab population SO JOURNAL OF EXPERIMENTAL MARINE BIOLOGY AND ECOLOGY LA English DT Article; Proceedings Paper CT Blue Crab Symposium CY JUN 01-05, 2003 CL Williamsburg, VA SP Crustacian Soc DE blue crab; Callinectes supidus; sex ratio; sperm limitation ID CALLINECTES-SAPIDUS RATHBUN; OPERATIONAL SEX-RATIO; CHESAPEAKE BAY; SEMINAL FLUID; DROSOPHILA-MELANOGASTER; COPULATION DURATION; SPERM COMPETITION; DYNAMICS; BEHAVIOR; DENSITY AB A male-focused size-selective fishery, like the one targeting the blue crab (Callinectes sapidus Rathbun) along the Atlantic and Gulf coasts of the U.S., has the potential to reduce the average size of the males in the population, reduce the density of males in the population, and/or raise the ratio of females to males. All of these may affect the mating dynamics of the population by reducing the amount of sperm that males provide to females and decreasing the number of males available for copulation. We investigated the effect of the fishery on a blue crab population in upper Chesapeake Bay by collecting crabs in areas of markedly different fishing pressure. Crabs were taken as individuals and as mating pairs, which permitted assessing the size of males currently mating in nature, and the seminal resources they possess and transfer to females. Average size of males in subpopulations that have been subjected to heavier fishing pressure is indeed smaller, and the smaller males pass less sperm and accessory fluid to females than would larger males if they were still present. Some males in pre-copulatory pairs are as sperm depleted as males that had just completed copulation, indicating that they are mating more frequently than they can replace their seminal resources. The most sperm-depleted males in the population are not even pairing or attempting to mate. (c) 2005 Elsevier B.V. All rights reserved. C1 N Carolina State Univ, Dept Marine Earth & Atmospher Sci, Raleigh, NC 27695 USA. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Wolcott, TG (reprint author), N Carolina State Univ, Dept Marine Earth & Atmospher Sci, Box 8208, Raleigh, NC 27695 USA. EM adinacarver@earthlink.net; tom_wolcott@ncsu.edu NR 32 TC 31 Z9 33 U1 0 U2 14 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 JUN 1 PY 2005 VL 319 IS 1-2 SI SI BP 29 EP 41 DI 10.1016/j.jembe.2004.06.013 PG 13 WC Ecology; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 933ZK UT WOS:000229671400004 ER PT J AU King, RS Hines, AH Craige, FD Grap, S AF King, RS Hines, AH Craige, FD Grap, S TI Regional, watershed and local correlates of blue crab and bivalve abundances in subestuaries of Chesapeake Bay, USA SO JOURNAL OF EXPERIMENTAL MARINE BIOLOGY AND ECOLOGY LA English DT Article; Proceedings Paper CT Blue Crab Symposium CY JUN 01-05, 2003 CL Williamsburg, VA SP Crustacian Soc DE Callineetes sapidus; ecological indicators; estuaries; Macoma spp.; watershed land use; wetlands ID CALLINECTES-SAPIDUS RATHBUN; DENSITY-DEPENDENT PREDATION; ESTUARINE BENTHIC INDEX; BIOTIC INTEGRITY; BEHAVIORAL-RESPONSES; POPULATION-DYNAMICS; SPATIAL SCALES; SHALLOW-WATER; HYPOXIA; FISH AB Blue crabs (Callinectes sapidus) and deposit- and suspension-feeding bivalves (Macoma balthica and M. mitchelli) play important roles in the food web of Chesapeake Bay and may serve as indicators of ecological health, particularly in small subestuaries where conditions may be strongly linked to watershed and local factors. We sampled 19 subestuaries of Chesapeake Bay to test hypothesized relationships of blue crabs and bivalves with salinity (a regional indicator), watershed- and local-scale land use, and local habitat and water quality. We divided the subestuaries into five land-use categories: forested, developed, agricultural, mixed agricultural and mixed-developed. We measured water quality, sediment class, physical habitat and adjacent land use/land cover at each of six stations within each subestuary. Fyke nets were employed to estimate blue crab abundance and size-structure, while cores were used to estimate bivalve densities and biomass. Classification and regression tree (CART) analysis indicated that 51% of the variance in blue crab abundance was explained by salinity, watershed land use and shoreline marsh habitat. Crab abundance was greatest at salinities > 16 ppt, but in lower salinities crabs were most abundant along marsh shorelines in forested and mixed land-use watersheds. Juvenile crabs < 85 mm were more strongly associated with shoreline marshes, particularly in subestuaries with forested and mixed land-use watersheds. Macoma spp. were similarly associated with shoreline marshes but mainly in muddy bottoms at moderate-to-high salinities; however the best CART model only explained 25% of variance in bivalve abundance. These results were consistent with our predictions that shoreline wetlands and watershed land use may have important effects on these taxa along the estuarine salinity gradient, and are consistent with hypotheses based on previous descriptive and experimental research linking blue crabs and deposit-feeding bivalves to habitats rich in allochtonous detritus. (c) 2005 Elsevier B.V. All rights reserved. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP King, RS (reprint author), Baylor Univ, Dept Biol, Ctr Reservoir & Aquat Syst Res, Waco, TX 76798 USA. EM kingry@si.edu NR 55 TC 38 Z9 39 U1 0 U2 11 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 JUN 1 PY 2005 VL 319 IS 1-2 SI SI BP 101 EP 116 DI 10.1016/j.jembe.2004.05.022 PG 16 WC Ecology; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 933ZK UT WOS:000229671400009 ER PT J AU Aguilar, R Hines, AH Wolcott, TG Wolcott, DL Kramer, MA Lipcius, RN AF Aguilar, R Hines, AH Wolcott, TG Wolcott, DL Kramer, MA Lipcius, RN TI The timing and route of movement and migration of post-copulatory female blue crabs, Callinectes sapidus Rathbun, from the upper Chesapeake Bay SO JOURNAL OF EXPERIMENTAL MARINE BIOLOGY AND ECOLOGY LA English DT Article; Proceedings Paper CT Blue Crab Symposium CY JUN 01-05, 2003 CL Williamsburg, VA SP Crustacian Soc DE Callinectes sapidus; Chesapeake Bay; female blue crab; mark-recapture; migration; tagging ID ULTRASONIC TELEMETRY; CHIONOECETES-OPILIO; PAGURUS-LONGICARPUS; PANULIRUS-ARGUS; SPAWNING STOCK; SPINY LOBSTER; HERMIT CRAB; BEHAVIOR; POPULATION; TRANSPORT AB The movement of mature female blue crabs Callinectes sapidus Rathbun from lower salinity areas to spawn near the months of estuaries is well documented, but specific details of the post-copulatory phase of their migratory behavior are poorly understood in Chesapeake Bay. To test the hypotheses about the timing and route of this migration, we conducted a mark-recapture study of mature females released in a mesohaline portion of the upper Chesapeake Bay. From June 1999 to October 2002, 1440 mature female blue crabs were obtained from fishers, tagged, and released in the vicinity of the Rhode River, Maryland, approximately 200 km distant from the mouth of the Bay. As of the end of 2002, 167 crabs were recaptured (11.6%), with considerable variation in recapture rates among years. All recaptures except one (in Flagler Beach, Florida) were caught within the Chesapeake Bay proper. Recaptures of female crabs released at monthly intervals from June-November indicated that migration Occurred during a short fall period rather than over the prolonged period of summer to fall mating. The distances traveled by crabs before recapture differed significantly among release months. On average, crabs released in September and October traveled greater distances than crabs released in earlier months (June August). Depths of recapture sites differed significantly among months, with shallow depths in June-August increasing in September to a maximum in November. The locations and bathymetry of recapture sites showed that female crabs used areas near the deep channel, especially the eastern shoulder. of the Bay as a migration corridor to the spawning areas of the lower estuary. The distinct fall season and route of migration should provide valuable management information for protecting the declining spawning stock of Chesapeake blue crabs. Published by Elsevier B.V. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. N Carolina State Univ, Dept Earth & Atmospher Sci, Raleigh, NC 27695 USA. Coll William & Mary, Virginia Inst Marine Sci, Gloucester Point, VA 23062 USA. RP Aguilar, R (reprint author), Smithsonian Environm Res Ctr, POB 28,647 Contees Wharf Rd, Edgewater, MD 21037 USA. EM aguilarr@si.edu RI Aguilar, Robert/O-2480-2016 OI Aguilar, Robert/0000-0001-8732-5382 NR 59 TC 46 Z9 49 U1 0 U2 14 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 JUN 1 PY 2005 VL 319 IS 1-2 SI SI BP 117 EP 128 DI 10.1016/j.jembe.2004.08.030 PG 12 WC Ecology; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 933ZK UT WOS:000229671400010 ER PT J AU Rome, MS Young-Williams, AC Davis, GR Hines, AH AF Rome, MS Young-Williams, AC Davis, GR Hines, AH TI Linking temperature and salinity tolerance to winter mortality of of Chesapeake Bay blue crabs (Callinectes sapidus) SO JOURNAL OF EXPERIMENTAL MARINE BIOLOGY AND ECOLOGY LA English DT Article; Proceedings Paper CT Blue Crab Symposium CY JUN 01-05, 2003 CL Williamsburg, VA SP Crustacian Soc DE blue crab; Callinectes sapidus; salinity tolerance; temperature tolerance; winter mortality ID POPULATION-DYNAMICS; RATHBUN; ABUNDANCE; AUTOTOMY; GROWTH; REGENERATION; PATTERNS; STOCK; RECRUITMENT; CRUSTACEANS AB Blue crabs (Callinectes sapidus) form one of the most important and largest commercial fisheries in Chesapeake Bay. Blue crabs have evolutionary origins in the tropics, although they currently inhabit temperature estuaries that exhibit major fluctuations in diurnal. monthly, and seasonal environmental conditions. Therefore, harsh winter conditions in Chesapeake Bay are a potentially important source of blue crab stock loss. However, this variable has been largely unexamined. To assess the effects of variation in winter environmental conditions on blue crab survival, we measured winter morality of crabs in the field and conducted laboratory experiments to test the interactive effects of low temperature, salinity, and blue crab life stage. Field studies indicated that blue crabs suffered relatively low winter morality rates (<= 3%) during five out of eight winters, when bottom water temperature in February was at or above the 8-year average (3.4 degrees C). However, in years when bottom water temperature fell below the February average, annual mortality rates rose to 6.0-14.5%. Mortality rates were highest in the coldest regions of Chesapeake Bay, and larger crabs and female crabs were most vulnerable to these stressful conditions. Similarly.. in the laboratory, mortality was highest in the lowest temperature (1 degrees C) and salinity (8 ppt) treatments. Mature females were more sensitive to winter conditions than juvenile crabs. Of the juvenile life stages, recruits (< 15 mm carapace width) were least tolerant to winter conditions. These results indicate that temperature, salinity, and blue crab life stage are important variables in predicting survivorship over winter months. Because winter mortality may be a significant source of stock loss for blue crabs, especially during severe winters and in low salinity areas of Chesapeake Bay, these predictions can be used to improve management estimates of stock size prior to each summer fishing season. (c) 2005 Published bv Elsevier B.V. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Maryland Dept Nat Resources, Stevensville, MD 21666 USA. RP Rome, MS (reprint author), Stanford Univ, Hopkins Marine Stn, Oceanview Blvd,Pacific Grove, Pacific Grove, CA 93950 USA. EM michrom@aol.com NR 56 TC 21 Z9 23 U1 0 U2 26 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 JUN 1 PY 2005 VL 319 IS 1-2 SI SI BP 129 EP 145 DI 10.1016/j.jembe.2004.06.014 PG 17 WC Ecology; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 933ZK UT WOS:000229671400011 ER PT J AU Meyer, CFJ Weinbeer, M Kalko, EKV AF Meyer, CFJ Weinbeer, M Kalko, EKV TI Home-range size and spacing patterns of Macrophyllum macrophyllum (Phyllostomidae) foraging over water SO JOURNAL OF MAMMALOGY LA English DT Article DE Barro Colorado Nature Monument; Chiroptera; Macrophyllum macrophyllum; movement patterns; radiotracking; Panama ID NOCTILIO-LEPORINUS CHIROPTERA; BAT CAROLLIA-PERSPICILLATA; NECTAR-FEEDING BAT; PAPUA-NEW-GUINEA; FRUGIVOROUS BAT; HABITAT USE; EPTESICUS-SEROTINUS; EUDERMA-MACULATUM; FISHING BAT; BEHAVIOR AB We studied home-range size and patterns of range use of long-legged bats, Macrophyllum macrophyllum (Phyllostomidae), at Barro Colorado Nature Monument, Panama, by using radiotelemetry. Movements of 4 males and 5 females fitted with radiotransmitters were monitored for 4-7 entire nights each between April and July 2002. M. macrophyllum had an extensive range compared to other similar-sized phyllostomid bats. Median home-range size for the 9 individuals tracked was 23.9 ha (range 7.3-150.7 ha). With a median of 17.3 ha (range = 7.3-24.9 ha), home ranges of males were somewhat, but not significantly, smaller than those of females (44.4 ha, range = 16.3-150.7 ha). The bats foraged exclusively over water, whereby hunting activity was restricted to the immediate shoreline of Gatun Lake. Foraging areas ranged from 2.7 to 96.1 ha, with a median of 12.3 ha for both sexes. In general, there was high night-to-night consistency in the use of foraging areas. Most bats had multiple foraging and core areas. Core-use areas corresponded to approximately 35% of the bats' foraging areas and were larger in females (median = 5.3 ha, range = 1.1-54.1 ha) than in males (3.3 ha, range = 2.6-8.7 ha). Maximum range span varied from 0.5 to 7.5 km, whereby males in general and I tracked harem male in particular foraged much closer to the day roost than did females. Individual M. macrophyllum traveled an estimated 35-47 km on a nightly basis, and females moved significantly greater distances than did males. Our results do not provide support for the proposition that small bats typically have small home ranges. In contrast, we conclude that foraging strategy, diet, dispersion of food resources, and wing morphology are generally better predictors of home-range size. Furthermore, reproductive condition, as well as intraspecific competition linked to colony size or social status, also strongly affect the spacing behavior and movement patterns of these bats. Our results suggest that, although M. macrophyllum employs a gleaning foraging strategy, it closely parallels aerial insectivorous bats in terms of range size and movement distances. C1 Univ Wurzburg, Dept Anim Ecol & Trop Biol, Theodor Boveri Inst, Biozentrum, D-97074 Wurzburg, Germany. Univ Ulm, Dept Expt Ecol, D-89069 Ulm, Germany. Smithsonian Trop Res Inst, Balboa, Panama. RP Kalko, EKV (reprint author), Univ Wurzburg, Dept Anim Ecol & Trop Biol, Theodor Boveri Inst, Biozentrum, Hubland, D-97074 Wurzburg, Germany. EM elisabeth.kalko@biologie.uni-ulni.de RI Meyer, Christoph/A-4363-2012 OI Meyer, Christoph/0000-0001-9958-8913 NR 67 TC 29 Z9 31 U1 1 U2 27 PU ALLIANCE COMMUNICATIONS GROUP DIVISION ALLEN PRESS PI LAWRENCE PA 810 EAST 10TH STREET, LAWRENCE, KS 66044 USA SN 0022-2372 J9 J MAMMAL JI J. Mammal. PD JUN PY 2005 VL 86 IS 3 BP 587 EP 598 DI 10.1644/1545-1542(2005)86[587:HSASPO]2.0.CO;2 PG 12 WC Zoology SC Zoology GA 934PH UT WOS:000229720200017 ER PT J AU Scharler, UM Baird, D AF Scharler, UM Baird, D TI A comparison of selected ecosystem attributes of three South African estuaries with different freshwater inflow regimes, using network analysis SO JOURNAL OF MARINE SYSTEMS LA English DT Review DE food webs; ecological network analysis; ecosystem attributes; freshwater inflow; estuaries; south coast of South Africa ID ST-FRANCIS BAY; EELGRASS ZOSTERA-MARINA; WARM-TEMPERATE ESTUARY; EASTERN CAPE ESTUARIES; SUNDAYS RIVER ESTUARY; ACARTIA-TONSA DANA; SWARTKOPS ESTUARY; KROMME ESTUARY; ORGANIC-CARBON; POPULATION-DYNAMICS AB Carbon flow networks of the Kromme, Swartkops and Sundays estuaries, situated on the south coast of South Africa, were analysed using ecological network analysis. A major difference between the three estuaries is the freshwater inflow regimes: The Kromme Estuary receives very little freshwater (annual mean 0.07 m(-3) s(-1)), the Swartkops Estuary receives annually about 0.82 m(-3) s(-1) while the Sundays Estuary receives on average about 2.74 m(-3) s(-1) annually. Ecological network analysis revealed differences between most ecosystem attributes such as the cycling of carbon, trophic structure, the organisational and developmental status in terms of ascendency and redundancy, and regarding the contribution to and dependencies of compartments to and on one another in the network. Due to the lack of frequent freshwater inflow and consequently the renewal of the nutrient pool, the Kromme Estuary recycles most of its material and showed the highest detritivory/herbivory ratio (57: 1), whereas the Sundays recycles the least proportion and had the lowest detritivory/herbivory ratio at 10:1. The Sundays Estuary, hitherto believed to be dominated by pelagic production, was found to rely more on the benthic biota in terms of carbon throughput as inferred from the contribution and dependency coefficients, than on pelagic communities. Due to the low rate of fresh water inflow into the Kromme Estuary, the absence of an axial salinity gradient, a comparatively high Finn Cycling Index of 40%, and the long water exchange time, this system appears to have developed into an "arm" of the sea. System level properties such as the A/C ratio, the Average Mutual Information index, and the food web connectance index, increase from the lowest values calculated for the Kromme Estuary, intermediate for the Swartkops Estuary, and highest for the Sundays Estuary, while the FCI followed an inverse trend between the three systems. (c) 2005 Elsevier B.V. All rights reserved. C1 Univ Maryland, Ctr Environm Studies, Chesapeake Biol Lab, Solomons, MD 20688 USA. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Univ Port Elizabeth, Dept Zool, ZA-6001 Port Elizabeth, South Africa. RP Scharler, UM (reprint author), Oude Eekmolenweg 35, NL-6706 AN Wageningen, Netherlands. EM scharler@cbl.umces.edu RI Scharler, Ursula/F-3598-2010; Ross, Donald/F-7607-2012 OI Ross, Donald/0000-0002-8659-3833 NR 172 TC 45 Z9 46 U1 3 U2 19 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0924-7963 J9 J MARINE SYST JI J. Mar. Syst. PD JUN PY 2005 VL 56 IS 3-4 BP 283 EP 308 DI 10.1016/j.jmarsys.2004.12.003 PG 26 WC Geosciences, Multidisciplinary; Marine & Freshwater Biology; Oceanography SC Geology; Marine & Freshwater Biology; Oceanography GA 946OI UT WOS:000230581300004 ER PT J AU Beadell, JS Fleischer, RC AF Beadell, JS Fleischer, RC TI A restriction enzyme-based assay to distinguish between avian hemosporidians SO JOURNAL OF PARASITOLOGY LA English DT Article ID MALARIA PLASMODIUM-RELICTUM; MITOCHONDRIAL-DNA; BIRDS; PARASITES; PATHOGENICITY; PREVALENCE; FALCIPARUM; MORTALITY; ORIGIN AB We describe a reliable and relatively inexpensive method for detecting and differentiating between the commonly studied avian blood parasite genera Haemoproteus, Plasmodium, and Leitcocytozooll. The assay takes advantage of a Haemoproteus-specific restriction site identified by sequencing full rnitochondrial genomes from two Haemoproteus and three Plosmodium lineages and an adjacent, genus-specific restriction site identified in Leucocytozoon spp. The assay was sensitive to simulated parasitemas of approximately 8 x 10(-6) per erythrocyte and was 100% accurate in differentiating between parasite genera isolated from a broad geographical and taxonomic sampling of infected hosts. C1 Smithsonian Inst, Natl Museum Nat Hist, Genet Program, Washington, DC 20008 USA. Univ Maryland, Dept Biol, College Pk, MD 20742 USA. RP Beadell, JS (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Genet Program, 3001 Connecticut Ave NW, Washington, DC 20008 USA. EM beadellj@si.edu FU NIGMS NIH HHS [1R01GM063258] NR 21 TC 45 Z9 45 U1 1 U2 12 PU AMER SOC PARASITOLOGISTS PI LAWRENCE PA 810 EAST 10TH STREET, LAWRENCE, KS 66044 USA SN 0022-3395 J9 J PARASITOL JI J. Parasitol. PD JUN PY 2005 VL 91 IS 3 BP 683 EP 685 DI 10.1645/GE-3412RN PG 3 WC Parasitology SC Parasitology GA 941LU UT WOS:000230217100034 PM 16108566 ER PT J AU Gasca, R AF Gasca, R TI Hyperoche shihi sp nov (Crustacea : Peracarida : Amphipoda): a symbiont of a deep-living medusa in the Gulf of California SO JOURNAL OF PLANKTON RESEARCH LA English DT Article ID GELATINOUS-ZOOPLANKTON; HYPERIA-GALBA; ASSOCIATIONS AB From samples of deep-water zooplankton obtained in the Gulf of California, an undescribed species of the genus Hyperoche Bovallius was collected. The new species is similar to Hyperoche medusarum Kroyer and Hyperoche luetkenides Walker. It differs from its congeners mainly by the strong, large chela of pereopod 2 and the absence of processes or denticles along the posterior distal margin of same structure. It was collected at a depth of 1136 m as a symbiont of the bathypelagic hydromedusa Chromatonema erythrogonon (Bigelow). The amphipod remained grasped to the medusa subumbrellar cavity. Seven other associations are known between hyperiids and jellies in the Gulf of California, most from the epipelagic layer. This is the only deep-living species of Hyperoche known. C1 ECOSUR, Unidad Chetumal, Chetumal 77000, Q Roo, Mexico. Smithsonian Inst, Museum Natl Hist Nat, Washington, DC 20560 USA. RP Gasca, R (reprint author), ECOSUR, Unidad Chetumal, Carr Chetumal Calderitas Km 5-5,Apdo Postal 424, Chetumal 77000, Q Roo, Mexico. EM rgasca@ecosur-qroo.mx RI Gasca, Rebeca/Q-7720-2016 OI Gasca, Rebeca/0000-0002-9716-1964 NR 21 TC 8 Z9 8 U1 1 U2 2 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0142-7873 J9 J PLANKTON RES JI J. Plankton Res. PD JUN PY 2005 VL 27 IS 6 BP 617 EP 621 DI 10.1093/plankt/fbi037 PG 5 WC Marine & Freshwater Biology; Oceanography SC Marine & Freshwater Biology; Oceanography GA 957HZ UT WOS:000231362200011 ER PT J AU Swider, JR Smith, M AF Swider, JR Smith, M TI Funori: Overview of a 300-year-old consolidant SO JOURNAL OF THE AMERICAN INSTITUTE FOR CONSERVATION LA English DT Article ID RED SEAWEED; POLYSACCHARIDES AB Funori, a product from seaweed found mostly in Japan, has been used as an adhesive and a consolidant for centuries. Many conservators are familiar with funori but may be unaware of its chemistry and reliable methods for its preparation. Funori has been used successfully for decades at the Freer Gallery of Art and Arthur M. Sackler Gallery's Department of Conservation and Scientific Research in the paper, East Asian paintings, and object conservation laboratories. This article is a review of the conservation and scientific literature to give conservators insight into the chemistry of funori and related seaweeds and to propose methods for its preparation. C1 McCrone Assoc Inc, Westmont, IL 60559 USA. Natl Gallery Art, Dept Sci, Washington, DC 20565 USA. Smithsonian Inst, Freer Gallery Art & Arthur M Sackler Gallery, Dept Conservat & Sci Res, Washington, DC 20560 USA. RP Swider, JR (reprint author), McCrone Assoc Inc, 850 Pasquinelli Dr, Westmont, IL 60559 USA. NR 34 TC 5 Z9 5 U1 0 U2 7 PU AMER INST CONSERVATION HISTORIC ARTISTIC WORKS PI WASHINGTON PA 1717 K ST, NW, STE 301, WASHINGTON, DC 20006 USA SN 0197-1360 J9 J AM INST CONSERV JI J. Am. Inst. Conserv. PD SUM PY 2005 VL 44 IS 2 BP 117 EP 126 PG 10 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA 002RJ UT WOS:000234628800005 ER PT J AU Kaminitz, MA AF Kaminitz, MA TI Caring fora American Indian objects: A practical and cultural guide. SO JOURNAL OF THE AMERICAN INSTITUTE FOR CONSERVATION LA English DT Book Review C1 Smithsonian Inst, Natl Museum Amer Indian, Cultural Resources Ctr, Suitland, MD 20746 USA. RP Kaminitz, MA (reprint author), Smithsonian Inst, Natl Museum Amer Indian, Cultural Resources Ctr, 4220 Silver Hill Rd, Suitland, MD 20746 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU AMER INST CONSERVATION HISTORIC ARTISTIC WORKS PI WASHINGTON PA 1717 K ST, NW, STE 301, WASHINGTON, DC 20006 USA SN 0197-1360 J9 J AM INST CONSERV JI J. Am. Inst. Conserv. PD SUM PY 2005 VL 44 IS 2 BP 147 EP 149 PG 3 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA 002RJ UT WOS:000234628800009 ER PT J AU Reinert, JF Harbach, RE AF Reinert, JF Harbach, RE TI Corrections to the spelling of species names in genera Psorophora and Verrallina, with a note on the correct gender of Udaya SO JOURNAL OF THE AMERICAN MOSQUITO CONTROL ASSOCIATION LA English DT Article DE Diptera; Culicidae; Psorophora; Udaya; Verrallina AB The spelling of specific names for a species of Psorophora and 4 species of Verrallina are corrected to correspond with the gender of the corresponding genus. An explanation is given for treating Udaya as masculine, rather than feminine as indicated in A Catalog of the Mosquitoes of the World. C1 USDA ARS, Ctr Med Agr & Vet Entomol, CMAVE, Gainesville, FL 32608 USA. Smithsonian Inst, Museo Nacl Hist Nat, WRBU, Washington, DC 20560 USA. Nat Hist Museum, Dept Entomol, London SW7 5BD, England. RP Reinert, JF (reprint author), USDA ARS, Ctr Med Agr & Vet Entomol, CMAVE, 1600-1700 SW 23rd Dr, Gainesville, FL 32608 USA. NR 10 TC 0 Z9 0 U1 0 U2 2 PU AMER MOSQUITO CONTROL ASSOC PI EATONTOWN PA P O BOX 234, EATONTOWN, NJ 07724-0234 USA SN 8756-971X J9 J AM MOSQUITO CONTR JI J. Am. Mosq. Control Assoc. PD JUN PY 2005 VL 21 IS 2 BP 227 EP 228 DI 10.2987/8756-971X(2005)21[227:CTTSOS]2.0.CO;2 PG 2 WC Entomology SC Entomology GA 934MJ UT WOS:000229712600019 PM 16033128 ER PT J AU Deem, SL Emmons, LH AF Deem, SL Emmons, LH TI Exposure of free-ranging maned wolves (Chrysocyon brachyurus) to infectious and parasitic disease agents in the Noel Kempff Mercado National Park, Bolivia SO JOURNAL OF ZOO AND WILDLIFE MEDICINE LA English DT Article DE Bolivia; Chrysocyon brachyurus; infectious diseases; maned wolf; parasitic diseases ID DOGS LYCAON-PICTUS; CANINE-DISTEMPER; PARVOVIRUS INFECTION; WILDLIFE; CORONAVIRUS; CARNIVORES; HEALTH; WOLF AB Maned wolves (Chrysocyon brachyurus) are neotropic mammals, listed as a CITES Appendix 11 species, with a distribution south of the Amazon forest from Bolivia, through northern Argentina and Paraguay and into eastern Brazil and northern Uruguay. Primary threats to the survival of free-ranging maned wolves include habitat loss, road kills, and shooting by farmers. An additional threat to the conservation of maned wolves is the risk of morbidity and mortality due to infectious and parasitic diseases. Captive maned wolves are susceptible to, and die from, common infectious diseases of domestic dogs (Canis Jamiliaris) including canine distemper virus (CDV), canine parvovirus (CPV), rabies virus, and canine adenovirus (CAV). Results from this study show that free-ranging maned wolves in a remote area of Bolivia have been exposed to multiple infectious and parasitic agents of domestic carnivores, including CAV, CDV, CPV, canine coronavirus, rabies virus, Leptospira interrogans spp., Toxoplasma gondii, and Dirafilaria immitis, and may be at increased risk for disease due to these agents. C1 Smithsonian Inst, Dept Systemat Biol, Washington, DC 20013 USA. Wildlife Conservat Soc, Field Vet Program, Bronx, NY 10460 USA. RP Deem, SL (reprint author), Smithsonian Inst, Natl Zool Pk, Dept Anim Hlth, 3001 Connecticut Ave, Washington, DC 20008 USA. NR 38 TC 25 Z9 31 U1 0 U2 17 PU AMER ASSOC ZOO VETERINARIANS PI YULEE PA 581705 WHITE OAK ROAD, YULEE, FL 32097 USA SN 1042-7260 J9 J ZOO WILDLIFE MED JI J. Zoo Wildl. Med. PD JUN PY 2005 VL 36 IS 2 BP 192 EP 197 DI 10.1638/04-076.1 PG 6 WC Veterinary Sciences SC Veterinary Sciences GA 959MS UT WOS:000231522600005 PM 17323558 ER PT J AU Smith, KM Murray, S Sanchez, C AF Smith, KM Murray, S Sanchez, C TI Successful treatment of suspected exertional myopathy in a rhea (Rhea americana) SO JOURNAL OF ZOO AND WILDLIFE MEDICINE LA English DT Article DE anxiolytics; hyperexcitability; myopathy; physical therapy; Rhea americana ID CAPTURE MYOPATHY; RHABDOMYOLYSIS AB A 7-yr-old, adult, female greater rhea (Rhea americana) from the National Zoological Park presented with a 24-hr history of severe left leg lameness that progressed to an inability to stand. Blood work revealed creatine phosphokinase (CPK) above 50,000 U/L and elevated lactate dehydrogenase. The bird's condition deteriorated over the next week. The bird's CPK increased to over 208,400 U/L. Aggressive intravenous fluids and physical therapy along with oral anxiolytic and muscle-relaxant drugs were instituted. After 2 wk of aggressive therapy, initial signs of improvement were noted. By day 28, the bird was able to walk unassisted with no noticeable lameness. This is one of the few reported cases of successful treatment of suspected ratite exertional myopathy. It is believed that success in this case can be attributed to persistent, aggressive physical therapy, muscle relaxants, and anxiolytics aimed to counteract the hyperexcitable nature of these birds. C1 Smithsonian Inst, Natl Zool Pk, Dept Anim Hlth, Washington, DC 20008 USA. RP Smith, KM (reprint author), Wildlife Conservat Soc, 2300 So Blvd, Bronx, NY 10460 USA. NR 12 TC 7 Z9 7 U1 0 U2 5 PU AMER ASSOC ZOO VETERINARIANS PI MEDIA PA 6 NORTH PENNELL ROAD, MEDIA, PA 19063 USA SN 1042-7260 J9 J ZOO WILDLIFE MED JI J. Zoo Wildl. Med. PD JUN PY 2005 VL 36 IS 2 BP 316 EP 320 DI 10.1638/04-050.1 PG 5 WC Veterinary Sciences SC Veterinary Sciences GA 959MS UT WOS:000231522600023 PM 17323576 ER PT J AU Bergenius, MAJ McCormick, MI Meekan, MG Robertson, DR AF Bergenius, MAJ McCormick, MI Meekan, MG Robertson, DR TI Environmental influences on larval duration, growth and magnitude of settlement of a coral reef fish SO MARINE BIOLOGY LA English DT Article ID COD GADUS-MORHUA; MARINE FISH; DAMSELFISHES POMACENTRIDAE; CARIBBEAN PANAMA; HERRING LARVAE; TEMPERATURE; MORTALITY; MICROSTRUCTURE; RECRUITMENT; DETERMINES AB The influence of environmental variables on the planktonic growth, pelagic larval duration and settlement magnitude was examined for the coral reef surgeonfish Acanthurus chirurgus. Newly settled fish were collected daily from patch reefs in the San Blas Archipelago, Caribbean Panama for 3.5 years. Environmental influences on growth were examined at three different life history stages: from 0 to 6 days, 7 to 25 days and from 26 to 50 days after hatching. Larval growth was correlated, using multiple regression techniques, with a combination of factors including solar radiation, rainfall, and along-shore winds. Depending on the life history stage, these accounted for 13-38% of the variation in growth rates when all the months were included in the analyses. Correlations between environmental variables and growth also varied among seasons and were stronger in the dry than in the wet season. During the dry season solar radiation, rainfall and along-shore winds described 57%, 86% and 74% of the variability in growth between 0 and 6 days, 7 and 25 days and 26 and 50 days, respectively. During the wet season rainfall, along-shore winds and temperature only described 38% of the variability in early growth and 27% of growth just before settlement. No significant model was found to describe growth 7-25 days after hatching during the wet season. Rainfall, solar radiation and along-shore winds were negatively correlated with growth up to 25 days after hatching but positively correlated as larvae approached settlement at a mean age of 52 days. Over 65% of the variability in pelagic larval duration was accounted for by a regression model that included solar radiation and along-shore winds. When data sets from wet and dry seasons were analysed separately, along-shore winds accounted for 67% of the change in larval duration in the dry season, and solar radiation accounted for 23% of the variation in larval duration in the wet season. Only 22% of the variability in settlement intensity could be described by solar radiation and temperature, when all months of the year were included in the analysis. Solar radiation and rainfall were included in a regression model that accounted for 40% of the variation in numbers of fish settling during the dry season. This study suggests that the levels of solar radiation, along-shore winds and rainfall during the early larval life can have important effects on the growth, larval duration and consequently, the settlement magnitude of marine fishes. Results also highlight the need to account for seasonality and ontogeny in studies of environmental influences. C1 James Cook Univ N Queensland, Sch Marine Biol & Aquaculture, Townsville, Qld 4811, Australia. Australian Inst Marine Sci, Casuarina MC, NT 0811, Australia. Smithsonian Trop Res Inst Balboa Panama, APO, AA 34002 USA. RP James Cook Univ N Queensland, Sch Marine Biol & Aquaculture, Townsville, Qld 4811, Australia. EM mikaela.bergenius@jcu.edu.au RI McCormick, Mark/J-8301-2014 OI McCormick, Mark/0000-0001-9289-1645 NR 47 TC 39 Z9 40 U1 9 U2 29 PU SPRINGER HEIDELBERG PI HEIDELBERG PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY SN 0025-3162 EI 1432-1793 J9 MAR BIOL JI Mar. Biol. PD JUN PY 2005 VL 147 IS 2 BP 291 EP 300 DI 10.1007/s00227-005-1575-z PG 10 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 933KE UT WOS:000229626500002 ER PT J AU Verling, E Barnes, DKA Crook, AC AF Verling, E Barnes, DKA Crook, AC TI Smashing tests? Patterns and mechanisms of adult mortality in a declining echinoid population SO MARINE BIOLOGY LA English DT Article ID URCHINS STRONGYLOCENTROTUS-DROEBACHIENSIS; PARACENTROTUS-LIVIDUS ECHINOIDEA; LOUGH INE; COVERING BEHAVIOR; MASS MORTALITY; NOVA-SCOTIA; ECOLOGY; DISTURBANCE; COMMUNITY; VARIABILITY AB Mass mortality of echinoids is well documented, and has potentially profound effects on benthic communities. However, no study to date has quantitatively investigated how regular, predictable events such as winter storms might lead to large mortality events in pivotal echinoid species. Hydrodynamic disturbances can be major drivers of crucial biological processes in benthic communities. For echinoid populations in particular, wave action in shallow waters generated by high winds (winter storms) can cause displacement, damage and even death to individuals. However, evidence for displacement-mediated mortality is scant in the literature, in part because it is so difficult to demonstrate in exposed environments where echinoids are frequently found. In this study, we examined mortality in a sheltered subtidal population of the European purple sea urchin Paracentrotus lividus over a 3-year period, and examined the role that dislodgement by wave action or predation might play in these mortality patterns. Because our study population has been in decline for the past three decades, we considered it important to evaluate its current status in addition to assessing the contribution that adult mortality makes to that decline. We sampled twice per month, using the density of freshly dead echinoid material to assess the extent of adult mortality. The Irish Meteorological Service provided our estimates of wind speed data. We compared historical and recent data on P. lividus size frequency data to investigate change the population structure (Poor recruitment would be caused by failure to spawn over a prolonged period). Our data suggest ongoing declines in this population, and support the theory that the decline of the P. lividus population of Lough Hyne is a result of persistent recruitment failure linked to repeated cool maximum sea surface temperatures. Although we found peaks of P. lividus mortality were coincident with spikes in wind speed, mortality was low, and seems unlikely to have contributed significantly to the dramatic decline in P. lividus in the past three decades. C1 Univ Coll, Dept Zool Ecol & Plant Sci, Cork, Ireland. British Antarctic Survey, Div Biol Sci, Cambridge CB3 0ET, England. Univ Reading, Ctr Dev Teaching & Learning, Reading RG6 6AA, Berks, England. RP Verling, E (reprint author), Smithsonian Environm Res Ctr, Marine Invas Res Lab, 647 Contees Wharf Rd, Edgewater, MD 21037 USA. EM verlinge@si.edu NR 39 TC 8 Z9 8 U1 1 U2 4 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013 USA SN 0025-3162 J9 MAR BIOL JI Mar. Biol. PD JUN PY 2005 VL 147 IS 2 BP 509 EP 515 DI 10.1007/s00227-005-1563-3 PG 7 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 933KE UT WOS:000229626500023 ER PT J AU Sallum, MAM Peyton, EL Wilkerson, RC AF Sallum, MAM Peyton, EL Wilkerson, RC TI Six new species of the Anopheles leucosphyrus group, reinterpretation of An. elegans and vector implications SO MEDICAL AND VETERINARY ENTOMOLOGY LA English DT Review DE Anopheles baimaii; An. cracens; An. dirus; An. elegans; An. latens; An. leucosphyrus; An. mirans; An. recens; An. scanloni; Plasmodium falciparum; P. cynomolgi; P. fragile; P. inui; P. vivax; Wuchereria; Culicidae; filaria vector; forest malaria vectors; malaria transmission; new species; morphology; mosquito systematics; Oriental Region ID POLYMERASE-CHAIN-REACTION; DIRUS COMPLEX; BALABACENSIS COMPLEX; SOUTHEAST-ASIA; MALARIA VECTORS; SIMIAN MALARIA; PLASMODIUM-CYNOMOLGI; CYTOGENETIC EVIDENCE; POPULATION-STRUCTURE; GENUS ANOPHELES AB Among Oriental anopheline mosquitoes (Diptera: Culicidae), several major vectors of forest malaria belong to the group of Anopheles (Cellia) leucosphyrus Donitz. We have morphologically examined representative material (> 8000 specimens from seven countries) for taxonomic revision of the Leucosphyrus Group. Six new species are here described from adult, pupal and larval stages (with illustrations of immature stages) and formally named as follows: An. latens n. sp. (= An. leucosphyrus species A of Baimai etal., 1988b), Ail. cracens n. sp., Ail. scanloni n. sp., An. baimaii n. sp. (formerly An. dirus species B, C, D, respectively), An. mirans n. sp. and Ail. recens n. sp. Additionally, An. elegans (James) is redescribed and placed in the complex of An. dirus Peyton & Harrison (comprising Ail. baimaii, An. cracens, An. dirus, An. elegans, An. nemophilous Peyton & Ramalingam, An. scanloni and An. takasagoensis Morishita) of the Leucosphyrus Subgroup, together with An. baisasi Colless and the An. leucosphyrus complex (comprising An. balabacensis Balsas, Ail. introlatus Baisas, An. latens and An. leucosphyrus). Hence, the former Elegans Subgroup is renamed the Hackeri Subgroup (comprising An. hackeri Edwards, An. pujutensis Colless, Ail. recens and An. sulawesi Waktoedi). Distribution data and bionomics of the newly defined species are given, based on new material and published records, with discussion of morphological characters for species distinction and implications for ecology and vector roles of such species. Now these and other members of the Leucosphyrus Group are identifiable, it should be possible to clarify the medical importance and distribution of each species. Those already regarded as vectors of human malaria are: Ail. baimaii [Bangladesh, China (Yunnan), India (Andamans, Assam, Meghalaya, West Bengal), Myanmar, Thailand]; An. latens [Borneo (where it also transmits Bancroftian filariasis), peninsular Malaysia, Thailand]; probably Ail. cracens (Sumatra, peninsular Malaysia, Thailand); presumably An. scanloni (Thailand); perhaps All. elegans (the Western Ghat form of An. dirus, restricted to peninsular India); but apparently not An. recens (Sumatra) nor Ail. mirans [Sri Lanka and south-west India (Karnataka, Kerala, Tamil Nadu)), which is a natural vector of simian malarias. Together with typical An. balabacensis, An. dirus and An. leucosphyrus, therefore, the Leucosphyrus Group includes about seven important vectors of forest malaria, plus at least a dozen species of no known medical importance, with differential specific distributions collectively spanning > 5000 km from India to the Philippines. C1 Univ Sao Paulo, Fac Saude Publ, Dept Epidemiol Nucl Pesquisas Taxon & Sistemat En, BR-01246904 Sao Paulo, Brazil. Smithsonian Inst, Museum Support Ctr, Walter Reed Biosystemat Unit, Suitland, MD USA. RP Sallum, MAM (reprint author), Univ Sao Paulo, Fac Saude Publ, Dept Epidemiol Nucl Pesquisas Taxon & Sistemat En, Ave Dr Arnaldo 715, BR-01246904 Sao Paulo, Brazil. EM masallum@usp.br RI Sallum, Maria/B-8537-2012 NR 129 TC 65 Z9 76 U1 2 U2 14 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0269-283X J9 MED VET ENTOMOL JI Med. Vet. Entomol. PD JUN PY 2005 VL 19 IS 2 BP 158 EP 199 DI 10.1111/j.0269-283X.2005.00551.x PG 42 WC Entomology; Veterinary Sciences SC Entomology; Veterinary Sciences GA 933FB UT WOS:000229613200006 PM 15958025 ER PT J AU Vessot, RFC AF Vessot, RFC TI The atomic hydrogen maser oscillator SO METROLOGIA LA English DT Article ID LOW-TEMPERATURE; BINDING-ENERGY AB The basic operational requirements and present technology for high stability hydrogen maser (H-maser) oscillators are described. Design features of a high stability maser oscillator for use in space, maser operation at 0.5 K and present uses of high stability H-masers are discussed. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Vessot, RFC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 24 TC 8 Z9 8 U1 1 U2 1 PU BUREAU INT POIDS MESURES PI SEVRES CEDEX PA B1 PM PAVILLION DE BRETUEIL, F-92312 SEVRES CEDEX, FRANCE SN 0026-1394 J9 METROLOGIA JI Metrologia PD JUN PY 2005 VL 42 IS 3 SI SI BP S80 EP S89 DI 10.1088/0026-1394/42/3/S09 PG 10 WC Instruments & Instrumentation; Physics, Applied SC Instruments & Instrumentation; Physics GA 947OB UT WOS:000230654500010 ER PT J AU Moeser, AA Bermingham, E AF Moeser, AA Bermingham, E TI Isolation and characterization of eight microsatellite loci for the Neotropical freshwater catfish Pimelodella chagresi (Teleostei : Pimelodidae) SO MOLECULAR ECOLOGY NOTES LA English DT Article DE freshwater fish; microsatellites; Neotropical AB We report eight (CA)(10-35) unlinked microsatellite loci from the Neotropical freshwater catfish, Pimelodella chagresi (Siluriformes: Pimelodidae). These loci were characterized with 23 individuals collected in Panama. Number of alleles per locus varied from 7 to 23 (mean=12.9) and observed heterozygosity ranged from 0.522 to 0.909 (mean=0.732). These loci will be used to investigate the existence of cryptic species within the P. chagresi clade, and to study fine-scale population structure. C1 McGill Univ, Redpath Museum, Dept Biol, Montreal, PQ H3A 2K6, Canada. Smithsonian Trop Res Inst, Balboa, Panama. RP Moeser, AA (reprint author), McGill Univ, Redpath Museum, Dept Biol, 859 Sherbrooke St W, Montreal, PQ H3A 2K6, Canada. EM andrew.moeser@mail.mcgill.ca NR 8 TC 3 Z9 3 U1 1 U2 3 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 1471-8278 J9 MOL ECOL NOTES JI Mol. Ecol. Notes PD JUN PY 2005 VL 5 IS 2 BP 363 EP 365 DI 10.1111/j.1471-8286.2005.00928.x PG 3 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 934FC UT WOS:000229691300051 ER PT J AU Crawford, AJ Smith, EN AF Crawford, AJ Smith, EN TI Cenozoic biogeography and evolution in direct-developing frogs of Central America (Leptodactylidae : Eleutherodactylus) as inferred from a phylogenetic analysis of nuclear and mitochondrial genes SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Review DE chortis block; Craugastor; Eleutherodactylinac; paleogeography; mesoamerica; molecular phylogenetics; proto-antilles; systematics ID SEA-LEVEL CHANGES; DNA-SEQUENCES; CARIBBEAN BIOGEOGRAPHY; SPECIES GROUP; NUCLEOTIDE SUBSTITUTION; GENUS ELEUTHERODACTYLUS; MOLECULAR EVOLUTION; IGUANIAN LIZARDS; DIVERGENCE TIME; SOUTH-AMERICA AB We report the first phylogenetic analysis of DNA sequence data for the Central American component of the genus Eleutherodactylus (Anura: Leptodactylidae: Eleutherodactylinae), one of the most ubiquitous. diverse. and abundant components of the Neo-tropical amphibian fauna. We obtained DNA sequence data from 55 specimens representing 45 species. Sampling was focused on Central America, but also included Bolivia, Brazil, Jamaica. and the USA. We sequenced 1460 contiguous base pairs (bp) of the mitochondrial genome containing ND2 and five neighboring tRNA genes, plus 1300 bp of the c-myc nuclear gene. The resulting phylogenetic inferences were broadly concordant between data sets and among analytical methods. The subgenus Craugastor is monophyletic and its initial radiation was potentially rapid and adaptive. Within Craugastor. the earliest splits separate three northern Central American species groups, milesi, augusti, and alfredi. from a clade comprising the rest of Craugastor, Within the latter clade, the rhodopis group as formerly recognized comprises three deeply divergent clades that do not form a monophyletic group, we therefore restrict the content of the rho(h)pis group to one of two northern clades. and use new names for the other northern (mexicanus group) and one southern clade (bransfordii group). The new rhodopis and bransfordii groups together form the sister taxon to a clade comprising the biporcatus,fitzingeri, mexicanus, and rugulosus groups, We used a Bayesian MCMC approach together with geological and biogeographic assumptions to estimate divergence times from the combined DNA sequence data, Our results corroborated three independent dispersal events for the origins of Central American Elentherodactylus: ( 1) an ancestor of Craugastor entered northern Central America from South American in the early Paleocene, (2) an ancestor of the subgenus syrrhophits entered northern Central America from the Caribbean at the end of the Eocene. and (3) a wave of independent dispersal events from South America coincided with formation of the Isthmus of Panama during the Pliocene. We elevate the subgenus Craugastor to the genus rank. (c) 2005 Elsevier Inc. All rights reserved. C1 Univ Texas, Dept Biol, Arlington, TX 76019 USA. Smithsonian Trop Res Inst, Naos Labs, Balboa, Ancon, Panama. RP Crawford, AJ (reprint author), Smithsonian Trop Res Inst, Unit 0948, Andrew J Crawford Naos Labs, APO, Miami, FL 34002 USA. EM andrew@dna.ac OI Crawford, Andrew J./0000-0003-3153-6898 NR 129 TC 79 Z9 88 U1 4 U2 17 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 1055-7903 EI 1095-9513 J9 MOL PHYLOGENET EVOL JI Mol. Phylogenet. Evol. PD JUN PY 2005 VL 35 IS 3 BP 536 EP 555 DI 10.1016/j.ympev.2005.03.006 PG 20 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 929SM UT WOS:000229366200003 PM 15878124 ER PT J AU Cherigo, L Polanco, V Ortega-Barria, E Heller, MV Capson, TL Rios, LC AF Cherigo, L Polanco, V Ortega-Barria, E Heller, MV Capson, TL Rios, LC TI Antitrypanosomal activity of a novel norlignan purified from Nectandra lineata SO NATURAL PRODUCT RESEARCH LA English DT Article DE Trypanosoma cruzi; norlignan; Nectandra lineata; Lauraceae; Chagas' disease; ICBG ID TRYPANOSOMA-CRUZI AB Bioactivity-guided fractionation of a MeOH-EtOAc extract from the young leaves of Nectandra lineata (Lauraceae), using a Trypanosoma cruzi bioassay resulted in the isolation of a novel norlignan 3'-methoxy-3,4-methylenedioxy-4',7-epoxy-9-nor-8,5'-neolignan-9'-acetoxy (1), together with the known compound, 3'-methoxy-3,4-methylenedioxy-4'-7-epoxy-9-nor-8,5'-neolignan-7,8'-diene (2). Compounds 1 and 2 were shown to inhibit the growth of T. cruzi epimastigotes in axenic culture. C1 Univ Panama, Fac Nat & Exact Sci & Technol, Lab Nat Prod, Panama City, Panama. Florida State Univ, Inst Trop Med & Hlth Sci, Panama City, FL USA. Smithsonian Trop Res Inst, Panama City, Panama. RP Rios, LC (reprint author), Univ Panama, Fac Nat & Exact Sci & Technol, Lab Nat Prod, Apdo 0824, Panama City, Panama. EM lucr@ancon.up.ac.pa NR 10 TC 13 Z9 15 U1 0 U2 2 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 1478-6419 J9 NAT PROD RES JI Nat. Prod. Res. PD JUN PY 2005 VL 19 IS 4 BP 373 EP 377 DI 10.1080/1478641042000261950 PG 5 WC Chemistry, Applied; Chemistry, Medicinal SC Chemistry; Pharmacology & Pharmacy GA 930DB UT WOS:000229394900012 PM 15938145 ER PT J AU Hearty, PJ Karner, DB Renne, PR Olson, SL Fletcher, S AF Hearty, PJ Karner, DB Renne, PR Olson, SL Fletcher, S TI Ar-40/Ar-39 age of a young rejuvenation basalt flow: implications for the duration of volcanism and the timing of carbonate platform development during the Quaternary on Kaua'i, Hawaiian Islands SO NEW ZEALAND JOURNAL OF GEOLOGY AND GEOPHYSICS LA English DT Article DE lithospheric flexure; carbonate platform; bioclastic dunes ("eolianite"); argon dating; basalt flow; Quaternary; stratigraphy; Hawaiian Islands ID SEA-LEVEL; BERMUDA; HISTORY; STRATIGRAPHY; CALIBRATION; OAHU; AMINOSTRATIGRAPHY; GEOCHRONOLOGY; MOLOKAI; BAHAMAS AB Remnants of an extensive carbonate platform crop out along, the southeast coast of Kaua'i, Hawaii. A basalt flow within this succession has a whole-rock Ar-40/Ar-39 step-heating plateau age of 375 +/- 4 ka. The plateau age, which we interpret as the eruption age, indicates that rejuvenation volcanism persisted on Kaua'i for considerably longer (c. 200 000 yr) than previously thought, and also that published whole-rock K-Ar determinations may not accurately reflect eruption ages. The succession of younger sedimentary deposits and age of the basalt imply that the eruption occurred near the end of marine isotope stage (MIS) 11. Preservation of limestone dune assemblages and extensive paleosols above present-day sea level indicates that Kaua'i underwent a period of emergence during the early and middle Pleistocene, probably due to passage over the lithospheric arch or forebulge created by crustal loading of Maui Nui. The presence of at least eight major limestone-soil "couplets", together with extrapolated ages from the Ar-40/Ar-39 dating, make this the oldest surficial record of limestone formation in the Hawaiian Islands. This work provides a framework for further interpretation of the stratigraphy and paleoecology of Kaua'i and the tropical Hawaiian Islands. C1 Univ Wollongong, Sch Earth & Environm Sci, Wollongong, NSW 2522, Australia. Sonoma State Univ, Dept Geol, Rohnert Pk, CA 94928 USA. Berkeley Geochronol Ctr, Berkeley, CA 94985 USA. Univ Calif Berkeley, Dept Earth & Planetary Sci, Berkeley, CA 94720 USA. Smithsonian Inst, Natl Museum Natl Hist, Washington, DC 20560 USA. James Cook Univ N Queensland, Sch Earth Sci, Townsville, Qld 4811, Australia. RP Hearty, PJ (reprint author), Univ Wollongong, Sch Earth & Environm Sci, Wollongong, NSW 2522, Australia. EM paulh@uow.edu.au NR 50 TC 9 Z9 9 U1 1 U2 1 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 0028-8306 J9 NEW ZEAL J GEOL GEOP JI N. Z. J. Geol. Geophys. PD JUN PY 2005 VL 48 IS 2 BP 199 EP 211 PG 13 WC Geology; Geosciences, Multidisciplinary SC Geology GA 950DS UT WOS:000230838400001 ER PT J AU Pavlovic, Z Krems, RV Cote, R Sadeghpour, HR AF Pavlovic, Z Krems, RV Cote, R Sadeghpour, HR TI Magnetic Feshbach resonances and Zeeman relaxation in bosonic chromium gas with anisotropic interaction SO PHYSICAL REVIEW A LA English DT Article ID BOSE-EINSTEIN CONDENSATION; ATOM-MOLECULE; FERMI GAS; PHYSICS; STATES; FIELD AB Rigorous calculations of magnetic Feshbach resonances and Zeeman relaxation cross sections in an ultracold and cold chromium gas are reported. This work presents the calculation of such inelastic processes in collisions of atoms with large magnetic moments. Using our recently constructed accurate interaction potentials for the chromium dimer, we compute the positions and widths of magnetically tuned resonances in an optically trapped ultracold Cr gas. We find good agreement with recent experimental data and report that spin-change collision cross sections quickly increase with decreasing collision energy and magnetic-field strength at energies below 1 K and magnetic fields larger than 40 G. C1 Univ Connecticut, Dept Phys, Storrs, CT 06268 USA. Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. Harvard Univ, Dept Phys, Ctr Ultracold Atoms, Cambridge, MA 02138 USA. RP Univ Connecticut, Dept Phys, 2152 Hillside Rd, Storrs, CT 06268 USA. NR 39 TC 27 Z9 27 U1 0 U2 3 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 JUN PY 2005 VL 71 IS 6 AR 061402 DI 10.1103/PhysRevA.71.061402 PG 4 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 942ID UT WOS:000230275200017 ER PT J AU Cervino, JM Littler, M Littler, D Polson, S Goreau, TJ Brooks, B Smith, GW AF Cervino, J. M. Littler, M. Littler, D. Polson, S. Goreau, T. J. Brooks, B. Smith, G. W. TI Identification of microbes associated with coralline lethal algal disease and its relationship to glacial ice melt (global warming) SO PHYTOPATHOLOGY LA English DT Meeting Abstract C1 [Cervino, J. M.] Pace Univ, New York, NY 10038 USA. [Goreau, T. J.] Med Univ S Carolina, Charleston, SC 29425 USA. [Littler, M.; Littler, D.; Polson, S.; Brooks, B.] Smithsonian, Washington, DC USA. [Brooks, B.] Global Coral Reef Alliance, Cambridge, MA USA. [Smith, G. W.] Univ S Carolina, Aiken, SC USA. RI Brooks, Barrett/C-5306-2008; Polson, Shawn/B-7696-2011 OI Polson, Shawn/0000-0002-3398-6932 NR 0 TC 1 Z9 1 U1 2 U2 8 PU AMER PHYTOPATHOLOGICAL SOC PI ST PAUL PA 3340 PILOT KNOB ROAD, ST PAUL, MN 55121 USA SN 0031-949X J9 PHYTOPATHOLOGY JI Phytopathology PD JUN PY 2005 VL 95 IS 6 SU S BP S120 EP S121 PG 2 WC Plant Sciences SC Plant Sciences GA V44GO UT WOS:000202991401195 ER PT J AU Herre, EA Mejia, LC Kyllo, DA Castillo, M Ramirez, LA AF Herre, E. A. Mejia, L. C. Kyllo, D. A. Castillo, M. Ramirez, L. A. TI Anti-pathogen effects of fungal endophytes in tropical host plants SO PHYTOPATHOLOGY LA English DT Meeting Abstract C1 [Herre, E. A.; Mejia, L. C.; Kyllo, D. A.; Castillo, M.; Ramirez, L. A.] Smithsonian Trop Res Inst, Balboa, Panama. NR 0 TC 0 Z9 0 U1 1 U2 1 PU AMER PHYTOPATHOLOGICAL SOC PI ST PAUL PA 3340 PILOT KNOB ROAD, ST PAUL, MN 55121 USA SN 0031-949X J9 PHYTOPATHOLOGY JI Phytopathology PD JUN PY 2005 VL 95 IS 6 SU S BP S138 EP S138 PG 1 WC Plant Sciences SC Plant Sciences GA V44GO UT WOS:000202991401304 ER PT J AU Van Dyk, SD Filippenko, AV Chornock, R Li, WD Challis, PM AF Van Dyk, SD Filippenko, AV Chornock, R Li, WD Challis, PM TI Supernova 1954J (Variable 12) in NGC 2403 unmasked SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID LUMINOUS BLUE VARIABLES; SPACE-TELESCOPE IMAGES; MASSIVE STAR-CLUSTERS; ETA-CARINAE ANALOG; WOLF-RAYET STARS; NEARBY GALAXIES; STELLAR CONTENT; RHO-CASSIOPEIAE; SN 1987A; EVOLUTION AB We have confirmed that the precursor star of the unusual supernova 1954J ( also known as Variable 12) in NGC 2403 survived what appears to have been a superoutburst, similar to the 1843 Great Eruption of eta Carinae in the Galaxy. The apparent survivor has changed little in brightness and color over the last 8 years, and a Keck spectrum reveals characteristics broadly similar to those of eta Car. This is further suggested by our identification of the actual outburst-surviving star in high-resolution images obtained with the Advanced Camera for Surveys on the Hubble Space Telescope. We reveal this "supernova impostor" as a highly luminous (M-V(o) approximate to -8.0 mag), very massive (M-initial greater than or similar to 25 M-.) eruptive star, now surrounded by a dusty` (A(V) approximate to mag) nebula, similar to eta Car's famous Homunculus. C1 CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Van Dyk, SD (reprint author), CALTECH, Spitzer Sci Ctr, Mail Code 220-6, Pasadena, CA 91125 USA. EM vandyk@ipac.caltech.edu; alex@astro.berkeley.edu; chornock@astro.berkeley.edu; weidong@astro.berkeley.edu; challis@cfa.harvard.edu OI Van Dyk, Schuyler/0000-0001-9038-9950 NR 59 TC 24 Z9 24 U1 0 U2 2 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 JUN PY 2005 VL 117 IS 832 BP 553 EP 562 DI 10.1086/430238 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 932CL UT WOS:000229531700002 ER PT J AU Phillips, JD Reasenberg, RD AF Phillips, JD Reasenberg, RD TI Tracking frequency laser distance gauge SO REVIEW OF SCIENTIFIC INSTRUMENTS LA English DT Article ID QUANTUM-NOISE; METROLOGY; INTERFEROMETRY; REFRACTOMETER; NONLINEARITY; POINTS; SIGNAL; INDEX AB Advanced astronomical missions with greatly enhanced resolution and physics missions of unprecedented accuracy will require laser distance gauges of substantially improved performance. We describe a laser gauge, based on Pound-Drever-Hall locking, in which the optical frequency is adjusted to maintain an interferometer's null condition. This technique has been demonstrated with pm performance. Automatic fringe hopping allows it to track arbitrary distance changes. The instrument is intrinsically free of the nm-scale cyclic bias present in traditional (heterodyne) high-precision laser gauges. The output is a radio frequency, readily measured to sufficient accuracy. The laser gauge has operated in a resonant cavity, which improves precision, can suppress the effects of misalignments, and makes possible precise automatic alignment. The measurement of absolute distance requires little or no additional hardware, and has also been demonstrated. The proof-of-concept version, based on a stabilized HeNe laser and operating on a 0.5 m path, has achieved 10 pm precision with 0.1 s integration time, and 0.1 mm absolute distance accuracy. This version has also followed substantial distance changes as fast as 16 mm/s. We show that, if the precision in optical frequency is a fixed fraction of the linewidth, both incremental and absolute distance precision are independent of the distance measured. We discuss systematic error sources, and present plans for a new version of the gauge based on semiconductor lasers and fiber-coupled components. C1 Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Phillips, JD (reprint author), Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, 60 Garden St,MS63, Cambridge, MA 02138 USA. EM jphillips@cfa.harvard.edu NR 28 TC 14 Z9 14 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 0034-6748 J9 REV SCI INSTRUM JI Rev. Sci. Instrum. PD JUN PY 2005 VL 76 IS 6 AR 064501 DI 10.1063/1.1921408 PG 9 WC Instruments & Instrumentation; Physics, Applied SC Instruments & Instrumentation; Physics GA 937YG UT WOS:000229962000086 ER PT J AU Hacker, BC AF Hacker, BC TI The military and society in Russia, 1450-1917. SO SIXTEENTH CENTURY JOURNAL LA English DT Book Review C1 Smithsonian Inst, Washington, DC 20560 USA. RP Hacker, BC (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU SIXTEENTH CENTURY JOURNAL PUBL PI KIRKSVILLE PA MC111-L, TRUMAN STATE UNIV, 100 E NORMAL ST, KIRKSVILLE, MO 63501-4211 USA SN 0361-0160 J9 SIXTEENTH CENT J JI Sixt. Century J. PD SUM PY 2005 VL 36 IS 2 BP 497 EP 498 PG 2 WC History SC History GA 941NK UT WOS:000230221300028 ER PT J AU Small, LM AF Small, LM TI Reversing the clock (Conserving the nation's treasures) 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 JUN PY 2005 VL 36 IS 3 BP 14 EP 14 PG 1 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA 928HO UT WOS:000229262400002 ER PT J AU Cotrufo, MF Drake, B Ehleringer, JR AF Cotrufo, MF Drake, B Ehleringer, JR TI Palatability trials on hardwood leaf litter grown under elevated CO2: a stable carbon isotope study SO SOIL BIOLOGY & BIOCHEMISTRY LA English DT Article DE stable C isotopes; elevated CO2; leaf litter; Porcellio sp.; decomposition ID SOIL ORGANIC-MATTER; ATMOSPHERIC CO2; DECOMPOSITION; QUALITY; ENRICHMENT; PLANTS; C-13 AB The palatability to isopods and microbes of a broad range of hardwood leaf litter, derived from three field CO2-enrichment experiments in the USA, was investigated, using delta(13)C, to trace the C flow from litter to isopods and to CO2 respired by microbial decomposition. Leaf litter grown under elevated CO2 had delta(13)C values ranging from - 39 to -45 parts per thousand, which were significantly different from ambient litter delta(13)C values of around - 30 parts per thousand. Litter palatability to isopods of the Porcellio sp. was tested by incubating ambient- and elevated-CO2 litter, and a mixture of the two, in the presence of isopods for 14 days, under environmentally controlled conditions; delta(13)C was measured on litter and isopods' body before and after incubation. In an additional experiment, litter was incubated in the absence of fauna for 30 days, and on five occasions the delta(13)C of the CO2 respired from litter was measured. The C-13 label was clearly carried from the litter source to the isopods' bodies, and their faeces. For microbial-respired CO2, delta(13)C was significantly higher than that of the litter source, suggesting preferential degradation of substrates enriched in C-13 as compared to those in the overall litter. With the exception of Quercus myrtifolia leaf litter, elevated CO2 did not affect the palatability to isopods nor the microbial degradation of any of the litters, possibly as a result of unaltered litter N concentration. However, significant differences in litter palatability and decay rates were observed among the different species. With this study, the use of isotopically labelled litter material was confirmed as a key methodology that can significantly contribute to the advancement of the understanding of litter decomposition and of the quantification of C fluxes in the process. (c) 2005 Elsevier Ltd. All rights reserved. C1 Univ Naples 2, Dept Environm Sci, I-81100 Caserta, Italy. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Univ Utah, Dept Biol, Salt Lake City, UT 84112 USA. RP Cotrufo, MF (reprint author), Univ Naples 2, Dept Environm Sci, Via Vivaldi 43, I-81100 Caserta, Italy. EM mfrancesca.cotrufo@unina2.it RI Cotrufo, M. Francesca/C-1614-2013 OI Cotrufo, M. Francesca/0000-0002-6191-8953 NR 22 TC 12 Z9 12 U1 1 U2 13 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0038-0717 J9 SOIL BIOL BIOCHEM JI Soil Biol. Biochem. PD JUN PY 2005 VL 37 IS 6 BP 1105 EP 1112 DI 10.1016/j.soilbio.2004.11.009 PG 8 WC Soil Science SC Agriculture GA 920TJ UT WOS:000228712700010 ER PT J AU Megonigal, JP Vann, CD Wolf, AA AF Megonigal, JP Vann, CD Wolf, AA TI Flooding constraints on tree (Taxodium distichum) and herb growth responses to elevated CO2 SO WETLANDS LA English DT Article DE elevated CO2; emergent aquatic macrophyte; photosynthesis; wetland; Taxodium; global change; flooding ID CANOPY STOMATAL CONDUCTANCE; CARBON-DIOXIDE ENRICHMENT; VAPOR-PRESSURE DEFICIT; LEAF GAS-EXCHANGE; ATMOSPHERIC CO2; SOIL; WETLAND; STRESS; RICE; ALLOCATION AB Elevated CO2 generally stimulates C-3-type photosynthesis, but it is unclear how an increase in CO2, assimilation will interact with other factors that influence plant growth. In wetlands, the response of plants to elevated CO2, will interact with soil saturation, particularly in forested wetlands where soil saturation is a strong regulator of plant productivity. We performed a four-month experiment to determine whether elevated CO2 and flooding interact to influence the growth of a flood-tolerant tree (Taxodium distichum) and a flood-tolerant herbaceous emergent macrophyte (Orontium aquaticum). Seedlings were grown in glasshouses at two CO2 levels (350 and 700 mu L L-1) crossed with two water depths (5 cm above and >= 5 cm below the soil surface). We hypothesized that elevated CO2, would increase photosynthesis regardless of water depth and species; however, we also expected flooding to prevent elevated CO2, from increasing the growth of the tree species due to 0, limitation or other physiological stresses associated with reduced soil environments. We found that elevated CO2, increased whole-plant photosynthesis in both species regardless of the flooding treatment. For T. distichum, this higher photosynthetic rate resulted in greater biomass only in the non-flooded treatment. This result suggests that some factor related to flooding constrained the biomass response of the flooded woody plants to elevated CO2. In contrast, elevated CO2, increased O. aquaticum biomass regardless of the flooding regime, perhaps because it occurs in wetter landscape positions than T. distichum and is less sensitive to flooding. We conclude that flooding may limit plant growth responses to elevated CO2, particularly in woody plant species. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Megonigal, JP (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM megonigalp@si.edu NR 48 TC 7 Z9 9 U1 0 U2 9 PU SOC WETLAND SCIENTISTS PI LAWRENCE PA 810 E TENTH ST, P O BOX 1897, LAWRENCE, KS 66044 USA SN 0277-5212 J9 WETLANDS JI Wetlands PD JUN PY 2005 VL 25 IS 2 BP 430 EP 438 DI 10.1672/17 PG 9 WC Ecology; Environmental Sciences SC Environmental Sciences & Ecology GA 940OD UT WOS:000230152900017 ER PT J AU Peer, BD Rothstein, SI Rivers, JW AF Peer, BD Rothstein, SI Rivers, JW TI First record of Bronzed Cowbird parasitism on the Great-tailed Grackle SO WILSON BULLETIN LA English DT Article ID BROOD PARASITISM; HOST COEVOLUTION; EGG REJECTION AB We report the first record of Bronzed Cowbird (Molothrus aeneus) parasitism on the Great-tailed Grackle (Quiscalus mexicanus), which represents the 96th known host for this cowbird species. The record is based on a parasitized clutch, collected from Sinaloa, Mexico, in the collection at the Western Foundation of Vertebrate Zoology. The clutch contained four grackle eggs and one Bronzed Cowbird egg. This record is unusual because the Great-tailed Grackle is extremely intolerant of foreign eggs, ejecting them from their nests almost immediately. As the Bronzed Cowbird expands its range and is studied in greater depth, more hosts will undoubtedly be recorded. C1 Univ Calif Santa Barbara, Dept Ecol Evolut & Marine Biol, Santa Barbara, CA 93106 USA. Smithsonian Inst, Genet Program, Museum Natl Hist Nat, Washington, DC 20008 USA. RP Peer, BD (reprint author), Simpson Coll, Dept Biol, 701 N C St, Indianola, IA 50125 USA. EM brian.peer@simpson.edu NR 19 TC 1 Z9 1 U1 0 U2 1 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 JUN PY 2005 VL 117 IS 2 BP 194 EP 196 DI 10.1676/04-077 PG 3 WC Ornithology SC Zoology GA 939ES UT WOS:000230055800011 ER PT J AU Graves, GR Rahbek, C AF Graves, GR Rahbek, C TI Source pool geometry and the assembly of continental avifaunas SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE assemblage dispersion fields; birds ID AVIAN SPECIES RICHNESS; GEOGRAPHIC RANGE; NULL HYPOTHESES; ANDEAN BIRDS; DIVERSITY; PATTERNS; SIZE; SPECIATION; ABUNDANCE; FOREST AB Classical niche-assembly models propose that the composition of biotic communities in continental landscapes is determined chiefly by the autecology of species, interspecific competition, and the diversity of resources and habitats within a region. In contrast, stochastic models propose that simulation algorithms can replicate the macroecological patterns, if not the mechanisms, of community assembly. Despite fundamental differences in assumptions, both categories of models assume that species are drawn from regional source pools. We explored the implications of source pool geometry on the assembly of avian communities with an analysis of assemblage dispersion fields, which can be visualized by overlaying the geographic ranges of all species that occur in an assemblage. Contours of species richness surrounding focal quadrats illustrate the decay rate of assemblage similarity with distance and the probable geometry of assemblage source pools. We used a geographic database for 2,891 species of South American birds to characterize dispersion fields for assemblages sampled by 1&DEG; latitude-longitude quadrats (n = 1,676). We show that the median range size of dispersion fields varies by an order of magnitude across the continent. Because abundance generally correlates with geographic range size within taxonomic groups, the number of individuals per species in avifaunal source pools must also vary by an order of magnitude. Most significantly, dispersion field geometry was surprisingly asymmetrical and exhibited complex geographical patterns that were associated with the distribution of biomes. These results are broadly consistent with the predictions of niche-assembly models but offer little support for stochastic assembly models. C1 Smithsonian Inst, Museum Natl Hist Nat, Dept Vertebrate Zool, Washington, DC 20013 USA. Univ Copenhagen, Inst Biol, DK-2100 Copenhagen, Denmark. RP Graves, GR (reprint author), Smithsonian Inst, Museum Natl Hist Nat, Dept Vertebrate Zool, MRC-116,POB 37012, Washington, DC 20013 USA. EM gravesg@si.edu RI Rahbek, Carsten/D-9372-2013; Rahbek, Carsten/L-1129-2013; publist, CMEC/C-3010-2012; publicationpage, cmec/B-4405-2017 NR 70 TC 71 Z9 71 U1 4 U2 21 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 MAY 31 PY 2005 VL 102 IS 22 BP 7871 EP 7876 DI 10.1073/pnas.0500424102 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 932CE UT WOS:000229531000018 PM 15911769 ER PT J AU Greenberg, JA Kefauver, SC Stimson, HC Yeaton, CJ Ustin, SL AF Greenberg, JA Kefauver, SC Stimson, HC Yeaton, CJ Ustin, SL TI Survival analysis of a neotropical rainforest using multitemporal satellite imagery SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE remote sensing; change detection; multitemporal; survival analysis; neotropical rainforests; deforestation; roads; Ecuador Parque National Yasuni ID LAND-COVER-CHANGE; DEFORESTATION; DYNAMICS; PATTERNS; SYSTEMS; MEXICO; RATES; ROADS AB We present results of an analysis of deforestation at a UNESCO Biosphere Reserve, the Parque National Yasuni, located in the rainforests of eastern Ecuador using multitemporal Landsat TM and ETM+ satellite imagery. Using survival analysis, we assessed both cut-rent and future trends in deforestation rates, and investigated the impact of spatial, cultural, and economic factors oil deforestation. These factors included the distance from roads, rivers, research facilities, oil facilities, markets and towns. and land ownership by colonists, native inhabitants, and an oil company. We found the annual rate of deforestation is currently only 0.11%, but that this rate is increasing with time and, assuming that the trend of increasing rate of forest loss continues, we would predict that by 2063, 50% of the forest within 2 kill of an oil access road will be lost to unhindered colonization and anthropogenic conversion. The Quechua colonists are associated with areas of the highest rate of deforestation, followed by the native Huaorani and the lowest region of deforestation was in areas Occupied by a local oil company. By far, the strongest predictor of where deforestation is predicted to occur was proximity to the road. Proximity to research sites, oil facilities, market, and rivers significantly decreases deforestation rates, and proximity to towns significantly increases deforestation rates. (c) 2005 Elsevier Inc. All rights reserved. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Univ Calif Davis, Davis, CA 95616 USA. Smithsonian Inst, Conservat Res Ctr, Washington, DC 20560 USA. RP Greenberg, JA (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM jgreenberg@arc.nasa.gov OI Greenberg, Jonathan/0000-0001-8435-9077; Kefauver, Shawn/0000-0002-1687-1965 NR 31 TC 21 Z9 21 U1 0 U2 9 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD MAY 30 PY 2005 VL 96 IS 2 BP 202 EP 211 DI 10.1016/j.rse.2005.02.010 PG 10 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 942LV UT WOS:000230284800006 ER PT J AU Johnson, GD Britz, R AF Johnson, GD Britz, R TI Description of the smallest Triodon on record (Teleostei : Tetraodontiformes : Triodontidae) SO ICHTHYOLOGICAL RESEARCH LA English DT Article DE Triodon; early juvenile; external anatomy; Tetraodontiformes AB The smallest known specimen (20mm standard length: SL) of Triodon macropterus Lesson is described and illustrated. It is easily distinguished from superficially similar tetraodontid and diodontid larvae or early juveniles of comparable size by the following characters: separate premaxillae in conjunction with the fused dentaries; the presence of multicuspid spinoid scales; the jet-black mark in front of the soft dorsal fin; the developing pelvis, which is visible through the distended skin of the belly; and the presence of a number of procurrent caudal fin rays. The small Triodon differs from the adult in possessing a huge head that measures 45% SL (vs. 28.5-32.7% in adult), the absence of the characteristic dewlap with the conspicuous lateral ocellus, and the structure of the scales and nostrils. C1 Smithsonian Inst, Natl Museum Nat Hist, Div Fishes, Washington, DC 20560 USA. Nat Hist Museum, Dept Zool, London SW7 5BD, England. RP Johnson, GD (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Div Fishes, Washington, DC 20560 USA. EM johnsond@si.edu NR 11 TC 3 Z9 3 U1 0 U2 0 PU SPRINGER TOKYO PI TOKYO PA 3-3-13, HONGO, BUNKYO-KU, TOKYO, 113-0033, JAPAN SN 1341-8998 J9 ICHTHYOL RES JI Ichthyol. Res. PD MAY 25 PY 2005 VL 52 IS 2 BP 176 EP 181 DI 10.1007/s10228-005-0271-9 PG 6 WC Zoology SC Zoology GA 935RW UT WOS:000229802100008 ER PT J AU Anderson, WD Springer, VG AF Anderson, WD Springer, VG TI Review of the perciform fish genus Symphysanodon Bleeker (Symphysanodontidae), with descriptions of three new species, S-mona, S-parini, and S-rhax SO ZOOTAXA LA English DT Review DE Symphysanodontidae; Symphysanodon mona; new species; Symphysanodon parini; new species; Symphysanodon rhax; new species; key to Symphysanodon; review of Symphysanodon; Puerto Rico; Mona Passage; Sala y Gomez Ridge; Maldives ID GOMEZ SUBMARINE RIDGES; EASTERN PACIFIC; OCEAN; ATLANTIC; OUTPOST; REGION; SCALES; FAUNA; NAZCA AB Symphysanodon mona, a new species of perciform fish, is described from a single specimen collected in Mona Passage off the west coast of Puerto Rico. It differs from all other species of Symphysanodon in having fewer gillrakers on the first gill arch (4 or 5 + 19-21 = 24 or 25 total vs. 8-14 + 20-29 = 28-42 total) and, additionally, from the other two Atlantic species of the genus (S. berryi and S. octoactinus) in two other features of gill-arch morphology, viz., in having a ventral branch of the obliquus dorsalis 3 muscle (vs. its absence in the other two species) and in having a posteriorly projecting extension of the cartilaginous lateral end of ceratobranchial 4 (vs. its absence in the other two species; S. berryi has a small accessory cartilage associated with the lateral end of ceratobranchial 4 which may also be present in S. octoactinus). Symphysanodon parini, new species, known from 10 specimens collected over Sala y Gomez Ridge in the eastern South Pacific, can be distinguished from all other species of Symphysanodon, except S. maunaloae from the central and western Pacific, by the following combination of characters: segmented anal-fin rays 7, tubed lateral-line scales 45-50, total gillrakers on first gill arch 31 34 ( 9 or 10 + 22-24), sum of lateral-line scales and gillrakers on individual specimens 77-84, depth of body 22.5-24.7% SL (4.0-4.4 times in SL), length of depressed anal fin 24.8-26.4% SL, hypurals 1&2 autogenous, hypurals 3&4 represented by a single plate, and first caudal vertebra without parapophyses. It is distinguished from S. maunaloae by differences in mean numbers of tubed lateral-line scales (mean = 47.89 for S. parini vs. mean = 44.94 for S. maunaloae) and pectoral-fin rays (mean = 16.90 for S. parini vs. mean = 16.13 for S. maunaloae) and by differences in a few morphometric characters. Symphysanodon rhax, new species, known from specimens collected off the Maldive Islands, northern Indian Ocean, is separable from all other species of Symphysanodon, except S. berryi from the Atlantic, by the following combination of characters: segmented rays in the anal fin 7, tubed lateral-line scales 50, gillrakers on the first gill arch 35-38 (10 or 11 + 25-27), sum of lateral-line scales and gillrakers on individual specimens 85 - 88, depth of body 20.6-24.8% SL (4.0-4.9 times in SL), length of depressed anal fin 21.8-23.9% SL, hypurals 1&2 autogenous, hypurals 3&4 represented by a single plate, and first caudal vertebra without parapophyses. It can be distinguished from S. berryi by its shorter second anal-fin spine and a suite of other morphometric characters. A key to Symphysanodon and a review of the other species of the genus are also presented. C1 Coll Charleston, Grice Marine Biol Lab, Charleston, SC 29412 USA. Smithsonian Inst, Div Fishes, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Anderson, WD (reprint author), Coll Charleston, Grice Marine Biol Lab, 205 Ft Johnson, Charleston, SC 29412 USA. EM andersonwd@cofc.edu; springer.victor@nmnh.si.edu NR 67 TC 7 Z9 9 U1 1 U2 3 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41-383, AUCKLAND, 1030, NEW ZEALAND SN 1175-5334 J9 ZOOTAXA JI Zootaxa PD MAY 25 PY 2005 IS 996 BP 1 EP 44 PG 44 WC Zoology SC Zoology GA 929FQ UT WOS:000229327900001 ER PT J AU Brunken, S Behnke, M Thorwirth, S Yamada, KMT Giesen, T Lewen, F Hahn, J Winnewisser, G AF Brunken, S Behnke, M Thorwirth, S Yamada, KMT Giesen, T Lewen, F Hahn, J Winnewisser, G TI Asymmetric rotor analysis of DSOD spectra up to the (r)Q(3) branch near 653 GHz SO JOURNAL OF MOLECULAR STRUCTURE LA English DT Article DE oxadisulfane-d(2); high resolution spectroscopy; molecular spectroscopy ID GAS-PHASE DETECTION; HSOH AB We report the unequivocal identification of the (r)Q(3) branch of perdeutero oxadisulfane, DSOD, which has been produced in a discharge of D2S together with D2O. By employing the Cologne Terahertz Spectrometer, we have located the band center near 653 GHz, in very close agreement with earlier results deduced from the (r)Q(0) and (r)Q(2) branches. The A(0), B-0, and C-0 rotational constants have been determined by carrying out an asymmetric rotor least squares fit with all presently available data, including new R- and P-branch lines. Both, b- and c-type transitions have been observed and the relative dipole moment μ(c)/μ(b) has been determined from relative line strengths. All results agree very well with quantum chemically calculated values. © 2005 Elsevier B.V. All rights reserved. C1 Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. Univ Cologne, Inst Anorgan Chem, D-50937 Cologne, Germany. Harvard Univ, Dept Engn & Appl Sci, Cambridge, MA 02138 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. AIST, Tsukuba, Ibaraki 3058569, Japan. RP Giesen, T (reprint author), Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. EM giesen@ph1.uni-koeln.de RI Thorwirth, Sven/C-6217-2011; Brunken, Sandra/B-1880-2010; Giesen, Thomas /B-9476-2015 OI Thorwirth, Sven/0000-0001-8200-6710; Brunken, Sandra/0000-0001-7175-4828; Giesen, Thomas /0000-0002-2401-0049 NR 6 TC 10 Z9 10 U1 0 U2 1 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0022-2860 J9 J MOL STRUCT JI J. Mol. Struct. PD MAY 24 PY 2005 VL 742 IS 1-3 BP 237 EP 242 DI 10.1016/j.molstruc.2005.01.039 PG 6 WC Chemistry, Physical SC Chemistry GA 932AT UT WOS:000229527300027 ER PT J AU Cocroft, RB AF Cocroft, RB TI Vibrational communication facilitates cooperative foraging in a phloem-feeding insect SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE cooperation; chorusing; social behaviour; insect-plant interactions ID BEHAVIORAL ECOLOGY; SELFISH HERD; LARVAE; CURCULIONIDAE; HYMENOPTERA; PIPERACEAE; COLEOPTERA; DEFENSE; SIGNALS; PLANTS AB Insects are the dominante herbivores tropical forests, with a range of mechanisms exploiting plant resources. For group-living species, such mechanisms may involve communication. The Neotropical treehopper Calloconophora pinguis (Hemiptera: Membracidae) is a sap-feeding species in which groups of siblings feed on new leaves during the brief period of leaf expansion. Using an experimental approach, a process of cooperative foraging among siblings was documented, in which a few individuals in a group behave as scouts, locating a new feeding site and advertising it using plant-borne vibrational signals. Signalling leads to a period of positive feedback in which newly recruited individuals signal in concert with those already there. The food signalling system of C. pinguis is unique in its use of synchronized group displays and in the tight coordination of receiver responses with collective signals. Examples from a number of taxonomic groups show that vibrational communication can allow group-living insects to solve the challenges of feeding on plants, such as remaining in a foraging group or avoiding predation. While most research has focused on leaf-feeding species, sap-feeding species may remove just as much biomass. This study shows that cooperative vibrational communication underlies the ability of a sap-feeding species to exploit plant resources during a narrow window of availability. C1 Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. RP Cocroft, RB (reprint author), Univ Missouri, Div Biol Sci, Columbia, MO 65211 USA. EM cocroftr@missouri.edu NR 41 TC 24 Z9 25 U1 3 U2 11 PU ROYAL SOCIETY PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8452 J9 P ROY SOC B-BIOL SCI JI Proc. R. Soc. Lond. Ser. B-Biol. Sci. PD MAY 22 PY 2005 VL 272 IS 1567 BP 1023 EP 1029 DI 10.1098/rspb.2004.3041 PG 7 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 941GS UT WOS:000230203900006 PM 16024360 ER PT J AU Hendry, MA Smartt, SJ Maund, JR Pastorello, A Zampieri, L Benetti, S Turatto, M Cappellaro, E Meikle, WPS Kotak, R Irwin, MJ Jonker, PG Vermaas, L Peletier, RF van Woerden, H Exter, KM Pollacco, DL Leon, S Verley, S Benn, CR Pignata, G AF Hendry, MA Smartt, SJ Maund, JR Pastorello, A Zampieri, L Benetti, S Turatto, M Cappellaro, E Meikle, WPS Kotak, R Irwin, MJ Jonker, PG Vermaas, L Peletier, RF van Woerden, H Exter, KM Pollacco, DL Leon, S Verley, S Benn, CR Pignata, G TI A study of the Type II-P supernova 2003gd in M74 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars : evolution; supernovae : general; supernovae : individual : SN 2003gd; galaxies : distances and redshifts; galaxies : individual : M74 ID EXPANDING PHOTOSPHERE METHOD; PLATEAU SUPERNOVA; SPIRAL GALAXIES; CCD PHOTOMETRY; STELLAR PHOTOMETRY; HUBBLE CONSTANT; PROGENITOR STAR; DISTANCE SCALE; IA SUPERNOVAE; LIGHT CURVES AB We present photometric and spectroscopic data of the Type II-P supernova (SN II-P) 2003gd, which was discovered in M74 close to the end of its plateau phase. SN 2003gd is the first Type II supernova ( SN) to have a directly confirmed red supergiant ( RSG) progenitor. We compare SN 2003gd to SN 1999 em, a similar SN II-P, and estimate an explosion date of 2003 March 18. We determine a reddening towards the SN of E(B-V) = 0.14 +/- 0.06, using three different methods. We also calculate three new distances to M74 of 9.6 +/- 2.8, 7.7 +/- 1.7 and 9.6 +/- 2.2 Mpc. The former was estimated using the standard candle method (SCM), for Type II supernovae (SNe II), and the latter two using the brightest supergiants method (BSM). When combined with existing kinematic and BSM distance estimates, we derive a mean value of 9.3 +/- 1.8 Mpc. SN 2003gd was found to have a lower tail luminosity compared with other normal Type II-P supernovae ( SNe II-P) bringing into question the nature of this SN. We present a discussion concluding that this is a normal SN II-P, which is consistent with the observed progenitor mass of 8(-2)(+4) M-circle dot. C1 Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. Queens Univ Belfast, Dept Phys & Astron, Belfast BT7 1NN, Antrim, North Ireland. Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy. Osserv Astron Padova, INAF, I-35122 Padua, Italy. Osserv Astron Capodimonte, INAF, I-80131 Naples, Italy. Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2BZ, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Groningen, Kapteyn Inst, NL-9700 AV Groningen, Netherlands. Inst Astrofis Canarias, E-38200 San Cristobal la Laguna, Tenerife, Spain. Queens Univ Belfast, Sch Pure & Appl Phys, Belfast BT7 9NN, Antrim, North Ireland. CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain. Isaac Newton Grp, E-38700 Santa Cruz De La Palma, Spain. ESO, D-85748 Garching, Germany. RP Hendry, MA (reprint author), Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. EM mah@ast.cam.ac.uk RI Peletier, Reynier/B-9633-2012; OI Benetti, Stefano/0000-0002-3256-0016; Turatto, Massimo/0000-0002-9719-3157; Kotak, Rubina/0000-0001-5455-3653; Zampieri, Luca/0000-0002-6516-1329; Maund, Justyn/0000-0003-0733-7215 NR 67 TC 75 Z9 75 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 MAY 21 PY 2005 VL 359 IS 3 BP 906 EP 926 DI 10.1111/j.1365-2966.2005.08928.x PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 924XY UT WOS:000229015700010 ER PT J AU Rebusco, P Churazov, E Bohringer, H Forman, W AF Rebusco, P Churazov, E Bohringer, H Forman, W TI Impact of stochastic gas motions on galaxy cluster abundance profiles SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE cooling flows; galaxies : clusters : general; galaxies : clusters : individual : Perseus ID XMM-NEWTON OBSERVATIONS; X-RAY-CLUSTERS; PERSEUS CLUSTER; INTRACLUSTER MEDIUM; ELLIPTIC GALAXIES; COOLING FLOWS; VIRGO CLUSTER; METALLICITY GRADIENTS; THERMAL CONDUCTION; NEARBY CLUSTERS AB The impact of stochastic gas motions on the metal distribution in cluster cores is evaluated. Peaked abundance profiles are a characteristic feature of clusters with cool cores, and abundance peaks are probably associated with the brightest cluster galaxies (BCGs), which dwell in cluster cores. However, the width of the abundance peaks is significantly broader than the BCG light distribution, suggesting that some gas motions are transporting metals originating from within the BCG. Assuming that this process can be treated as diffusive, and using the brightest X-ray cluster A426 (Perseus) as an example, we estimate that a diffusion coefficient of the order of 2 x 10(29) cm(2) s(-1) is needed to explain the width of the observed abundance profiles. Much lower (higher) diffusion coefficients would result in too peaked (too shallow) profiles. Such diffusion could be produced by stochastic gas motions, and our analysis provides constraints on the product of their characteristic velocity and their spatial coherence scale. We speculate that the activity of the supermassive black hole of the BCG is driving the stochastic gas motions in cluster cores. When combined with the assumption that the dissipation of the same motions is a key gas heating mechanism, one can estimate both the velocity and the spatial scale of such diffusive processes. C1 Max Planck Inst Astrophys, D-85741 Garching, Germany. Space Res Inst IKI, Moscow 117810, Russia. Max Planck Inst Extraterr Phys, D-85740 Garching, Germany. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Rebusco, P (reprint author), Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85741 Garching, Germany. EM pao@mpa-garching.mpg.de RI Churazov, Eugene/A-7783-2013; OI Forman, William/0000-0002-9478-1682 NR 52 TC 88 Z9 88 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 MAY 21 PY 2005 VL 359 IS 3 BP 1041 EP 1048 DI 10.1111/j.1365-2966.2005.08965.x PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 924XY UT WOS:000229015700022 ER PT J AU Wyithe, JSB Loeb, A AF Wyithe, JSB Loeb, A TI Undetected sources allow transmission of the Ly alpha line from galaxies prior to reionization SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : theory; galaxies : formation ID INTERGALACTIC MEDIUM; EMISSION-LINES; HIGH-REDSHIFT; UNIVERSE; QUASARS; DISCOVERY; ABSORPTION; EMITTERS; HYDROGEN; HISTORY AB The discovery of Ly alpha emission from galaxies at redshifts beyond z similar to 6: 5 should not be naively interpreted as implying that the intergalactic medium ( IGM) had been reionized at higher redshifts. We show that a cluster of faint undetected sources around each observed galaxy can increase the volume of the galaxy's H (II) region by an order of magnitude. As a result, we find that the H (II) regions around massive galaxies would have been large enough to allow transmission of the galaxy's Ly alpha line prior to reionization. We also show that quasars may contribute a significant fraction of the ionizing photons to H (II) regions around galaxies with a velocity dispersion larger than similar to 100 km s(-1). These contributing quasars are not usually seen because of the small fraction of time they spend in a luminous phase. C1 Univ Melbourne, Parkville, Vic 3010, Australia. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Univ Melbourne, Parkville, Vic 3010, Australia. EM swyithe@isis.ph.unimelb.edu.au; aloeb@cfa.harvard.edu NR 36 TC 44 Z9 44 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 MAY 20 PY 2005 VL 625 IS 1 BP 1 EP 5 PN 1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 925IK UT WOS:000229046600001 ER PT J AU Krivonos, R Vikhlinin, A Churazov, E Lutovinov, A Molkov, S Sunyaev, R AF Krivonos, R Vikhlinin, A Churazov, E Lutovinov, A Molkov, S Sunyaev, R TI Extragalactic source counts in the 20-50 kev energy band from the deep observation of the coma region by INTEGRAL IBIS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : Seyfert; X-rays : diffuse background; X-rays : general ID X-RAY SOURCES; CATALOG; CHANDRA; TELESCOPES; NGC-4151; HEAO-1; IMAGER AB We present the analysis of serendipitous sources in a deep, 500 ks, hard X-ray observation of the Coma Cluster region with the IBIS instrument on board INTEGRAL. In addition to the Coma Cluster, the final 20-50 keV image contains 12 serendipitous sources with statistical significance > 4 sigma. We use these data (after correcting for expected number of false detections) to extend the extragalactic source counts in the 20-50 keV energy band down to a limiting flux of 1: 0; 10(-1)1 ergs s(-1) cm(-2) (similar or equal to 1 mcrab). This is a more than a factor of 10 improvement in sensitivity compared to the previous results in this energy band obtained with the HEAO 1 A-4 instrument. The derived source counts are consistent with the Euclidean relation N(> f) infinity f(--3/2). A large fraction of identified serendipitous sources are low-redshift, z < 0: 02, active galactic nuclei (AGNs), mostly of Seyfert 1 type. The surface density of hard X-ray sources is ( 1: 4 +/- 0: 5); 10(-2) deg(-2) above a flux threshold of 10(-11) ergs s(-1) cm(-2). These sources directly account for similar to 3% of the cosmic X-ray background in the 20-50 keV energy band. Given the low redshift depth of our sample, we expect that similar sources at higher redshifts account for a significant fraction of the hard X-ray background. Our field covers only 3% of the sky; a systematic analysis of other extragalactic INTEGRAL observations can produce much larger source samples and is, therefore, critically important. C1 Russian Acad Sci, Inst Space Res, Moscow 117997, Russia. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Max Planck Inst Astrophys, D-85741 Garching, Germany. RP Russian Acad Sci, Inst Space Res, 84-32 Profsojuznaya St,GSP7, Moscow 117997, Russia. EM krivonos@hea.iki.rssi.ru RI Churazov, Eugene/A-7783-2013 NR 29 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 MAY 20 PY 2005 VL 625 IS 1 BP 89 EP 94 DI 10.1086/429657 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 925IK UT WOS:000229046600009 ER PT J AU Kulesa, CA Hungerford, AL Walker, CK Zhang, XL Lane, AP AF Kulesa, CA Hungerford, AL Walker, CK Zhang, XL Lane, AP TI Large-scale CO and [C-I] emission in the p Ophiuchi molecular cloud SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : atoms; ISM : clouds; ISM : individual (p Ophiuchi); ISM : molecules; radio lines : ISM ID FINE-STRUCTURE TRANSITIONS; CLUMPY PHOTODISSOCIATION REGIONS; DARK CLOUD; STAR-FORMATION; INTERSTELLAR CLOUDS; WATER ABUNDANCE; LINE EMISSION; ATOMIC CARBON; RHO OPH; SUBMILLIMETER AB We present a comprehensive study of the rho Ophiuchi molecular cloud that addresses aspects of the physical structure and condition of the molecular cloud and its photodissociation region ( PDR) by combining far- infrared and submillimeter- wave observations with a wide range of angular scale and resolution. We present 1600 arcmin(2) maps ( 2.3 pc(2)) with 0.1 pc resolution in submillimeter CO ( 4 -> 3) and [ C (I)] ( P-3(1) -> P-3(0)) line emission from the Antarctic Submillimeter Telescope and Remote Observatory ( AST/ RO) and pointed observations in the CO ( 7 -> 6) and [ C (I)] ( P-3(2)-> P-3(1)) lines. Within the large- scale maps, smaller spectral line maps of 3000 AU resolution over similar to 90 arcmin(2) ( 0.2 pc(2)) of the cloud in CO, CS, HCO+, and their rare isotopomers are made at the Heinrich Hertz Telescope ( HHT) in Arizona. Comparison of CO, HCO+, and [ C (I)] maps with far- infrared observations of atomic and ionic species from the Infrared Space Observatory ( ISO) far- infrared and submillimeter continuum emission and near- infrared H-2 emission allows clearer determination of the physical and chemical structure of the rho Oph PDR, since each species probes a different physical region of the cloud structure. Although a homogeneous plane- parallel PDR model can reproduce many of the observations described here, the excitation conditions needed to produce the observed HCO+ and [O (I)] emission imply inhomogeneous structure. Strong chemical gradients are observed in HCO+ and CS; the former is ascribed to a local enhancement in the H2 ionization rate, and the latter is principally due to shocks. Under the assumption of a simple two- component gas model for the cloud, we find that [ C (II)] and [ C-I] emission predominantly arises from the lower density envelopes ( 10(3) - 10(4) cm (-3)) that surround denser cloud condensations, or `` clumps.'' The distribution of [ C (I)] is very similar to that of (CO)-O-18 and is generally consistent with illumination from the `` far'' side of the cloud. A notable exception is found at the western edge of the cloud, where UV photons create a PDR viewed `` edge- on.'' The abundance of atomic carbon is accurately modeled using a radiation field that decreases with increasing projected distance from the exciting star HD 147889 and a total gas column density that follows that of C18O, decreasing toward the edges of the cloud. In contrast to the conclusions of other studies, we find that no nonequilibrium chemistry is needed to enhance the [ C (I)] abundance. Each spectral line is traced to a particular physical component of the cloud and PDR. Although CO rotational line emission originates from both dense condensations and diffuse envelopes, the millimeter- wave transitions mostly find their origins in envelope material, whereas the high- J submillimeter lines stem more from the dense clumps. Submillimeter HCO+ and infrared [ O (I)] and [ C (II)] emission indicate clump surface temperatures of 50 - 200 K, an ultraviolet radiation field with I-UV approximate to 10-90, densities of 10(5) - 10(6) cm(-3), and interior temperatures of <= 20 K. This study highlights the value of large- scale infrared and submillimeter mapping for the interpretation of molecular cloud pysical and chemical structure, and important future observations are highlighted. C1 Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. EM ckulesa@as.arizona.edu; aimee@as.arizona.edu; cwalker@as.arizona.edu; zhang@rosette.gsfc.nasa.gov; adair@cfa.harvard.edu NR 64 TC 26 Z9 26 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 MAY 20 PY 2005 VL 625 IS 1 BP 194 EP 209 DI 10.1086/426096 PN 1 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 925IK UT WOS:000229046600018 ER PT J AU Desai, P Brickhouse, NS Drake, JJ Dupree, AK Edgar, RJ Hoogerwerf, R Kashyap, V Wargelin, BJ Smith, RK Huenemoerder, DP Liedahl, DA AF Desai, P Brickhouse, NS Drake, JJ Dupree, AK Edgar, RJ Hoogerwerf, R Kashyap, V Wargelin, BJ Smith, RK Huenemoerder, DP Liedahl, DA TI An assessment of the Fe XVIII and Fe XIX line ratios from the Chandra grating observations of Capella SO ASTROPHYSICAL JOURNAL LA English DT Article DE atomic data; atomic processes; stars : individual ( Capella); ultraviolet : stars; X-rays : stars ID FLUORINE-LIKE IONS; L-SHELL IONS; LABORATORY MEASUREMENTS; EXTREME-ULTRAVIOLET; ATOMIC DATABASE; EMISSION-LINES; XMM-NEWTON; IRON; ABUNDANCES; SPECTROMETER AB Observations of Fe XVIII and Fe XIX X-ray, extreme-UV, and far-UV line emission, formed at the peak of Capella's (α Aurigae's) emission measure distribution and ubiquitous in spectra of many cool stars and galaxies, provide a unique opportunity to test the robustness of Fe XVIII and Fe XIX spectral models. The Astrophysical Plasma Emission Code (APEC) is used to identify over 35 lines from these two ions alone, and to compare model predictions with spectra obtained with the Chandra Low Energy Transmission Grating and High Energy Transmission Grating Spectrometers, the Far Ultraviolet Spectroscopic Explorer (FUSE), and the Extreme Ultraviolet Explorer. Some flux discrepancies larger than a factor of 2 are found between observations of Fe XVIII and Fe XIX lines and predictions by APEC and other models in common use. In particular, the X-ray resonance lines for both ions are stronger than predicted by all models relative to the EUV resonance lines. The multi-wavelength observations demonstrate the importance of including dielectronic recombination and proton-impact excitation, and of using accurate wavelengths in spectral codes. These ions provide important diagnostic tools for 10(7) K plasmas currently observed with Chandra, XMM-Newton, and FUSE. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA. Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. MIT, Space Res Ctr, Cambridge, MA 02139 USA. Lawrence Livermore Natl Lab, Livermore, CA 94551 USA. RP Desai, P (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM pdesai@cfa.harvard.edu OI Brickhouse, Nancy/0000-0002-8704-4473 NR 30 TC 25 Z9 25 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 MAY 20 PY 2005 VL 625 IS 1 BP L59 EP L62 DI 10.1086/430882 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 925IQ UT WOS:000229047200015 ER PT J AU Nulsen, PEJ Hambrick, DC McNamara, BR Rafferty, D Birzan, L Wise, MW David, LP AF Nulsen, PEJ Hambrick, DC McNamara, BR Rafferty, D Birzan, L Wise, MW David, LP TI The powerful outburst in hercules A SO ASTROPHYSICAL JOURNAL LA English DT Article DE cooling flows; galaxies : clusters : individual ( Hercules A); intergalactic medium; X-rays : galaxies : clusters ID X-RAY CAVITIES; COOLING FLOWS; RADIO-SOURCES; GALAXIES; CLUSTERS; MULTIBAND; MODELS; GAS AB The radio source Hercules A resides at the center of a cooling flow cluster of galaxies at redshift z = 0.154. A Chandra X-ray image reveals a shock front in the intracluster medium (ICM) surrounding the radio source, about 160 kpc from the active galactic nucleus (AGN) that hosts it. The shock has a Mach number of 1.65, making it the strongest of the cluster-scale shocks driven by an AGN outburst found so far. The age of the outburst is &SIME; 5.9 x 10(7) yr, its energy &SIM; 3 x 10(61) ergs, and its mean power &SIM; 1.6 x 10(46) ergs s(-1). As for the other large AGN outbursts in cooling flow clusters, this outburst overwhelms radiative losses from the ICM of the Hercules A Cluster by a factor of &SIM; 100. It adds to the case that AGN outbursts are a significant source of preheating for the ICM. Unless the mechanical efficiency of the AGN in Hercules A exceeds 10%, the central black hole must have grown by more than 1.7 x 10(8) M-&ODOT; to power this one outburst. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Harvey Mudd Coll, Claremont, CA 91711 USA. Ohio Univ, Inst Astrophys, Athens, OH 45701 USA. Ohio Univ, Dept Phys & Astron, Clippinger Labs, Athens, OH 45701 USA. MIT, Ctr Space Res, Cambridge, MA 02139 USA. RP Nulsen, PEJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM pnulsen@cfa.harvard.edu NR 26 TC 95 Z9 95 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 MAY 20 PY 2005 VL 625 IS 1 BP L9 EP L12 DI 10.1086/430945 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 925IQ UT WOS:000229047200003 ER PT J AU Sanz, ME McCarthy, MC Thaddeus, P AF Sanz, ME McCarthy, MC Thaddeus, P TI Vibrational excitation and relaxation of five polyatomic molecules in an electrical discharge SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID TRANSFORM MICROWAVE SPECTROSCOPY; MILLIMETER-WAVE SPECTRUM; SEEDED SUPERSONIC BEAMS; TRICARBON OXIDE SULFIDE; AB-INITIO THEORY; EXCITED-STATES; INFRARED-SPECTRUM; CARBON CHAINS; ISOTOPIC-SUBSTITUTION; ENERGY TRANSFER AB Vibrational excitation and relaxation of five linear polyatomic molecules, OCS, OC3S, HC3N, HC5N, and SiC2S, have been studied by Fourier transform microwave spectroscopy in a supersonic expansion after the application of a low-current dc electric discharge. For each chain, the populations in bending and stretching modes have been characterized as a function of the applied discharge current; for stable OCS and HC3N, vibrational populations were studied as well in the absence of a discharge. With no discharge present the derived vibrational temperatures are slightly below T, the temperature of the gas before the supersonic expansion (i.e., 300 K). In the presence of the discharge, vibrational excitation occurs via inelastic collisions with the electrons and the vibrational temperatures rise as the applied current increases. Global vibrational relaxation is governed by rapid vibration-vibration (VV) energy transfer and slow vibration-translation (VT) energy transfer. The latter process is rate-determining and depends primarily on the wave number of the vibration. Vibrational modes with wave numbers near and below kT/hc (where T=300 K and kT/hc similar to 210 cm(-1)) are efficiently cooled by VT transfer because a sufficient number of collisions occur in the initial stages of the supersonic expansion. Vibrational modes with wave numbers around 450 cm(-1) appear to be inefficiently cooled in the molecular beam; at these energies VV and VT rates are probably comparable. For high-frequency vibrations, VV energy transfer dominates. For the longer chains:OC3S and HC5N, higher-lying modes are generally not detectable and vibrational temperatures of most lower-lying modes were found to be lower than those of OCS and HC3N, suggesting that as the size of the molecules increases, intermode VV transfer becomes more efficient, plausibly due to the higher density of vibrational levels. New high resolution spectroscopic data have been obtained for several vibrationally excited states of OC3S, HC3N, and HC5N. Rotational lines of the C-13 and N-15 isotopic species of HC5N have been measured, yielding improved rotational and centrifugal distortion constants; N-14 nitrogen quadrupole coupling constants for the isotopic species of HC5N with C-13 have been determined for the first time. (c) 2005 American Institute of Physics. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Harvard Univ, Div Engn & Appl Sci, Cambridge, MA 02138 USA. RP Sanz, ME (reprint author), Univ Valladolid, Fac Ciencias, Dept Quim Fis & Quim Inorgan, Prado Magdalena,S-N, E-47005 Valladolid, Spain. EM msanz@cfa.harvard.edu RI Sanz, Maria Eugenia/F-7054-2013; OI McCarthy, Michael/0000-0001-9142-0008 NR 42 TC 20 Z9 20 U1 1 U2 10 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0021-9606 J9 J CHEM PHYS JI J. Chem. Phys. PD MAY 15 PY 2005 VL 122 IS 19 AR 194319 DI 10.1063/1.1869988 PG 10 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 934XS UT WOS:000229743500031 PM 16161585 ER PT J AU Riley, S AF Riley, S TI Better than chocolate SO LIBRARY JOURNAL LA English DT Book Review C1 Smithsonian Inst, Libs, Washington, DC 20560 USA. RP Riley, S (reprint author), Smithsonian Inst, Libs, Washington, DC 20560 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 MAY 15 PY 2005 VL 130 IS 9 BP 109 EP 109 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 925ZE UT WOS:000229091500061 ER PT J AU Haygarth, PM Condron, LM Heathwaite, AL Turner, BL Harris, GP AF Haygarth, PM Condron, LM Heathwaite, AL Turner, BL Harris, GP TI The phosphorus transfer continuum: Linking source to impact with an interdisciplinary and multi-scaled approach SO SCIENCE OF THE TOTAL ENVIRONMENT LA English DT Article DE phosphorus; source; mobilisation; detachment; solubilisation; incidental; delivery; impact; eutrophication ID WATER-QUALITY; NUTRIENT CONCENTRATIONS; AGRICULTURAL LAND; RIVER WATERS; SOIL; DYNAMICS; CATCHMENTS; GRASSLAND; PATTERNS; EROSION AB This critical review introduces a template that links phosphorus (P) sources and mobilisation processes to the delivery of P to receiving waters where deleterious impact is of concern. It therefore serves as a key introductory paper in this special issue. The entire process is described in terms of a 'P transfer continuum' to emphasise the interdisciplinary and inter-scale nature of the problem. Most knowledge to date is derived from mechanistic studies on the sources and mobilisation of P using controlled experiments that have formed the basis for mitigation strategies aimed at minimising transfer from agricultural fields. However, our ability to extrapolate this information to larger scales is limited by a poor knowledge base while new conceptual advances in the areas of complex systems and fractal dynamics indicate the limitations of past theoretical frameworks. This is compounded by the conceptual and physical separation of scientists working at different scales within the terrestrial and aquatic sciences. Multi-scaled approaches are urgently required to integrate different disciplines and provide a platform to develop mechanistic modelling frameworks, collect new data and identify critical research questions. (c) 2005 Elsevier B.V All rights reserved. C1 Inst Grassland & Environm Res, Soil Sci & Environm Qual Team, N Wyke Res Stn, Okehampton EX20 2SB, Devon, England. Lincoln Univ, Canterbury 8150, New Zealand. Univ Lancaster, Lancaster Environm Ctr, Ctr Sustainable Water Management, Lancaster LA1 4YQ, England. Smithsonian Trop Res Inst, Ancon, Panama. Univ Tasmania, Sandy Bay, Tas, Australia. RP Haygarth, PM (reprint author), Inst Grassland & Environm Res, Soil Sci & Environm Qual Team, N Wyke Res Stn, Okehampton EX20 2SB, Devon, England. EM phil.haygarth@bbsrc.ac.uk RI Turner, Benjamin/E-5940-2011; Condron, Leo/E-9458-2013; Haygarth, Philip/F-6790-2014; Ross, Donald/F-7607-2012; OI Turner, Benjamin/0000-0002-6585-0722; Ross, Donald/0000-0002-8659-3833; Heathwaite, Ann Louise/0000-0001-8791-0039 NR 69 TC 123 Z9 134 U1 11 U2 82 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0048-9697 J9 SCI TOTAL ENVIRON JI Sci. Total Environ. PD MAY 15 PY 2005 VL 344 IS 1-3 BP 5 EP 14 DI 10.1016/j.scitotenv.2005.02.001 PG 10 WC Environmental Sciences SC Environmental Sciences & Ecology GA 938QY UT WOS:000230019100002 PM 15907506 ER PT J AU Turner, BL Haygarth, PM AF Turner, BL Haygarth, PM TI Phosphatase activity in temperate pasture soils: Potential regulation of labile organic phosphorus turnover by phosphodiesterase activity SO SCIENCE OF THE TOTAL ENVIRONMENT LA English DT Article DE pasture; soil; phosphatase; phosphomonoestemse; phosphodiesterase; organic phosphorus ID MYCORRHIZAL-P SOURCES; MICROBIAL BIOMASS; NITROGEN DEPOSITION; EXTRACTION; GRASSLAND; FOREST AB Phosphatase enzymes regulate organic phosphorus (P) turnover in soil, but a clear understanding remains elusive. To investigate this, phosphomonoesterase and phosphodiesterase activities were determined by using para-nitrophenol (pNP) analogue substrates in a range of temperate pasture soils from England and Wales. Substrate-induced phosphatase activity ranged between 2.62 and 12.19 mu mol pNP g(-1) soil h(-1) for phosphomonoesterase and between 0.25 and 2.24 mu mol pNP g(-1) soil h-1 for phosphodiesterase. Activities were correlated strongly with soil pH and labile organic P extracted in sodium bicarbonate, although the relationships differed markedly for the two enzymes. Acidic soils contained high phosphomonoesterase activity, low phosphodiesterase activity, and high concentrations of labile organic P, whereas the reverse was true in more neutral soils. As most of the organic P inputs to soil are phosphate diesters, it therefore seems likely that phosphodiesterase activity regulates labile organic P turnover in pasture soils. The low phosphodiesterase activity in acidic soils may be linked to the dominance of fungi or an effect of sorption on the enzyme. These results suggest that greater emphasis should be placed on understanding the role of phosphodiesterase activity in the cycling of soil organic P. (c) 2005 Elsevier B.V. All rights reserved. C1 IGER, N Wyke Res Stn, Okehampton EX20 2SB, Devon, England. RP Turner, BL (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Ancon, Panama. EM turnerbl@si.edu RI Turner, Benjamin/E-5940-2011; Haygarth, Philip/F-6790-2014 OI Turner, Benjamin/0000-0002-6585-0722; NR 41 TC 58 Z9 68 U1 6 U2 41 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0048-9697 J9 SCI TOTAL ENVIRON JI Sci. Total Environ. PD MAY 15 PY 2005 VL 344 IS 1-3 BP 27 EP 36 DI 10.1016/j.scitotenv.2005.02.003 PG 10 WC Environmental Sciences SC Environmental Sciences & Ecology GA 938QY UT WOS:000230019100004 PM 15907508 ER PT J AU Andre, A Eisaman, MD Walsworth, RL Zibrov, AS Lukin, MD AF Andre, A Eisaman, MD Walsworth, RL Zibrov, AS Lukin, MD TI Quantum control of light using electromagnetically induced transparency SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS LA English DT Article ID ATOMIC ENSEMBLES; NONLINEAR OPTICS; SINGLE PHOTONS; GROUP-VELOCITY; STATE TRANSFER; COMMUNICATION; PULSES; VAPOR; ENTANGLEMENT; GENERATION AB We present an overview of recent theoretical and experimental work on the control of the propagation and quantum properties of light using electromagnetically induced transparency in atomic ensembles. Specifically, we discuss techniques for the generation and storage of few-photon quantum-mechanical states of light as well as novel approaches to manipulate weak pulses of light via enhanced nonlinear optical processes. C1 Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. Harvard Univ, Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. PN Lebedev Phys Inst, Moscow 117924, Russia. RP Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. RI Eisaman, Matthew/E-8006-2011; Zibrov, Alexander/G-7419-2014 OI Eisaman, Matthew/0000-0002-3814-6430; NR 55 TC 32 Z9 32 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0953-4075 EI 1361-6455 J9 J PHYS B-AT MOL OPT JI J. Phys. B-At. Mol. Opt. Phys. PD MAY 14 PY 2005 VL 38 IS 9 SI SI BP S589 EP S604 DI 10.1088/0953-4075/38/9/010 PG 16 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 930EY UT WOS:000229399800011 ER PT J AU Petrov, DS Salomon, C Shlyapnikov, GV AF Petrov, DS Salomon, C Shlyapnikov, GV TI Diatomic molecules in ultracold Fermi gases - novel composite bosons SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS LA English DT Article ID BOSE-EINSTEIN CONDENSATION; SHORT-RANGE FORCES; INTERACTING PARTICLES; SUPERCONDUCTIVITY; COLLISIONS; ATOMS; SCATTERING; NEUTRONS; STATE AB We give a brief overview of recent studies of weakly bound homonuclear molecules in ultracold two-component Fermi gases. It is emphasized that they represent novel composite bosons, which exhibit features of Fermi statistics at short intermolecular distances. In particular, the Pauli exclusion principle for identical fermionic atoms provides a strong suppression of collisional relaxation of such molecules into deep bound states. We then analyse heteronuclear molecules which are expected to be formed in mixtures of different fermionic atoms. We show how an increase in the mass ratio for the constituent atoms changes the physics of collisional stability of such molecules compared to homonuclear ones. We discuss Bose-Einstein condensation of these composite bosons and consider prospects for future studies. C1 Harvard Univ, Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. Harvard Univ, MIT, Ctr Ultracolds Atoms, Dept Phys, Cambridge, MA 02138 USA. Lab Kastler Brossel, F-75231 Paris, France. Univ Paris 11, Lab Phys Theor & Modeles Stat, F-91405 Orsay, France. Univ Amsterdam, Van Waals Zeeman Inst, NL-1018 XE Amsterdam, Netherlands. RP Petrov, DS (reprint author), Harvard Univ, Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. NR 76 TC 63 Z9 63 U1 0 U2 4 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 MAY 14 PY 2005 VL 38 IS 9 SI SI BP S645 EP S660 DI 10.1088/0953-4075/38/9/014 PG 16 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 930EY UT WOS:000229399800015 ER PT J AU Blake, CH Bloom, JS Starr, DL Falco, EE Skrutskie, M Fenimore, EE Duchene, G Szentgyorgyi, A Hornstein, S Prochaska, JX McCabe, C Ghez, A Konopacky, Q Stapelfeldt, K Hurley, K Campbell, R Kassis, M Chaffee, F Gehrels, N Barthelmy, S Cummings, JR Hullinger, D Krimm, HA Markwardt, CB Palmer, D Parsons, A McLean, K Tueller, J AF Blake, CH Bloom, JS Starr, DL Falco, EE Skrutskie, M Fenimore, EE Duchene, G Szentgyorgyi, A Hornstein, S Prochaska, JX McCabe, C Ghez, A Konopacky, Q Stapelfeldt, K Hurley, K Campbell, R Kassis, M Chaffee, F Gehrels, N Barthelmy, S Cummings, JR Hullinger, D Krimm, HA Markwardt, CB Palmer, D Parsons, A McLean, K Tueller, J TI An infrared flash contemporaneous with the gamma-rays of GRB 041219a SO NATURE LA English DT Article ID EARLY OPTICAL-EMISSION; EARLY AFTERGLOW; BURST; RADIATION; GRB-021211; MISSION AB The explosion that results in a cosmic gamma-ray burst (GRB) is thought to produce emission from two physical processes: the central engine gives rise to the high-energy emission of the burst through internal shocking(1), and the subsequent interaction of the flow with the external environment produces long-wavelength afterglows(2-4). Although observations of afterglows(5) continue to refine our understanding of GRB progenitors and relativistic shocks, gamma-ray observations alone have not yielded a clear picture of the origin of the prompt emission(6) nor details of the central engine. Only one concurrent visible-light transient has been found(7) and it was associated with emission from an external shock. Here we report the discovery of infrared emission contemporaneous with a GRB, beginning 7.2 minutes after the onset of GRB 041219a ( ref. 8). We acquired 21 images during the active phase of the burst, yielding early multi-colour observations. Our analysis of the initial infrared pulse suggests an origin consistent with internal shocks. C1 Harvard Univ, Coll Observ, Cambridge, MA 02138 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Santa Cruz, CA 95064 USA. Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. WM Keck Observ, Kamuela, HI 96743 USA. Los Alamos Natl Lab, Los Alamos, NM 87545 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. Univ Calif Los Angeles, Los Angeles, CA 90095 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Observ Grenoble, Astrophys Lab, F-38041 Grenoble, France. Gemini Observ, Hilo, HI 96720 USA. Univ Maryland, College Pk, MD 20742 USA. Univ Space Res Assoc, Columbia, MD 21044 USA. RP Bloom, JS (reprint author), Harvard Univ, Coll Observ, Cambridge, MA 02138 USA. EM jbloom@astro.berkeley.edu RI Barthelmy, Scott/D-2943-2012; Gehrels, Neil/D-2971-2012; Tueller, Jack/D-5334-2012; Stapelfeldt, Karl/D-2721-2012; Parsons, Ann/I-6604-2012 NR 30 TC 92 Z9 94 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 MAY 12 PY 2005 VL 435 IS 7039 BP 181 EP 184 DI 10.1038/nature03520 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 924ZO UT WOS:000229021100033 PM 15889085 ER PT J AU Smith, GP Kneib, JP Smail, I Mazzotta, P Ebeling, H Czoske, O AF Smith, GP Kneib, JP Smail, I Mazzotta, P Ebeling, H Czoske, O TI A Hubble Space Telescope lensing survey of X-ray luminous galaxy clusters - IV. Mass, structure and thermodynamics of cluster cores at z=0.2 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Review DE gravitational lensing; galaxies : clusters : general; cosmology : observations; dark matter; large scale structure of Universe; X-rays : galaxies : clusters ID FLUX-LIMITED SAMPLE; COLD DARK-MATTER; ALL-SKY SURVEY; FIELD SPECTROSCOPIC SURVEY; REDSHIFT SURVEY; RICH CLUSTERS; COOLING FLOWS; T RELATION; COSMOLOGICAL CONSTRAINTS; TEMPERATURE RELATION AB We present a comprehensive space-based study of 10 X-ray luminous galaxy clusters (L-X >= 8 x 10(44) erg s(-1), 0.1 - 2.4 keV) at z = 0.2. Hubble Space Telescope (HST) observations reveal numerous gravitationally lensed arcs for which we present four new spectroscopic redshifts, bringing the total to 13 confirmed arcs in this cluster sample. The confirmed arcs reside in just half of the clusters; we thus obtain a firm lower limit on the fraction of clusters with a central projected mass density exceeding the critical density required for strong lensing of 50 per cent. We combine the multiple-image systems with the weakly sheared background galaxies to model the total mass distribution in the cluster cores ( R <= 500 kpc). These models are complemented by high-resolution X-ray data from Chandra and used to develop quantitative criteria to classify the clusters as relaxed or unrelaxed. Formally, ( 30 +/- 20) per cent of the clusters form a relatively homogeneous subsample of relaxed clusters; the remaining ( 70 +/- 20) per cent are unrelaxed and are a much more diverse population. Most of the clusters therefore appear to be experiencing a cluster - cluster merger or relaxing after such an event. We also study the normalization and scatter of scaling relations between the cluster mass, the X-ray luminosity and the temperature. The scatter in these relations is dominated by the unrelaxed clusters and is typically sigma similar or equal to 0.4. Most notably, we detect two to three times more scatter in the mass - temperature relation than theoretical simulations and models predict. The observed scatter is also asymmetric - the unrelaxed clusters are systematically 40 per cent hotter than the relaxed clusters at 2.5 sigma significance. This structural segregation should be a major concern for experiments designed to constrain cosmological parameters using galaxy clusters. Overall our results are consistent with a scenario of cluster - cluster merger-induced boosts to cluster X-ray luminosities and temperatures. C1 CALTECH, Pasadena, CA 91125 USA. Univ Durham, Dept Phys, Durham DH1 3LE, England. Observ Midi Pyrenees, F-31400 Toulouse, France. Univ Durham, Inst Computat Cosmol, Durham DH1 3LE, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. Univ Bonn, Inst Astrophys & Extraterr Forsch, D-53121 Bonn, Germany. RP Smith, GP (reprint author), CALTECH, Mail Code 105-24, Pasadena, CA 91125 USA. EM gps@astro.caltech.edu RI Smail, Ian/M-5161-2013; Kneib, Jean-Paul/A-7919-2015; Mazzotta, Pasquale/B-1225-2016 OI Smail, Ian/0000-0003-3037-257X; Kneib, Jean-Paul/0000-0002-4616-4989; Mazzotta, Pasquale/0000-0002-5411-1748 NR 141 TC 195 Z9 195 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 MAY 11 PY 2005 VL 359 IS 2 BP 417 EP 446 DI 10.1111/j.1365-2966.2005.08911.x PG 30 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 921DY UT WOS:000228745600003 ER PT J AU Moore, TJT Lumsden, SL Ridge, NA Puxley, PJ AF Moore, TJT Lumsden, SL Ridge, NA Puxley, PJ TI The near-infrared extinction law in regions of high A(V) SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE dust, extinction; HII regions; infrared : ISM ID H-II REGIONS; YOUNG STELLAR OBJECTS; COMPACT HII-REGIONS; DARK CLOUD; INTERSTELLAR EXTINCTION; REFLECTION NEBULAE; ISO SPECTROSCOPY; DUST; G29.96-0.02; GRAINS AB We present a spectroscopic study of the shape of the dust-extinction law between 1.0 and 2.2 mu m towards a set of nine ultracompact H II regions with A(V)greater than or similar to 15 mag. We find some evidence that the reddening curve may tend to flatten at higher extinctions, but just over half of the sample has extinction consistent with or close to the average for the interstellar medium (ISM). There is no evidence of extinction curves significantly steeper than the standard law, even where water ice is present. Comparing the results to the predictions of a simple extinction model, we suggest that a standard extinction law implies a robust upper limit to the grain-size distribution at around 0.1-0.3 mu m. Flatter curves are most likely the result of changes in this upper limit, although the effects of flattening as a result of unresolved clumpy extinction cannot be ruled out. C1 Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England. Univ Leeds, Dept Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. AURA, Gemini Observ, La Serena, Chile. RP Moore, TJT (reprint author), Liverpool John Moores Univ, Astrophys Res Inst, 12 Quays House, Birkenhead CH41 1LD, Merseyside, England. EM tjtm@astro.livjm.ac.uk NR 42 TC 18 Z9 19 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 MAY 11 PY 2005 VL 359 IS 2 BP 589 EP 596 DI 10.1111/j.1365-2966.2005.08923.x PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 921DY UT WOS:000228745600018 ER PT J AU Zentner, AR Berlind, AA Bullock, JS Kravtsov, AV Wechsler, RH AF Zentner, AR Berlind, AA Bullock, JS Kravtsov, AV Wechsler, RH TI The physics of galaxy clustering. I. A model for subhalo populations SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : theory; dark matter; galaxies : formation; galaxies : halos; galaxies : structure; large-scale structure of universe ID DARK-MATTER HALOES; N-BODY SIMULATIONS; MISSING-SATELLITES PROBLEM; X-RAY-CLUSTERS; RADIAL-DISTRIBUTION; DYNAMICAL FRICTION; DENSITY PROFILES; REDSHIFT SURVEY; OCCUPATION DISTRIBUTION; HIERARCHICAL-MODELS AB We present a semianalytic model for cold dark matter halo substructure that can be used as a framework for studying the physics of galaxy formation and as an ingredient in halo models of galaxy clustering. The model has the following main ingredients: ( 1) extended Press-Schechtermass accretion histories, ( 2) host halo density profiles computed according to the trends observed in cosmological simulations, ( 3) distributions of initial orbital parameters of accreting subhalos measured in a high-resolution simulation of three MilkyWay - size halos, and ( 4) integration of the orbital evolution of subhalos including the effects of dynamical friction and tidal mass loss. We perform a comprehensive comparison of the model calculations to the results of a suite of high-resolution cosmological simulations. The comparisons show that subhalo statistics such as the velocity and mass functions, the radial distributions, and the halo occupation distributions agree well over 3 orders of magnitude in host halo mass and at various redshifts. We find that both in the simulations and in our model the radial distributions of subhalos are significantly shallower than that of the dark matter density. The abundance of subhalos in a host is set by competition between tidal disruption and new accretion. Halos of high mass and halos at high redshift tend to host more subhalos because the subhalos have, on average, been accreted more recently. Similarly, at a fixed mass and epoch, halos that formed more recently host a larger number of subhalos. Observed "fossil groups'' may represent an extreme tail of this correlation. We find a related correlation between host halo concentration and satellite abundance at fixed host mass, N(sat) proportional to c(vir)(-a), where a changes with redshift and host-to-subhalo mass ratio. Lastly, we use our substructure model to populate host halos in one of the high-resolution cosmological simulations, replacing the actual subhalos resolved in this simulation and using the host mass as the only input for the model calculation. We show that the resulting correlation function of such a hybrid halo ensemble is indistinguishable from that measured directly in the simulation. This supports one of the key tenets of the standard halo model, i.e., the assumption that the halo occupation distribution is statistically independent of the host halo environment. C1 Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. NYU, Ctr Cosmol & Particle Phys, New York, NY 10003 USA. NYU, Dept Phys, New York, NY 10003 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA. Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. RP Zentner, AR (reprint author), Univ Chicago, Kavli Inst Cosmol Phys, 5640 S Ellis Ave, Chicago, IL 60637 USA. EM zentner@kicp.uchicago.edu; aberlind@cosmo.nyu.edu; jbullock@cfa.harvard.edu; andrey@oddjob.uchicago.edu; risa@kicp.uchicago.edu RI Bullock, James/K-1928-2015; OI Bullock, James/0000-0003-4298-5082; Wechsler, Risa/0000-0003-2229-011X NR 92 TC 214 Z9 215 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2005 VL 624 IS 2 BP 505 EP 525 DI 10.1086/428898 PN 1 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 923NG UT WOS:000228916000004 ER PT J AU Silverman, JD Green, PJ Barkhouse, WA Cameron, RA Foltz, C Jannuzi, BT Kim, DW Kim, M Mossman, A Tananbaum, H Wilkes, BJ Smith, MG Smith, RC Smith, PS AF Silverman, JD Green, PJ Barkhouse, WA Cameron, RA Foltz, C Jannuzi, BT Kim, DW Kim, M Mossman, A Tananbaum, H Wilkes, BJ Smith, MG Smith, RC Smith, PS TI Comoving space density of X-ray-selected active galactic nuclei SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; quasars : general; surveys; X-rays : galaxies ID CHANDRA MULTIWAVELENGTH PROJECT; DEEP FIELD-SOUTH; DIGITAL SKY SURVEY; AGN LUMINOSITY FUNCTION; HIGH-REDSHIFT QUASARS; OPTICAL IDENTIFICATIONS; COSMOLOGICAL EVOLUTION; SOURCE CATALOGS; ROSAT SURVEYS; NORTH SURVEY AB For measurement of the active galactic nucleus (AGN) luminosity function and its evolution, X-ray selection samples all types of AGNs and provides reduced obscuration bias in comparison with UV excess or optical surveys. The apparent decline in optically selected quasars above z &SIM; 3 may be strongly affected by such a bias. The Chandra Multiwavelength Project (CHAMP) is characterizing serendipitously detected X-ray sources in a large number of fields with archival Chandra imaging. We present a preliminary measure of the comoving space density using a sample of 311 AGNs found in 23 CHAMP fields (&SIM; 1.8 deg(2)) supplemented with 57 X-ray-bright AGNs from the Chandra Deep Field-North and Chandra Deep Field-South. Within our X-ray flux (f(0.3-8.0 keV) > 4 x 10(-15) ergs cm(-2) s(-1)) and optical magnitude (r' < 22.5) limits, our sample includes 14 broad emission-line AGNs at z > 3. Using this X-ray selected sample, we detect a turnover in the comoving space density of luminous type 1 AGNs (log L-X > 44.5 ergs s(-1), measured in the 0.3-8.0 keV band and corrected for Galactic absorption) at z > 2.5. Our X-ray sample is the first to show a behavior similar to the well-established evolution of the optical quasar luminosity function. A larger sample of high-redshift AGNs and with a greater fraction of identified sources, either spectroscopic or photometric, at faint optical magnitudes (r' > 22.5) are required to remove the remaining uncertainty in our measure of the X-ray luminosity function, particularly given the possibility that AGNs might be more easily obscured optically at high redshift. We confirm that for z < 1, lower luminosityAGNs (log L-X < 44.5) are more prevalent by more than an order of magnitude than those with high luminosity. We have combined the Chandra sample with AGNs from the ROSAT surveys to present a measure of the space density of luminous type 1 AGNs in the soft X-ray band (0.5-2.0 keV) that confirms the broadband turnover described above. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA. Natl Sci Fdn, Arlington, VA 22230 USA. Natl Opt Astron Observ, Tucson, AZ 85726 USA. Natl Opt Astron Observ, Cerro Tololo Interamer Observ, La Serena, Chile. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. RP Silverman, JD (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jsilverman@mpe.mpg.de OI Wilkes, Belinda/0000-0003-1809-2364 NR 44 TC 59 Z9 59 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 MAY 10 PY 2005 VL 624 IS 2 BP 630 EP 637 DI 10.1086/429361 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 923NG UT WOS:000228916000012 ER PT J AU Fegan, SJ Badran, HM Bond, IH Boyle, PJ Bradbury, SM Buckley, JH Carter-Lewis, DA Catanese, M Celik, O Cui, W Daniel, M D'Vali, M Perez, IDC Duke, C Falcone, A Fegan, DJ Finley, JP Fortson, LF Gaidos, JA Gammell, S Gibbs, K Gillanders, GH Grube, J Hall, J Hall, TA Hanna, D Hillas, AM Holder, J Horan, D Jarvis, A Jordan, M Kenny, GE Kertzman, M Kieda, D Kildea, J Knapp, J Kosack, K Krawczynski, H Krennrich, F Lang, MJ Le Bohec, S Lessard, RW Linton, E Lloyd-Evans, J Milovanovic, A McEnery, J Moriarty, P Mukherjee, R Muller, D Nagai, T Nolan, S Ong, RA Pallassini, R Petry, D Power-Mooney, B Quinn, J Quinn, M Ragan, K Rebillot, P Reynolds, PT Rose, HJ Schroedter, M Sembroski, GH Swordy, SP Syson, A Vassiliev, VV Wakely, SP Walker, G Weekes, TC Zweerink, J AF Fegan, SJ Badran, HM Bond, IH Boyle, PJ Bradbury, SM Buckley, JH Carter-Lewis, DA Catanese, M Celik, O Cui, W Daniel, M D'Vali, M Perez, IDC Duke, C Falcone, A Fegan, DJ Finley, JP Fortson, LF Gaidos, JA Gammell, S Gibbs, K Gillanders, GH Grube, J Hall, J Hall, TA Hanna, D Hillas, AM Holder, J Horan, D Jarvis, A Jordan, M Kenny, GE Kertzman, M Kieda, D Kildea, J Knapp, J Kosack, K Krawczynski, H Krennrich, F Lang, MJ Le Bohec, S Lessard, RW Linton, E Lloyd-Evans, J Milovanovic, A McEnery, J Moriarty, P Mukherjee, R Muller, D Nagai, T Nolan, S Ong, RA Pallassini, R Petry, D Power-Mooney, B Quinn, J Quinn, M Ragan, K Rebillot, P Reynolds, PT Rose, HJ Schroedter, M Sembroski, GH Swordy, SP Syson, A Vassiliev, VV Wakely, SP Walker, G Weekes, TC Zweerink, J TI A survey of unidentified egret sources at very high energies SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : jets; gamma rays : observations; surveys ID GAMMA-RAY SOURCES; SOURCE 3EG J2227+6122; X-RAY; GALACTIC PLANE; LS I+61-DEGREES-303; SUPERNOVA-REMNANTS; GALAXY CLUSTERS; SAX J0635+0533; TEV ENERGIES; ERROR BOX AB The Whipple Observatory 10 m γ-ray telescope has been used to survey the error boxes of EGRET unidentified sources in an attempt to find counterparts at energies of 350 GeV and above. Twenty-one unidentified sources detected by EGRET (more than 10% of the total number) have been included in this survey. In no case is a statistically significant signal found in the EGRET error box, which implies that, at least for this sample, the γ-ray spectra of these sources steepen between 100 MeV and 350 GeV. For each EGRET source location, we list candidate associations and derive upper limits on the integral γ-ray flux above 350 GeV. C1 Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. Univ Arizona, Dept Phys, Tucson, AZ 85721 USA. Tanta Univ, Dept Phys, Tanta, Egypt. Univ Leeds, Dept Phys, Leeds LS2 9JT, W Yorkshire, England. Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. Washington Univ, Dept Phys, St Louis, MO 63130 USA. Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. Univ Calif Los Angeles, Dept Phys, Los Angeles, CA 90095 USA. Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. Univ Oxford, Dept Phys, Oxford OX1 3RH, England. Grinnell Coll, Dept Phys, Grinnell, IA 50112 USA. Natl Univ Ireland, Expt Phys Dept, Dublin 4, Ireland. Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL USA. Natl Univ Ireland, Dept Phys, Galway, Ireland. Univ Utah, High Energy Astrophys Inst, Salt Lake City, UT 84112 USA. Univ Arkansas, Dept Phys & Astron, Little Rock, AR 72204 USA. McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. DePauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA. Galway Mayo Inst Technol, Sch Sci, Galway, Ireland. Univ Maryland Baltimore Cty, Baltimore, MD 21228 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Columbia Univ Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA. Cork Inst Technol, Dept Appl Phys & Instrumentat, Cork, Ireland. RP Fegan, SJ (reprint author), Univ Calif Los Angeles, Dept Phys, Los Angeles, CA 90095 USA. EM sfegan@astro.ucla.edu RI McEnery, Julie/D-6612-2012; Hall, Jeter/E-9294-2015; 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 74 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 MAY 10 PY 2005 VL 624 IS 2 BP 638 EP 655 DI 10.1086/429123 PN 1 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 923NG UT WOS:000228916000013 ER PT J AU Monnier, JD Millan-Gabet, R Billmeier, R Akeson, RL Wallace, D Berger, JP Calvet, N D'Alessio, P Danchi, WC Hartmann, L Hillenbrand, LA Kuchner, M Rajagopal, J Traub, WA Tuthill, PG Boden, A Booth, A Colavita, M Gathright, J Hrynevych, M Le Mignant, D Ligon, R Neyman, C Swain, M Thompson, R Vasisht, G Wizinowich, P Beichman, C Beletic, J Creech-Eakman, M Koresko, C Sargent, A Shao, M van Belle, G AF Monnier, JD Millan-Gabet, R Billmeier, R Akeson, RL Wallace, D Berger, JP Calvet, N D'Alessio, P Danchi, WC Hartmann, L Hillenbrand, LA Kuchner, M Rajagopal, J Traub, WA Tuthill, PG Boden, A Booth, A Colavita, M Gathright, J Hrynevych, M Le Mignant, D Ligon, R Neyman, C Swain, M Thompson, R Vasisht, G Wizinowich, P Beichman, C Beletic, J Creech-Eakman, M Koresko, C Sargent, A Shao, M van Belle, G TI The near-infrared size-luminosity relations for Herbig Ae/Be disks SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; circumstellar matter; instrumentation : interferometers; radiative transfer; stars : formation; stars : pre-main-sequence ID Z-CANIS-MAJORIS; YOUNG STELLAR OBJECTS; INTERMEDIATE-MASS STARS; T-TAURI STARS; CIRCUMSTELLAR DISKS; KECK INTERFEROMETER; ACCRETION DISKS; AB-AURIGAE; EMISSION; SPECTROSCOPY AB We report the results of a sensitive K-band survey of Herbig Ae/Be disk sizes using the 85 m baseline Keck Interferometer. Targets were chosen to span the maximum range of stellar properties to probe the disk size dependence on luminosity and effective temperature. For most targets, the measured near-infrared sizes (ranging from 0.2 to 4 AU) support a simple disk model possessing a central optically thin (dust-free) cavity, ringed by hot dust emitting at the expected sublimation temperatures (T-s &SIM; 1000-1500 K). Furthermore, we find a tight correlation of disk size with source luminosity R &PROP; L-1/2 for Ae and late Be systems (valid over more than two decades in luminosity), confirming earlier suggestions based on lower quality data. Interestingly, the inferred dust-free inner cavities of the highest luminosity sources (Herbig B0-B3 stars) are undersized compared to predictions of the "optically thin cavity'' model, likely because of optically thick gas within the inner AU. C1 Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. CALTECH, Michelson Sci Ctr, Pasadena, CA 91125 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Lab Astrophys Grenoble, F-38400 St Martin Dheres, France. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Nacl Autonoma Mexico, Mexico City 04510, DF, Mexico. CALTECH, Dept Astron, Pasadena, CA 91125 USA. Princeton Univ, Princeton, NJ 08544 USA. Univ Sydney, Dept Phys, Sydney, NSW 2006, Australia. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Calif Assoc Res Astron, WM Keck Observ, Kamuela, HI 96743 USA. RP Monnier, JD (reprint author), Univ Michigan, Dept Astron, 941 Dennison Bldg, Ann Arbor, MI 48109 USA. EM monnier@umich.edu RI Kuchner, Marc/E-2288-2012 NR 65 TC 111 Z9 112 U1 1 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 MAY 10 PY 2005 VL 624 IS 2 BP 832 EP 840 DI 10.1086/429266 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 923NG UT WOS:000228916000029 ER PT J AU Lee, CF Ho, PTP AF Lee, CF Ho, PTP TI Outflow interaction in the late stages of star formation SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : individual (L43, RNO 91); ISM : jets and outflows; stars : formation ID YOUNG STELLAR OBJECTS; MOLECULAR OUTFLOWS; JET-DRIVEN; DENSE CORES; HYDRODYNAMIC SIMULATIONS; INFALL INTERACTIONS; DARK CLOUDS; CO OUTFLOWS; PROTOSTARS; L43 AB We have mapped the CO, HCO+, N2H+, and CS emission around a nearby T Tauri star, IRAS 16316-1540. A molecular outflow is seen in CO, HCO+, N2H+, and CS emission originating from the IRAS source, while an envelope is seen in N2H+ and HCO+ emission surrounding the IRAS source. The molecular outflow is bipolar with a southeastern (SE) lobe and a northwestern ( NW) lobe. The structure and the kinematics of the SE lobe are well defined and can be explained with a simple kinematic model. In this model, the SE lobe is a U-shaped shell consisting of a wide-opening base mimicking the reflection nebula RNO 91 and a cylindrical shell with a constant radius mimicking the CO outflow shell. The wide-opening base is expanding toward the circumstellar envelope, while the cylindrical shell is expanding mainly laterally into the ambient medium. If the base of the SE lobe continues to expand at its current velocity, it will meet with the base of the NW lobe and disperse the circumstellar envelope in a few times 10(4) yr. The circumstellar envelope is elongated perpendicular to the outflow axis, extending to the northeast and southwest of the IRAS source. The envelope has differential rotation with the velocity increasing toward the source. It may result from material infalling toward the source carrying its angular momentum. The HCO+ emission near the source may arise from an unresolved inner ring of the envelope, showing two peaks with one on each side of the IRAS source and a position-velocity structure consistent with the rotation law derived from the N2H+ emission. The HCO+ emission in the outer part of the envelope likely traces the swept up envelope material, showing both the outflow motion and probably rotation. C1 Harvard Smithsonian Ctr Astrophys, Submillimeter Array, Hilo, HI 96720 USA. Univ Maryland, Dept Astron, College Pk, MD 20742 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Lee, CF (reprint author), Harvard Smithsonian Ctr Astrophys, Submillimeter Array, 645 N Aohoku Pl, Hilo, HI 96720 USA. EM cflee@cfa.harvard.edu; ho@cfa.harvard.edu NR 43 TC 12 Z9 12 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 MAY 10 PY 2005 VL 624 IS 2 BP 841 EP 852 DI 10.1086/429535 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 923NG UT WOS:000228916000030 ER PT J AU De Pree, CG Wilner, DJ Deblasio, J Mercer, AJ Davis, LE AF De Pree, CG Wilner, DJ Deblasio, J Mercer, AJ Davis, LE TI The morphologies of ultracompact HII regions in W49A and sagittarius B2: The prevalence of shells and a modified classification scheme SO ASTROPHYSICAL JOURNAL LA English DT Article DE HII regions; instrumentation : interferometers; ISM : individual (Sagittarius B2, W49N); techniques : interferometric ID H-II REGIONS; STAR-FORMING REGION; MASSIVE STARS; AU SCALES; EVOLUTION; MAIN AB We have used Very Large Array (VLA) observations of the massive star-forming regions W49A and Sgr B2, obtained with resolutions from 2.&DPRIME; 0 to 0.&DPRIME; 04, to classify the morphologies of nearly 100 ultracompact (UC) H II regions. These high-resolution, multifrequency, multiconfiguration VLA observations motivate us to make several modifications of the existing morphological classification scheme for UC H II regions. In this work, we describe the modified morphology scheme and the criteria used in source classification. In particular, we drop the "core-halo" classification, add a "bipolar" classification, and change the shell classification to "shell-like." We tally the percentage of each morphology found in the Sgr B2 and W49A regions and find broad agreement with the Galactic plane surveys in the distribution of morphologies for most types. However, we find that nearly a third of the sources in these regions are shell-like, which is a higher percentage by nearly a factor of 10 than found in the surveys of Galactic plane star-forming regions by Wood & Churchwell and Kurtz et al. This difference may be due to physical differences in the environments of these two extreme star-forming regions. Alternatively, differences in observational technique may be responsible. C1 Agnes Scott Coll, Dept Phys & Astron, Decatur, GA 30030 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. Univ Florida, Dept Astron, Bryant Space Sci Ctr 211, Gainesville, FL 32611 USA. RP De Pree, CG (reprint author), Agnes Scott Coll, Dept Phys & Astron, 141 E Coll Ave, Decatur, GA 30030 USA. EM cdepree@agnesscott.edu; dwilner@cfa.harvard.edu; jdeblasio@agnesscott.edu; allison-mercer@uiowa.edu; ledavis@astro.ufl.edu NR 17 TC 17 Z9 17 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 MAY 10 PY 2005 VL 624 IS 2 BP L101 EP L104 DI 10.1086/430738 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 923NK UT WOS:000228916400010 ER PT J AU Labbe, I Huang, JS Franx, M Rudnick, G Barmby, P Daddi, E van Dokkum, PG Fazio, GG Schreiber, NMF Moorwood, AFM Rix, HW Rottgering, H Trujillo, I van der Werf, P AF Labbe, I Huang, JS Franx, M Rudnick, G Barmby, P Daddi, E van Dokkum, PG Fazio, GG Schreiber, NMF Moorwood, AFM Rix, HW Rottgering, H Trujillo, I van der Werf, P TI Irac mid-infrared imaging of the Hubble Deep Field-South: Star formation histories and stellar masses of red galaxies at z > 2 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : evolution; galaxies : high-redshift; infrared : galaxies ID LYMAN BREAK GALAXIES; HIGH-REDSHIFT GALAXIES; SUBSTANTIAL POPULATION; SPACE-TELESCOPE; LUMINOSITY; UNIVERSE; COLOR AB We present deep 3.6 - 8 μ m imaging of the Hubble Deep Field - South with the Infrared Array Camera (IRAC) on the Spitzer Space Telescope. We study distant red galaxies (DRGs) at z > 2 selected by J(s) - K-s 1 2.3 and compare them with a sample of Lyman break galaxies (LBGs) at z = 2 - 3. The observed UV - to - 8 μ m spectral energy distributions are fitted with stellar population models to constrain star formation histories and derive stellar masses. We find that 70% of the DRGs are best described by dust-reddened star-forming models and 30% are very well fitted with old and "dead" models. Using only the I - K-s and K-s - 4.5 μ m colors, we can effectively separate the two groups. The dead systems are among the most massive at z &SIM; 2.5 ( mean stellar mass [M*] = 0.8 x 10(11) M-.) and likely formed most of their stellar mass at z > 5. To a limit of 0.5 x 10(11) M-., their number density is &SIM; 10 times lower than that of local early-type galaxies. Furthermore, we use the IRAC photometry to derive rest-frame near-infrared J, H, and K fluxes. The DRGs and LBGs together show a large variation ( a factor of 6) in the rest-frame K-band mass-to-light ratios (M/L-K), implying that even a Spitzer 8 μ m-selected sample would be very different from a mass-selected sample. The average M/L-K of the DRGs is about 3 times higher than that of the LBGs, and DRGs dominate the high-mass end. The M/L-K values and ages of the two samples appear to correlate with derived stellar mass, with the most massive galaxies being the oldest and having the highest mass-to-light ratios, similar to what is found in the low-redshift universe. C1 Carnegie Observ, Pasadena, CA 91101 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Sterrewacht Leiden, NL-2300 RA Leiden, Netherlands. Natl Opt Astron Observ, Tucson, AZ 85719 USA. Yale Univ, Dept Astron, New Haven, CT 06520 USA. Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. European So Observ, D-85748 Garching, Germany. Max Planck Inst Astron, D-69117 Heidelberg, Germany. RP Labbe, I (reprint author), Carnegie Observ, 813 Santa Barbara, Pasadena, CA 91101 USA. EM ivo@ociw.edu RI Daddi, Emanuele/D-1649-2012; Barmby, Pauline/I-7194-2016 OI Daddi, Emanuele/0000-0002-3331-9590; Barmby, Pauline/0000-0003-2767-0090 NR 23 TC 191 Z9 191 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 MAY 10 PY 2005 VL 624 IS 2 BP L81 EP L84 DI 10.1086/430700 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 923NK UT WOS:000228916400005 ER PT J AU O'Sullivan, E Vrtilek, JM Kempner, JC AF O'Sullivan, E Vrtilek, JM Kempner, JC TI Active galactic nucleus feedback and gas mixing in the core of NGC 4636 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : halos; galaxies : individual (NGC 4636); intergalactic medium; X-rays : galaxies ID EARLY-TYPE GALAXIES; GIANT ELLIPTIC GALAXIES; BLACK-HOLE MASS; X-RAY; XMM-NEWTON; NGC 4636; HOT GAS; CHANDRA; RADIO; ASCA AB Chandra observations of NGC 4636 show disturbances in the galaxy X-ray halo, including armlike high surface brightness features ( tentatively identified as active galactic nucleus - driven shocks) and a possible cavity on the west side of the galaxy core. We present Chandra and XMM-Newton spectral maps of NGC 4636 that confirm the presence of the cavity and show it to be bounded by the arm features. The maps also reveal a &SIM; 15 kpc wide plume of low-temperature, high-abundance gas extending 25 - 30 kpc to the southwest of the galaxy. The cavity appears to be embedded in this plume, and we interpret the structure as being entrained gas drawn out of the galaxy core during previous episodes of active galactic nucleus (AGN) activity. The end of the plume is marked by a well-defined edge, with significant falls in surface brightness, temperature, and abundance, indicating a boundary between galaxy and group/cluster gas. This may be evidence that as well as preventing gas cooling through direct heating, AGN outbursts can produce significant gas mixing, disturbing the temperature structure of the halo and transporting metals out from the galaxy into the surrounding intragroup medium. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Bowdoin Coll, Dept Phys & Astron, Brunswick, ME 04011 USA. RP O'Sullivan, E (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM eosullivan@head.cfa.harvard.edu; jvrtilek@head.cfa.harvard.edu; jkempner@bowdoin.edu OI O'Sullivan, Ewan/0000-0002-5671-6900 NR 30 TC 42 Z9 42 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 MAY 10 PY 2005 VL 624 IS 2 BP L77 EP L80 DI 10.1086/430600 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 923NK UT WOS:000228916400004 ER PT J AU Wake, DB Hanken, J Ibanez, R AF Wake, DB Hanken, J Ibanez, R TI A new species of big black Bolitoglossa (Amphibia : Caudata) from central Panama SO COPEIA LA English DT Article ID PLETHODONTIDAE; EVOLUTIONARY; SALAMANDERS AB A new species of Bolitoglossa is described from the Cordillera Central of central Panama. This is a large black species, which is likely related to the B. (Eladinea) schizodactyla group of Costa Rica and Panama. The new species, known from a single specimen, differs from other large black Bolitoglossa in having white pigmentation on the lower face and on the ventral portions of the head and chest. It also has more interdigital webbing than most members of the B. (E.) schizodactyla group. C1 Harvard Univ, Dept Orgasm & Evolutionary Biol, Cambridge, MA 02138 USA. Harvard Univ, Museum Comparat Zool, Cambridge, MA 02138 USA. Smithsonian Trop Res Inst, Panama City, Panama. Estafeta Univ, Circulo Herpetol Panama, Panama City, Panama. Univ Panama, Dept Zool, Panama City, Panama. RP Hanken, J (reprint author), Harvard Univ, Dept Orgasm & Evolutionary Biol, 26 Oxford St, Cambridge, MA 02138 USA. EM hanken@oeb.harvard.edu NR 5 TC 4 Z9 5 U1 1 U2 1 PU AMER SOC ICHTHYOLOGISTS HERPETOLOGISTS PI CHARLESTON PA UNIV CHARLESTON, GRICE MARINE LABORATORY, 205 FORT JOHNSON RD, CHARLESTON, SC 29412 USA SN 0045-8511 J9 COPEIA JI Copeia PD MAY 9 PY 2005 IS 2 BP 223 EP 226 DI 10.1643/CH-04-082R1 PG 4 WC Zoology SC Zoology GA 925NR UT WOS:000229060300001 ER PT J AU Smith, DG AF Smith, DG TI Victor Gruschka Springer SO COPEIA LA English DT Biographical-Item C1 Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Smith, DG (reprint author), Smithsonian Inst, Natl Museum Nat Hist, MRC 159, Washington, DC 20013 USA. EM sruithd@si.edu NR 1 TC 1 Z9 1 U1 0 U2 0 PU AMER SOC ICHTHYOLOGISTS HERPETOLOGISTS PI CHARLESTON PA UNIV CHARLESTON, GRICE MARINE LABORATORY, 205 FORT JOHNSON RD, CHARLESTON, SC 29412 USA SN 0045-8511 J9 COPEIA JI Copeia PD MAY 9 PY 2005 IS 2 BP 431 EP 439 DI 10.1643/OT-04-322 PG 9 WC Zoology SC Zoology GA 925NR UT WOS:000229060300024 ER PT J AU Thorwirth, S McCarthy, MC Dudek, JB Thaddeus, P AF Thorwirth, S McCarthy, MC Dudek, JB Thaddeus, P TI Fourier transform microwave spectroscopy of vinyldiacetylene, vinyltriacetylene, and vinylcyanodiacetylene SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID VINYL CYANIDE; CARBON CHAINS; ELECTRONIC SPECTROSCOPY; MOLECULAR-STRUCTURE; WAVE SPECTRUM; 1-CYANOBUT-3-ENE-1-YNE; VINYLACETYLENE; CH2=CH-C=C-C=N; DIACETYLENE; ACETYLENE AB The rotational spectra of the three carbon chain molecules vinyldiacetylene (hex-1-ene-3,5-diyne, C6H4), vinyltriacetylene (oct-1-ene-3,5,7-triyne, C8H4), and its cyano analog vinylcyanodiacetylene (1-cyanohex-5-ene-1,3-diyne, C7H3N) have been observed for the first time by Fourier transform microwave spectroscopy of a supersonic molecular beam. The molecules were observed as products of an electrical discharge through selected precursor mixtures: ethylene/diacetylene and vinylacetylene/diacetylene for the pure hydrocarbon molecules and vinylacetylene/cyanoacetylene for vinylcyanodiacetylene. The measurements yield precise sets of rotational constants that compare very well with theoretical constants obtained by quantum chemical calculations at the B3LYP/cc-pVTZ level of theory. Since these three carbon chains are similar in structure and composition to known astronomical molecules and because of their significant polarity, all three are candidates for radio astronomical detection. (c) 2005 American Institute of Physics. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Harvard Univ, Div Engn & Appl Sci, Cambridge, MA 02138 USA. RP Thorwirth, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM sthorwirth@cfa.harvard.edu RI Thorwirth, Sven/C-6217-2011; OI Thorwirth, Sven/0000-0001-8200-6710; McCarthy, Michael/0000-0001-9142-0008 NR 34 TC 4 Z9 4 U1 0 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 MAY 8 PY 2005 VL 122 IS 18 AR 184308 DI 10.1063/1.1893920 PG 7 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 928MK UT WOS:000229275600024 PM 15918705 ER PT J AU Santra, R Arimondo, E Ido, T Greene, CH Ye, J AF Santra, R Arimondo, E Ido, T Greene, CH Ye, J TI High-accuracy optical clock via three-level coherence in neutral bosonic Sr-88 SO PHYSICAL REVIEW LETTERS LA English DT Article ID ALKALINE-EARTH ATOMS; OSCILLATOR-STRENGTHS; ION; STRONTIUM; FREQUENCY; STATE AB An optical atomic clock scheme is proposed that utilizes two lasers to establish coherent coupling between the 5s(2) S-1(0) ground state of Sr-88 and the first excited state, 5s5p P-3(0). The coupling is mediated by the broad 5s5p P-1(1) state, exploiting the phenomenon of electromagnetically induced transparency. The effective linewidth of the clock transition can be chosen at will by adjusting the laser intensity. By trapping the Sr-88 atoms in an optical lattice, long interaction times with the two lasers are ensured; Doppler and recoil effects are eliminated. Based on a careful analysis of systematic errors, a clock accuracy of better than 2x10(-17) is expected. C1 Natl Inst Stand & Technol, Joint Inst Lab Astrophys, Boulder, CO 80309 USA. Univ Colorado, Dept Phys, Boulder, CO 80309 USA. Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. Univ Pisa, Dipartimento Fis E Fermi, INFM, UdR Pisa, I-56127 Pisa, Italy. RP Santra, R (reprint author), Natl Inst Stand & Technol, Joint Inst Lab Astrophys, Boulder, CO 80309 USA. EM Y@jila.colorado.edu RI Ye, Jun/C-3312-2011; Greene, Chris/C-3821-2011; Santra, Robin/E-8332-2014 OI Greene, Chris/0000-0002-2096-6385; Santra, Robin/0000-0002-1442-9815 NR 21 TC 80 Z9 81 U1 1 U2 9 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 MAY 6 PY 2005 VL 94 IS 17 AR 173002 DI 10.1103/PhysRevLett.94.173002 PG 4 WC Physics, Multidisciplinary SC Physics GA 923TM UT WOS:000228932200017 PM 15904285 ER PT J AU Schindel, DE Miller, SE AF Schindel, DE Miller, SE TI DNA barcoding a useful tool for taxonomists SO NATURE LA English DT Letter C1 Smithsonian Inst, Natl Museum Nat Hist, Consortium Barcode Life, Washington, DC 20013 USA. RP Schindel, DE (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Consortium Barcode Life, POB 37012,MRC-105, Washington, DC 20013 USA. OI Miller, Scott/0000-0002-4138-1378 NR 1 TC 144 Z9 209 U1 7 U2 55 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD MAY 5 PY 2005 VL 435 IS 7038 BP 17 EP 17 DI 10.1038/435017b PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 922UL UT WOS:000228864600014 PM 15874991 ER PT J AU West-Eberhard, MJ AF West-Eberhard, MJ TI Developmental plasticity and the origin of species differences SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article; Proceedings Paper CT Colloquium on Systematics and the Origin of Species CY DEC 16-18, 2004 CL Irvine, CA SP Natl Acad Sci & Engn DE speciation; genetic accommodation; adaptive evolution; novelty; parallel evolution ID DROSOPHILA-MELANOGASTER; DIRECTIONAL ASYMMETRY; SYMPATRIC SPECIATION; SPOTTED SANDPIPER; EVOLUTION; SELECTION; PROLACTIN; ADAPTATION; EXPRESSION; CHARACTER AB Speciation is the origin of reproductive isolation and divergence between populations, according to the "biological species concept" of Mayr. Studies of reproductive isolation have dominated research on speciation, leaving the origin of species differences relatively poorly understood. Here, I argue that the origin of species differences, and of novel phenotypes in general, involves the reorganization of ancestral phenotypes (developmental recombination) followed by the genetic accommodation of change. Because selection acts on phenotypes, not directly on genotypes or genes, novel traits can originate by environmental induction as well as mutation, then undergo selection and genetic accommodation fueled by standing genetic variation or by subsequent mutation and genetic recombination. Insofar as phenotypic novelties arise from adaptive developmental plasticity, they are not "random" variants, because their initial form reflects adaptive responses with an evolutionary history, even though they are initiated by mutations or novel environmental factors that are random with respect to (future) adaptation. Change in trait frequency involves genetic accommodation of the threshold or liability for expression of a novel trait, a process that follows rather than directs phenotypic change. Contrary to common belief, environmentally initiated novelties may have greater evolutionary potential than mutationally induced ones. Thus, genes are probably more often followers than leaders in evolutionary change. Species differences can originate before reproductive isolation and contribute to the process of speciation itself. Therefore, the genetics of speciation can profit from studies of changes in gene expression as well as changes in gene frequency and genetic isolation. C1 Smithsonian Trop Res Inst, Unit 2511, APO, AA 34020 USA. RP West-Eberhard, MJ (reprint author), Univ Costa Rica, Escuela Biol, Ciudad Univ, San Jose, Costa Rica. EM mjwe@sent.com NR 63 TC 346 Z9 365 U1 13 U2 172 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 MAY 3 PY 2005 VL 102 SU 1 BP 6543 EP 6549 DI 10.1073/pnas.0501844102 PG 7 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 925AK UT WOS:000229023700006 PM 15851679 ER PT J AU Machado, CA Robbins, N Gilbert, MTP Herre, EA AF Machado, CA Robbins, N Gilbert, MTP Herre, EA TI Critical review of host specificity and its coevolutionary implications in the fig/fig-wasp mutualism SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article; Proceedings Paper CT Colloquium on Systematics and the Origin of Species CY DEC 16-18, 2004 CL Irvine, CA SP Natl Acad Sci & Engn ID FIG-POLLINATING WASPS; PHYLOGENETIC-RELATIONSHIPS; MOLECULAR PHYLOGENY; DIOECIOUS FICUS; DNA-SEQUENCES; DROSOPHILA-PSEUDOOBSCURA; FRUIT CHARACTERISTICS; POPULATION-GENETICS; ACTIVE POLLINATION; BREEDING STRUCTURE AB Figs (Ficus spp., Moraceae) and their pollinating wasps (Agaonidae, Chalcidoidea) constitute perhaps the most tightly integrated pollination mutualism that is known. Figs are characterized by extraordinarily high global and local species diversity. It has been proposed that the diversification of this mutualism has occurred through strict-sense coadaptation and cospeciation between pairs of fig and wasp species that are associated in highly specific one-to-one relationships. However, existing studies cast doubt on the generality of this proposition. Here, we review our current knowledge of the evolutionary history of the fig/fig-wasp mutualism. We critically examine the idea that codivergence between figs and their pollinators has been dominated by strict-sense cospeciation. We present phylogenetic and population genetic data from neotropical fig and fig wasp species that suggest that a more accurate model for diversification in this mutualism is that of groups of genetically well defined wasp species coevolving with genetically less well defined (frequently hybridizing) groups of figs. Last, we use our results to assess previously proposed hypotheses on models of speciation in this mutualism. C1 Univ Arizona, Dept Ecol & Evolutionary Biol, Tucson, AZ 85721 USA. Smithsonian Trop Res Inst, Unit 0948, Miami, FL 34002 USA. RP Machado, CA (reprint author), Univ Arizona, Dept Ecol & Evolutionary Biol, 1041 E Lowell St,Biosci W Bldg, Tucson, AZ 85721 USA. EM cmachado@email.arizona.edu RI Machado, Carlos/B-8855-2009; Gilbert, Marcus/A-8936-2013 OI Machado, Carlos/0000-0003-1546-7415; Gilbert, Marcus/0000-0002-5805-7195 NR 95 TC 135 Z9 144 U1 1 U2 59 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 MAY 3 PY 2005 VL 102 SU 1 BP 6558 EP 6565 DI 10.1073/pnas.0501840102 PG 8 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 925AK UT WOS:000229023700008 PM 15851680 ER PT J AU Palumbi, SR Lessios, HA AF Palumbi, SR Lessios, HA TI Evolutionary animation: How do molecular phylogenies compare to Mayr"s reconstruction of speciation patterns in the sea? SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article; Proceedings Paper CT Colloquium on Systematics and the Origin of Species CY DEC 16-18, 2004 CL Irvine, CA SP Natl Acad Sci & Engn DE bindin; sea urchins; speciation; mitochondrial DNA ID GAMETE RECOGNITION; REPRODUCTIVE ISOLATION; GENUS ECHINOMETRA; RAPID EVOLUTION; POPULATION-STRUCTURE; ADAPTIVE EVOLUTION; URCHIN TRIPNEUSTES; SEXUAL SELECTION; EASTERN PACIFIC; SPERM BINDIN AB Ernst Mayr used the geography of closely related species in various stages of increasing divergence to "animate" the process of geographic, or allopatric, speciation. This approach was applied to a wide set of taxa, and a seminal paper by Mayr used it to explore speciation patterns in tropical sea urchins. Since then, taxonomic information in several of these genera has been augmented by detailed molecular phylogenies. We compare Mayr's animation with the phylogenies of eight sea urchin genera placed by Mayr into four speciation groups. True to Mayr's predictions, early-stage genera have on average lower species divergence and more polytypic species than genera in later stages. For six of these genera, we also have information about the evolution of the gamete recognition protein bindin, which is critical to reproductive isolation. These comparisons show that later-stage genera with many sympatric species tend to be those with rapid bindin evolution. By contrast, early-stage genera with few sympatric species are not necessarily earlier in the divergence process; they happen to be those with slow rates of bindin evolution. These results show that the rate of speciation in sea urchins does not only depend on the steady accumulation of genome divergence over time, but also on the rate of evolution of gamete recognition proteins. The animation method used by Mayr is generally supported by molecular phylogenies. However, the existence of multiple rates in the acquisition of reproductive isolation complicates placement of different genera in an evolutionary series. C1 Stanford Univ, Dept Biol Sci, Hopkins Marine Stn, Pacific Grove, CA 93950 USA. Smithsonian Trop Res Inst, Unit 2072, Balboa 03092, Panama. RP Palumbi, SR (reprint author), Stanford Univ, Dept Biol Sci, Hopkins Marine Stn, Pacific Grove, CA 93950 USA. EM spalumbi@stanford.edu NR 51 TC 50 Z9 53 U1 0 U2 5 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 MAY 3 PY 2005 VL 102 SU 1 BP 6566 EP 6572 DI 10.1073/pnas.0501806102 PG 7 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 925AK UT WOS:000229023700009 PM 15851681 ER PT J AU de Queiroz, K AF de Queiroz, K TI Ernst Mayr and the modern concept of species SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article; Proceedings Paper CT Colloquium on Systematics and the Origin of Species CY DEC 16-18, 2004 CL Irvine, CA SP Natl Acad Sci & Engn ID TAXONOMY AB Ernst Mayr played a central role in the establishment of the general concept of species as metapopulation lineages, and he is the author of one of the most popular of the numerous alternative definitions of the species category. Reconciliation of incompatible species definitions and the development of a unified species concept require rejecting the interpretation of various contingent properties of metapopulation lineages, including intrinsic reproductive isolation in Mayr's definition, as necessary properties of species. On the other hand, the general concept of species as metapopulation lineages advocated by Mayr forms the foundation of this reconciliation, which follows from a corollary of that concept also advocated by Mayr: the proposition that the species is a fundamental category of biological organization. Although the general metapopulation lineage species concept and Mayr's popular species definition are commonly confused under the name "the biological species concept," they are more or less clearly distinguished in Mayr's early writings on the subject. Virtually all modern concepts and definitions of the species category, not only those that require intrinsic reproductive isolation, are to be considered biological according to the criterion proposed by Mayr. Definitions of the species category that identify a particular contingent property of metapopulation lineages (including intrinsic reproductive isolation) as a necessary property of species reduce the number of metapopulation lineages that are to be recognized taxonomically as species, but they cause conflicts among alternative species definitions and compromise the status of the species as a basic category of biological organization. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA. RP de Queiroz, K (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA. EM dequeirk@si.edu NR 52 TC 215 Z9 228 U1 9 U2 83 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 MAY 3 PY 2005 VL 102 SU 1 BP 6600 EP 6607 DI 10.1073/pnas.0502030102 PG 8 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 925AK UT WOS:000229023700014 PM 15851674 ER PT J AU Ortner, DJ AF Ortner, DJ TI The life and death of smallpox SO AMERICAN JOURNAL OF HUMAN BIOLOGY LA English DT Book Review C1 Smithsonian Inst, Dept Anthropol, Washington, DC USA. RP Ortner, DJ (reprint author), Smithsonian Inst, Dept Anthropol, Washington, DC USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU WILEY-LISS PI HOBOKEN PA DIV JOHN WILEY & SONS INC, 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 1042-0533 J9 AM J HUM BIOL JI Am. J. Hum. Biol. PD MAY-JUN PY 2005 VL 17 IS 3 BP 386 EP 387 DI 10.1002/ajhb.20117 PG 2 WC Anthropology; Biology SC Anthropology; Life Sciences & Biomedicine - Other Topics GA 922XH UT WOS:000228872700018 ER PT J AU Ortner, DJ Hotz, G AF Ortner, DJ Hotz, G TI \Skeletal manifestations of hypothyroidism from Switzerland SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Article DE cretinism; endocrine diseases; dwarfism AB Hypothyroidism is caused by a deficiency in the synthesis of thyroid hormone. Dwarfism is the most obvious skeletal manifestation, but most people with hypothyroidism do not have any skeletal evidence of the disease. When the skeleton is affected, the severity of this manifestation depends on the degree of the deficiency and age of onset. Endemic hypothyroidism typically is linked to specific ecological settings such as the high mountains where iodine is absent, or else it occurs with very low concentrations in water and soil. In these areas, the prevalence may be as high as 8%. The disease can be expected to occur in archaeological human skeletal samples from endemic regions. Sporadic hypothyroidism is caused by a deficiency in the thyroid gland itself, and is not linked to any specific environmental context. The disease may be the result of a genetic defect, but can also be caused by other pathological conditions that may affect the thyroid gland, including infection and cancer. The skeletal abnormalities of the two variants will be indistinguishable in archaeological human remains. In order to identify hypothyroidism in archaeological skeletal samples, one must be aware of the differences in pathological skeletal changes seen in hypothyroidism in comparison with other diseases, such as achondroplasia, that can cause similar abnormalities. Twelve clinically documented cases of hypothyroidism provide data for understanding the skeletal abnormalities associated with this disease. All 12 are modern documented cases from Switzerland, where endemic hypothyroidism occurred in the iodine-deficient Alpine regions. However, at least one case in the sample was caused by a defect in the thyroid gland itself. Am J Phys Anthropol 127:1-6, 2005. Published 2004 Wiley-Liss, Inc. C1 Natl Museum Nat Hist, Dept Anthropol, Smithsonian Inst, Washington, DC 20560 USA. Univ Bradford, Dept Archaeol Sci, Bradford BD7 1DP, W Yorkshire, England. Naturhist Museum Basel, CH-4001 Basel, Switzerland. RP Ortner, DJ (reprint author), Natl Museum Nat Hist, Dept Anthropol, Smithsonian Inst, Washington, DC 20560 USA. EM Ortner.Don@nmnh.sl.edu NR 14 TC 9 Z9 9 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PD MAY PY 2005 VL 127 IS 1 BP 1 EP 6 DI 10.1002/ajpa.20033 PG 6 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 915UQ UT WOS:000228337200001 PM 15386228 ER PT J AU Sorensen, SS Carlson, W AF Sorensen, SS Carlson, W TI An Ernstfest Festschrift: Mineralogy and petrology of high P/T terranes, P-T-ometry, and experimental phase relations SO AMERICAN MINERALOGIST LA English DT Editorial Material C1 Natl Museum Nat Hist, Dept Mineral Sci, Smithsonian Inst, Washington, DC 20560 USA. Univ Texas, Dept Geol Sci, Austin, TX 78712 USA. RP Sorensen, SS (reprint author), Natl Museum Nat Hist, Dept Mineral Sci, Smithsonian Inst, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU MINERALOGICAL SOC AMER PI WASHINGTON PA 1015 EIGHTEENTH ST, NW SUITE 601, WASHINGTON, DC 20036 USA SN 0003-004X J9 AM MINERAL JI Am. Miner. PD MAY-JUN PY 2005 VL 90 IS 5-6 BP 777 EP 778 DI 10.2138/am.2005.446 PG 2 WC Geochemistry & Geophysics; Mineralogy SC Geochemistry & Geophysics; Mineralogy GA 928XN UT WOS:000229305300001 ER PT J AU Eberhard, WG AF Eberhard, WG TI Evolutionary conflicts of interest: Are female sexual decisions different? SO AMERICAN NATURALIST LA English DT Article; Proceedings Paper CT Meeting of the Society-for-the-Study-of-Evolution CY 2003 CL Chico, CA SP Soc Study Evolution DE female choice; sexually antagonistic coevolution; male-female conflict; parent-offspring conflict ID PARENT-OFFSPRING CONFLICT; GENETIC CONFLICTS; MATE CHOICE; SELECTION; PERSPECTIVE; COMPETITION; COEVOLUTION; ADAPTATIONS; RESISTANCE; SEPSIDAE AB Analyses of reproductive conflicts of interests have yielded important evolutionary insights in many areas of biology. The usefulness of conflict analyses of traits that have been traditionally interpreted as resulting from female choice is controversial, however. This article explores a possible explanation for why conflicts of interest may be ameliorated in female choice situations. In contrast to most other evolutionary contexts in which conflicts of interest are thought to have been important, sexual reproduction usually involves an extensive, irretrievable mixing of the genomes of the participants. Under certain combinations of costs and benefits to females, the genes in the female's genome can benefit, through increased reproduction of her offspring, from the very genes that produce sexually antagonistic traits in the male. In short, females can sometimes gain by "losing." Such Fisherian payoffs are also possible, though probably less important, for males. Gaining by losing is not feasible in most other contexts of evolutionary conflict, except under some conditions in parent-offspring conflict. Some apparent parent-offspring conflicts may instead be parental choice among offspring that is analogous to traditional female choice. Parent-offspring conflict may be relatively common, however, because offspring manipulation of their parents is likely to be damaging to the parents. C1 Univ Costa Rica, Smithsonian Trop Res Inst, San Jose, Costa Rica. Univ Costa Rica, Escuela Biol, San Jose, Costa Rica. RP Eberhard, WG (reprint author), Univ Costa Rica, Smithsonian Trop Res Inst, Ciudad Univ, San Jose, Costa Rica. EM archisepsis@biologia.ucr.ac.cr NR 63 TC 23 Z9 23 U1 1 U2 11 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0003-0147 EI 1537-5323 J9 AM NAT JI Am. Nat. PD MAY PY 2005 VL 165 IS 5 SU S BP S19 EP S25 DI 10.1086/429348 PG 7 WC Ecology; Evolutionary Biology SC Environmental Sciences & Ecology; Evolutionary Biology GA 912QO UT WOS:000228094600003 PM 15795858 ER PT J AU Ovruski, SM Norrbom, AL Schliserman, P Aluja, M AF Ovruski, SM Norrbom, AL Schliserman, P Aluja, M TI Biology and taxonomy of Rhagoletotrypeta (Diptera : Tephritidae): A new species from Cuba and new host plant, parasitoid, and distribution records from northwestern Argentina SO ANNALS OF THE ENTOMOLOGICAL SOCIETY OF AMERICA LA English DT Article DE Rhagoletotqjpeta cubensis n. sp.; Tephritidae; Celtis; taxonomy; host plants ID FRUIT-FLIES DIPTERA; FLY; HYMENOPTERA; DIAPAUSE AB Rhagoletotrypeta argentinensis (Aczel) was recovered from Celtis iguanaea (Jacquin) Sargent, and R. parallela Norrbom and R. pastranai Aczel from Celtis pubescens (Kunth) Sprengel fruit (Ulmaceae) in the provinces of Catamarca, Tucuman, and Salta (northwestern Argentina). All represent new host plant records, and for R. parallela, the first host plant record. Mean pupal weight of flies from C. pubescens (mean fruit weight 1.2 g) was 5.2 &PLUSMN; 2.3 mg and of flies from C. iguanaea (mean fruit weight 1.8 g) was 7.8 &PLUSMN; 1.3. Mean degree of infestation (number of larvae/100 g of fruit) was 29.6 for C. iguanaea and varied between 18.7 and 50.5 for C. pubescens. Most adults emerged after an 8-12-mo diapause period. Sixteen specimens of the larval-prepupal parasitoid Utetes sp., near U. anastraphae (Viereck) (Hymenoptera: Braconidae, Opiinae) were recovered from all fruit samples (overall parasitization rate was 37.2%). Parasitoids entered diapause that lasted up to 12 mo. We also describe a new species of Rhagoletotrypeta from Cuba belonging to the xanthogastra species group. Rhagoletotrypeta cubensis Norrbom, n. sp., is the only species in this genus known from the West Indies. The distribution records reported here also extend the known ranges for all four species of Rhagoletotrypeta known from Argentina. We discuss our findings in light of their taxonomic and ecological significance and with respect to the possibilities they open for the badly needed study of the zoogeography and behavior of flies in tephritid genera of no apparent economic importance. C1 Planta Piloto Proc Ind Microbiol & Biotecnol, Div Control Biol Plagas, San Miguel De Tucuman T4001MVB, Argentina. Inst Ecol, Unidad Entomol Aplicada, Xalapa 91000, Veracruz, Mexico. USDA ARS, PSI, Syst Entomol Lab, Smithsonian Inst, Washington, DC 20013 USA. RP Ovruski, SM (reprint author), Planta Piloto Proc Ind Microbiol & Biotecnol, Div Control Biol Plagas, Av Belgrano & Pasaje Caseros, San Miguel De Tucuman T4001MVB, Argentina. EM ovruskisergio@yahoo.com.ar NR 34 TC 1 Z9 2 U1 0 U2 1 PU ENTOMOL SOC AMER PI LANHAM PA 9301 ANNAPOLIS RD, LANHAM, MD 20706 USA SN 0013-8746 J9 ANN ENTOMOL SOC AM JI Ann. Entomol. Soc. Am. PD MAY PY 2005 VL 98 IS 3 BP 252 EP 258 DI 10.1603/0013-8746(2005)098[0252:BATORD]2.0.CO;2 PG 7 WC Entomology SC Entomology GA 924FD UT WOS:000228963400002 ER PT J AU Franceschini, A Manners, J Polletta, MD Lonsdale, C Gonzalez-Solares, E Surace, J Shupe, D Fang, F Xu, CK Farrah, D Berta, S Rodighiero, G Perez-Fournon, I Hatziminaoglou, E Smith, HE Siana, B Rowan-Robinson, M Nandra, K Babbedge, T Vaccari, M Oliver, S Wilkes, B Owen, F Padgett, D Frayer, D Jarrett, T Masci, F Stacey, G Almaini, O McMahon, R Johnson, O Lawrence, A Willott, C AF Franceschini, A Manners, J Polletta, MD Lonsdale, C Gonzalez-Solares, E Surace, J Shupe, D Fang, F Xu, CK Farrah, D Berta, S Rodighiero, G Perez-Fournon, I Hatziminaoglou, E Smith, HE Siana, B Rowan-Robinson, M Nandra, K Babbedge, T Vaccari, M Oliver, S Wilkes, B Owen, F Padgett, D Frayer, D Jarrett, T Masci, F Stacey, G Almaini, O McMahon, R Johnson, O Lawrence, A Willott, C TI A complete multiwavelength characterization of faint CHANDRA X-ray sources seen in the Spitzer Wide-Area Infrared Gxtragalactic (SWIRE) Survey SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies : evolution; quasars : general; X-rays : galaxies ID ACTIVE GALACTIC NUCLEI; DEEP FIELD-SOUTH; SPECTRAL ENERGY-DISTRIBUTIONS; STAR-FORMATION RATE; XMM-NEWTON; PHOTOMETRIC REDSHIFTS; STARBURST GALAXIES; LEGACY SURVEY; NORTH SURVEY; EMISSION AB We exploit deep combined observations with Spitzer and Chandra of the Spitzer Wide-Area Infrared Extragalactic Survey (SWIRE) in the ELAIS N1 region to investigate the nature of the faint X-ray and IR sources in common, to identify active galactic nucleus (AGN)/starburst diagnostics, and to study the sources of the X-ray and IR cosmic backgrounds (XRB and CIRB). In the 17' x 17' area of the Chandra ACIS-I image there are approximately 3400 SWIRE near-IR sources with 4 sigma detections in at least two Infrared Array Camera (IRAC) bands and 988 sources detected at 24 mu m with the Multiband Imaging Photometer (MIPS) brighter than S-24 similar or equal to 0.1 mJy. Of these, 102 IRAC and 59 MIPS sources have Chandra counterparts, out of a total of 122 X-ray sources present in the area with S0.5-8 keV > 10(-15) ergs cm(-2) s(-1). We have constructed spectral energy distributions (SEDs) for each source using data from the four IRAC wavebands, Chandra fluxes in the hard ( 2 - 8 keV) and soft (0.5 - 2 keV) X-rays, and optical follow-up data in the wavebands U, g', r', i', Z, and H. We fit a number of spectral templates to the SEDs at optical and IR wavelengths to determine photometric redshifts and spectral categories and also make use of diagnostics based on the X-ray luminosities, hardness ratios, X-ray to IR spectral slopes, and optical morphologies. Although we have spectroscopic redshifts for only a minority of the Chandra sources ( 10 type 1 QSOs or Seyfert sources and three galaxies), the available SEDs constrain the redshifts for most of the sample sources, which turn out to be typically at 0: 5 < z < 2. We find that 39% of the Chandra sources are dominated by type 1 AGN emission ( QSOs or Seyfert 1), 23% display optical/IR spectra typical of type 2 AGNs, while the remaining 38% show starburst-like or even normal galaxy spectra ( including five passively evolving early-type galaxies). Since we prove that all these galaxies are dominated by AGN emission in X-rays ( considering their large 0.5 - 8 keV rest-frame X-ray luminosities and their high X-ray to IR flux ratios), this brings the fraction of type 1 AGNs to 80% of the type 2 AGNs; even assuming that all the Chandra sources undetected by Spitzer are type 2 AGNs, the type 1 fraction would exceed 1/3 of the total population. Our analysis of the mid-IR MIPS 24 mu m - selected sources, making up similar to 50% of the CIRB, shows that the fraction of those dominated by an AGN ( either type 1 or type 2) is relatively constant with the IR flux and around 10% - 15%. Our combined IR and hard X-ray observations allow us to verify that the dust covering fraction in type 1 AGNs is widely distributed between similar to 10% and 100%. A significant fraction, from 15% to 30% or more, of the sources of the XRB are hosted in galaxies whose optical/IR spectra are dominated by starburst ( or normal galaxy) emission and for which only the hard X-ray spectra reveal the presence of a moderately luminous hidden AGN. C1 Univ Padua, Dipartimento Astron, I-35122 Padua, Italy. Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA. CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. Inst Astrofis Canarias, Tenerife 38200, Spain. Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2BW, England. Univ Sussex, Ctr Astron, Brighton BN1 9QJ, E Sussex, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Natl Radio Astron Observ, Socorro, NM 87801 USA. Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. RP Franceschini, A (reprint author), Univ Padua, Dipartimento Astron, Vicolo Osservatorio 5, I-35122 Padua, Italy. RI Vaccari, Mattia/R-3431-2016; OI McMahon, Richard/0000-0001-8447-8869; Vaccari, Mattia/0000-0002-6748-0577; Polletta, Maria del Carmen/0000-0001-7411-5386; Rodighiero, Giulia/0000-0002-9415-2296; Wilkes, Belinda/0000-0003-1809-2364 NR 65 TC 69 Z9 69 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 MAY PY 2005 VL 129 IS 5 BP 2074 EP 2101 DI 10.1086/428004 PG 28 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 922AG UT WOS:000228807100003 ER PT J AU Blair, WP Sankrit, R Raymond, JC AF Blair, WP Sankrit, R Raymond, JC TI Hubble Space Telescope imaging of the primary shock front in the Cygnus Loop supernova remnant SO ASTRONOMICAL JOURNAL LA English DT Article DE ISM : individual (Cygnus Loop); shock waves; supernova remnants ID NONRADIATIVE SHOCK; OPTICAL-EMISSION; RADIATIVE SHOCKS; NORTHEAST LIMB; WAVE; SPECTRA; STABILITY; NOVA; HI AB We present Hubble Space Telescope WFPC2 narrowband H alpha ( F656N) and [O III] lambda 5007 (F502N) imaging of two fields on the northeastern limb of the Cygnus Loop supernova remnant. This region provides an outstanding example of the initial encounter between the primary blast wave and the surrounding interstellar medium. The H alpha images show the primary nonradiative shock front, which, when viewed edge-on, is unresolved at WFPC2 resolution. The [ O III] images show portions offilaments that are beginning to become radiative, and in these images the filaments are resolved, appearing fuzzy at WFPC2 resolution. The [ O III] filament regions are not bounded directly by H alpha filaments, indicating that the shock emission from the nascent radiative region is sufficient to fully ionize the local preshock gas. One field, imaged 4 yr earlier in H alpha with WFPC2, is used to study the proper motion of the filament and constrain any brightness variations over this time period. In conjunction with improved models of nonradiative shocks, these data are used to place limits on the possible deceleration of the filament and refine the distance to the Cygnus Loop, arriving at a revised value of d = 540(-80)(+100) pc ( assuming no deceleration). The second field imaged contains examples of coherent H alpha filaments with much more dramatic curvatures than identified previously. We discuss the possible reasons for the different morphology of these filaments and conclude that they can be accommodated with relatively modest variations in local density and shock velocity. C1 Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Blair, WP (reprint author), Johns Hopkins Univ, Dept Phys & Astron, 3400 N Charles St, Baltimore, MD 21218 USA. EM wpb@pha.jhu.edu; ravi@pha.jhu.edu; raymond@cfa.harvard.edu NR 24 TC 63 Z9 64 U1 1 U2 2 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 MAY PY 2005 VL 129 IS 5 BP 2268 EP 2280 DI 10.1086/429381 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 922AG UT WOS:000228807100014 ER PT J AU Massarotti, A Latham, DW Torres, G Brown, RA Oppenheimer, BD AF Massarotti, A Latham, DW Torres, G Brown, RA Oppenheimer, BD TI A search for substellar companions around 15 weak-lined T Tauri stars with the Planetary Camera 2 of the Hubble Space Telescope SO ASTRONOMICAL JOURNAL LA English DT Article DE binaries : spectroscopic; planetary systems; stars : imaging; stars : low-mass, brown dwarfs; stars : pre-main-sequence ID MAIN-SEQUENCE STARS; X-RAY SOURCES; EXTRASOLAR GIANT PLANETS; BROWN DWARF COMPANION; LOW-MASS STARS; SPECTROSCOPIC BINARIES; RADIAL-VELOCITIES; FORMING REGIONS; IMAGING SURVEY; YOUNG STARS AB To search for thermal emission from substellar companions, we have obtained Z-band images of 15 weak-lined T Tauri stars in the Taurus-Auriga and Ophiuchus star-forming regions using the Planetary Camera 2 on the Hubble Space Telescope. We found 18 faint nearby objects at separations larger than 4 '' but none at smaller separations. For 11 of these we have enough color information to suggest that they are not substellar members of the star-forming regions. The remaining seven faint nearby objects are candidate substellar objects. Our detection limit for companions with separations larger than about 1 '' is apparent Z = 19.5 mag, corresponding to substellar objects in the mass range 3M(J) - 15M(J) for the age range of our targets, 1.2 - 25 Myr. Our detection limit degrades for smaller separations and is 4 - 6 mag poorer at a separation of 0.'' 2, corresponding to a projected separation of 30 AU. Inside 0.'' 2 our sensitivity is insufficient to detect substellar companions. To complement the imaging program, extensive spectroscopic observations were obtained with the Center for Astrophysics Digital Speedometers. Four of our targets proved to be spectroscopic binaries, one of them double-lined. We report orbital solutions for these four stars. Our radial velocities support the membership of all our targets to their respective star-forming regions, except for HD 283759, which must be rejected as a member. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Stonehill Coll, Dept Phys & Astron, Easton, MA 02357 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Harvard Univ, Dept Astron, Cambridge, MA 02138 USA. RP Massarotti, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM amassaro@cfa.harvard.edu; dlatham@cfa.harvard.edu; gtorres@cfa.harvard.edu; rbrown@stsci.edu; boppenheimer@as.arizona.edu NR 48 TC 17 Z9 17 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 MAY PY 2005 VL 129 IS 5 BP 2294 EP 2307 DI 10.1086/429349 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 922AG UT WOS:000228807100016 ER PT J AU Matheson, T Blondin, S Foley, RJ Chornock, R Filippenko, AV Leibundgut, B Smith, RC Sollerman, J Spyromilio, J Kirshner, RP Clocchiatti, A Aguilera, C Barris, B Becker, AC Challis, P Covarrubias, R Garnavich, P Hicken, M Jha, S Krisciunas, K Li, WD Miceli, A Miknaitis, G Prieto, JL Rest, A Riess, AG Salvo, ME Schmidt, BP Stubbs, CW Suntzeff, NB Tonry, JL AF Matheson, T Blondin, S Foley, RJ Chornock, R Filippenko, AV Leibundgut, B Smith, RC Sollerman, J Spyromilio, J Kirshner, RP Clocchiatti, A Aguilera, C Barris, B Becker, AC Challis, P Covarrubias, R Garnavich, P Hicken, M Jha, S Krisciunas, K Li, WD Miceli, A Miknaitis, G Prieto, JL Rest, A Riess, AG Salvo, ME Schmidt, BP Stubbs, CW Suntzeff, NB Tonry, JL TI Spectroscopy of high-redshift supernovae from the essence project: The first 2 years SO ASTRONOMICAL JOURNAL LA English DT Article DE distance scale; galaxies : distances and redshifts; supernovae : general ID HUBBLE-SPACE-TELESCOPE; IA SUPERNOVAE; ACCELERATING UNIVERSE; OPTICAL-SPECTRA; SPECTROGRAPH; DECELERATION; CONSTRAINTS; IDENTIFICATION; RESOLUTION; EVOLUTION AB We present the results of spectroscopic observations of targets discovered during the first 2 years of the ESSENCE project. The goal of ESSENCE is to use a sample of similar to 200 Type Ia supernovae (SNe Ia) at moderate redshifts (0.2 less than or similar to z less than or similar to 0.8) to place constraints on the equation of state of the universe. Spectroscopy not only provides the redshifts of the objects but also confirms that some of the discoveries are indeed SNe Ia. This confirmation is critical to the project, as techniques developed to determine luminosity distances to SNe Ia depend on the knowledge that the objects at high redshift have the same properties as the ones at low redshift. We describe the methods of target selection and prioritization, the telescopes and detectors, and the software used to identify objects. The redshifts deduced from spectral matching of high-redshift SNe Ia with low-redshift SNe Ia are consistent with those determined from host-galaxy spectra. We show that the high-redshift SNe Ia match well with low-redshift templates. We include all spectra obtained by the ESSENCE project, including 52 SNe Ia, five core-collapse SNe, 12 active galactic nuclei, 19 galaxies, four possibly variable stars, and 16 objects with uncertain identifications. C1 Natl Opt Astron Observ, Tucson, AZ 85719 USA. European So Observ, D-85748 Garching, Germany. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Cerro Tololo Interamer Observ, Natl Opt Astron Observ, La Serena, Chile. Stockholm Observ, AlbaNova Univ Ctr, SE-10691 Stockholm, Sweden. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 22, Chile. Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. Univ Washington, Dept Astron, Seattle, WA 98195 USA. Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. Univ Washington, Dept Phys, Seattle, WA 98195 USA. Ohio State Univ, Dept Astron, McPherson Lab 4055, Columbus, OH 43210 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Australian Natl Univ, Mt Stromlo & Siding Spring Observ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. RP Matheson, T (reprint author), Natl Opt Astron Observ, 950 N Cherry Ave, Tucson, AZ 85719 USA. EM matheson@noao.edu; sblondin@eso.org; rfoley@astro.berkeley.edu; chornock@astro.berkeley.edu; alex@astro.berkeley.edu; bleibund@eso.org; csmith@noao.edu; jesper@astro.su.se; jspyromi@eso.org; kirshner@cfa.harvard.edu; aclocchi@astro.puc.cl; caguilera@ctio.noao.edu; barris@ifa.hawaii.edu; becker@astro.washington.edu; pchallis@cfa.harvard.edu; ricardo@astro.washington.edu; pgarnavi@nd.edu; mhicken@cfa.harvard.edu; sjha@astro.berkeley.edu; kkrisciu@nd.edu; weidong@astro.berkeley.edu; amiceli@astro.washington.edu; gm@u.washington.edu; prieto@astronomy.ohio-state.edu; arest@noao.edu; ariess@stsci.edu; salvo@mso.anu.edu.au; brian@mso.anu.edu.au; cstubbs@fas.harvard.edu; nsuntzeff@noao.edu; jt@ifa.hawaii.edu RI Stubbs, Christopher/C-2829-2012; OI Stubbs, Christopher/0000-0003-0347-1724; Schmidt, Brian/0000-0001-6589-1287; Sollerman, Jesper/0000-0003-1546-6615; Schmidt, Brian/0000-0002-8538-9195 NR 50 TC 50 Z9 50 U1 0 U2 2 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 MAY PY 2005 VL 129 IS 5 BP 2352 EP 2375 DI 10.1086/429679 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 922AG UT WOS:000228807100018 ER PT J AU Jorgensen, JK Schoier, FL van Dishoeck, EF AF Jorgensen, JK Schoier, FL van Dishoeck, EF TI Molecular freeze-out as a tracer of the thermal and dynamical evolution of pre- and protostellar cores SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars : formation; ISM : molecules; ISM : abundances ID MASS STAR-FORMATION; CHEMICAL EVOLUTION; CHEMISTRY; ENVELOPES; PROTOSTARS; ABUNDANCE; EMISSION; COLLAPSE; CLOUDS; LINE AB Radiative transfer models of multi-transition observations are used to determine molecular abundances as functions of position in pre- and protostellar cores. The data require a "drop" abundance profile with radius, with high abundances in the outermost regions probed by low excitation 3 mm lines, and much lower abundances at intermediate zones probed by higher frequency lines. The results are illustrated by detailed analysis of CO and HCO+ lines for a subset of objects. We propose a scenario in which the molecules are frozen out in a region of the envelope where the temperature is low enough (less than or similar to 40 K) to prevent immediate desorption, but where the density is high enough (> 10(4) - 10(5) cm(-3)) that the freeze-out timescales are shorter than the lifetime of the core. The size of the freeze-out zone is thereby a record of the thermal and dynamical evolution of the cores. Fits to CO data for a sample of 16 objects indicate that the size of the freeze-out zone decreases significantly between class 0 and I objects, explaining the variations in, for example, CO abundances with envelope masses. However, the corresponding timescales are 10(5 +/- 0.5) years, with no significant difference between class 0 and I objects. These timescales suggest that the dense pre- stellar phase with heavy depletions lasts only a short time, of the order of 10(5) yr, in agreement with recent chemical-dynamical models. C1 Leiden Observ, NL-2300 RA Leiden, Netherlands. Stockholm Observ, S-10691 Stockholm, Sweden. RP Jorgensen, JK (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St MS42, Cambridge, MA 02138 USA. EM jjorgensen@cfa.harvard.edu NR 32 TC 50 Z9 50 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 MAY PY 2005 VL 435 IS 1 BP 177 EP 182 DI 10.1051/0004-6361:20042092 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 920LM UT WOS:000228690500022 ER PT J AU Verhoelst, T Borde, PJ Perrin, G Decin, L Eriksson, K Ridgway, ST Schuller, PA Traub, WA Millan-Gabet, R Lacasse, MG Waelkens, C AF Verhoelst, T Borde, PJ Perrin, G Decin, L Eriksson, K Ridgway, ST Schuller, PA Traub, WA Millan-Gabet, R Lacasse, MG Waelkens, C TI Is Arcturus a well-understood K giant? Test of model atmospheres and potential companion detection by near-infrared interferometry SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE techniques : interferometric; stars : individual : Arcturus; stars : atmospheres; stars : binaries : general ID SPECTRAL IRRADIANCE CALIBRATION; COOL-STAR ATMOSPHERES; ISO-SWS CALIBRATION; RADIAL-VELOCITY; IOTA INTERFEROMETER; WATER-VAPOR; LONG-PERIOD; INSTRUMENT; VARIABLES; CONFIRMATION AB We present near-IR interferometric measurements of the K1.5 giant Arcturus (alpha Bootis), obtained at the IOTA interferometer with the FLUOR instrument, in four narrow filters with central wavelengths ranging from 2.03 mu m to 2.39 mu m. These observations were expected to allow us to quantify the wavelength dependence of the diameter of a typical K giant. They are compared to predictions from both plane-parallel and spherical model atmospheres. Unexpectedly, neither can explain the observed visibilities. We show that these data suggest the presence of a companion, in accordance with the Hipparcos data on this star, and discuss this solution with respect to Arcturus' single star status. C1 Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Observ Paris, LESIA, F-92195 Meudon, France. Inst Astron & Space Phys, S-75120 Uppsala, Sweden. Natl Opt Astron Observ, Tucson, AZ 85726 USA. CALTECH, Michelson Sci Ctr, Pasadena, CA 91125 USA. RP Verhoelst, T (reprint author), Katholieke Univ Leuven, Inst Sterrenkunde, Celestijnenlaan 200B, B-3001 Louvain, Belgium. EM Tijl.verhoelst@ster.kuleuven.ac.be NR 56 TC 12 Z9 12 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 MAY PY 2005 VL 435 IS 1 BP 289 EP 301 DI 10.1051/0004-6361:20042356 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 920LM UT WOS:000228690500034 ER PT J AU Werner, K Drake, JJ AF Werner, K Drake, JJ TI Line identification in soft X-ray spectra of stellar coronae by comparison with the hottest white dwarf's photosphere: Procyon, alpha Cen A+B, and H1504+65 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars : atmospheres; stars : coronae; X-rays : stars; stars : individual H1504+65 ID EXTREME-ULTRAVIOLET REGION; SOLAR SPECTRUM; EMISSION-LINES; FE-VII; ANGSTROM; CHANDRA; SPECTROSCOPY; ABUNDANCES; CENTAURI AB H1504+ 65 is a young white dwarf with an effective temperature of 200 000 K and is the hottest post- AGB star ever analysed with detailed model atmospheres. Chandra LETG+ HRC- S spectra have revealed the richest X- ray absorption line spectrum recorded from a stellar photosphere to date. The line forming regions in this extremely hot photosphere produce many transitions in absorption that are also observed in emission in cool star coronae. We have performed a detailed comparison of Chandra spectra of H1504+ 65 with those of Procyon and alpha Cen A and B. State of the art non- LTE model spectra for the hot white dwarf have enabled us to identify a wealth of absorption lines from highly ionized O, Ne and Mg. In turn, these features have allowed us to identify coronal lines whose origins were hitherto unknown. C1 Univ Tubingen, Inst Astron & Astrophys, D-72076 Tubingen, Germany. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Werner, K (reprint author), Univ Tubingen, Inst Astron & Astrophys, Sand 1, D-72076 Tubingen, Germany. EM werner@astro.uni-tuebingen.de NR 20 TC 2 Z9 2 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 MAY PY 2005 VL 434 IS 2 BP 707 EP 712 DI 10.1051/0004-6361:20042057 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 915SO UT WOS:000228326900031 ER PT J AU Fruscione, A Greenhill, LJ Filippenko, AV Moran, JM Herrnstein, JR Galle, E AF Fruscione, A Greenhill, LJ Filippenko, AV Moran, JM Herrnstein, JR Galle, E TI X-ray luminosity and absorption column fluctuations in the H2O maser galaxy NGC 4258 from weeks to years SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; galaxies : active; galaxies : individual (NGC 4258); galaxies : Seyfert; X-rays : galaxies ID ACTIVE GALACTIC NUCLEI; SEYFERT 2 GALAXIES; NGC 4258; ANOMALOUS ARMS; ACCRETION RATE; BEPPOSAX VIEW; BLACK-HOLE; DISK; EMISSION; JET AB We report monitoring of the 0.3 - 10 keV spectrum of NGC 4258 with the XMM-Newton Observatory at five epochs over 1.5 yr. We also report reprocessing of an overlapping four-epoch series of archival Chandra observations (0.5 - 10 keV). By including earlier ASCA and BeppoSAX observations, we present a new, 9 year time series of models fitted to the X-ray spectrum of NGC 4258. We model the Chandra and XMM-Newton data self-consistently with partially absorbed, hard power-law, soft thermal plasma, and soft power-law components. Over the 9 years, the photoelectric absorbing column (similar to 10(23) cm(-2)) did not vary detectably, except for a similar to 40% drop between two ASCA epochs separated by 3 years ( in 1993 and 1996) and a similar to 60% rise between two XMM-Newton epochs separated by just 5 months ( in 2001 and 2002). In contrast, factor of 2 - 3 changes are seen in absorbed flux on the timescale of years. These are uncorrelated with changes in absorbing column and indicative of central engine variability. The most rapid change in luminosity ( 5 - 10 keV) that we detect ( with XMM-Newton and Chandra) is similar to 30% over 19 days. The warped disk, a known source of H2O maser emission in NGC 4258, is believed to cross the line of sight to the central engine. We propose that the variations in absorbing column arise from inhomogeneities sweeping across the line of sight in the rotating disk at the radius at which the disk crosses the line of sight. We estimate that the inhomogeneities are similar to 10(15) cm in size at the crossing radius of 0.29 pc, slightly smaller than the expected scale height of the disk. This result thus provides strong evidence that the warped accretion disk is the absorber in this ( and possibly other) active galactic nuclei (AGNs). This is the first direct confirmation that obscuration in type 2 AGNs may, in some cases, arise in thin, warped accretion disks rather than in geometrically thick tori. Some previous studies report detection of weak Fe K alpha emission in NGC 4258. We do not detect this line emission in any of our XMM-Newton spectra with a 90% upper limit to the equivalent width of similar to 49 eV for one observation. Weak, time-variable Fe line absorption has also been reported for a previous Chandra study. We do not observe evidence of absorption lines in the XMM-Newton or reprocessed Chandra data. The absence of Fe line emission is consistent with the disk being optically thin to hard photons, as well as subtending a small solid angle as seen from the central engine because of the known shallowness of the warp. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Renaissance Technol Inc, E Setauket, NY 11733 USA. RP Fruscione, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM afruscione@cfa.harvard.edu; greenhill@cfa.harvard.edu; alex@astro.berkeley.edu; moran@cfa.harvard.edu; jrh@rentec.com; egalle@cfa.harvard.edu NR 47 TC 28 Z9 28 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 MAY 1 PY 2005 VL 624 IS 1 BP 103 EP 117 DI 10.1086/428658 PN 1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 918OI UT WOS:000228554200013 ER PT J AU Schnee, S Goodman, A AF Schnee, S Goodman, A TI Density and temperature structure of TMC-1C from 450 and 850 micron maps SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; stars : formation; submillimeter ID MOLECULAR CLOUD CORES; CLERK-MAXWELL-TELESCOPE; MASS STAR-FORMATION; AMBIPOLAR DIFFUSION; DARK CLOUDS; AXISYMMETRICAL SOLUTIONS; PROTOSTELLAR COLLAPSE; CLUMP DISTRIBUTION; INITIAL CONDITIONS; INTERSTELLAR DUST AB We have mapped the central 100; 100 of the dense core TMC-1C at 450 and 850 mu m using SCUBA on the James Clerk Maxwell Telescope. The unusually high quality of the 450 mu m map allows us to make a detailed analysis of the temperature and column density profiles of the core. We find that the dust temperature at the center of TMC-1C is similar to 7 K, rising to similar to 11 K at the edges. We discuss the possibility and effects of a variable emissivity spectral index on the derived mass profile. The low dust temperature of TMC-1C results in a high derived mass for the core, significantly larger than the virial mass estimated from the line width of the N2H+ ( 1 - 0) transition. This result is valid within a wide range of dust properties and ellipticities of the core. The N2H+ ( 1 - 0) spectra, taken with the IRAM 30 m telescope, show signs of self-absorption, which provide evidence of subsonic infall motions. The derived density profile and infall velocity are compared to the predictions of several popular star formation models, and the Bonnor-Ebert model is the best-fit analytic model. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Schnee, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM sschnee@cfa.harvard.edu RI Goodman, Alyssa/A-6007-2010 OI Goodman, Alyssa/0000-0003-1312-0477 NR 55 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 MAY 1 PY 2005 VL 624 IS 1 BP 254 EP 266 DI 10.1086/429156 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 918OI UT WOS:000228554200027 ER PT J AU Konacki, M Torres, G Sasselov, DD Jha, S AF Konacki, M Torres, G Sasselov, DD Jha, S TI A transiting extrasolar giant planet around the star OGLE-TR-10 SO ASTROPHYSICAL JOURNAL LA English DT Article DE line : profiles; planetary systems; stars : evolution; stars : individual (OGLE-TR-10); techniques : radial velocities ID GRAVITATIONAL LENSING EXPERIMENT; LUMINOSITY OBJECT TRANSITS; TESTING BLEND SCENARIOS; GALACTIC DISK; 2001 CAMPAIGN; PARENT STAR; FOLLOW-UP; CANDIDATES; PARAMETERS; TELESCOPE AB We report a transiting extrasolar giant planet around the star OGLE-TR-10 (orbital period = 3.1 days), which was uncovered as a candidate by the OGLE team in their photometric survey toward the Galactic center. We observed OGLE-TR- 10 spectroscopically over a period of 2 yr ( 2002 - 2004), using the HIRES instrument with an iodine cell on the Keck I telescope, and measured small radial velocity variations that are consistent with the presence of a planetary companion. This confirms the earlier identification of OGLE-TR- 10b by our team and also recently by Bouchy and coworkers as a possible planet. In addition, in this paper we are able to rule out a blend scenario as an alternative explanation. From an analysis combining all available radial velocity measurements with the OGLE light curve, we find that OGLE-TR- 10b has a mass of 0.57 +/- 0.12M(J) and a radius of 1.24 +/- 0.09R(J). These parameters bear close resemblance to those of the first known transiting extrasolar planet, HD 209458b. C1 CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. RP Konacki, M (reprint author), CALTECH, Div Geol & Planetary Sci, MS 150-21, Pasadena, CA 91125 USA. EM maciej@gps.caltech.edu RI Konacki, Maciej/A-1220-2007 NR 29 TC 77 Z9 78 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 MAY 1 PY 2005 VL 624 IS 1 BP 372 EP 377 DI 10.1086/429127 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 918OI UT WOS:000228554200036 ER PT J AU Sollins, PK Zhang, QH Keto, E Ho, PTP AF Sollins, PK Zhang, QH Keto, E Ho, PTP TI Spherical infall in G10.6-0.4: Accretion through an ultracompact HII region SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; HII regions; ISM : individual (G10.6-0.4); stars : formation ID MASSIVE STAR-FORMATION; H-II REGIONS; CORE; EVOLUTION; FLOW; MAPS; GAS AB We present high-resolution (0.'' 12 x 0.'' 079) observations of the ultracompact H II region G10.6 - 0.4 in 23 GHz radio continuum and the NH3 (3, 3) line. Our data show that the infall in the molecular material is largely spherical and does not flatten into a thin disk at radii as small as 0.03 pc. The spherical infall in the molecular gas matches in location and velocity the infall seen in the ionized gas. We use a nondetection to place a stringent upper limit on the mass of an expanding molecular shell associated with pressure-driven expansion of the H II region. These data support a scenario in which the molecular accretion flow passes through the ionization front and becomes an ionized accretion flow onto one or more main-sequence stars, not the classical pressure-driven expansion scenario. In the continuum emission, we see evidence for externally ionized clumps of molecular gas and cavities evacuated by an outflow from the central source. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Sollins, PK (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM psollins@cfa.harvard.edu OI Zhang, Qizhou/0000-0003-2384-6589 NR 25 TC 39 Z9 39 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 MAY 1 PY 2005 VL 624 IS 1 BP L49 EP L52 DI 10.1086/430270 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 918OJ UT WOS:000228554300013 ER PT J AU Iono, D Yun, MS Ho, PTP AF Iono, D Yun, MS Ho, PTP TI Atomic and molecular gas in colliding galaxy systems. I. The data SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE galaxies : evolution; galaxies : individual (NGC 5257/5258; NGC 5394/5395, UGC 12914/12915, NGC 5331; NGC 6621/6622, UGC 813/816, NGC 7253/7254; NGC 4567/4568, NGC 7592, NGC 5953/5954); galaxies : interactions; galaxies : ISM; galaxies : kinematics and dynamics ID LUMINOUS INFRARED GALAXIES; STAR-FORMATION RATES; INTERACTING GALAXIES; SPIRAL GALAXIES; GLOBAL PROPERTIES; NEUTRAL HYDROGEN; CENTRAL REGIONS; CO OBSERVATIONS; ARP 220; SAMPLE AB We present H I and CO (1-0) interferometric observations of 10 comparable-mass interacting systems obtained at the Very Large Array (VLA) and the Owens Valley Radio Observatory (OVRO) millimeter array. The primary intent of this study is to investigate the response of cold gas during the early stages of collision of massive disk galaxies. The sample sources are selected based on their luminosity (M-B <= -19), projected separation (5-40 kpc), and single-dish CO (1-0) content (S-CO >= 20 Jy km s(-1)). These selection criteria result in a sample that primarily consists of systems in the early stages of an interaction or a merger. Despite this sample selection, 50% of the systems show long H I tidal tails indicative of a tidal disruption in a prograde orbit. In addition, all (4/4) of the infrared luminous pairs (LIRGs) in the sample show long H I tails, suggesting that the presence of a long H I tail can be a possible signature of enhanced star formation activity in a collision of gas-rich galaxies. More than half of the groups show a displacement of H I peaks from the stellar disks. The CO (1-0) distribution is generally clumpy and widely distributed, unlike in most IR-selected late stage mergers - in fact, CO peaks are displaced from the stellar nucleus in 20% (4/18) of the galaxies with robust CO detection. H I and CO (1-0) position-velocity diagrams (PVDs) and rotation curves are also presented, and their comparison with the numerical simulation analyzed in Paper I show evidence for radial inflow and wide occurrences of nuclear molecular rings. These results are further quantified by examining physical and structural parameters derived in comparison with isolated systems in the BIMA SONG sample in our forthcoming paper. C1 Univ Massachusetts, Dept Astron, Amherst, MA 01002 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Smithsonian Astrophys Observ, Cambridge, MA USA. RP Univ Massachusetts, Dept Astron, Amherst, MA 01002 USA. NR 81 TC 34 Z9 34 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 EI 1538-4365 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD MAY PY 2005 VL 158 IS 1 BP 1 EP 37 DI 10.1086/429093 PG 37 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 922AF UT WOS:000228807000001 ER PT J AU Lidgard, DC Boness, DJ Bowen, WD McMillan, JI AF Lidgard, DC Boness, DJ Bowen, WD McMillan, JI TI State-dependent male mating tactics in the grey seal: the importance of body size SO BEHAVIORAL ECOLOGY LA English DT Article DE body size; conditional mating tactics; endurance rivalry; energetics; Halichoerus grypus; pinnipeds; reproductive behavior ID HYDROGEN-ISOTOPE-DILUTION; MALE REPRODUCTIVE SUCCESS; NORTHERN ELEPHANT SEALS; ANTARCTIC FUR SEALS; HALICHOERUS-GRYPUS; SEXUAL SELECTION; GRAY SEALS; LACTATION PERFORMANCE; MESOCRICETUS-AURATUS; RANA-CATESBEIANA AB The purpose of this study was to examine the importance of body size and body composition as determinants of conditional mating tactics exhibited in male grey seals. We combined behavioral observations with measures of energy expenditure and success on 42 known-age individuals during the breeding seasons of 1997-2001 at Sable Island, Canada. Males with a large body mass arrived at the breeding grounds with more body fat and body energy and catabolized less body protein than smaller males. Males consumed 1.9 +/- 0.2 MJ day(-1), and those with a smaller percentage of body fat had higher rates of food energy intake. The amount of body energy on arrival was positively correlated with the duration of the breeding period. Males that exhibited the primary mating tactic of consortship were heavier, had absolutely more body fat and body energy, and sustained breeding longer than those males that did not exhibit the primary tactic. Amongst all males, body mass showed a quadratic relationship with the number of female consorts mated and the estimated number of pups sired. Thus, intermediate-sized males mated with the most consorts and achieved the highest success. Intermediate body size may be optimal during breeding due to greater agility in male combat. Body size was an important determinant of mating tactics used by male grey seals. A large body size provided an energetic advantage of greater endurance while an intermediate body size may provide greater competitive ability in acquiring consortships. C1 Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, Washington, DC 20008 USA. Univ La Rochelle, Lab Biol & Environm Marins, F-17000 La Rochelle, France. Fisheries & Oceans Canada, Bedford Inst Oceanog, Marine Fish Div, Dartmouth, NS B2Y 4A2, Canada. RP Lidgard, DC (reprint author), Dalhousie Univ, Dept Biol, Halifax, NS B3H 4J1, Canada. EM damian.lidgard@dal.ca RI Bowen, William/D-2758-2012 NR 75 TC 37 Z9 38 U1 3 U2 16 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1045-2249 J9 BEHAV ECOL JI Behav. Ecol. PD MAY PY 2005 VL 16 IS 3 BP 541 EP 549 DI 10.1093/beheco/ari023 PG 9 WC Behavioral Sciences; Biology; Ecology; Zoology SC Behavioral Sciences; Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Zoology GA 916RA UT WOS:000228402100007 ER PT J AU Shapiro, JA von Sternberg, R AF Shapiro, JA von Sternberg, R TI Why repetitive DNA is essential to genome function SO BIOLOGICAL REVIEWS LA English DT Review DE transposable element; non-coding DNA; satellite DNA; junk DNA; transcriptional regulation; chromatin domains; evolution; biocomputing; systems biology; data storage ID POSITION-EFFECT VARIEGATION; OUTER-MEMBRANE PROTEIN; CLASS-SWITCH RECOMBINATION; MATRIX-ATTACHMENT REGIONS; X-CHROMOSOME INACTIVATION; TRANSCRIPTION FACTOR YY1; ALPHA-SATELLITE DNA; TRANSPOSABLE ELEMENTS; NEISSERIA-MENINGITIDIS; DROSOPHILA-MELANOGASTER AB There are clear theoretical reasons and many well-documented examples which show that repetitive DNA is essential for genome function. Generic repeated signals in the DNA are necessary to format expression of unique coding sequence files and to organise additional functions essential for genome replication and accurate transmission to progeny cells. Repetitive DNA sequence elements are also fundamental to the cooperative molecular interactions forming nucleoprotein complexes. Here, we review the surprising abundance of repetitive DNA in many genomes, describe its structural diversity, and discuss dozens of cases where the functional importance of repetitive elements has been studied in molecular detail. In particular, the fact that repeat elements serve either as initiators or boundaries for heterochromatin domains and provide a significant fraction of scaffolding/matrix attachment regions (S/MARs) suggests that the repetitive 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 organisation of cellular genomes and provides several novel possibilities involving repeat elements in evolutionarily significant genome reorganisation. These ideas may facilitate the interpretation of comparisons between sequenced genomes, where the repetitive DNA component is often greater than the coding sequence component. C1 Univ Chicago, Dept Biochem & Mol Biol, Chicago, IL 60637 USA. NIH, Natl Ctr Biotechnol Informat, Bethesda, MD 20894 USA. Natl Museum Nat Hist, Smithsonian Inst, Dept Syst Biol, Washington, DC 20013 USA. RP Shapiro, JA (reprint author), Univ Chicago, Dept Biochem & Mol Biol, 920 E 58th St, Chicago, IL 60637 USA. EM jsha@uchicago.edu; sternber@ncbi.nlm.nih.gov NR 246 TC 74 Z9 77 U1 3 U2 38 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1464-7931 EI 1469-185X J9 BIOL REV JI Biol. Rev. PD MAY PY 2005 VL 80 IS 2 BP 227 EP 250 DI 10.1017/S1464793104006657 PG 24 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 928NT UT WOS:000229279300003 PM 15921050 ER PT J AU Feitoza, BM Rosa, RS Rocha, LA AF Feitoza, BM Rosa, RS Rocha, LA TI Ecology and zoogeography of deepreef fishes in northeastern Brazil SO BULLETIN OF MARINE SCIENCE LA English DT Article ID REEF FISHES; CONTINENTAL-SHELF; MARSHALL-ISLANDS; ABUNDANCE; ASSEMBLAGES; TRANSPORT; PATTERNS; ENEWETAK; OREGON; DEPTH AB With the advent of SCUBA, the reef fish fauna has been substantially studied around the world, but the great majority of in situ studies have focused exclusively on a limited portion of this fauna, to depths of < 30 m. The present study represents the first SCUBA- based survey of the deep reef fishes off the Brazilian coast between 35 and 70 m. A species list was compiled based on visual observations, collections, video recording, and fishes obtained from commercial fishing boats. A total of 158 fish species belonging to 49 families was recorded. Thirty-two species were formally recorded for the first time from the study area, four of which [Apogon robbyi Gilbert, 1997; Coryphopterus eidolon Bohlke & Robins, 1960; Psilotris batrachodes Bohlke, 1963; and Xanthichthys ringens (Linnaeus, 1758)] represent new records for the western South Atlantic. Fifty-seven species had their depth range extended to depths > 40 m. The most species rich families were Carangidae (14 species), Gobiidae (12), Lutjanidae (11), Labridae (11), Serranidae (10), Haemulidae (8), and Scaridae (7). The presence of several species previously considered to have disjunct, or anti-equatorial distribution, indicates that the deep reefs may function as a faunal corridor between habitats in southeastern Brazil and the Caribbean. C1 Univ Florida, Florida Museum Nat Hist, Gainesville, FL 32653 USA. Smithsonian Trop Res Inst, Naos Lab, Unit 0948, Miami, FL 34002 USA. Univ Fed Paraiba, CCEN, Depto Sistemat & Ecol, BR-58059900 Joao Pessoa, Paraiba, Brazil. RP Rocha, LA (reprint author), Univ Florida, Florida Museum Nat Hist, Gainesville, FL 32653 USA. EM RochaL@naos.si.edu RI Rocha, Luiz/C-5107-2011; Rosa, Ricardo/C-8266-2014 OI Rosa, Ricardo/0000-0002-4289-2241 NR 58 TC 43 Z9 48 U1 0 U2 8 PU ROSENSTIEL SCH MAR ATMOS SCI PI MIAMI PA 4600 RICKENBACKER CAUSEWAY, MIAMI, FL 33149 USA SN 0007-4977 EI 1553-6955 J9 B MAR SCI JI Bull. Mar. Sci. PD MAY PY 2005 VL 76 IS 3 BP 725 EP 742 PG 18 WC Marine & Freshwater Biology; Oceanography SC Marine & Freshwater Biology; Oceanography GA 932SM UT WOS:000229573700010 ER PT J AU Braun, MJ Isler, ML Isler, PR Bates, JM Robbins, MB AF Braun, MJ Isler, ML Isler, PR Bates, JM Robbins, MB TI Avian speciation in the Pantepui: The case of the Roraiman Antbird (Percnostola [Schistocichla] "leucostigma" saturata) SO CONDOR LA English DT Article DE biodiversity; Neotropics; Percnostola; speciation; systematics; tepuis; Thamnophilidae ID SPECIES LIMITS; THAMNOPHILIDAE; AVES; PASSERIFORMES; BIRDS; DENDROCOLAPTIDAE; DIVERSIFICATION; COMPLEX; ANDES; ZONE AB We document the first records for Guyana of Roraiman Antbird (Percnostola [Schistocichla] "leucostigma" saturata), an endemic of the tepui highlands of southeastern Venezuela, northern Brazil and western Guyana. This form is well differentiated from nominate leucostigma (Spot-winged Antbird) of the Guianan lowlands in morphology, vocalizations, and genetics, and replaces it both altitudinally and ecologically. The two taxa are distributed parapatrically on the continuously forested northeastern slopes of the eastern tepuis, and they almost certainly come into contact, yet there is no evidence of intermediacy. We recommend that saturata be treated as a distinct species of Percnostola, and consider its ' origin in the light of various models of speciation in the tepuis. C1 Smithsonian Inst, Dept Vertebrate Zool, Natl Museum Nat Hist, Suitland, MD 20746 USA. Natl Museum Nat Hist, Dept Vertebrate Zool Birds, Washington, DC 20560 USA. Field Museum Nat Hist, Dept Zool, Chicago, IL 60605 USA. Univ Kansas, Museum Nat Hist, Div Birds, Lawrence, KS 66045 USA. RP Braun, MJ (reprint author), Smithsonian Inst, Dept Vertebrate Zool, Natl Museum Nat Hist, 4210 Silver Hill Rd, Suitland, MD 20746 USA. EM braun@lab.si.edu NR 65 TC 14 Z9 15 U1 0 U2 2 PU COOPER ORNITHOLOGICAL SOC PI LAWRENCE PA ORNITHOLOGICAL SOC NORTH AMER PO BOX 1897, LAWRENCE, KS 66044-8897 USA SN 0010-5422 J9 CONDOR JI Condor PD MAY PY 2005 VL 107 IS 2 BP 327 EP 341 DI 10.1650/7647 PG 15 WC Ornithology SC Zoology GA 926PT UT WOS:000229135800012 ER PT J AU Bowring, SA Erwin, D Parrish, R Renne, P AF Bowring, SA Erwin, D Parrish, R Renne, P TI EARTHTIME: A community-based effort towards high-precision calibration of earth history SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 15th Annual V M Goldschmidt Conference CY MAY, 2005 CL Moscow, ID C1 MIT, EAPS, Cambridge, MA 02319 USA. Smithsonian Inst, NMNH, Washington, DC 20560 USA. NIGL, Keyworth, Notts, England. BGC, Berkeley, CA 94709 USA. EM sbowring@mit.edu RI Erwin, Douglas/A-9668-2009; Parrish, Randall/A-3787-2010 NR 0 TC 4 Z9 4 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD MAY PY 2005 VL 69 IS 10 SU S BP A316 EP A316 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 930EX UT WOS:000229399701022 ER PT J AU Lopano, CL Heaney, PJ Post, JE Brantley, SL AF Lopano, CL Heaney, PJ Post, JE Brantley, SL TI Determination of cation exchange rates in synthetic birnessite using time-resolved synchrotron X-ray diffraction SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 15th Annual V M Goldschmidt Conference CY MAY, 2005 CL Moscow, ID C1 Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. EM clopano@geosc.psu.edu; heaney@geosc.psu.edu; post.jeffrey@nmnh.si.edu; brantley@essc.psu.edu NR 0 TC 1 Z9 1 U1 0 U2 1 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD MAY PY 2005 VL 69 IS 10 SU S BP A623 EP A623 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 930EX UT WOS:000229399702026 ER PT J AU Peslier, AH Luhr, JF AF Peslier, AH Luhr, JF TI Water contents in anhydrous minerals from the upper-mantle (peridotites and eclogites) SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 15th Annual V M Goldschmidt Conference CY MAY, 2005 CL Moscow, ID C1 Univ Houston, Texas Ctr Superconduct & Adv Mat, Houston, TX 77204 USA. Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. EM apeslier@mail.uh.edu; jluhr@volcano.si.edu RI Peslier, Anne/F-3956-2010 NR 0 TC 0 Z9 0 U1 0 U2 1 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD MAY PY 2005 VL 69 IS 10 SU S BP A745 EP A745 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 930EX UT WOS:000229399702263 ER PT J AU Post, JE Heaney, PJ Hanson, J AF Post, JE Heaney, PJ Hanson, J TI Temperature-resolved synchrotron X-ray diffraction study of dehydration of birnessite-like phases SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 15th Annual V M Goldschmidt Conference CY MAY, 2005 CL Moscow, ID C1 Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. Brookhaven Natl Lab, Dept Chem, Upton, NY 11793 USA. EM post.jeffrey@nmnh.si.edu NR 0 TC 1 Z9 1 U1 0 U2 1 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD MAY PY 2005 VL 69 IS 10 SU S BP A627 EP A627 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 930EX UT WOS:000229399702033 ER PT J AU Rost, D Vicenzi, EP AF Rost, D Vicenzi, EP TI Carbonate-silicate assemblages in the Lafayette martian meteorite SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 15th Annual V M Goldschmidt Conference CY MAY, 2005 CL Moscow, ID ID AQUEOUS ALTERATION C1 Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. EM rostd@si.edu; vicenzi@volcano.si.edu NR 6 TC 0 Z9 0 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD MAY PY 2005 VL 69 IS 10 SU S BP A526 EP A526 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 930EX UT WOS:000229399701434 ER PT J AU Sisson, VB Harlow, GE Sorensen, SS AF Sisson, VB Harlow, GE Sorensen, SS TI Jadeitite: A record of metasomatism at various depths in Guatemalan subduction zones SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 15th Annual V M Goldschmidt Conference CY MAY, 2005 CL Moscow, ID C1 Amer Museum Nat Hist, Dept Earth & Planetary Sci, New York, NY 10024 USA. Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. EM j_sisson@netzero.net; gharlow@amnh.org; sorensen@volcano.si.edu NR 0 TC 1 Z9 1 U1 0 U2 1 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD MAY PY 2005 VL 69 IS 10 SU S BP A785 EP A785 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 930EX UT WOS:000229399702340 ER PT J AU Smith, FA Wing, S Freeman, KH AF Smith, FA Wing, S Freeman, KH TI Using carbon and hydrogen isotope ratios of terrestrial organic matter to understand climate change at the PETM SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 15th Annual V M Goldschmidt Conference CY MAY, 2005 CL Moscow, ID C1 Penn State Univ, University Pk, PA 16802 USA. Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA. EM fsmith@geose.psu.edu; Wing.Scott@nmnh.si.edu; kate@essc.psu.edu RI Freeman, Katherine/H-5140-2011 OI Freeman, Katherine/0000-0002-3350-7671 NR 0 TC 0 Z9 0 U1 0 U2 3 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD MAY PY 2005 VL 69 IS 10 SU S BP A345 EP A345 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 930EX UT WOS:000229399701080 ER PT J AU Sorensen, SS AF Sorensen, SS TI Accessory minerals, trace elements, fluids and subduction SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 15th Annual V M Goldschmidt Conference CY MAY, 2005 CL Moscow, ID C1 Natl Museum Nat Hist, Dept Min Sci, Smithsonian Inst, Washington, DC 20013 USA. EM sorena@volcano.si.edu NR 0 TC 0 Z9 0 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD MAY PY 2005 VL 69 IS 10 SU S BP A24 EP A24 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 930EX UT WOS:000229399700048 ER PT J AU Vicenzi, EP Sorensen, SS Rose, T AF Vicenzi, EP Sorensen, SS Rose, T TI From luminoscope to SEM-based hyperspectral imaging: An evolution of CL technology SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 15th Annual V M Goldschmidt Conference CY MAY, 2005 CL Moscow, ID C1 Smithsonian Inst, Natl Museum Amer Hist, Dept Mineral Sci, Washington, DC 20560 USA. EM vicenzi@si.edu; sorena@si.edu; rose.timothy@nmnh.si.edu NR 1 TC 0 Z9 0 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD MAY PY 2005 VL 69 IS 10 SU S BP A594 EP A594 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 930EX UT WOS:000229399701563 ER PT J AU Vicenzi, EP Rost, D AF Vicenzi, EP Rost, D TI Hyperspectral data analysis of martian meteorite alteration: A tool for constraining surface processes on Mars? SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 15th Annual V M Goldschmidt Conference CY MAY, 2005 CL Moscow, ID C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. EM vicenzi@si.edu; rostd@si.edu NR 2 TC 0 Z9 0 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD MAY PY 2005 VL 69 IS 10 SU S BP A526 EP A526 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 930EX UT WOS:000229399701433 ER PT J AU Wise, MA AF Wise, MA TI Distribution and geochemistry of gem tourmaline-bearing pegmatites in western Maine SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 15th Annual V M Goldschmidt Conference CY MAY, 2005 CL Moscow, ID C1 Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. EM wise.michael@nmnh.si.edu NR 0 TC 1 Z9 1 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD MAY PY 2005 VL 69 IS 10 SU S BP A277 EP A277 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 930EX UT WOS:000229399700538 ER PT J AU Liutkus, CM Wright, JD Ashley, GM Sikes, NE AF Liutkus, CM Wright, JD Ashley, GM Sikes, NE TI Paleoenvironmental interpretation of lake-margin deposits using delta C-13 and delta O-18 results from early Pleistocene carbonate rhizoliths, Olduvai Gorge, Tanzania SO GEOLOGY LA English DT Article DE Olduvai Gorge; rhizolith; oxygen isotope; carbon isotope; paleoclimate ID KENYA; TURKANA; RECORD; KA AB Isotope analyses of lake-margin rhizoliths from paleo-Lake Olduvai (ca. 1.75 Ma) form the basis of a new model proposed here for interpreting stable isotope values of phreatic rhizolith carbonates. Average delta(18)O and delta(13)C values from rhizoliths formed in transgressive lacustrine (waxy) claystones are relatively low. Low delta(18)O averages (-5.5 parts per thousand) reflect meteoric water values consistent with increased precipitation during wet periods that would increase the outflow of fresh water from subsurface seeps and shift a brackish groundwater zone lakeward. Low delta(13)C averages (-4.1 parts per thousand) could indicate little atmospheric exchange, high plant decay, and/or increased groundwater (low delta(13)C) flow. Higher averages in delta(18)O (-3.6 parts per thousand) and delta(13)C (-2.0 parts per thousand) occur during dry periods and lake regressions (earthy claystones), when hydraulic head is reduced, the lake recedes, and water within the wetlands is subjected to intense evaporation and gas exchange with the atmosphere. The isotope ratios of the rhizoliths from lowermost Bed II change in response to groundwater hydrology on Milankovitch time scales, but the isotopes also provide evidence of shorter-term (decadal to centennial scale) climate fluctuations. The orbitally driven climate changes are recorded faithfully by lithologic variations and stable isotope patterns. C1 Rutgers State Univ, Dept Geol Sci, Piscataway, NJ 08854 USA. Smithsonian Inst, Natl Museum Nat Hist, Human Origins Program, Washington, DC 20560 USA. RP Liutkus, CM (reprint author), Bucknell Univ, Dept Geol, Lewisburg, PA 17837 USA. NR 26 TC 32 Z9 34 U1 4 U2 15 PU GEOLOGICAL SOC AMERICA, INC PI BOULDER PA PO BOX 9140, BOULDER, CO 80301-9140 USA SN 0091-7613 J9 GEOLOGY JI Geology PD MAY PY 2005 VL 33 IS 5 BP 377 EP 380 DI 10.1130/G21132.1 PG 4 WC Geology SC Geology GA 922AW UT WOS:000228809000012 ER PT J AU Latychev, K Mitrovica, JX Tromp, J Tamisiea, ME Komatitsch, D Christara, CC AF Latychev, K Mitrovica, JX Tromp, J Tamisiea, ME Komatitsch, D Christara, CC TI Glacial isostatic adjustment on 3-D Earth models: a finite-volume formulation SO GEOPHYSICAL JOURNAL INTERNATIONAL LA English DT Article DE crustal motions; finite volumes; glacial isostatic adjustment; 3-D viscoelastic Earth models ID SEA-LEVEL CHANGE; COMPUTING 3-DIMENSIONAL DEFORMATIONS; VISCOELASTIC EARTH; LOWER MANTLE; PLEISTOCENE DEGLACIATION; NORTH-AMERICA; PRECESSION CONSTANT; SPECTRAL FORMALISM; LINEAR-SYSTEMS; GENERAL-THEORY AB We describe and present results from a finite-volume (FV) parallel computer code for forward modelling the Maxwell viscoelastic response of a 3-D, self-gravitating, elastically compressible Earth to an arbitrary surface load. We implement a conservative, control volume discretization of the governing equations using a tetrahedral grid in Cartesian geometry and a low-order, linear interpolation. The basic starting grid honours all major radial discontinuities in the Preliminary Reference Earth Model ( PREM), and the models are permitted arbitrary spatial variations in viscosity and elastic parameters. These variations may be either continuous or discontinuous at a set of grid nodes forming a 3-D surface within the ( regional or global) modelling domain. In the second part of the paper, we adopt the FV methodology and a spherically symmetric Earth model to generate a suite of predictions sampling a broad class of glacial isostatic adjustment (GIA) data types (3-D crustal motions, long-wavelength gravity anomalies). These calculations, based on either a simple disc load history or a global Late Pleistocene ice load reconstruction (ICE-3G), are benchmarked against predictions generated using the traditional normal-mode approach to GIA. The detailed comparison provides a guide for future analyses ( e. g. what grid resolution is required to obtain a specific accuracy?) and it indicates that discrepancies in predictions of 3-D crustal velocities less than 0.1 mm yr(-1) are generally obtainable for global grids with similar to 3 x 10(6) nodes; however, grids of higher resolution are required to predict large-amplitude (> 1 cm yr(-1)) radial velocities in zones of peak post-glacial uplift ( e. g. James bay) to the same level of absolute accuracy. We conclude the paper with a first application of the new formulation to a 3-D problem. Specifically, we consider the impact of mantle viscosity heterogeneity on predictions of present-day 3-D crustal motions in North America. In these tests, the lateral viscosity variation is constructed, with suitable scaling, from tomographic images of seismic S-wave heterogeneity, and it is characterized by approximately 2 orders of magnitude (peak-to-peak) lateral variations within the lower mantle and 1 order of magnitude variations in the bulk of the upper mantle ( below the asthenosphere). We find that the introduction of 3-D viscosity structure has a profound impact on horizontal velocities; indeed, the magnitude of the perturbation ( of order 1 mm yr(-1)) is as large as the prediction generated from the underlying (1-D) radial reference model and it far exceeds observational uncertainties currently being obtained from space-geodetic surveying. The relative impact of lateral viscosity variations on predicted radial motions is significantly smaller. C1 Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada. CALTECH, Seismol Lab, Pasadena, CA 91125 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Pau & Pays Adour, Geophys Imaging Lab, F-64013 Pau, France. Univ Toronto, Dept Comp Sci, Toronto, ON M5S 2E4, Canada. 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; Komatitsch, Dimitri/E-7153-2012 OI Tromp, Jeroen/0000-0002-2742-8299; Komatitsch, Dimitri/0000-0003-2309-8269 NR 86 TC 58 Z9 59 U1 4 U2 9 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0956-540X J9 GEOPHYS J INT JI Geophys. J. Int. PD MAY PY 2005 VL 161 IS 2 BP 421 EP 444 DI 10.1111/j.1365-246X.2005.02536.x PG 24 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 921DR UT WOS:000228744900019 ER PT J AU Gurwell, MA Bergin, EA Melnick, GJ Tolls, V AF Gurwell, MA Bergin, EA Melnick, GJ Tolls, V TI Mars surface and atmospheric temperature during the 2001 global dust storm SO ICARUS LA English DT Article DE Mars; atmosphere; radio observations; atmospheres; structure ID THERMAL EMISSION SPECTROMETER; WAVE-ASTRONOMY-SATELLITE; VAPOR VERTICAL-DISTRIBUTION; WATER-VAPOR; INTERANNUAL VARIABILITY; MARTIAN ATMOSPHERE; ANNUAL CYCLE; SUBMILLIMETER; LINE; MILLIMETER AB The dramatic growth and evolution of the 2001 martian global dust storm were captured using the Submillimeter Wave Astronomy Satellite (SWAS). While the lower and middle atmosphere (pressures greater than 50 mu bar, up to similar to 45 km altitude) showed rapid heating of up to 40 K, the average surface brightness temperature plummeted by similar to 20 K at the peak of the storm. The storm appears to have had little impact on the global temperature structure at attitudes above similar to 10 mu bar (similar to 60 km). (c) 2004 Elsevier Inc. All rights reserved. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. RP Gurwell, MA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mgurwell@cfa.harvard.edu NR 34 TC 14 Z9 15 U1 0 U2 0 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD MAY PY 2005 VL 175 IS 1 BP 23 EP 31 DI 10.1016/j.icarus.2004.10.009 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 921AA UT WOS:000228735400003 ER PT J AU McCarthy, MC Thaddeus, P AF McCarthy, MC Thaddeus, P TI Rotational spectrum and carbon-13 hyperfine structure of the C3H, C5H, C6H, and C7H radicals SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article AB By means of Fourier transform microwave spectroscopy of a supersonic molecular beam, we have detected the singly substituted carbon-13 isotopic species of C5H, C6H, and C7H. Hyperfine structure in the rotational transitions of the lowest-energy fine structure component ((2)Pi(1/2) for C5H and C7H, and (2)Pi(3/2) for C6H) of each species was measured between 6 and 22 GHz, and precise rotational, centrifugal distortion, Lambda-doubling, and C-13 hyperfine coupling constants were determined. In addition, resolved hyperfine structure in the lowest rotational transition (J=3/2 -> 1/2) of the three C-13 isotopic species of C3H was measured by the same technique. By combining the centimeter-wave measurements here with previous millimeter-wave data, a complete set of C-13 hyperfine coupling constants were derived to high precision for each isotopic species. Experimental structures (r(0)) have been determined for C5H and the two longer carbon-chain radicals, and these are found to be in good agreement with the predictions of high-level coupled-cluster calculations. C3H, C5H, and C7H exhibit a clear alternation in the magnitude and sign of the C-13 hyperfine coupling constants along the carbon-chain backbone. Because the electron spin density is nominally zero at the central carbon atom of C3H, C5H, and C7H, and at alternating sets of carbon atoms of C5H and C7H, owing to spin polarization, almost all of the C-13 coupling constants at these atoms are small in magnitude and negative in sign. Spin-polarization effects are known to be important for the Fermi-contact (b(F)) term, but prior to the work here they have generally been neglected for the hyperfine terms a, c, and d. (c) 2005 American Institute of Physics. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Harvard Univ, Div Engn & Appl Sci, Cambridge, MA 02138 USA. RP McCarthy, MC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 35 TC 19 Z9 19 U1 1 U2 8 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 MAY 1 PY 2005 VL 122 IS 17 AR 174308 DI 10.1063/1.1867356 PG 9 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 925PI UT WOS:000229064600019 PM 15910033 ER PT J AU Thorne, AP Rufus, J Yoshino, K Cheung, ASC Imajo, T AF Thorne, AP Rufus, J Yoshino, K Cheung, ASC Imajo, T TI The application of a VUV Fourier transform spectrometer and synchrotron radiation source to measurements of absorption bands of NO (vol 119, pg 8373, 2003) SO JOURNAL OF CHEMICAL PHYSICS LA English DT Correction C1 Univ London Imperial Coll Sci Technol & Med, Blackett Lab, London SW7 2BZ, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Hong Kong, Dept Chem, Hong Kong, Hong Kong, Peoples R China. Japan Womens Univ, Tokyo 1128681, Japan. RP Yoshino, K (reprint author), Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Prince Consort Rd, London SW7 2BZ, England. EM kyoshino@cfa.harvard.edu NR 13 TC 1 Z9 1 U1 3 U2 4 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 MAY 1 PY 2005 VL 122 IS 17 AR 179901 DI 10.1063/1.1883648 PG 3 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 925PI UT WOS:000229064600063 ER PT J AU Thorne, AP Rufus, J Yoshino, K Cheung, ASC Imajo, T AF Thorne, AP Rufus, J Yoshino, K Cheung, ASC Imajo, T TI The application of a VUV Fourier transform spectrometer and synchrotron radiation source to measurements of absorption bands of NO (vol 117, pg 10621, 2002) SO JOURNAL OF CHEMICAL PHYSICS LA English DT Correction C1 Univ London Imperial Coll Sci Technol & Med, Blackett Lab, London SW7 2BZ, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Hong Kong, Dept Chem, Hong Kong, Hong Kong, Peoples R China. Japan Womens Univ, Tokyo 1128681, Japan. RP Yoshino, K (reprint author), Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Prince Consort Rd, London SW7 2BZ, England. EM kyoshino@cfa.harvard.edu NR 13 TC 1 Z9 1 U1 3 U2 4 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 MAY 1 PY 2005 VL 122 IS 17 AR 179901 DI 10.1063/1.1883648 PG 3 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 925PI UT WOS:000229064600062 ER PT J AU Thorne, AP Rufus, J Yoshino, K Cheung, ASC Imajo, T AF Thorne, AP Rufus, J Yoshino, K Cheung, ASC Imajo, T TI The application of a VUV Fourier transform spectrometer and synchrotron radiation source to measurements of absorption bands of NO (vol 116, pg 155, 2002) SO JOURNAL OF CHEMICAL PHYSICS LA English DT Correction C1 Univ London Imperial Coll Sci Technol & Med, Blackett Lab, London SW7 2BZ, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Hong Kong, Dept Chem, Hong Kong, Hong Kong, Peoples R China. Japan Womens Univ, Tokyo 1128681, Japan. RP Yoshino, K (reprint author), Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Prince Consort Rd, London SW7 2BZ, England. EM kyoshino@cfa.harvard.edu NR 14 TC 1 Z9 1 U1 3 U2 4 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 MAY 1 PY 2005 VL 122 IS 17 AR 179901 DI 10.1063/1.1883648 PG 3 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 925PI UT WOS:000229064600061 ER PT J AU Thorne, AP Rufus, J Yoshino, K Cheung, ASC Imajo, T AF Thorne, AP Rufus, J Yoshino, K Cheung, ASC Imajo, T TI The application of a VUV Fourier transform spectrometer and synchrotron radiation source to measurements of absorption bands of NO (vol 115, pg 3719, 2001) SO JOURNAL OF CHEMICAL PHYSICS LA English DT Correction C1 Univ London Imperial Coll Sci Technol & Med, Blackett Lab, London SW7 2BZ, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Hong Kong, Dept Chem, Hong Kong, Hong Kong, Peoples R China. Japan Womens Univ, Tokyo 1128681, Japan. RP Yoshino, K (reprint author), Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Prince Consort Rd, London SW7 2BZ, England. EM kyoshino@cfa.harvard.edu NR 13 TC 0 Z9 0 U1 0 U2 0 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 MAY 1 PY 2005 VL 122 IS 17 AR 1799014 DI 10.1063/1.1883648 PG 3 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 925PI UT WOS:000229064600060 ER PT J AU Utz, LRP Coats, DW AF Utz, LRP Coats, DW TI Spatial and temporal patterns in the occurrence of peritrich ciliates as epibionts on calanoid copepods in the Chesapeake Bay, USA SO JOURNAL OF EUKARYOTIC MICROBIOLOGY LA English DT Article DE Acartia tonsa; epibiosis; Epistylis; estuary; Eurytemora affinis; infestation; protist; zooplankton; Zoothamnium intermedium ID PLANKTONIC COPEPODS; EPISTYLIS-DAPHNIAE; EPIZOIC CILIATE; ACARTIA-TONSA; HOST; INFESTATION; ZOOPLANKTON; COLACIUM; EUGLENOPHYCEAE; COLONIZATION AB We investigated temporal and spatial patterns of distribution in two peritrich ciliates (i.e. Zoothamnium intermedium and Epistylis sp.) living as epibionts on calanoid copepods (i.e. Acartia tonsa and Eurytemora affinis) in Chesapeake Bay. Net tow samples collected along the main axis of the Bay were analyzed to estimate the occurrence of epibionts on copepods and to explore relationships among infestation prevalence, host abundance, and environmental variables. Zoothamnium intermedium and Epistylis sp. colonized populations of A. tonsa during spring and summer months, while only Z intermedium colonized E. affinis during spring. Occurrence of epibionts on copepods showed high interannual variation, marked seasonality, and geographic heterogeneity. Extensive statistical analyses rejected simple scenarios of interactions between epibiosis, environmental variables, and host density, suggesting a more complex dynamics for the system. Analyses of epibiont colonies and zooids per host area (i.e. the sum of width and length of the body including antennae and swimming legs calculated assuming a cylindrical shape) were also performed. Overall, epibiont infestation prevalence (i.e. colonies/host area) and load (i.e. zooids/host area) were higher on copepodites than on adults for both host species, suggesting a preferential attachment to juveniles, or a higher predation pressure on adult stages. Infestation density and loads of both epibiont species were higher on the cephalothorax and abdomen of A. tonsa and E. affinis in comparison to the antennae and swimming legs, suggesting that ciliates can more easily colonize less active parts of the host. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Univ Maryland, Dept Biol, College Pk, MD 20742 USA. RP Utz, LRP (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM laurautz@yahoo.com RI Utz, Laura/P-5247-2014 NR 40 TC 18 Z9 23 U1 3 U2 5 PU BLACKWELL PUBLISHING INC PI MALDEN PA 350 MAIN ST, MALDEN, MA 02148 USA SN 1066-5234 J9 J EUKARYOT MICROBIOL JI J. Eukaryot. Microbiol. PD MAY-JUN PY 2005 VL 52 IS 3 BP 236 EP 244 DI 10.1111/j.1550-7408.2005.00025.x PG 9 WC Microbiology SC Microbiology GA 936EW UT WOS:000229839300010 PM 15927000 ER PT J AU Lambert, JB Wu, YY Santiago-Blay, JA AF Lambert, JB Wu, YY Santiago-Blay, JA TI Taxonomic and chemical relationships revealed by nuclear magnetic resonance spectra of plant exudates SO JOURNAL OF NATURAL PRODUCTS LA English DT Article ID RESINS; AMBER AB Exudates collected from 65 species of gymnosperms and angiosperms were examined by solid-state carbon-13 (C-13) nuclear magnetic resonance (NMR) spectroscopy. Diagnostic criteria were developed to distinguish resins, gums, and gum resins. The typology generated from the exudate spectra generally follows current taxonomic classifications, suggesting that C-13 NMR spectroscopy may have applications in exudate identification, at least at the familial level, and in some cases at the generic or specific levels. C1 Northwestern Univ, Dept Chem, Evanston, IL 60208 USA. Natl Museum Nat Hist, Smithsonian Inst, Dept Paleobiol, Washington, DC 20013 USA. RP Lambert, JB (reprint author), Northwestern Univ, Dept Chem, 2145 Sheridan Rd, Evanston, IL 60208 USA. EM jlambert@northwestern.edu NR 46 TC 20 Z9 23 U1 6 U2 11 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 MAY PY 2005 VL 68 IS 5 BP 635 EP 648 DI 10.1021/np050005f PG 14 WC Plant Sciences; Chemistry, Medicinal; Pharmacology & Pharmacy SC Plant Sciences; Pharmacology & Pharmacy GA 933AT UT WOS:000229596900001 PM 15921402 ER PT J AU Sanmartin, JR Lorenzini, EC AF Sanmartin, JR Lorenzini, EC TI Exploration of outer planets using tethers for power and propulsion SO JOURNAL OF PROPULSION AND POWER LA English DT Article ID CYLINDRICAL LANGMUIR PROBES; DEPLOYMENT SYSTEM C1 Univ Politecn Madrid, Escuela Tecn Super Ingn Aeronaut, Dept Phys, E-28040 Madrid, Spain. Harvard Smithsonian Ctr Astrophys, Geoastron Div, Cambridge, MA 02138 USA. RP Sanmartin, JR (reprint author), Univ Politecn Madrid, Escuela Tecn Super Ingn Aeronaut, Dept Phys, Plaza Cardenal,Cisneros 3, E-28040 Madrid, Spain. NR 20 TC 20 Z9 21 U1 0 U2 1 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0748-4658 J9 J PROPUL POWER JI J. Propul. Power PD MAY-JUN PY 2005 VL 21 IS 3 BP 573 EP 576 DI 10.2514/1.10772 PG 4 WC Engineering, Aerospace SC Engineering GA 926OO UT WOS:000229132700023 ER PT J AU Petkie, DT Helminger, P Winnewisser, BP Winnewisser, M Butler, RAH Jucks, KW De Lucia, FC AF Petkie, DT Helminger, P Winnewisser, BP Winnewisser, M Butler, RAH Jucks, KW De Lucia, FC TI The simulation of infrared bands from the analyses of rotational spectra: the 2v(9)-v(9) and v(5)-v(9) hot bands of HNO3 SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE HNO3; hot band intensities; infrared spectra ID NITRIC-ACID; VIBRATIONAL-STATES; LINE-INTENSITIES; NU(9) AB The results of millimeter and submillimeter wave rotational spectroscopy are used to simulate the complex structure of the 2v(9)-v(9) (438 cm(-1)) and v(5)-v(9) (421 cm(-1)) hot bands. The comparison data were obtained with a high-resolution Bruker FTIR. The combination of the quality of these data and the complexity of the spectra of these interacting states represents a stringent test for the simulation. It is shown that the agreement is very good and that this approach is generally advantageous. From this simulation, the ratios of the transition dipole moments for the 2v(9)-v(9) and v(5)-v(9) hot bands with respect to the v(9) fundamental band were found to be 1.38(11) and 0.67(20), respectively. Using these results, the calculated integrated band intensities for the hot bands at 296 K were determined to be S-v(2v(9)-v(9))=1.63 x 10(-18) cm(-1)/(mol cm(-2)) and Sv(v(5)-v(9))=0.36 x 10(-18) cm(-1)/(mol cm(-2)). These results were used to successfully simulate high-resolution stratospheric spectra obtained from a balloon flight of the FIRS-2 spectrometer. The more general problem of the rotation-vibration database and the optimal use of both microwave and infrared data to define it is discussed. It is concluded that it is best if the combination of data takes place at the level of the original spectra. (C) 2004 Elsevier Ltd. All rights reserved. C1 Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. Wright State Univ, Dept Phys, Dayton, OH 45435 USA. Univ S Alabama, Dept Phys, Mobile, AL 36688 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP De Lucia, FC (reprint author), Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. EM fcd@mps.ohio-state.edu NR 18 TC 12 Z9 12 U1 0 U2 0 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 MAY 1 PY 2005 VL 92 IS 2 BP 129 EP 141 DI 10.1016/j.jqsrt.2004.03.003 PG 13 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 875JM UT WOS:000225416400001 ER PT J AU Mandin, JY Jacquemart, D Dana, V Regalia-Jarlot, L Barbe, A AF Mandin, JY Jacquemart, D Dana, V Regalia-Jarlot, L Barbe, A TI Line intensities of acetylene at 3 mu m SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE acetylene; infrared; vibro-rotational transitions; line intensities; transition dipole moment ID FOURIER-TRANSFORM SPECTROMETER; INTERNAL PARTITION SUMS; FITTING TECHNIQUE; (C2H2)-C-12; REGION; BANDS; C2H2; SPECTRUM; PARAMETERS; 13.7-MU-M AB More than 400 absolute line positions and intensities of acetylene have been measured for the two cold bands v(3) and v(2) + (v(4) + v(5))(+)(0), and four strong hot bands occuring in the 3-mum spectral region, from Fourier-transform spectra. Accuracies are on the average 0.0005 cm(-1) for line positions and 5% for line intensities. Vibrational transition dipole moment values have been deduced, as also empirical Herman-Wallis coefficients, and comparisons have been made with previous results. (C) 2004 Published by Elsevier Ltd. C1 Univ Paris 06, CNRS, UMR 7092, Lab Phys Mol & Applicat, F-75252 Paris 05, France. Harvard Univ, Sch Med, Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA. Univ Reims, Fac Sci, CNRS, UMR 6089,Grp Spectrometrie Mol & Atmospher, F-51687 Reims, France. RP Dana, V (reprint author), Univ Paris 06, CNRS, UMR 7092, Lab Phys Mol & Applicat, 4 Pl Jussieu,Case Courrier 76,Tour 13, F-75252 Paris 05, France. EM vdana@ccr.jussieu.fr NR 25 TC 18 Z9 18 U1 1 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 MAY 1 PY 2005 VL 92 IS 2 BP 239 EP 260 DI 10.1016/j.jqsrt.2004.07.024 PG 22 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 875JM UT WOS:000225416400009 ER PT J AU Daniel, P AF Daniel, P TI David L. Smiley - Obituaries SO JOURNAL OF SOUTHERN HISTORY LA English DT Biographical-Item C1 Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. RP Daniel, P (reprint author), Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SOUTHERN HISTORICAL ASSOC PI ATHENS PA UNIV GEORGIA, HISTORY DEPT, ATHENS, GA 30602 USA SN 0022-4642 J9 J SOUTHERN HIST JI J. South. Hist. PD MAY PY 2005 VL 71 IS 2 BP 527 EP 528 PG 2 WC History SC History GA 924NB UT WOS:000228984400084 ER PT J AU Parker, G Tinoco-Ojanguren, C Martinez-Yrizar, A Maass, M AF Parker, G Tinoco-Ojanguren, C Martinez-Yrizar, A Maass, M TI Seasonal balance and vertical pattern of photosynthetically active radiation within canopies of a tropical dry deciduous forest ecosystem in Mexico SO JOURNAL OF TROPICAL ECOLOGY LA English DT Article DE absorbance; canopy structure; Chamela; light profile; transmittance; reflectance; seasonality ID NET PRIMARY PRODUCTIVITY; SOIL-WATER CONTENT; LEAF-AREA INDEX; LIGHT TRANSMITTANCE; WESTERN MEXICO; ENERGY-BALANCE; LAND-SURFACE; RAIN-FOREST; DYNAMICS; CLIMATE AB Major components of the flux density of global photosynthetically active radiation (PAR) were measured above and within canopies in a tropical deciduous forest on the Pacific coast of Mexico. At each of 69 locations grouped along a topographic sequence the PAR reflected from the top of the canopy. the vertical profile of transmittance, and the reflectance from the ground, were measured as many as four times in the year, including the extremes of the wet and dry seasons. With these observations an annual balance of the portion of PAR radiation reflected and absorbed by the canopy and ground was assembled and the detailed spatial and temporal dynamics of PAR within canopy layers were estimated. Canopy stature declined along the topographic sequence and the shape of the transmittance profiles reflected this. In locations of declining moisture availability the fraction of PAR absorbed by the ground increased and the fraction absorbed by non-foliar tissues decreased. Seasonal variation in canopy structure was the dominant influence on the partitioning of radiation - spatial variation was less important. Of a total annual PAR input of 15 200 mot m(-1), about 95% of incident PAR was absorbed, 50% by leaves, 25% by non-foliar tissues and 20% by the ground. The remaining 5% was reflected by the top of the canopy. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Univ Nacl Autonoma Mexico, Inst Ecol, Hermosillo, Sonora, Mexico. Univ Nacl Autonoma Mexico, Ctr Invest Ecosistemas, Morelia 58089, Michoacan, Mexico. RP Parker, G (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM parkerg@si.cdu OI Parker, Geoffrey/0000-0001-7055-6491 NR 60 TC 17 Z9 17 U1 1 U2 10 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 MAY PY 2005 VL 21 BP 283 EP 295 DI 10.1017/S0266467405002282 PN 3 PG 13 WC Ecology SC Environmental Sciences & Ecology GA 945JS UT WOS:000230499400005 ER PT J AU Kursar, TA Engelbrecht, BMJ Tyree, MT AF Kursar, TA Engelbrecht, BMJ Tyree, MT TI A comparison of methods for determining soil water availability in two sites in Panama with similar rainfall but distinct tree communities SO JOURNAL OF TROPICAL ECOLOGY LA English DT Article DE distribution; diversity; drought; edaphic; matric potential; Panama; productivity; soil texture ID BARRO COLORADO ISLAND; TROPICAL FOREST; FLORISTIC COMPOSITION; CLIMATIC GRADIENT; SEVERE DROUGHT; DRY SEASON; EL-NINO; DIVERSITY; TEXTURE; RETENTION AB Plant productivity. distribution and diversity in tropical rain forests correlate with water availability. Water availability is determined by rainfall and also by the available water capacity of the soil. However, while rainfall is recognized as important, linkages between plant distribution and differences among soils in available water capacity have not been demonstrated. One reason for this may be that measurements of soil moisture, such as gravimetric water content, may be overly Simplistic. To investigate this, we compared two sites in Panama, Allee and Rio Paja, which have similar rainfall but different plant communities. Soil water release curves were obtained from about - 0.1 MPa to - 9 MPa, permitting us to calculate available water capacity. The Rio Paja site had 17% greater available water capacity (between - 0.1 MPa to - 3 MPa), whereas the gravimetric water content at Rio Paja was lower by 16% in rainy season and by 41% at the end of the dry season. Hence soil gravimetric water content and soil available water capacity did not correspond. The results suggest that available water capacity may better predict plant distributions. Hence, whenever possible, available water capacity should be determined in addition to gravimetric water content. C1 Univ Utah, Dept Biol, Salt Lake City, UT 84112 USA. Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. USDA, Forest Serv, Burlington, VT 05402 USA. RP Kursar, TA (reprint author), Univ Utah, Dept Biol, 257 S 1400 E, Salt Lake City, UT 84112 USA. EM kursar@biology.utah.edu RI Engelbrecht, Bettina/E-9914-2012 NR 68 TC 9 Z9 9 U1 5 U2 14 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0266-4674 J9 J TROP ECOL JI J. Trop. Ecol. PD MAY PY 2005 VL 21 BP 297 EP 305 DI 10.1017/S0266467405002324 PN 3 PG 9 WC Ecology SC Environmental Sciences & Ecology GA 945JS UT WOS:000230499400006 ER PT J AU Wright, SJ Jaramillo, MA Pavon, J Condit, R Hubbell, SP Foster, RB AF Wright, SJ Jaramillo, MA Pavon, J Condit, R Hubbell, SP Foster, RB TI Reproductive size thresholds in tropical trees: variation among individuals, species and forests SO JOURNAL OF TROPICAL ECOLOGY LA English DT Article DE Barro Colorado Island; lianas; Pasoh Forest Reserve; reproductive size thresholds; tropical trees ID NEOTROPICAL FOREST; RECRUITMENT LIMITATION; AMAZONIAN FORESTS; BARRO-COLORADO; RELATIVE SIZE; GROWTH; COMMUNITIES; LIANAS; DISPERSAL; MATURITY AB Relative size at onset of maturity (RSCM) is defined assize at first reproduction divided by asymptotic maximal size. RSOM is remarkably constant among species within many higher clades of animals, but varies widely among tree species from the Pasoh Forest Reserve, Malaysia according to the work of S. C. Thomas. RSOM was examined for 16 mid-storey and canopy tree species from a second tropical forest at Barro Colorado Island (BCI), Panama. Interspecific variation in RSOM was equally large for BCI and Pasoh and was unrelated to gap dependence or life form for BCI species. The shape of the relationship between size and the proportion of individuals that were reproductive differed between forests, with an abrupt increase over a narrow range of sizes at Pasoh and a more gradual increase over a wider range of sizes at BCI. Both overtopping trees and heavy liana infestation reduced the probability that BCI trees were reproductive. This presumably reflects reduced availability of carbon for reproduction. We speculate that greater liana loads and a greater abundance of large, shade-casting trees at BCI may increase variation among individuals and contribute to the relatively wide range of sizes characterized by a mixture of sterile and fertile individuals observed for most BCI species. C1 Smithsonian Trop Res Inst, Balboa, Ancon, Panama. Harvard Univ Hebaria, Cambridge, MA 02138 USA. Univ Alcala De Henares, Dept Biol Vegetal, Madrid, Spain. Univ Georgia, Dept Plant Sci, Athens, GA 30602 USA. Field Museum, Chicago, IL 60605 USA. RP Wright, SJ (reprint author), Smithsonian Trop Res Inst, APO, AA 34002 USA. EM wrightj@si.edu RI Wright, Stuart/M-3311-2013 OI Wright, Stuart/0000-0003-4260-5676 NR 30 TC 73 Z9 76 U1 1 U2 19 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 MAY PY 2005 VL 21 BP 307 EP 315 DI 10.1017/S0266467405002294 PN 3 PG 9 WC Ecology SC Environmental Sciences & Ecology GA 945JS UT WOS:000230499400007 ER PT J AU Charles, E Bassett, Y AF Charles, E Bassett, Y TI Vertical stratification of leaf-beetle assemblages (Coleoptera : Chrysomelidae) in two forest types in Panama SO JOURNAL OF TROPICAL ECOLOGY LA English DT Article DE canopy; dry forest; rain forest; resource availability; species richness; understorey ID TREES AB To study vertical gradients of arthropod species richness in tropical forests, adult chrysomelids were surveyed with similar sampling effort by beating in four plots of 0.8 ha, representative of the canopy and understorey of one wet and one dry forest in Panama. Samples included in total 4615 individuals representing 253 species, and were of similar species richness at the two study sites. At both sites, chrysomelids were significantly more species-rich in the canopy than in the understorey. The proportion of species shared between the two study sites was 24%, whereas 16% and 28% of species were shared between the canopy and understorey of the wet and dry sites, respectively. Mature trees supported more and different chrysomelid species than conspecific saplings. A higher proportion of liana feeders vs. tree feeders occurred at the dry site than at the wet site, Multivariate analyses confirmed the faunal differences between the wet and dry sites and that stratification was more marked at the wet site than at the dry site. The latter observation may relate to differences in forest physiognomy (a tall and closed canopy at the wet site) and to the high interconnectivity via lianas between the understorey and canopy at the dry site. C1 Univ Guyana, Fac Agr & Forestry, Georgetown, Guyana. Smithsonian Trop Res Inst, Panama City, Panama. RP Charles, E (reprint author), Univ Guyana, Fac Agr & Forestry, Turkeyen Campus, Georgetown, Guyana. EM elroy_c@yahoo.co.uk NR 27 TC 28 Z9 31 U1 0 U2 10 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 MAY PY 2005 VL 21 BP 329 EP 336 DI 10.1017/S0266467405002300 PN 3 PG 8 WC Ecology SC Environmental Sciences & Ecology GA 945JS UT WOS:000230499400009 ER PT J AU Thomasson, MA Tunberg, BG AF Thomasson, MA Tunberg, BG TI Composition and vertical distribution of the motile epifauna on a vertical rock wall in Gullmarsfjorden, western Sweden, using an alternative sampling approach SO MARINE BIOLOGY RESEARCH LA English DT Article DE epifauna; hard bottoms; sublittoral; Sweden; vertical distribution; zonation ID PHYTAL ANIMAL COMMUNITIES; MOBILE EPIFAUNA; ABUNDANCE; ECOLOGY; FAUNA; ORGANIZATION; AMPHIPODS; PATTERNS; ZONATION; BIOMASS AB The main purpose of this study was to evaluate the efficiency of the alternative quantitative sampling approach and if it was possible, by using this method, to elucidate temporal variations concerning the composition, vertical distribution, and abundance of the motile epifaunal community. The study was performed on a vertical rocky bottom in Gullmarsfjorden on the Swedish west coast. Quantitative sampling was performed at four depths (2, 6, 10 and 15 m) on three occasions (19 June, 23-24 July and 23 September 1996) by means of a water jet powered suction sampler (venturi principle). In total, 53 macrofaunal taxa were found, of which 29 taxa occurred on all sampling dates. Significant vertical zonation patterns were recorded in July and September, but not in June, with amphipods, polychaetes, and echinoderms (mainly Asterias rubens) as the most important contributors to these patterns. A temporal variation in the faunal assemblage also occurred. Species abundance was significantly different between the sampling dates at 2, 6 and 10 m, but not at 15 m. The abundance was higher in July and September than in June. Species with the highest observed differences in abundance were juvenile Asterias rubens, abundant in July, while juvenile shrimp, especially Thoralus cranchii, and some amphipods, especially Microdeutopus spp., increased in abundance in September. This sampling approach was highly effective, and the high abundance and diversity of the motile epifauna indicate that these species play an important role in hard-bottom communities. C1 Smithsonian Marine Stn, Ft Pierce, FL 34949 USA. Kristineberg Marine Res Stn, S-45034 Fiskebackskil, Sweden. RP Tunberg, BG (reprint author), Smithsonian Marine Stn, 701 Seaway Dr, Ft Pierce, FL 34949 USA. EM Tunberg@si.edu RI Langhamer, Olivia/J-3425-2012 NR 46 TC 15 Z9 15 U1 0 U2 2 PU TAYLOR & FRANCIS AS PI OSLO PA PO BOX 12 POSTHUSET, NO-0051 OSLO, NORWAY SN 1745-1000 J9 MAR BIOL RES JI Mar. Biol. Res. PD MAY PY 2005 VL 1 IS 2 BP 107 EP 117 DI 10.1080/17451000510019051 PG 11 WC Ecology; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 944LI UT WOS:000230429500003 ER PT J AU Defew, LH Mair, JM Guzman, HM AF Defew, LH Mair, JM Guzman, HM TI An assessment of metal contamination in mangrove sediments and leaves from Punta Mala Bay, Pacific Panama SO MARINE POLLUTION BULLETIN LA English DT Article DE coastal pollution; sediment; heavy metals; mangrove; Laguncularia racemosa; Panama ID MARINA FORSK. VIERH; HEAVY-METALS; GREY MANGROVE; TRACE-METALS; HONG-KONG; LEAD; ACCUMULATION; ECOSYSTEMS; TOXICITY; CADMIUM AB Due to the growing rate of urbanisation in many tropical coastal areas, there continues to be an increasing concern in relation to the impact of anthropogenic activities on mangrove forests. Punta Mala Bay is located on the Pacific coast of Panama and suffers from intense anthropogenic activities that are potentially harmful to the remaining mangrove forests. Field observations reveal that the mangrove stand within Punta Mala Bay receives high inputs of untreated domestic sewage, storm water run-off and a range of diffuse inputs from shipping activities. Results from analysis of eight metals (Mn, Cu, Zn, Ni, Pb, Fe, Cr, Cd) showed that Fe, Zn and Pb were in concentrations high enough to conclude moderate to serious contamination within the bay, and thus pose the most threat to the regeneration and growth of the mangrove. However, previous biological surveys indicate ongoing mangrove regeneration and domination of stand structure by Laguncularia racemosa, together with high numbers of seedlings and saplings. (c) 2004 Elsevier Ltd. All rights reserved. C1 Heriot Watt Univ, Sch Life Sci, Edinburgh EH14 4AS, Midlothian, Scotland. Smithsonian Trop Res Inst, Miami, FL 34002 USA. RP Ctr Ecol & Hydrol, Bush Estate, Penicuik EH26 0QB, Midlothian, Scotland. EM ldef@ceh.ac.uk NR 31 TC 64 Z9 75 U1 6 U2 21 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0025-326X EI 1879-3363 J9 MAR POLLUT BULL JI Mar. Pollut. Bull. PD MAY PY 2005 VL 50 IS 5 BP 547 EP 552 DI 10.1016/j.marpolbul.2004.11.047 PG 6 WC Environmental Sciences; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 935YM UT WOS:000229819300018 PM 15907496 ER PT J AU Hershler, R Mulvey, M Liu, HP AF Hershler, R Mulvey, M Liu, HP TI Genetic variation in the Desert Springsnail (Tryonia porrecta): implications for reproductive mode and dispersal SO MOLECULAR ECOLOGY LA English DT Article DE allozymes; biogeography; Gastropoda; mtDNA; parthenogenesis; Tryonia ID SNAIL MELANOIDES-TUBERCULATA; POTAMOPYRGUS-ANTIPODARUM; POPULATION-GENETICS; MITOCHONDRIAL-DNA; HYDROBIIDAE; GASTROPODA; DIVERSITY; REGION; PARTHENOGENESIS; PROSOBRANCHIA AB Allozymes and mitochondrial cytochrome c oxidase subunit I (mtCOI) sequences were analysed to determine whether populations of the western North American gastropod Tryonia porrecta (from California, Nevada, Utah, and northwest Mexico) are strongly differentiated in accordance with traditional interpretation of regional fauna as ancient relicts inhabiting isolated fragments of late Tertiary palaeodrainages. These data were also used to assess whether this species, for which males have not been recorded, is a rare example of a molluscan parthenogen. Both data sets strongly supported monophyly of T. porrecta populations. Five of the nine sampled populations consisted of a single monoallelic allozyme genotype while the others contained two to 10 distinct genotypes. Allozymic data for genetically diverse Utah populations provided evidence of clonal and sexual reproduction. mtCOI haplotypes of T. porrecta formed two subgroups which differed by 1.99-2.60%. The common haplotype was found in seven populations with rare haplotypes observed in single populations. Based on these results and an available mtCOI molecular clock for related hydrobiid snails, T. porrecta is interpreted as a primarily parthenogenetic species that undergoes occasional sexual reproduction and has accumulated substantial diversity following its mid-Pliocene to mid-Pleistocene origin. Our results also suggest that the distribution of present-day populations of these gill-breathing snails did not result from fragmentation of an ancient, well-integrated drainage but instead reflects overland colonization of habitats which only recently became available following desiccation of late Quaternary pluvial lakes. C1 Smithsonian Inst, Dept Invertebrate Zool, Washington, DC 20013 USA. Univ Denver, Dept Biol Sci, Denver, CO 80208 USA. RP Hershler, R (reprint author), Smithsonian Inst, Dept Invertebrate Zool, POB 37012,NHB W-305,MRC 163, Washington, DC 20013 USA. EM hershler.robert@nmnh.si.edu NR 53 TC 22 Z9 23 U1 1 U2 2 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0962-1083 EI 1365-294X J9 MOL ECOL JI Mol. Ecol. PD MAY PY 2005 VL 14 IS 6 BP 1755 EP 1765 DI 10.1111/j.1365-294X.2005.02522.x PG 11 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 916OV UT WOS:000228395900012 PM 15836647 ER PT J AU Zhu, C Babb, JF Dalgarno, A AF Zhu, C Babb, JF Dalgarno, A TI Theoretical study of pressure broadening of lithium resonance lines by helium atoms SO PHYSICAL REVIEW A LA English DT Article ID TRANSMISSION SPECTRA; DIPOLE-MOMENTS; EXCITED-STATES; ENERGY CURVES; LI ATOMS; POTENTIALS; EMISSION; GASES; HE; ATMOSPHERES AB Quantum mechanical calculations are performed of the emission and absorption profiles of the lithium 2s-2p resonance line under the influence of a helium perturbing gas. We use carefully constructed potential energy surfaces and transition dipole moments to compute the emission and absorption coefficients at temperatures from 200 to 3000 K at wavelengths between 500 nm and 1000 nm. Contributions from quasibound states are included. The resulting red and blue wing profiles are compared with previous theoretical calculations and with an experiment, carried out at a temperature of 670 K. C1 Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. RP Zhu, C (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, 60 Garden St, Cambridge, MA 02138 USA. NR 27 TC 26 Z9 26 U1 0 U2 2 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 MAY PY 2005 VL 71 IS 5 AR 052710 DI 10.1103/PhysRevA.71.052710 PG 6 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 932HA UT WOS:000229543600066 ER PT J AU Robeck, TR Steinman, KJ Yoshioka, M Jensen, E O'Brien, JK Katsumata, E Gili, C McBain, JF Sweeney, J Monfort, SL AF Robeck, TR Steinman, KJ Yoshioka, M Jensen, E O'Brien, JK Katsumata, E Gili, C McBain, JF Sweeney, J Monfort, SL TI Estrous cycle characterisation and artificial insemination using frozen-thawed spermatozoa in the bottlenose dolphin (Tursiops truncatus) SO REPRODUCTION LA English DT Article ID FOLLICLE-STIMULATING-HORMONE; WHALES ORCINUS-ORCA; LUTEINIZING-HORMONE; ENZYME-IMMUNOASSAY; RESOURCE BANKS; OVULATION; SERUM; MARES; GONADOTROPINS; REPRODUCTION AB The reproductive endocrinology of the bottlenose dolphin, Tursiops truncatus, was characterized to facilitate the development of artificial insemination using cryopreserved spermatozoa. Specific objectives were: (i) to determine the excretory dynamics of urinary luteinizing hormone (LH) and ovarian steroid metabolites during the estrous cycle; (ii) to evaluate the effect of an exogenously administered synthetic progesterone analog (altrenogest) on reproductive hormone excretion; (iii) to correlate follicular growth and ovulation (as determined by transabdominal ultrasound) to urinary LH and ovarian steroid metabolites; (iv) examine the in vivo fertilisation capacity of cryopreserved semen, and (v) to develop an intrauterine insemination technique. Based on urinary endocrine monitoring of natural estrous cycles (2 consecutive cycles) and nine post altrenogest cycles in ten females, estrous cycles were found to be 36 days long and comprised of an 8 day and 19 day follicular and luteal phase, respectively. Peak estrogen conjugates (EC; 5.4 &PLUSMN; 3.8 ng/mg creatinine (Cr)) occurred 8 h prior to the LH surge (70.9 &PLUSMN; 115.7 ng/mg Cr). The time of ovulation, as determined by ultrasonography, occurred 32.1 &PLUSMN; 8.9 h and 24.3 &PLUSMN; 7.0 h after the onset of the LH surge and LH peak, respectively. Mean preovulatory follicular diameter and circumference were 2.1 &PLUSMN; 0.5 cm and 6.5 &PLUSMN; 1.5 cm, respectively. Of the 27 estrous synchronisation attempts, 13 resulted in an ovulatory cycle, with ovulation occurring 21 days post-altrenogest treatment. Intrauterine (4 of 5) and intracornual (1 of 3) inseminations conducted across eight estrous cycles resulted in five pregnancies (63%), one pregnancy resulted from the use of liquid stored semen, whereas four were achieved using cryopreserved semen. These data provide new information on female bottlenose dolphin reproductive physiology, and demonstrate that the combination of endocrine monitoring and serial ultrasonography contributed to successful AI using liquid-stored and cryopreserved semen. C1 SeaWorld Texas, San Antonio, TX 78251 USA. Smithsonian Inst, Conservat & Res Ctr, Natl Zool Pk, Front Royal, VA 22630 USA. Mie Univ, Lab Fish Culture, Fac Bioresources, Tsu, Mie 5148507, Japan. USN, Marine Mammal Program, San Diego, CA 92152 USA. Univ Sydney, Fac Vet Sci, Ctr Adv Technol Anim Genet & Reprod, Sydney, NSW 2006, Australia. Acquario Genova, I-16128 Genoa, Italy. Kamogawa SeaWorld, Chiba 2960041, Japan. SeaWorld Calif, San Diego, CA 92109 USA. Dolphin Quest Oahu, Honolulu, HI 96816 USA. RP Robeck, TR (reprint author), SeaWorld Texas, 10500 SeaWorld Dr, San Antonio, TX 78251 USA. EM Todd.Robeck@SeaWorld.com NR 48 TC 44 Z9 49 U1 2 U2 17 PU BIO SCIENTIFICA LTD PI BRISTOL PA EURO HOUSE, 22 APEX COURT WOODLANDS, BRADLEY STOKE, BRISTOL BS32 4JT, ENGLAND SN 1470-1626 J9 REPRODUCTION JI Reproduction PD MAY PY 2005 VL 129 IS 5 BP 659 EP 674 DI 10.1530/rep.1.00516 PG 16 WC Developmental Biology; Reproductive Biology SC Developmental Biology; Reproductive Biology GA 925VA UT WOS:000229080200012 PM 15855629 ER PT J AU Turner, BL AF Turner, BL TI Storage-induced changes in phosphorus solubility of air-dried soils SO SOIL SCIENCE SOCIETY OF AMERICA JOURNAL LA English DT Article ID WESTERN UNITED-STATES; ORGANIC PHOSPHORUS; MICROBIAL BIOMASS; PASTURE SOILS; ARABLE SOILS; PHOSPHATE; EXTRACTION; GRASSLAND AB Soil is commonly stored in an air-dried state for extended periods before chemical analysis. The effect of storage on P solubility was assessed by determining NaHCO3-extractable P concentrations in a range of pasture soils from England and Wales (total C = 28.9-80.4 g kg(-1), clay = 219-681 g kg(-1), pH = 4.4-6.8) immediately following air drying and after 3 yr of storage at ambient laboratory temperature. Following storage, NaHCO3-extractable inorganic P concentrations decreased by between 2 and 60% (mean decrease = 21%), while NaHCO3-extractable organic P concentrations increased by between 48 and 156% (mean increase = 95%). The greatest changes occurred in soils of pH < 5.3. The changes appear to result from the disruption of organic matter coatings on mineral surfaces, continuous solid-phase diffusion of phosphate into soil particles, and decomposition of microbial cells. The results have important implications for the determination of NaHCO3-extractable P in stored soils and highlight the importance of working with fresh samples to derive information with relevance to field conditions. C1 Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Turner, BL (reprint author), Smithsonian Trop Res Inst, Box 2072, Balboa, Ancon, Panama. EM turnerbl@si.edu RI Turner, Benjamin/E-5940-2011 OI Turner, Benjamin/0000-0002-6585-0722 NR 22 TC 19 Z9 19 U1 1 U2 13 PU SOIL SCI SOC AMER PI MADISON PA 677 SOUTH SEGOE ROAD, MADISON, WI 53711 USA SN 0361-5995 J9 SOIL SCI SOC AM J JI Soil Sci. Soc. Am. J. PD MAY-JUN PY 2005 VL 69 IS 3 BP 630 EP 633 DI 10.2136/sssaj2004.0295 PG 4 WC Soil Science SC Agriculture GA 924VV UT WOS:000229009800007 ER PT J AU Launius, RD AF Launius, RD TI Perceptions of Apollo: Myth, nostalgia, memory or all of the above? SO SPACE POLICY LA English DT Article AB This essay explores the place of the Apollo program in the popular recollection of Americans more than 30 years after the last Moon landings in 1972, partly through a discussion of films and popular music. The collective memory of this singular episode in the history of the USA has altered over time. It has taken on mythical qualities, as well as a nostalgia for a time long gone. From a postmodern, post-cold war perspective Project Apollo appears increasingly unique, an experience born out of cold war rivalries long gone in which a demonstration of American technological capability was required. Many in the spaceflight community seek to become a multi-planetary species, and they point to Apollo in an increasingly mythical way as a representation of something that should be replicated. But the circumstances that made Apollo succeed have long since passed. (c) Published by Elsevier Ltd. C1 Smithsonian Inst, Div Space Hist, Natl Air & Space Museum, Washington, DC 20013 USA. RP Launius, RD (reprint author), Smithsonian Inst, Div Space Hist, Natl Air & Space Museum, POB 37012,NASM Room 3550,MRC 311, Washington, DC 20013 USA. EM launiusr@nasm.si.edu OI Launius, Roger/0000-0003-1633-1253 NR 38 TC 7 Z9 7 U1 0 U2 4 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0265-9646 J9 SPACE POLICY JI Space Policy PD MAY PY 2005 VL 21 IS 2 BP 129 EP 139 DI 10.1016/j.spacepol.2005.02.001 PG 11 WC International Relations; Social Sciences, Interdisciplinary SC International Relations; Social Sciences - Other Topics GA 942CJ UT WOS:000230260200009 ER PT J AU Roalson, EH Boggan, JK Skog, LE Zimmer, EA AF Roalson, EH Boggan, JK Skog, LE Zimmer, EA TI Untangling Gloxinieae (Gesneriaceae). I. Phylogenetic patterns and generic boundaries inferred from nuclear, chloroplast, and morphological cladistic datasets SO TAXON LA English DT Article DE generic boundaries; Gesneriaceae; Gesnerieae; Gloxinieae; ITS; molecular phylogenetics; morphology; trnL-F ID TRIBAL RELATIONSHIPS; NDHF SEQUENCES; EVOLUTION; DNA; STREPTOCARPUS; INCONGRUENCE; SYSTEMATICS; CHARACTERS; CONFIDENCE; ACHIMENES AB Tribe Gloxinieae has been estimated to include 22 genera and approximately 290 species. This study presents maximum parsimony phylogenetic analyses of nuclear ribosomal DNA internal transcribed spacer regions sequences, the chloroplast DNA trnL intron and trnL-trnF intergenic spacer region sequences, a morphological cladistic dataset, and combined analyses of these datasets. These analyses suggest that the genera Gloxinia, Phinaea, and (possibly) Diastema are polyphyletic; Kohleria is paraphyletic in relation to Capanea; Bellonia and Pheidonocarpa should be considered members of tribe Gesnerieae; and Lembocarpus is a member of tribe Episcieae. Furthermore, the historically recognized genus Seemannia, now included in Gloxinia, appears to form a strongly supported monophyletic group; several Gloxinia species from southern Brazil appear to be most closely related to Goyazia; Capanea, Kohleria, Pearcea s.l., and Diastema vexans appear to form a strongly supported clade; and Diastema, Monopyle, Phinaea (in part), and a few Gloxinia species (Gloxinia dodsonii, G lindeniana, and G racemosa) form a clade. Classification issues and generic boundaries of these lineages are discussed in detail. C1 Washington State Univ, Sch Biol Sci, Pullman, WA 99164 USA. Washington State Univ, Ctr Integrated Biotechnol, Pullman, WA 99164 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA. Smithsonian Inst, Natl Museum Nat Hist, Labs Analyt Biol, Suitland, MD 20746 USA. RP Roalson, EH (reprint author), Washington State Univ, Sch Biol Sci, Pullman, WA 99164 USA. EM roalson@mail.wsu.edu; bogganj@si.edu; skogl@si.edu; zimmer@lab.si.edu RI Zimmer, Elizabeth/G-3890-2011 NR 58 TC 28 Z9 39 U1 2 U2 8 PU INT ASSOC PLANT TAXONOMY PI VIENNA PA C/O UNIV VIENNA, INST BOTANY, RENNWEG 14, A-1030 VIENNA, AUSTRIA SN 0040-0262 J9 TAXON JI Taxon PD MAY PY 2005 VL 54 IS 2 BP 389 EP 410 PG 22 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA 938JS UT WOS:000229996500016 ER PT J AU Engelbrecht, BMJ Kursar, TA Tyree, MT AF Engelbrecht, BMJ Kursar, TA Tyree, MT TI Drought effects on seedling survival in a tropical moist forest SO TREES-STRUCTURE AND FUNCTION LA English DT Article DE mortality; drought performance; irrigation; soil moisture; tropical moist forest ID EL-NINO DROUGHT; TREE SEEDLINGS; RAIN-FOREST; DESICCATION-TOLERANCE; FLORISTIC COMPOSITION; HABITAT ASSOCIATIONS; VIROLA-SURINAMENSIS; CLIMATIC GRADIENT; NEOTROPICAL TREE; DRY FOREST AB The amount and seasonality of rainfall varies strongly in the tropics, and plant species abundance, distribution and diversity are correlated with rainfall. Drought periods leading to plant stress occur not only in dry forests, but also in moist and even wet forests. We quantified experimentally the effect of drought on survival of first year seedlings of 28 co-occurring tropical woody plant species in the understory of a tropical moist forest. The seedlings were transplanted to plots and subjected to a drought and an irrigation treatment for 22 weeks during the dry season. Drought effects on mortality and wilting behavior varied greatly among species, so that relative survival in the dry treatment ranged from 0% to about 100% of that in the irrigated treatment. Drought stress was the main factor in mortality, causing about 90% (median) of the total mortality observed in the dry treatment. In almost half of the species, the difference in survival between treatments was not significant even after 22 weeks, implying that many of the species are well adapted to drought in this forest. Relative drought survival was significantly higher in species associated with dry habitats than in those associated with wet habitats, and in species with higher abundance on the dry side of the Isthmus of Panama, than in those more abundant on the wet side. These data show that differential species survival in response to drought, combined with variation in soil moisture availability, may be important for species distribution at the local and regional scale in many tropical forests. C1 Smithsonian Trop Res Inst, Balboa, Panama. Univ Utah, Dept Biol, Salt Lake City, UT 84112 USA. USDA, Forest Serv, Burlington, VT 05446 USA. RP Engelbrecht, BMJ (reprint author), Smithsonian Trop Res Inst, POB 2072, Balboa, Panama. EM engelbrb@bci.si.edu RI Engelbrecht, Bettina/E-9914-2012 NR 52 TC 69 Z9 78 U1 4 U2 35 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013 USA SN 0931-1890 J9 TREES-STRUCT FUNCT JI Trees-Struct. Funct. PD MAY PY 2005 VL 19 IS 3 BP 312 EP 321 DI 10.1007/s00468-004-0393-0 PG 10 WC Forestry SC Forestry GA 931UD UT WOS:000229510100010 ER PT J AU Labandeira, CC AF Labandeira, CC TI Invasion of the continents: cyanobacterial crusts to tree-inhabiting arthropods SO TRENDS IN ECOLOGY & EVOLUTION LA English DT Review ID EARLIEST LAND PLANTS; CLOSEST LIVING RELATIVES; TERRESTRIAL ECOSYSTEMS; EARLY EVOLUTION; RIBOSOMAL DNA; BILLION YEARS; ORIGIN; LIFE; HISTORY; PHYLOGENY AB The colonization of continental environments (land and fresh water) has focused historically on a major event during the mid-Paleozoic Era characterized by the relatively sudden emergence of megascopic embryophytes, fungi, arthropods and tetrapods. A significant earlier phase of Precambrian (Archean and Proterozoic Eons) terrestrialization extends to the first 80% of the history of life and records the colonization of subaerial soils or rock surfaces predominantly by cyanobacterial mats and crusts. These two phases are separated by a &SIM; 90-million-year early Paleozoic interlude of minimal terrestrial colonization. Trophically modern ecosystems appeared during the Late Silurian-Middle Devonian (425-375 million years ago), consisting of complex symbiotic, parasitic and other trophic associations, including detritivory and limited herbivory. The integration of these two historically disparate fields (Precambrian microorganisms and their biochemical and sedimentological signatures, and the paleoecology of mid-Paleozoic ecosystems) has resulted in a wider perspective on terrestrialization. Here, I present an ecological and evolutionary context for the emergence of terrestrial ecosystems and examine associations among organisms, from the endosymbiotic capture of organelles by eukaryotes to modes of metazoan nutrition on land. Such studies now enable the tracking, in ecological detail, of the invasion of continental environments during the past 3.5 billion years of life. C1 Natl Museum Nat Hist, Smithsonian Inst, Dept Paleobiol, Washington, DC 20013 USA. RP Labandeira, CC (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Dept Paleobiol, Washington, DC 20013 USA. EM labandec@si.edu NR 91 TC 50 Z9 54 U1 7 U2 48 PU ELSEVIER SCIENCE LONDON PI LONDON PA 84 THEOBALDS RD, LONDON WC1X 8RR, ENGLAND SN 0169-5347 J9 TRENDS ECOL EVOL JI Trends Ecol. Evol. PD MAY PY 2005 VL 20 IS 5 BP 253 EP 262 DI 10.1016/j.tree.2005.03.002 PG 10 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 926RX UT WOS:000229141400008 PM 16701377 ER PT J AU Collin, R AF Collin, R TI Development, phylogeny, and taxonomy of Bostrycapulus (Caenogastropoda : Calyptraeidae), an ancient cryptic radiation SO ZOOLOGICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Article DE biogeography; Crepidula aculeata; gastropod taxonomy; new species; sibling species ID POPULATION-STRUCTURE; SPECIES COMPLEX; CREPIDULA PROSOBRANCHIA; OCEAN CURRENTS; NORTHERN CHILE; PHYLOGEOGRAPHY; EVOLUTION; GASTROPODS; SPECIATION; PATTERNS AB Calyptraeid gastropods are well know for the taxonomic difficulties caused by their simple, phenotypically variable shells. In this paper I demonstrate that what was previously considered to be a single species, Crepidula aculeata, is an ancient (3-15 Myr) cryptic species complex made up of at least eight species, and that this group should be placed in the genus Bostrycapulus. Despite the difficulty in finding diagnostic adult shell and anatomical features upon which species can be unambiguously identified, DNA sequences, protoconch morphology, embryonic morphology and developmental characters clearly differentiate these eight species. A single species with direct development and nurse eggs is present in the South Atlantic, and a species with planktotrophic development occurs in the equatorial Pacific. The species from Japan, Australia, Florida, the Pacific coasts of Mexico and Central America, and the Cape Verde Islands all have direct development. Most of these species are separated by > 15% divergence in COI sequence data. The fossil record of Bostrycapulus goes back to the Miocene, which agrees with genetic estimates of divergences within the genus ranging from 3 to 15 Mya. Surprisingly, these ancient species differ only slightly in morphology from each other and genetic differentiation does not correlate with geographical distance. I revise the genus Bostrycapulus on the basis of differences in adult morphology, embryonic morphology, mode of development, protoconch morphology, and DNA sequence data. I also describe four new species (B. pritzkeri sp. nov., B. odites sp. nov., B. latebrus sp. nov. and B. urraca sp. nov.) and remove three others (B. gravispinosus, B. calyptraeformis, and B. cf. tegulicius) from synonymy with B. aculeatus. © 2005 The Linnean Society of London. C1 Smithsonian Trop Res Inst, Unit 0948, Miami, FL 34002 USA. RP Collin, R (reprint author), Smithsonian Trop Res Inst, Unit 0948, APO AA, Miami, FL 34002 USA. EM collinr@naos.si.edu RI Collin, Rachel/G-2001-2010; OI Collin, Rachel/0000-0001-5103-4460 NR 71 TC 28 Z9 30 U1 0 U2 5 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0024-4082 J9 ZOOL J LINN SOC-LOND JI Zool. J. Linn. Soc. PD MAY PY 2005 VL 144 IS 1 BP 75 EP 101 DI 10.1111/j.1096-3642.2005.00162.x PG 27 WC Zoology SC Zoology GA 925ZZ UT WOS:000229093700005 ER PT J AU Gaensler, BM Kouveliotou, C Gelfand, JD Taylor, GB Eichler, D Wijers, RAMJ Granot, J Ramirez-Ruiz, E Lyubarsky, YE Hunstead, RW Campbell-Wilson, D van der Horst, AJ McLaughlin, MA Fender, RP Garrett, MA Newton-McGee, KJ Palmer, DM Gehrels, N Woods, PM AF Gaensler, BM Kouveliotou, C Gelfand, JD Taylor, GB Eichler, D Wijers, RAMJ Granot, J Ramirez-Ruiz, E Lyubarsky, YE Hunstead, RW Campbell-Wilson, D van der Horst, AJ McLaughlin, MA Fender, RP Garrett, MA Newton-McGee, KJ Palmer, DM Gehrels, N Woods, PM TI An expanding radio nebula produced by a giant flare from the magnetar SGR 1806-20 SO NATURE LA English DT Article ID RAY REPEATER SGR1900+14; SOFT GAMMA-REPEATERS; RADIATIVE MECHANISM; SGR 1806-20; PULSAR; SGR-1900+14; AFTERGLOWS AB Soft gamma-ray repeaters (SGRs) are 'magnetars', a small class of slowly spinning neutron stars with extreme surface magnetic fields, B approximate to 10(15) gauss (refs 1-3). On 27 December 2004, a giant flare(4) was detected from the magnetar SGR 1806-20 (ref. 2), only the third such event recorded(5,6). This burst of energy was detected by a variety of instruments(7,8) and even caused an ionospheric disturbance in the Earth's upper atmosphere that was recorded around the globe(9). Here we report the detection of a fading radio afterglow produced by this outburst, with a luminosity 500 times larger than the only other detection of a similar source(10). From day 6 to day 19 after the flare from SGR 1806-20, a resolved, linearly polarized, radio nebula was seen, expanding at approximately a quarter of the speed of light. To create this nebula, at least 4 x 10(43) ergs of energy must have been emitted by the giant flare in the form of magnetic fields and relativistic particles. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35805 USA. Univ Space Res Assoc, NSSTC, Huntsville, AL 35805 USA. Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94309 USA. Natl Radio Astron Observ, Socorro, NM 87801 USA. Ben Gurion Univ Negev, Dept Phys, IL-84105 Beer Sheva, Israel. Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. Inst Adv Study, Princeton, NJ 08540 USA. Univ Sydney, Sch Phys, Sydney, NSW 2006, Australia. Univ Manchester, Jodrell Bank Observ, Macclesfield SK11 9DL, Cheshire, England. Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. Joint Inst VLBI Europe, NL-7990 AA Dwingeloo, Netherlands. CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. Los Alamos Natl Lab, Los Alamos, NM 87545 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Gaensler, BM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM bgaensler@cfa.harvard.edu RI Gaensler, Bryan/F-8655-2010; Gehrels, Neil/D-2971-2012; LYUBARSKY, YURY/F-2362-2012; OI Wijers, Ralph/0000-0002-3101-1808; Gaensler, Bryan/0000-0002-3382-9558 NR 27 TC 105 Z9 105 U1 0 U2 4 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD APR 28 PY 2005 VL 434 IS 7037 BP 1104 EP 1106 DI 10.1038/nature03498 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 920MD UT WOS:000228693300035 PM 15858566 ER PT J AU Palmer, DM Barthelmy, S Gehrels, N Kippen, RM Cayton, T Kouveliotou, C Eichler, D Wijers, RAMJ Woods, PM Granot, J Lyubarsky, YE Ramirez-Ruiz, E Barbier, L Chester, M Cummings, J Fenimore, EE Finger, MH Gaensler, BM Hullinger, D Krimm, H Markwardt, CB Nousek, JA Parsons, A Patel, S Sakamoto, T Sato, G Suzuki, M Tueller, J AF Palmer, DM Barthelmy, S Gehrels, N Kippen, RM Cayton, T Kouveliotou, C Eichler, D Wijers, RAMJ Woods, PM Granot, J Lyubarsky, YE Ramirez-Ruiz, E Barbier, L Chester, M Cummings, J Fenimore, EE Finger, MH Gaensler, BM Hullinger, D Krimm, H Markwardt, CB Nousek, JA Parsons, A Patel, S Sakamoto, T Sato, G Suzuki, M Tueller, J TI A giant gamma-ray flare from the magnetar SGR 1806-20 SO NATURE LA English DT Article ID REPEATER SGR 1900+14; 1998 AUGUST 27; RADIATIVE MECHANISM; BURST; OUTBURSTS; MISSION AB Two classes of rotating neutron stars-soft gamma-ray repeaters (SGRs) and anomalous X-ray pulsars-are magnetars(1), whose X-ray emission is powered by a very strong magnetic field (B approximate to 10(15) G). SGRs occasionally become 'active', producing many short X-ray bursts. Extremely rarely, an SGR emits a giant flare with a total energy about a thousand times higher than in a typical burst(2-4). Here we report that SGR 1806-20 emitted a giant flare on 27 December 2004. The total (isotropic) flare energy is 2 x 10(46) erg, which is about a hundred times higher than the other two previously observed giant flares. The energy release probably occurred during a catastrophic reconfiguration of the neutron star's magnetic field. If the event had occurred at a larger distance, but within 40 megaparsecs, it would have resembled a short, hard gamma-ray burst, suggesting that flares from extragalactic SGRs may form a subclass of such bursts. C1 Los Alamos Natl Lab, Los Alamos, NM 87545 USA. NASA, Goddard Space Flight Ctr, Univ Space Res Assoc, Greenbelt, MD 20771 USA. NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35805 USA. Univ Space Res Assoc, NSSTC, Huntsville, AL 35805 USA. Ben Gurion Univ Negev, Dept Phys, IL-84105 Beer Sheva, Israel. Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94309 USA. Inst Adv Study, Princeton, NJ 08540 USA. Penn State Univ, University Pk, PA 16802 USA. CNR, Washington, DC 20001 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Maryland, College Pk, MD 20742 USA. Inst Space & Astronaut Sci, JAXA, Kanagawa 2298510, Japan. Saitama Univ, Sakura Ku, Saitama 3388570, Japan. RP Palmer, DM (reprint author), Los Alamos Natl Lab, POB 1663, Los Alamos, NM 87545 USA. EM palmer@lanl.gov RI Gaensler, Bryan/F-8655-2010; Barthelmy, Scott/D-2943-2012; Gehrels, Neil/D-2971-2012; Tueller, Jack/D-5334-2012; LYUBARSKY, YURY/F-2362-2012; Parsons, Ann/I-6604-2012; OI Wijers, Ralph/0000-0002-3101-1808 NR 22 TC 289 Z9 292 U1 0 U2 9 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD APR 28 PY 2005 VL 434 IS 7037 BP 1107 EP 1109 DI 10.1038/nature03525 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 920MD UT WOS:000228693300036 PM 15858567 ER PT J AU Schotte, M AF Schotte, M TI Brian Frederick Kensley - In memoriam SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Biographical-Item 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, NHB 163 POB 37012, Washington, DC 20013 USA. NR 1 TC 0 Z9 0 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 APR 26 PY 2005 VL 118 IS 1 BP 1 EP 2 DI 10.2988/0006-324X(2005)118[1:IM]2.0.CO;2 PG 2 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 922CG UT WOS:000228812900001 ER PT J AU Schotte, M AF Schotte, M TI Discerceis kensleyi, n. sp., from Caribbean Colombia, the third species of the genus (Crustacea : Isopoda : Sphaeromatidae) SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article AB A third species of the genus Discerceis is described and a new generic diagnosis is offered. The distinctions in the new species are seen in morphological characters of the male, specifically the pleotelson, which bears an elongate, deeply set, apically upturned median tooth in the pleotelsonic notch, and in the uropods, which are much longer relative to the pleotelson as compared to its two cogeners. A key to the known species of the genus is given. C1 Smithsonian Inst, Museum Natl Hist Nat, Dept Invertebrate, Washington, DC 20013 USA. RP Schotte, M (reprint author), Smithsonian Inst, Museum Natl Hist Nat, Dept Invertebrate, POB 37012, Washington, DC 20013 USA. EM schottem@si.edu NR 2 TC 0 Z9 0 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 APR 26 PY 2005 VL 118 IS 1 BP 48 EP 54 DI 10.2988/0006-324X(2005)118[48:DKNSFC]2.0.CO;2 PG 7 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 922CG UT WOS:000228812900006 ER PT J AU Bishop, GA Williams, AB AF Bishop, GA Williams, AB TI Taphonomy and preservation of burrowing thalassinidean shrimps SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article ID CALLIANASSA CRUSTACEA; DECAPOD CRUSTACEANS; SOUTH-DAKOTA; BLACK HILLS; ENVIRONMENTS; FLORIDA; MEMBER AB Thalassinidean shrimp constitute six or seven families of highly specialized burrowing decapod crustaceans. Adaptations to a deep infaunal mode of life, exemplified by the ghost shrimps Callichirus and Callianassa, include an elongate subcylindrical body differentially sclerotized and divided into units functional for life in tubular burrows (i.e., burrowing, locomotion, flexion, pumping, and sealing). Death or molting within burrows may lead to positive biases of preservation of the more heavily sclerotized parts consisting of burrow buttons preserving chelipeds, anterior cephalothoracic regions, posterior abdomen, and walking legs. Thalassinidean chelipeds, particularly the fingers, are among the most common of decapod crustacean body fossils. Illustrations and examples are given to document the full range of fossil remains, including body fossils and trace fossils. An exceptional whole-body thalassinid, Axiopsis eximia, was described by Kensley and Williams (1990) from the Middle Eocene of South Carolina. The specimen is a silicified body fossil preserving virtually the entire animal except distal appendages. This specimen remains the only described silicified thalassinid. This paper is presented as a tribute to Brian Kensley and as closure for the Bishop-Williams collaborations spanning 25 years. C1 S Dakota Sch Mines & Technol, Museum Geol & Paleontol, Rapid City, SD 57701 USA. Georgia So Univ, Dept Geol & Geog, Statesboro, GA 30460 USA. Smithsonian Inst, Natl Marine Fisheries Lab Systemat, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Bishop, GA (reprint author), S Dakota Sch Mines & Technol, Museum Geol & Paleontol, 501 E St Joseph St, Rapid City, SD 57701 USA. EM Gale.Bishop@sdsmt.edu NR 78 TC 21 Z9 23 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 APR 26 PY 2005 VL 118 IS 1 BP 218 EP 236 DI 10.2988/0006-324X(2005)118[218:TAPOBT]2.0.CO;2 PG 19 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 922CG UT WOS:000228812900020 ER PT J AU Page, RA Ryan, MJ AF Page, RA Ryan, MJ TI Flexibility in assessment of prey cues: frog-eating bats and frog calls SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE behavioural flexibility; predator-prey interactions; reversal learning; eavesdropping; Trachops cirrhosus; Physalaemus pustulosus ID FRINGE-LIPPED BAT; TRACHOPS-CIRRHOSUS; DOMESTIC CHICKS; WARNING SIGNALS; APIS-MELLIFERA; PREDATION; HONEYBEES; PATTERN; PHYLLOSTOMIDAE; ECHOLOCATION AB Predators use cues associated with their prey to assess prey quality and to avoid consuming poisonous prey. Considerable attention has been given to predators' use of aposematic cues to assess prey quality, but little is known about predators that eavesdrop on prey cues that are not intended for them. Here we investigate the prey-cue/prey-quality associations of a predator that eavesdrops on the sexual advertisement signals of its prey. Stability is expected in prey-cue/prey-quality associations when mistakes in prey assessment are lethal. Conversely, flexibility is possible when mistakes are less costly. Predators that must respond to temporal and spatial fluctuations in prey availability should be more flexible in their assessment of prey quality. Given these predictions, we examined flexibility in the ability of wild-caught bats to reverse prey-cue/prey-quality associations for a preferred prey and a poisonous one. We found that the predatory bat, Trachops cirrhosus, has a heretofore undescribed ability to reverse its evaluations of the cues that signal preferred prey. C1 Univ Texas, Sect Integrat Biol, Austin, TX 78712 USA. Smithsonian Trop Res Inst, Balboa, Panama. RP Page, RA (reprint author), Univ Texas, Sect Integrat Biol, Austin, TX 78712 USA. EM rachelpage@mail.utexas.edu NR 48 TC 34 Z9 36 U1 1 U2 21 PU ROYAL SOCIETY PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8452 J9 P ROY SOC B-BIOL SCI JI Proc. R. Soc. Lond. Ser. B-Biol. Sci. PD APR 22 PY 2005 VL 272 IS 1565 BP 841 EP 847 DI 10.1098/rspb.2004.2998 PG 7 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 935LL UT WOS:000229783700010 PM 15888417 ER PT J AU Krot, AN Yurimoto, H Hutcheon, ID MacPherson, GJ AF Krot, AN Yurimoto, H Hutcheon, ID MacPherson, GJ TI Chronology of the early Solar System from chondrule-bearing calcium-aluminium-rich inclusions SO NATURE LA English DT Article ID REFRACTORY INCLUSIONS; FERROMAGNESIAN CHONDRULES; CONTEMPORANEOUS FORMATION; ISOTOPE EVIDENCE; NEBULA; EVAPORATION; CHONDRITES; GAS AB Chondrules and Ca-Al-rich inclusions (CAIs) are high-temperature components of meteorites that formed during transient heating events in the early Solar System. A major unresolved issue is the relative timing of CAI and chondrule formation(1-4). From the presence of chondrule fragments in an igneous CAI, it was concluded that some chondrules formed before CAIs (ref. 5). This conclusion is contrary to the presence of relict CAIs inside chondrules(6-10), as well as to the higher abundance of Al-26 in CAIs(11); both observations indicate that CAIs predate chondrules by 1-3 million years (Myr). Here we report that relict chondrule material in the Allende meteorite, composed of olivine and low-calcium pyroxene, occurs in the outer portions of two CAIs and is O-16-poor (Delta(17)O approximate to -1 parts per thousand to -5 parts per thousand). Spinel and diopside in the CAI cores are O-16-rich (Delta(17)O up to -20 parts per thousand), whereas diopside in their outer zones, as well as melilite and anorthite, are O-16-depleted (Delta(17)O = -8 parts per thousand to 2 parts per thousand). Both chondrule-bearing CAIs are Al-26-poor with initial Al-26/Al-27 ratios of (4.7 +/- 1.4) x 10(-6) and <1.2 x 10(-6). We conclude that these CAIs had chondrule material added to them during a re-melting episode similar to 2 Myr after formation of CAIs with the canonical Al-26/Al-27 ratio of 5 x 10(-5). C1 Univ Hawaii Manoa, Sch Ocean & Earth Sci & Technol, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA. Tokyo Inst Technol, Dept Earth & Planetary Sci, Meguro Ku, Tokyo 1528551, Japan. Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94451 USA. Lawrence Livermore Natl Lab, GT Seaborg Inst, Livermore, CA 94451 USA. Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. RP Krot, AN (reprint author), Univ Hawaii Manoa, Sch Ocean & Earth Sci & Technol, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA. EM sasha@higp.hawaii.edu NR 29 TC 55 Z9 55 U1 2 U2 9 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD APR 21 PY 2005 VL 434 IS 7036 BP 998 EP 1001 DI 10.1038/nature03470 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 918EH UT WOS:000228524600032 PM 15846340 ER PT J AU Fang, TT Croft, RAC Sanders, WT Houck, J Dave, R Katz, N Weinberg, DH Hernquist, L AF Fang, TT Croft, RAC Sanders, WT Houck, J Dave, R Katz, N Weinberg, DH Hernquist, L TI Simulation of soft X-ray emission lines from the missing baryons SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : theory; diffuse radiation; intergalactic medium; large-scale structure of universe; X-rays : diffuse background ID HOT INTERGALACTIC MEDIUM; LY-ALPHA FOREST; PARTICLE HYDRODYNAMICS SIMULATIONS; DARK-MATTER MODEL; LOW-REDSHIFT; O VI; COSMOLOGICAL SIMULATIONS; IONIZATION EQUILIBRIUM; SURFACE BRIGHTNESS; CHANDRA DETECTION AB We study the soft X-ray emission (0.1-1 keV) from the warm-hot intergalactic medium (WHIM) in a hydrodynamic simulation of a cold dark matter universe. Our main goal is to investigate how such emission can be explored with a combination of imaging and spectroscopy and to motivate future X-ray missions. We first present high-resolution images of the X-ray emission in several energy bands in which emission from different ion species dominates. We pick three different areas to study the high-resolution spectra of X-rays from the WHIM: (1) a galaxy group, (2) a filament, and (3) an underluminous region. By taking into account the background X-ray emission from AGNs and foreground emission from the Galaxy, we compute composite X-ray spectra of the selected regions. We briefly investigate angular clustering of the soft X-ray emission, finding a strong signal. Most interestingly, the combination of high spectral resolution and angular information allows us to map the emission from the WHIM in three dimensions. We cross-correlate the positions of galaxies in the simulation with this redshift map of emission and detect the presence of six different ion species (Ne IX, Fe XVII, O VII, O VIII, N VII, and C VI) in the large-scale structure traced by the galaxies. Finally, we show how such emission can be detected and studied with future X-ray satellites, with particular attention to a proposed mission, the Missing Baryon Explorer (MBE). We present simulated observations of the WHIM gas with MBE. C1 Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA. Univ Wisconsin, Madison, WI 53706 USA. MIT, Ctr Space Res, Cambridge, MA 02139 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Univ Massachusetts, Dept Phys & Astron, Amherst, MA 01003 USA. Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Fang, TT (reprint author), Carnegie Mellon Univ, Dept Phys, 5000 Forbes Ave, Pittsburgh, PA 15213 USA. EM fangt@astro.berkeley.edu RI Croft, Rupert/N-8707-2014 OI Croft, Rupert/0000-0003-0697-2583 NR 79 TC 16 Z9 16 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 20 PY 2005 VL 623 IS 2 BP 612 EP 626 DI 10.1086/428656 PN 1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 917GU UT WOS:000228445500002 ER PT J AU Narayan, R McClintock, JE AF Narayan, R McClintock, JE TI Inclination effects and beaming in black hole X-ray binaries SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; radiation mechanisms : nonthermal; X-rays : binaries ID ADVECTION-DOMINATED ACCRETION; NOVA MUSCAE 1991; OPTICAL LIGHT CURVES; CYGNUS X-1; GRO J1655-40; INFRARED PHOTOMETRY; DYNAMICAL EVIDENCE; RELATIVISTIC JETS; SPECTRAL STATE; LOW/HARD STATE AB We investigate the dependence of observational properties of black hole X-ray binaries on the inclination angle i of their orbits. We find the following: ( 1) Transient black hole binaries show no trend in their quiescent X-ray luminosities as a function of i, suggesting that the radiation is not significantly beamed. This is consistent with emission from an accretion disk. If the X-rays are from a jet, then the Lorentz factor gamma of the jet is < 1.24 at the 90% confidence level. ( 2) The X-ray binary 4U 1543 - 47 with i similar to 21 degrees has a surprisingly strong fluorescent iron line in the high soft state. Quantifying an earlier argument by Park et al., we conclude that if the continuum X-ray emission in this source is from a jet, then gamma < 1.04. (3) None of the known binaries has cos i < 0.25 or i > 75 degrees. This fact, plus the lack of eclipses among the 20 black hole binaries in our sample, strongly suggests at the 99.5% confidence level that systems with large inclination angles are hidden from view. The obscuration could be the result of disk flaring, as suggested by Milgrom for neutron star X-ray binaries. ( 4) Transient black hole binaries with i similar to 70 degrees - 75 degrees have significantly more complex X-ray light curves than systems with i less than or similar to 65 degrees. This may be the result of variable obscuration and/or variable height above the disk of the radiating gas. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Narayan, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM rnarayan@cfa.harvard.edu; jem@cfa.harvard.edu OI Narayan, Ramesh/0000-0002-1919-2730 NR 72 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 APR 20 PY 2005 VL 623 IS 2 BP 1017 EP 1025 DI 10.1086/428709 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 917GU UT WOS:000228445500032 ER PT J AU Luhman, KL McLeod, KK Goldenson, N AF Luhman, KL McLeod, KK Goldenson, N TI A Hubble Space Telescope search for substellar companions in the young cluster IC 348 SO ASTROPHYSICAL JOURNAL LA English DT Review DE binaries : close; planetary systems : formation; stars : low-mass, brown dwarfs; stars : pre-main-sequence; techniques : high angular resolution ID BROWN DWARF COMPANION; LOW-MASS BINARIES; STAR-FORMING REGIONS; MAIN-SEQUENCE STARS; SOLAR-TYPE STARS; T-TAURI STARS; ORION TRAPEZIUM CLUSTER; ADAPTIVE OPTICS SURVEY; PLANETARY CAMERA 2; IC 348 AB We present the results of a search for substellar companions to members of the star-forming cluster IC 348. Using the Wide Field Planetary Camera 2 on board the Hubble Space Telescope, we have obtained deep, high-resolution images of the cluster through the F791W and F850LP filters. These data encompass 150 known members of IC 348, including 14 primaries that are likely to be substellar (M-1 = 0.015-0.08 M-.). The detection limits for companions to low-mass stars and brown dwarfs in the PC images are Delta(m791) = 0, 2.5, and 5.5 at separations of 0.'' 05, 0.'' 1, and 0.'' 3, respectively, which correspond to M-2/M-1 = 1, 0.3, and 0.1 at 15, 30, and 90 AU. Meanwhile, for heavily saturated solar-mass primaries in the WFC images, the limits are Delta m(791) = 0 and 6 (M-2/M-1 = 1 and 0.04) at 0.'' 2 and 0.'' 4. The sky limiting magnitude of m(791) similar to 26 at large separations from a primary corresponds to a mass of similar to 0.006 M-. according to the evolutionary models of Chabrier and Baraffe. Point sources appearing near known and candidate cluster members are classified as either field stars or likely cluster members through their positions on the color-magnitude diagram constructed from the WFPC2 photometry. For the two faintest candidate companions appearing in these data, we have obtained 0.8 - 2.5 mu m spectra with SpeX at the IRTF. Through a comparison to spectra of optically classified dwarfs, giants, and pre-main-sequence objects, we classify these two sources as cluster members with spectral types near M6, corresponding to masses of similar to 0.1 M-. with the models of Chabrier and Baraffe. Thus, no probable substellar companions are detected in this survey. After considering all potential binaries within our WFPC2 images, we find that the frequencies of stellar and substellar companions within 0.'' 4 - 5 '' (120 - 1600 AU) from low-mass stars (M-1 = 0.08 0.5) in IC 348 agree within the uncertainties with measurements in the field. The factor of similar to 3 - 10 deficiency in brown dwarfs relative to stars among companions at wide separations in IC 348 and across the much larger range of separations probed for field stars in previous work is equal within the uncertainties to the deficiency in brown dwarfs in measurements of mass functions of isolated objects. In other words, when defined relative to stars, the brown dwarf "desert'' among companions is also present among isolated objects, which is expected if stellar and substellar companions form in the same manner as their free-floating counterparts. Meanwhile, among the 14 substellar primaries in our survey of IC 348, no companions are detected. This absence of wide binary brown dwarfs is statistically consistent with the frequency of wide binary stars in IC 348. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Wellesley Coll, Whitin Observ, Wellesley, MA 02481 USA. Wesleyan Univ, Dept Astron, Wesleyan Stn, Middletown, CT 06459 USA. RP Luhman, KL (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM kluhman@cfa.harvard.edu; kmcleod@wellesley.edu; ngoldenson@wesleyan.edu NR 106 TC 33 Z9 33 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 APR 20 PY 2005 VL 623 IS 2 BP 1141 EP 1156 DI 10.1086/429154 PN 1 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 917GU UT WOS:000228445500042 ER PT J AU Karovska, M Schlegel, E Hack, W Raymond, JC Wood, BE AF Karovska, M Schlegel, E Hack, W Raymond, JC Wood, BE TI A large X-ray outburst in Mira A SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : symbiotic; stars : activity; stars : AGB and post-AGB; stars : individual (Mira AB); stars : winds, outflows; X-rays : general ID HUBBLE-SPACE-TELESCOPE; GIANT BRANCH STARS; ULTRAVIOLET-SPECTRA; BINARY-SYSTEM; H-2 EMISSION; CH CYGNI AB We report the Chandra ACIS-S detection of a bright soft X-ray transient in the Mira AB interacting symbiotic-like binary. We have resolved the system for the first time in X-rays. Using Chandra and Hubble Space Telescope images, we determine that the unprecedented outburst is likely associated with the cool asymptotic giant branch (AGB) star, Mira A, the prototype of the Mira class of variables. X-rays have never before been detected from an AGB star, and the recent activity signals that the system is undergoing dramatic changes. The total X-ray luminosity of the system is several times higher than the luminosity estimated using previous XMM-Newton and ROSAT observations. The outburst may be caused by a giant flare in Mira A associated with a mass ejection or a jet and may have long-term consequences on the system. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Univ Colorado, Joint Inst Lab Astrophys, Boulder, CO 80309 USA. Natl Inst Stand & Technol, Boulder, CO 80309 USA. RP Karovska, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 21 TC 59 Z9 59 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 APR 20 PY 2005 VL 623 IS 2 BP L137 EP L140 DI 10.1086/430111 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 917GV UT WOS:000228445600019 ER PT J AU Risaliti, G Elvis, M Fabbiano, G Baldi, A Zezas, A AF Risaliti, G Elvis, M Fabbiano, G Baldi, A Zezas, A TI Rapid compton-thick/compton-thin transitions in the Seyfert 2 galaxy NGC 1365 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : individual (NGC 1365); X-rays : galaxies ID ACTIVE GALACTIC NUCLEI; ABSORBING COLUMN DENSITIES; NGC 1365; VARIABILITY; LUMINOSITY; NGC-4151; ATLAS AB We present multiple Chandra and XMM-Newton observations of the type 1.8 Seyfert galaxy NGC 1365, which shows the most dramatic X-ray spectral changes observed so far in an active galactic nucleus: the source switched from reflection-dominated to transmission-dominated and back in just 6 weeks. During this time the soft thermal component, arising from an similar to 1 kpc region around the center, remained constant. The reflection component is constant at all timescales, and its high flux relative to the primary component implies the presence of thick gas covering a large fraction of the solid angle. The presence of this gas, and the fast variability timescale, suggest that the Compton-thick to Compton-thin change is due to variation in the line-of-sight absorber rather than to extreme intrinsic emission variability. We discuss a structure of the circumnuclear absorber/reflector that can explain the observed X-ray spectral and temporal properties. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy. RP Risaliti, G (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM grisaliti@cfa.harvard.edu RI Zezas, Andreas/C-7543-2011; OI Zezas, Andreas/0000-0001-8952-676X; Risaliti, Guido/0000-0002-3556-977X NR 26 TC 149 Z9 149 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 APR 20 PY 2005 VL 623 IS 2 BP L93 EP L96 DI 10.1086/430252 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 917GV UT WOS:000228445600008 ER PT J AU Walker, GAH Kuschnig, R Matthews, JM Reegen, P Kallinger, T Kambe, E Saio, H Harmanec, P Guenther, DB Moffat, AFJ Rucinski, SM Sasselov, D Weiss, WW Bohlender, DA Bozic, H Hashimoto, O Koubsky, P Mann, R Ruzdjak, D Skoda, P Slechta, M Sudar, D Wolf, M Yang, S AF Walker, GAH Kuschnig, R Matthews, JM Reegen, P Kallinger, T Kambe, E Saio, H Harmanec, P Guenther, DB Moffat, AFJ Rucinski, SM Sasselov, D Weiss, WW Bohlender, DA Bozic, H Hashimoto, O Koubsky, P Mann, R Ruzdjak, D Skoda, P Slechta, M Sudar, D Wolf, M Yang, S TI Pulsations of the Oe star zeta Ophiuchi from MOST satellite1 photometry and ground-based spectroscopy SO ASTROPHYSICAL JOURNAL LA English DT Article DE line : profiles; stars : early-type; stars : emission-line, Be; stars : individual (zeta Ophiuchi); stars : oscillations; stars : rotation ID TIME-SERIES OBSERVATIONS; LINE-PROFILE VARIATIONS; EPISODIC MASS-LOSS; B-TYPE STARS; NONRADIAL OSCILLATIONS; LIGHT VARIATIONS; ROTATION; STELLAR; PARAMETERS; SPACE AB Twenty-four days of highly precise Microvariability and Oscillations of Stars ( MOST) satellite photometry obtained in mid-2004 of the rapidly rotating O9.5 V star zeta Oph have yielded at least a dozen significant oscillation frequencies between 1 and 10 cycles day(-1), clearly indicating its relationship to beta Cephei variables. Eight periods were found in He I lambda 4922 and H beta line profile variations (LPV) of which six coincide with those from the MOST photometry. This unique photometric and spectroscopic detection of radial and nonradial pulsations leads to a plausible model in which high l-modes are excited when their frequencies in the corotating frame are similar to those of low-order radial modes. We propose that the dominant photometric 4.6 hr period (f(1)) corresponds to a radial first overtone excited by the k-mechanism associated with the Fe opacity bump. No unambiguous rotational period can be identified in either the light curve or the LPV. C1 Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. Univ Vienna, Inst Astron, A-1180 Vienna, Austria. Natl Def Acad, Dept Earth & Ocean Sci, Kanagawa 2398686, Japan. Tohoku Univ, Inst Astron, Grad Sch Sci, Sendai, Miyagi 9808578, Japan. Charles Univ, Astron Inst, CZ-18000 Prague, Czech Republic. Acad Sci Czech Republ, Inst Astron, CZ-25165 Ondrejov, Czech Republic. St Marys Univ, Dept Astron & Phys, Halifax, NS B3H 3C3, Canada. Univ Montreal, Dept Phys, Mont Megant Observ, Montreal, PQ H3C 3J7, Canada. Univ Toronto, David Dunlap Observ, Dept Astron & Astrophys, Richmond Hill, ON L4C 4Y6, Canada. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. Univ Zagreb, Hvar Observ, Fac Geodesy, Zagreb 10000, Croatia. Gunma Astron Observ, Gunma 3770702, Japan. Univ Victoria, Dept Phys & Astron, Victoria, BC V8W 3P6, Canada. RP Walker, GAH (reprint author), Univ British Columbia, Dept Phys & Astron, 6224 Agr Rd, Vancouver, BC V6T 1Z1, Canada. EM gordonwa@uvic.ca; matthews@astro.ubc.ca; hec@pleione.asu.cas.cz RI Koubsky, Pavel/G-9031-2014; Slechta, Miroslav/G-9048-2014; Skoda, Petr/G-9047-2014 OI Skoda, Petr/0000-0002-7434-9518 NR 23 TC 44 Z9 44 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 APR 20 PY 2005 VL 623 IS 2 BP L145 EP L148 DI 10.1086/430254 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 917GV UT WOS:000228445600021 ER PT J AU Turner, BL Cade-Menun, BJ Condron, LM Newman, S AF Turner, BL Cade-Menun, BJ Condron, LM Newman, S TI Extraction of soil organic phosphorus SO TALANTA LA English DT Article DE bioavailability; DNA; extraction; inositol phosphate; NMR spectroscopy; organic phosphorus; sequential fractionation; soil AB Organic phosphorus is an important component of soil biogeochemical cycles, but must be extracted from soil prior to analysis. Here we critically review the extraction of soil organic phosphorus, including procedures for quantification, speciation, and assessment of biological availability. Quantitative extraction conventionally requires strong acids and bases, which inevitably alter chemical structure. However, a single-step procedure involving sodium hydroxide and EDTA (ethylenediaminetetraacetate) is suitable for most soils and facilitates subsequent speciation by nuclear magnetic resonance spectroscopy. Analysis of extracts by molybdate colorimetry is a potential source of error in all procedures, because organic phosphorus is overestimated in the presence of inorganic polyphosphates or complexes between inorganic phosphate and humic substances. Sequential extraction schemes fractionate organic phosphorus based on chemical solubility, but the link to potential bioavailability is misleading. Research should be directed urgently towards establishing extractable pools of soil organic phosphorus with ecological relevance. (c) 2004 Elsevier B.V. All rights reserved. C1 Smithsonian Trop Res Inst, Balboa, Ancon, Panama. Stanford Univ, Stanford, CA 94305 USA. Lincoln Univ, Canterbury 8150, New Zealand. S Florida Water Management Dist, W Palm Beach, FL 33406 USA. RP Turner, BL (reprint author), Smithsonian Trop Res Inst, Box 2072, Balboa, Ancon, Panama. EM bturner@ufl.edu RI Turner, Benjamin/E-5940-2011; Condron, Leo/E-9458-2013; OI Turner, Benjamin/0000-0002-6585-0722; Cade-Menun, Barbara/0000-0003-4391-3718 NR 0 TC 155 Z9 171 U1 17 U2 97 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0039-9140 J9 TALANTA JI Talanta PD APR 15 PY 2005 VL 66 IS 2 BP 294 EP 306 DI 10.1016/j.talanta.2004.11.012 PG 13 WC Chemistry, Analytical SC Chemistry GA 929WR UT WOS:000229377800003 PM 18969994 ER PT J AU Rueda, LM AF Rueda, LM TI Two new species of Anopheles (Anopheles) Hyrcanus Group (Diptera : Culicidae) from the Republic of South Korea SO ZOOTAXA LA English DT Article DE Anopheles belenrae; kleini; Culicidae; taxonomy; description; mosquitoes; Hyrcanus Group ID GENUS ANOPHELES AB Two new mosquito species belonging to the Hyrcanus Group, Anopheles (Anopheles) belenrae Rueda and An. (Ano.) kleini Rueda, are described from the Republic of South Korea, with illustrations of the larvae, pupae, adults, and male genitalia. C1 Walter Reed Army Inst Res, Dept Entomol, Silver Spring, MD 20910 USA. RP Rueda, LM (reprint author), Smithsonian Inst, Museum Support Ctr, Walter Reed Biosystemat Unit, 4210 Silver Hill Rd, Suitland, MD 20746 USA. EM ruedapol@si.edu NR 15 TC 42 Z9 52 U1 1 U2 1 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD APR 15 PY 2005 IS 941 BP 1 EP 26 PG 26 WC Zoology SC Zoology GA 918DC UT WOS:000228518600001 ER PT J AU Jamieson, MJ Cheung, ASC AF Jamieson, MJ Cheung, ASC TI Shifts in the A(2)Sigma(+)-(XII)-I-2 band systems of (OH)-O-16, (OH)-O-18, (OD)-O-16 and (OD)-O-18 SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS LA English DT Article ID THEORETICAL-ANALYSIS; OH A2-SIGMA+; LEVEL SHIFTS; PREDISSOCIATION; STATES; MOLECULE; LIFETIMES; ATOMS AB We calculate and present the shifts that are induced by predissociation of the band origins in the A(2)Sigma(+)-X(2)Pi system of the hydroxyl radical (OH)-O-16, using a sum rule method in which the projection of the predissociating interaction onto a complete set of states is replaced by a single linear response. We present also the corresponding shifts for the isotopomers (OH)-O-18, (OD)-O-16 and (OD)-O-16. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Hong Kong, Dept Chem, Hong Kong, Hong Kong, Peoples R China. Univ Glasgow, Dept Comp Sci, Glasgow G12 8QQ, Lanark, Scotland. RP Jamieson, MJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 28 TC 0 Z9 0 U1 0 U2 0 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 APR 14 PY 2005 VL 38 IS 7 BP 939 EP 947 DI 10.1088/0953-4075/38/7/014 PG 9 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 927NM UT WOS:000229200600016 ER PT J AU Spinoglio, L Malkan, MA Smith, HA Gonzalez-Alfonso, E Fischer, J AF Spinoglio, L Malkan, MA Smith, HA Gonzalez-Alfonso, E Fischer, J TI The far-infrared emission line and continuum spectrum of the Seyfert galaxy NGC 1068 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : individual (NGC 1068); galaxies : nuclei; galaxies : Seyfert; galaxies : starburst; infrared : galaxies ID LONG-WAVELENGTH SPECTROMETER; MOLECULAR GAS; NGC 1068; STAR-FORMATION; CIRCUMNUCLEAR ENVIRONMENT; SPECTROSCOPY; CHEMISTRY; PERFORMANCE; ABUNDANCE; NUCLEUS AB We report on the analysis of the first complete far-infrared spectrum ( 43 - 197 mu m) of the Seyfert 2 galaxy NGC 1068 as observed with the Long Wavelength Spectrometer (LWS) on board the Infrared Space Observatory (ISO). In addition to the seven expected ionic fine-structure emission lines, the OH rotational lines at 79, 119, and 163 mu m were all detected in emission, which is unique among galaxies with full LWS spectra, where the 119 mu m line, when detected, is always in absorption. The observed line intensities were modeled together with ISO -> Short Wavelength Spectrometer (SWS) and optical and ultraviolet line intensities from the literature, considering two independent emission components: the active galactic nucleus (AGN) component and the starburst component in the circumnuclear ring of similar to 3 kpc in size. Using the UV to mid-IR emission line spectrum to constrain the nuclear ionizing continuum, we have confirmed previous results: a canonical power-law ionizing spectrum is a poorer fit than one with a deep absorption trough, while the presence of a "big blue bump'' is ruled out. Based on the instantaneous starburst age of 5 Myr constrained by the Br gamma equivalent width in the starburst ring, and starburst synthesis models of the mid- and far-infrared fine-structure line emission, a low-ionization parameter ( U = 10(-3.5)) and low densities ( n = 100 cm(-3)) are derived. Combining the AGN and starburst components, we succeeded in modeling the overall UV to far-IR atomic spectrum of NGC 1068, reproducing the line fluxes to within a factor of 2.0 on average with a standard deviation of 1.3, and the overall continuum as the sum of the contribution of the thermal dust emission in the ionized and neutral components. The OH 119 mu m emission indicates that the line is collisionally excited and arises in a warm and dense region. The OH emission has been modeled using spherically symmetric, nonlocal, non-LTE radiative transfer models. The models indicate that the bulk of the emission arises from the nuclear region, although some extended contribution from the starburst is not ruled out. The OH abundance in the nuclear region is expected to be similar to 10(-5), characteristic of X-ray - dominated regions. C1 CNR, Ist Fis Spazio Interplanetario, I-00133 Rome, Italy. Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Alcala de Henares, Dept Fis, E-28871 Alcala De Henares, Madrid, Spain. USN, Res Lab, Washington, DC 20375 USA. RP Spinoglio, L (reprint author), CNR, Ist Fis Spazio Interplanetario, Via Fosso del Cavaliere 100, I-00133 Rome, Italy. EM luigi@ifsi.rm.cnr.it; malkan@astro.ucla.edu; hsmith@cfa.harvard.edu; eduardo.gonzalez@uah.es; jackie.fischer@nrl.navy.mil OI Spinoglio, Luigi/0000-0001-8840-1551 NR 55 TC 41 Z9 41 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 APR 10 PY 2005 VL 623 IS 1 BP 123 EP 136 DI 10.1086/428495 PN 1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 914AV UT WOS:000228197700012 ER PT J AU Smith, RK Edgar, RJ Plucinsky, PP Wargelin, BJ Freeman, PE Biller, BA AF Smith, RK Edgar, RJ Plucinsky, PP Wargelin, BJ Freeman, PE Biller, BA TI Chandra observations of MBM 12 and models of the local bubble SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : bubbles; plasmas; supernova remnants; X-rays : ISM ID RAY BACKGROUND FLUX; INTERSTELLAR-MEDIUM; SOLAR-WIND; CHARGE-TRANSFER; HOT GAS; O VI; EMISSION; LINE; RECOMBINATION; SPECTRA AB Chandra observations toward the nearby molecular cloud MBM 12 show unexpectedly strong and nearly equal foreground O VIII and O VII emission. As the observed portion of MBM 12 is optically thick at these energies, the emission lines must be formed nearby, coming from either the Local Bubble (LB) or charge exchange with ions from the Sun. Equilibrium models for the LB predict stronger O VII than O VIII, so these results suggest that the LB is far from equilibrium or that a substantial portion of OVIII is from another source, such as charge exchange within the solar system. Despite the likely contamination, we can combine our results with other EUV and X-ray observations to reject LB models that posit a cool recombining plasma as the source of LB X-rays. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Carnegie Mellon Univ, Dept Stat, Pittsburgh, PA 15213 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. RP Smith, RK (reprint author), NASA, Goddard Space Flight Ctr, Code 662, Greenbelt, MD 20771 USA. EM rsmith@milkyway.gsfc.nasa NR 66 TC 37 Z9 37 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 APR 10 PY 2005 VL 623 IS 1 BP 225 EP 234 DI 10.1086/428568 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 914AV UT WOS:000228197700021 ER PT J AU Fish, VL Reid, MJ Menten, KM AF Fish, VL Reid, MJ Menten, KM TI Magnetic field clumping in massive star-forming regions as determined from excited-state OH absorption and maser emission SO ASTROPHYSICAL JOURNAL LA English DT Article DE HII regions; ISM : magnetic fields; ISM : molecules; masers; radio lines : ISM; stars : formation ID H-II REGIONS; INTERSTELLAR HYDROXYL MASERS; VLA OBSERVATIONS; SATELLITE LINES; PROPER MOTIONS; DENSE GAS; W3 OH; 5 CM; W3(OH); GHZ AB We have observed six high-mass-star -forming regions in the (2)Pi(3/2), J = 7/2 lines of OH using the Green Bank Telescope (GBT) in order to investigate whether the magnetic field, and hence the density, measured in absorption differs from that implied by maser Zeeman splitting. We detect absorption in both the 13,441 and 13,434 MHz main lines in all six sources. Zeeman splitting in the F = 3(+) --> 3(-) absorption line in W3(OH) implies a line-of-sight magnetic field strength of 3.0 +/- 0.3 mG. This is significantly less than full magnetic field strengths detected from OH maser Zeeman splitting, suggesting that OH maser regions may be denser than the nonmasing OH material by a factor of several. Zeeman splitting is not detected in other sources, but we are able to place upper limits on B-parallel to of 1.2 mG in G10.624 - 0.385 and 2.9 mG in K3-50. These results are consistent with a density enhancement of the masers, but other explanations for the lower magnetic field in absorption compared to maser emission are possible for these two sources. Absorption in one or both of the 13,442 and 13,433 MHz satellite lines is also seen in four sources. This is the very first detection of the (2)Pi(3/2), J = 7/2 satellite lines. Ratios of satellite-line to main-line absorption suggest enhancement of the satellite lines from local thermodynamic equilibrium values. Masers are seen in the F = 4(+) --> 4(-) and 3(+) --> 3(-) transitions of W3(OH) and the 4(+) --> 4(-) transition of ON 1. A previously undetected 4(+) --> 4(-) maser is seen near -44.85 km s(-1) in W3(OH). C1 Natl Radio Astron Observ, Socorro, NM 87801 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Max Planck Inst Radioastron, D-53121 Bonn, Germany. RP Fish, VL (reprint author), Natl Radio Astron Observ, POB O,1003 Lopezville Rd, Socorro, NM 87801 USA. EM vfish@nrao.edu; reid@cfa.harvard.edu; kmenten@mpifr-bonn.mpg.de NR 37 TC 11 Z9 11 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 APR 10 PY 2005 VL 623 IS 1 BP 269 EP 279 DI 10.1086/428651 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 914AV UT WOS:000228197700025 ER PT J AU Myers, PC AF Myers, PC TI Centrally condensed collapse of starless cores SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : clouds; stars : formation ID MOLECULAR CLOUD CORES; PRE-PROTOSTELLAR CORES; DENSE CORES; DARK CLOUDS; GRAVITATIONAL COLLAPSE; AMBIPOLAR DIFFUSION; INITIAL CONDITIONS; INFALL MOTIONS; INTERSTELLAR CLOUDS; ISOTHERMAL SPHERES AB Models of self-gravitating gas in the early stages of pressure-free collapse are compared for initial states that are equilibrium layers, cylinders, and "Bonnor-Ebert'' spheres. For each geometrical case the density profile has an inner region of shallow slope surrounded by an outer region of steep slope, and the profile shape during early collapse remains similar to the profile shape of the initial equilibrium. The two-slope density structure divides the spherical collapse history into a starless infall phase and a protostellar accretion phase. The similarity of density profiles implies that Bonnor-Ebert fits to observed column density maps may not distinguish spherical cores from oblate or prolate cores and may not distinguish static cores from collapsing cores. The velocity profiles discriminate better than the density profiles between initial geometries and between collapse ages. The infall velocity generally has a subsonic maximum value, which is approximately equal to the initial velocity dispersion times the ratio of collapse age to central free-fall time. Observations of starless-core line profiles constrain collapse models. Collapse from initial states that are strongly condensed and slightly prolate is consistent with "infall asymmetry'' observed around starless cores and is more consistent than collapse from initial states that are weakly condensed and/or oblate. Spherical models match observed inward speeds of 0.05 - 0.09 km s(-1) over 0.1 - 0.2 pc if the collapse has a typical age of 0.3 - 0.5 free-fall times and if it began from a centrally condensed state that was not in stable equilibrium. In a collapsing core, optically thin line profiles should broaden and develop a two-peak structure, as seen in L1544, once the typical infall velocity approaches the molecular velocity dispersion or when the collapse age exceeds similar to 0.4 free-fall times, for typical parameters, independent of depletion. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Myers, PC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM pmyers@cfa.harvard.edu NR 87 TC 41 Z9 41 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 APR 10 PY 2005 VL 623 IS 1 BP 280 EP 290 DI 10.1086/428386 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 914AV UT WOS:000228197700026 ER PT J AU Homan, J Miller, JM Wijnands, R van der Klis, M Belloni, T Steeghs, D Lewin, WHG AF Homan, J Miller, JM Wijnands, R van der Klis, M Belloni, T Steeghs, D Lewin, WHG TI High- and low-frequency quasi-periodic oscillations in the X-ray light curves of the black hole transient H1743-322 SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars : individual (H1743-322); stars : oscillations; X-rays : binaries; X-rays : stars ID CANDIDATE XTE J1550-564; GRO J1655-40; TIMING EXPLORER; 4U 1630-47; UNIFIED DESCRIPTION; 2000 OUTBURST; GX 339-4; VARIABILITY; BINARIES; GRS-1915+105 AB We present a variability study of the black hole candidate and X-ray transient H1743 - 322 during its 2003 2004 outburst. We analyzed five Rossi X-Ray Timing Explorer observations that were performed as part of a multiwavelength campaign, as well as six observations from the early rise of the outburst. The source was observed in several black hole states and showed various types of X-ray variability, including high-frequency quasi-periodic oscillations (QPOs) at 240 and 160 Hz (i.e., with a 3: 2 frequency ratio), several types of low-frequency QPOs, and strong variations on a timescale of a few hundred seconds. The discovery of high-frequency QPOs in H1743 - 322 supports predictions that these QPOs should be more easily observed in high inclination systems. In one of our observations a transition in count rate and color occurred, during which we were able to follow the smooth evolution of the low-frequency QPOs from type B to type A. We classify the X-ray observations and QPOs and briefly discuss the QPOs in terms of recently proposed models. C1 MIT, Ctr Space Res, Cambridge, MA 02139 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. INAF, Osservatorio Astron Brera, I-23807 Merate, LC, Italy. RP Homan, J (reprint author), MIT, Ctr Space Res, 70 Vassar St, Cambridge, MA 02139 USA. RI Steeghs, Danny/C-5468-2009 OI Steeghs, Danny/0000-0003-0771-4746 NR 62 TC 80 Z9 81 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 APR 10 PY 2005 VL 623 IS 1 BP 383 EP 391 DI 10.1086/424994 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 914AV UT WOS:000228197700035 ER PT J AU Gaudi, BS Seager, S Mallen-Ornelas, G AF Gaudi, BS Seager, S Mallen-Ornelas, G TI On the period distribution of close-in extrasolar giant planets SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems : formation ID GRAVITATIONAL LENSING EXPERIMENT; LUMINOSITY OBJECT TRANSITS; GALACTIC DISK; SOLAR PLANETS; 2001 CAMPAIGN; HOT JUPITERS; PARENT STAR; FOLLOW-UP; SEARCH; MASS AB Transit (TR) surveys for extrasolar planets have recently uncovered a population of "very hot Jupiters,'' planets with orbital periods of P <= 3 days. At first sight this may seem surprising, given that radial velocity ( RV) surveys have found a dearth of such planets, despite the fact that their sensitivity increases with decreasing P. We examine the confrontation between RV and TR survey results, paying particular attention to selection biases that favor short-period planets in TR surveys. We demonstrate that, when such biases and small-number statistics are properly taken into account, the period distributions of planets found by RV and TR surveys are consistent at better than the 1 sigma level. This consistency holds for a large range of reasonable assumptions. In other words, there are not enough planets detected to robustly conclude that the RV and TR short-period planet results are inconsistent. Assuming a logarithmic distribution of periods, we find that the relative frequency of very hot Jupiters (VHJs; P = 1 3 days) to hot Jupiters (HJs; P = 3 9 days) is similar to 10% - 20%. Given an absolute frequency of HJs of similar to 1%, this implies that approximately one star in similar to 500 - 1000 has a VHJ. We also note that VHJs and HJs appear to be distinct in terms of their upper mass limits. We discuss the implications of our results for planetary migration theories as well as present and future TR and RV surveys. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC 20015 USA. RP Gaudi, BS (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM sgaudi@cfa.harvard.edu RI Gaudi, Bernard/I-7732-2012 NR 42 TC 95 Z9 96 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 APR 10 PY 2005 VL 623 IS 1 BP 472 EP 481 DI 10.1086/428478 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 914AV UT WOS:000228197700043 ER PT J AU Ko, YK Raymond, JC Gibson, SE Alexander, D Strachan, L Holzer, T Gilbert, H St Cyr, OC Thompson, BJ Pike, CD Mason, HE Burkepile, J Thompson, W Fletcher, L AF Ko, YK Raymond, JC Gibson, SE Alexander, D Strachan, L Holzer, T Gilbert, H St Cyr, OC Thompson, BJ Pike, CD Mason, HE Burkepile, J Thompson, W Fletcher, L TI Multialtitude observations of a coronal jet during the third Whole Sun Month Campaign SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun : corona; Sun : coronal mass ejections (CMEs) ID X-RAY JETS; EXTREME-ULTRAVIOLET JETS; H-ALPHA SURGES; MASS EJECTIONS; SOLAR MINIMUM; MAGNETIC RECONNECTION; OUTFLOW VELOCITIES; ATOMIC DATABASE; EMISSION-LINES; ACTIVE-REGION AB On 1999 August 26, a coronal jet occurred at the northwest limb near a sigmoid active region (AR 8668) that was the target for a joint observation plan ( SOHO joint observing program 106) during the third Whole Sun Month Campaign. This jet was observed by several instruments at the limb (SOHO/CDS, SOHO/EIT, TRACE, and Mauna Loa Solar Observatory CHIP and PICS) and at 1.64 R-. (SOHO/UVCS). At the limb, this jet event displayed both low- and high-temperature components. Both high- and low- temperature components were evident during the early phase ( first 20 minutes) of the event. However, the low- temperature component is maintained for similar to 1 hr after the higher temperature component is gone. There is a second brightening ( a possible second jet) seen by EIT and TRACE about 50 minutes after the onset of the first jet. The line-of-sight motion at the limb began with a 300 km s(-1) redshift and evolved to a 200 km s(-1) blueshift. At 1.64 R-., the intensities of Ly alpha and Ly beta in the jet increased by a factor of several hundred compared with the background corona. The C III lambda 977 line also brightened significantly. This indicates low- temperature [similar to(1-2) x 10(5) K] emission in the jet, while the intensities of O VI lambda 1032 and O VI lambda 1037 increased by as much as a factor of 8. The UVCS data show evidence of heating at the early phase of the event. The Doppler shift in the lines indicates that the line-of-sight (LOS) velocity in the jet started from similar to 150 km s(-1) in blueshift and ended at similar to 100 km s(-1) in redshift. This LOS motion seen at 1.64 R-. was apparently opposite to what was observed when the jet emerged from the limb. The Doppler dimming analysis indicates that the radial outflow speed correlates with the magnitude of the LOS speed. Interestingly, UVCS observations at 2.33 and 2.66 R-. show no trace of the jet and SOHO/LASCO observations also yield no firm detection. We find that a simple ballistic model can explain most of the dynamical properties of this jet, while the morphology and the thermal properties agree well with reconnection-driven X-ray jet models. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA. Rice Univ, Dept Phys & Astron, Houston, TX 77251 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Rutherford Appleton Lab, Dept Space Sci, Didcot OX11 0QX, Oxon, England. Univ Cambridge, Dept Appl Math & Theoret Phys, Cambridge CB3 0WA, England. GSI, Largo, MD 20774 USA. Univ Glasgow, Dept Phys & Astron, Glasgow G12 8QQ, Lanark, Scotland. RP Ko, YK (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Gibson, Sarah/A-9189-2011; Gilbert, Holly/C-7215-2012; Thompson, William/D-7376-2012; Thompson, Barbara/C-9429-2012 NR 42 TC 22 Z9 22 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 APR 10 PY 2005 VL 623 IS 1 BP 519 EP 539 DI 10.1086/428479 PN 1 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 914AV UT WOS:000228197700048 ER PT J AU Eksi, KY Hernquist, L Narayan, R AF Eksi, KY Hernquist, L Narayan, R TI Where are all the fallback disks? Constraints on propeller systems SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; pulsars : individual (SN 1987A); stars : neutron; X-rays : stars ID X-RAY PULSARS; NEUTRON-STAR ACCRETION; RADIO PULSARS; BLACK-HOLE; SPIN-DOWN; SN 1987A; MODEL; SUPERNOVAE; EVOLUTION; EMISSION AB Fallback disks are expected to form around newborn neutron stars following a supernova explosion. In almost all cases, the disk will pass through a propeller stage. If the neutron star is spinning rapidly ( initial period similar to 10 ms) and has an ordinary magnetic moment (similar to 10(30) G cm(3)), the rotational power transferred to the disk by the magnetic field of the neutron star will exceed the Eddington limit by many orders of magnitude, and the disk will be rapidly disrupted. Fallback disks can thus survive only around slow-born neutron stars and around black holes, assuming the latter do not torque their surrounding disks as strongly as do neutron stars. This might explain the apparent rarity of fallback disks around young compact objects. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Eksi, KY (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM yeksi@cfa.harvard.edu; lhernqui@cfa.harvard.edu; narayan@cfa.harvard.edu RI Eksi, Kazim/B-6434-2014; OI Eksi, Kazim/0000-0001-5999-0553; Narayan, Ramesh/0000-0002-1919-2730 NR 50 TC 31 Z9 31 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 APR 10 PY 2005 VL 623 IS 1 BP L41 EP L44 DI 10.1086/429915 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 914AX UT WOS:000228197900011 ER PT J AU Gupta, MP Solis, PN Calderon, AI Guionneau-Sinclair, F Correa, A Galdames, C Guerra, C Espinosa, A Alvenda, GI Robles, G Ocampo, R AF Gupta, MP Solis, PN Calderon, AI Guionneau-Sinclair, F Correa, A Galdames, C Guerra, C Espinosa, A Alvenda, GI Robles, G Ocampo, R TI Medical ethnobotany of the teribes of bocas del toro, panama (vol 96, pg 389, 2005) SO JOURNAL OF ETHNOPHARMACOLOGY LA English DT Correction C1 Univ Panama, Fac Farm, Ctr Invest Farmacognost Flora Panamena, CIFLORPAN,Estafeta Univ, Panama City, Panama. Smithsonian Trop Res Inst, Panama City, Panama. Univ Panama, Herbarium, Panama City, Panama. Ctr Agron Trop Invest & Ensenanza, Turrialba, Costa Rica. RP Gupta, MP (reprint author), Univ Panama, Fac Farm, Ctr Invest Farmacognost Flora Panamena, CIFLORPAN,Estafeta Univ, Apartado 10767, Panama City, Panama. EM cytedqff@ancon.up.ac.pa RI Guerra Torres, Carlos Patricio/H-3610-2014; OI Gupta, Mahabir/0000-0002-9302-7864 NR 1 TC 0 Z9 0 U1 0 U2 1 PU ELSEVIER SCI IRELAND LTD PI CLARE PA CUSTOMER RELATIONS MANAGER, BAY 15, SHANNON INDUSTRIAL ESTATE CO, CLARE, IRELAND SN 0378-8741 J9 J ETHNOPHARMACOL JI J. Ethnopharmacol. PD APR 8 PY 2005 VL 98 IS 1-2 BP 221 EP 221 DI 10.1016/j.jep.2005.01.001 PG 1 WC Plant Sciences; Chemistry, Medicinal; Integrative & Complementary Medicine; Pharmacology & Pharmacy SC Plant Sciences; Pharmacology & Pharmacy; Integrative & Complementary Medicine GA 912XR UT WOS:000228113700032 ER PT J AU Savov, IP Ryan, JG D'Antonio, M Kelley, K Mattie, P AF Savov, IP Ryan, JG D'Antonio, M Kelley, K Mattie, P TI Geochemistry of serpentinized peridotites from the Mariana Forearc Conical Seamount, ODP Leg 125: Implications for the elemental recycling at subduction zones SO GEOCHEMISTRY GEOPHYSICS GEOSYSTEMS LA English DT Article DE serpentinite; forearc; mantle; Marianas; subduction; Ocean Drilling Program; geochemistry : subduction zone processes; geochemistry : composition of the mantle; marine geology and geophysics : ocean drilling; geochemistry : geochemical cycles; volcanology : mud volcanism ID YOUNG VOLCANIC-ROCKS; RARE-EARTH PATTERNS; TRACE-ELEMENTS; OCEANIC-CRUST; MANTLE WEDGE; VENT-FIELD; ISLAND-ARC; BORON; SYSTEMATICS; ISOTOPES AB Recent examinations of the chemical fluxes through convergent plate margins suggest the existence of significant mass imbalances for many key species: only 20-30% of the to-the-trench inventory of large-ion lithophile elements (LILE) can be accounted for by the magmatic outputs of volcanic arcs. Active serpentinite mud volcanism in the shallow forearc region of the Mariana convergent margin presents a unique opportunity to study a new outflux: the products of shallow-level exchanges between the upper mantle and slab-derived fluids. ODP Leg 125 recovered serpentinized harzburgites and dunites from three sites on the crests and flanks of the active Conical Seamount. These serpentinites have U-shaped rare earth element (REE) patterns, resembling those of boninites. U, Th, and the high field strength elements (HFSE) are highly depleted and vary in concentration by up to 2 orders of magnitude. The low U contents and positive Eu anomalies indicate that fluids from the subducting Pacific slab were probably reducing in nature. On the basis of substantial enrichments of fluid-mobile elements in serpentinized peridotites, we calculated very large slab inventory depletions of B (79%), Cs (32%), Li (18%), As (17%), and Sb (12%). Such highly enriched serpentinized peridotites dragged down to depths of arc magma generation may represent an unexplored reservoir that could help balance the input-output deficit of these elements as observed by Plank and Langmuir (1993, 1998) and others. Surprisingly, many species thought to be mobile in fluids, such as U, Ba, Rb, and to a lesser extent Sr and Pb, are not enriched in the rocks relative to the depleted mantle peridotites, and we estimate that only 1-2% of these elements leave the subducting slabs at depths of 10 to 40 km. Enrichments of these elements in volcanic front and behind-the-front arc lavas point to changes in slab fluid composition at greater depths. C1 Univ S Florida, Dept Geol, Tampa, FL 33620 USA. Univ Naples Federico II, Dipartimento Sci Terra, Naples, Italy. INGV, Osservatorio Vesuviano, Naples, Italy. Boston Univ, Dept Earth Sci, Boston, MA USA. Adv Environm Technol Inc, Albany, GA USA. RP Savov, IP (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. EM savovi@si.edu RI D'Antonio, Massimo/C-5199-2012; Kelley, Katherine/J-3728-2013 OI D'Antonio, Massimo/0000-0003-2077-943X; Kelley, Katherine/0000-0002-7516-2683 NR 81 TC 73 Z9 73 U1 7 U2 24 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 1525-2027 J9 GEOCHEM GEOPHY GEOSY JI Geochem. Geophys. Geosyst. PD APR 7 PY 2005 VL 6 AR Q04J15 DI 10.1029/2004GC000777 PG 24 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 916HK UT WOS:000228375800001 ER PT J AU Kaspari, M AF Kaspari, M TI Global energy gradients and size in colonial organisms: Worker mass and worker number in ant colonies SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE biogeography; life history; productivity; temperature ID LIFE-HISTORY PUZZLE; BODY-SIZE; FREQUENCY-DISTRIBUTIONS; LATITUDINAL GRADIENT; PRIMARY PRODUCTIVITY; SPECIES RICHNESS; MOLECULAR CLOCK; BERGMANNS RULE; SOCIAL INSECTS; ABUNDANCE AB Body mass shapes processes from cell metabolism to community dynamics. Little is known, however, about how the average body mass of individuals varies among ecological communities. Ants alter colony mass by independently changing worker mass and/or worker number. In a survey of 49 ecosystems from tundra to tropical rainforest, average worker mass and worker number were uncorrelated (r(s) = 0.2, P > 0.14) and varied 100-fold. Data supported the hypothesis that higher mean monthly temperatures, T, reduce worker mass by increasing metabolic costs during worker development. In contrast, worker number was unimodal over a 1,000-fold gradient of net primary productivity (NPP, g of carbon per m(2) per yr), a measure of organic carbon available to consumers. At the lowest levels of NPP colonies appeared to be carbon-limited; above 60 g of carbon per m(2) per yr average worker number decreased to a global low. This decline in worker number with increasing NPP supports the hypothesis that abundant carbon ameliorates the Achilles heel of small taxa in competition with large taxa: their relatively high metabolic demands. Higher predation rates in resource-rich environments may also play a role in limiting worker number. In all, about half the global variation in worker mass and number was accounted for by gradients of NPP and T. Changes in global temperature and rainfall may thus mold gradients of ectotherm size, with consequences for the structure and function of the ecosystems. C1 Univ Oklahoma, Dept Zool, Norman, OK 73019 USA. Smithsonian Trop Res Inst, Balboa, Panama. RP Univ Oklahoma, Dept Zool, Norman, OK 73019 USA. EM mkaspari@ou.edu OI Kaspari, Michael/0000-0002-9717-5768 NR 70 TC 46 Z9 48 U1 3 U2 21 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 APR 5 PY 2005 VL 102 IS 14 BP 5079 EP 5083 DI 10.1073/pnas.0407827102 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 914AC UT WOS:000228195800030 PM 15788538 ER PT J AU Fallon, SM Bermingham, E Ricklefs, RE AF Fallon, SM Bermingham, E Ricklefs, RE TI Host specialization and geographic localization of avian malaria parasites: A regional analysis in the Lesser Antilles SO AMERICAN NATURALIST LA English DT Article DE avian malaria; host; parasite; specialization; biogeography; dispersal ID ANNOTATED CHECKLIST; GENE-SEQUENCES; CYTOCHROME-B; PLASMODIUM; HAEMOPROTEUS; BIOGEOGRAPHY; SPECIFICITY; BLOOD; BIRDS; APICOMPLEXA AB We recovered 26 genetically distinct avian malaria parasite lineages, based on cytochrome b sequences, from a broad survey of terrestrial avifauna of the Lesser Antilles. Here we describe their distributions across host species within a regional biogeographic context. Most parasite lineages were recovered from a few closely related host species. Specialization on one host species and distribution across many hosts were both rare. Geographic patterns of parasite lineages indicated limited dispersal and frequent local extinction. The central islands of the archipelago share similar parasite lineages and patterns of infection. However, the peripheral islands harbor well-differentiated parasite communities, indicating long periods of isolation. Nonetheless, 20 of 26 parasite lineages were recovered from at least one of three other geographic regions, the Greater Antilles, North America, and South America, suggesting rapid dispersal relative to rate of differentiation. Six parasite lineages were restricted to the Lesser Antilles, primarily to endemic host species. Host differences between populations of the same parasite lineage suggest that host preference may evolve more rapidly than mitochondrial gene sequences. Taken together, distributions of avian malarial parasites reveal evidence of coevolution, host switching, extinction, and periodic recolonization events resulting in ecologically dynamic as well as evolutionarily stable patterns of infection. C1 Univ Missouri, Dept Biol, St Louis, MO 63121 USA. Smithsonian Trop Res Inst, Unit 0948, APO AA, Miami, FL 34002 USA. RP Fallon, SM (reprint author), Smithsonian Inst, Genet Program, Washington, DC 20008 USA. EM fallon.sylvia@nmnh.si.edu; eb@naos.si.edu; ricklefs@umsl.edu NR 51 TC 91 Z9 93 U1 6 U2 36 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0003-0147 J9 AM NAT JI Am. Nat. PD APR PY 2005 VL 165 IS 4 BP 466 EP 480 DI 10.1086/428430 PG 15 WC Ecology; Evolutionary Biology SC Environmental Sciences & Ecology; Evolutionary Biology GA 904SC UT WOS:000227517000008 PM 15791538 ER PT J AU Woolfenden, BE Stutchbury, BJM Morton, ES AF Woolfenden, BE Stutchbury, BJM Morton, ES TI Male acadian flycatchers, Empidonax virescens, obtain extrapair fertilizations with distant females SO ANIMAL BEHAVIOUR LA English DT Article ID GREAT REED WARBLER; PAIR PATERNITY; HOODED WARBLERS; TREE SWALLOWS; FAIRY-WRENS; BIRDS; SYNCHRONY; BEHAVIOR; DENSITY AB We used genetic parentage analysis and radiotracking to determine how far male Acadian flycatchers travel from their territory in search of extrapair matings. Acadian flycatchers on our study site have a linear spatial distribution of territories associated with watercourses. With this type of spatial arrangement, males have only one or two immediate neighbouring females within 100 m and therefore have limited opportunities for extrapair (EP) fertilizations unless they travel far from their territory. In our sample of 53 nests collected over 4 years, 58% of nests contained EP young and 40% of nestlings were EP young. We identified the EP sire and the location of his territory at 13 nests with EP young, and over half (7/13) were not immediate neighbours. The mean distance between the territory of the EP sire and the territory where he attained EP fertilizations was 526 in. We were also able to exclude all immediate neighbours as EP sires for 12 additional nests containing EP young. The minimum average distance between an EP sire's territory and the territory containing an EP young that he sired was estimated to be 9 10 in. Overall, the EP sire was a neighbour in only 24% of nests with EP young. Radiotelemetry observations showed that six of seven mated males made off-territory forays and averaged 0.4 forays/h. Males travelled an average of 202 m off-territory (range 50-1500 m) and were away from their territories an average of 10.2 min/foray. Because our findings contrast sharply with those of other studies examining extrapair fertilization in passerines, in which most extrapair sires are neighbours, we suggest that when males have few adjacent neighbouring females, the benefits of searching widely to increase the number of potential extrapair mates can outweigh the costs of EP forays. (c) 2005 The Association for the Study of Animal Behaviour. Published by Elsevier Ltd. All rights reserved. C1 Smithsonian Inst, Natl Zool Pk, Migratory Bird Ctr, Dept Zool Res, Washington, DC 20008 USA. York Univ, Dept Biol, Toronto, ON M3J 1P3, Canada. RP Woolfenden, BE (reprint author), York Univ, Dept Biol, 4700 Keele St, Toronto, ON M3J 1P3, Canada. EM bwoolfen@yorku.ca NR 29 TC 36 Z9 36 U1 4 U2 19 PU ACADEMIC PRESS LTD ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0003-3472 J9 ANIM BEHAV JI Anim. Behav. PD APR PY 2005 VL 69 BP 921 EP 929 DI 10.1016/j.anbehav.2004.06.030 PN 4 PG 9 WC Behavioral Sciences; Zoology SC Behavioral Sciences; Zoology GA 918AY UT WOS:000228511900019 ER PT J AU Matthews, LD Gao, Y Uson, JM Combies, F AF Matthews, LD Gao, Y Uson, JM Combies, F TI Detections of CO in late-type, low surface brightness spiral galaxies SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies : general; galaxies : ISM; galaxies : spiral; ISM : molecules; radio lines : galaxies ID EDGE-ON GALAXIES; STAR-FORMATION THRESHOLDS; ROTATION CURVE SHAPES; WESTERBORK HI SURVEY; DIFFUSE IONIZED-GAS; DISK GALAXIES; IRREGULAR GALAXIES; MOLECULAR GAS; INTERSTELLAR-MEDIUM; IMAGING OBSERVATIONS AB Using the IRAM 30 m telescope, we have obtained (CO)-C-12 J = 1-0 and 2-1 spectral line observations toward the nuclear regions of 15 edge-on, low surface brightness (LSB) spiral galaxies. Our sample comprises extreme late-type LSB spirals with disk-dominated morphologies and rotational velocities V-rot less than or similar to 120 km s(-1). We report detections of four galaxies in at least one transition (greater than or similar to 5 sigma); for the remainder of the sample we provide upper limits on the nuclear CO content. Adopting a standard Galactic I-CO-to-H-2 conversion factor implies molecular gas masses of (3.3-9.8) x 10(6) M-circle dot in the nuclear regions (inner 1.1-1.8 kpc) of the detected galaxies. Combining our new data with samples of late-type spirals from the literature, we find that CO-detected LSB spirals adhere to the same M-H2-far-infrared correlation as more luminous and higher surface brightness galaxies. The amount of CO in the central regions of late-type spirals appears to depend more strongly on mass than on central optical surface brightness, and CO detectability declines significantly for moderate to low surface brightness spirals with V-rot less than or similar to 90 km s(-1); no LSB spirals have so far been detected in CO below this threshold. Metallicity effects alone are unlikely to account for this trend, and we speculate that we are seeing the effects of a decrease in the mean fraction of a galaxy disk able to support giant molecular cloud formation with decreasing galaxy mass. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Chinese Acad Sci, Purple Mt Observ, Nanjing 210008, Peoples R China. Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. Natl Radio Astron Observ, Charlottesville, VA 22903 USA. Observ Paris, LERMA, F-75014 Paris, France. RP Matthews, LD (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 42, Cambridge, MA 02138 USA. EM lmatthew@cfa.harvard.edu OI Combes, Francoise/0000-0003-2658-7893 NR 92 TC 33 Z9 34 U1 0 U2 2 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 APR PY 2005 VL 129 IS 4 BP 1849 EP 1862 DI 10.1086/428857 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 907TU UT WOS:000227741700007 ER PT J AU Johnson, JA Winn, JN Rampazzi, F Barbieri, C Mito, H Tarusawa, KI Tsvetkov, M Borisova, A Meusinger, H AF Johnson, JA Winn, JN Rampazzi, F Barbieri, C Mito, H Tarusawa, KI Tsvetkov, M Borisova, A Meusinger, H TI The history of the mysterious eclipses of KH 15D. II. Asiago, Kiso, Kitt Peak, Mount Wilson, Palomar, Tautenburg, and Rozhen Observatories, 1954-1997 SO ASTRONOMICAL JOURNAL LA English DT Article DE circumstellar matter; stars : individual ( KH 15D); stars : pre-main-sequence; techniques : photometric ID INITIAL MASS FUNCTION; STAR KH 15D; NGC 2264; PHOTOMETRY; EMISSION; BINARY; YOUNG AB The unusual pre-main-sequence binary star KH 15D undergoes remarkably deep and long-lasting periodic eclipses. Some clues about the reason for these eclipses have come from the observed evolution of the system's light curve over the last century. Here we present UBVRI photometry of KH 15D from 1954 to 1997 based on photographic plates from various observatories. The system has been variable at the approximate to 1 mag level since at least 1965. There is no evidence of color variations, with a typical limit of Delta( B - V) < 0.2 mag. We confirm some previously published results that were based on a smaller sample of plates: from approximately 1965 to 1990, the total flux was modulated with the 48 day orbital period of the binary, but the maximum flux was larger, the fractional variations were smaller, and the phase of minimum flux was shifted by almost a half-cycle relative to the modern light curve. All these results are consistent with the recently proposed theory that KH 15D is being occulted by an inclined, precessing, circumbinary ring. C1 Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Padua, Dept Astron, I-35122 Padua, Italy. Univ Tokyo, Sch Sci, Astron Inst, Kiso Observ, Mitake, Nagano 3970101, Japan. Bulgarian Acad Sci, Astron Inst, Sofia 1784, Bulgaria. Bulgarian Acad Sci, Inst Space Res, Sofia 1000, Bulgaria. Thuringer Landessternwarte Tautenburg, D-07778 Tautenburg, Germany. RP Johnson, JA (reprint author), Univ Calif Berkeley, Dept Astron, Mail Code 3411, Berkeley, CA 94720 USA. NR 19 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 0004-6256 J9 ASTRON J JI Astron. J. PD APR PY 2005 VL 129 IS 4 BP 1978 EP 1984 DI 10.1086/428597 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 907TU UT WOS:000227741700016 ER PT J AU Feng, WX An, T Hong, XY Zhao, JH Venturi, T Shen, ZQ Wang, WH AF Feng, WX An, T Hong, XY Zhao, JH Venturi, T Shen, ZQ Wang, WH TI The radio counter-jet of the QSO 3C 48 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies : quasars : individual : 3C 48; galaxies : jets; galaxies : interactions ID STEEP-SPECTRUM SOURCES; HOST GALAXY; CALIBRATORS; SCALE; 3C-48 AB We present multi- frequency radio observational results of the quasar 3C 48. The observations were carried out with the Very Large Array ( VLA) at five frequencies, 0.33, 1.5, 4.8, 8.4, and 22.5 GHz, and with the Multi- Element Radio Linked Interferometer Network ( MERLIN) at the two frequencies of 1.6 and 5 GHz. The source shows a one- sided jet to the north within 1", which then extends to the northeast and becomes diffuse. Two bright components ( N2 and N3), containing most of the flux density, are present in the northern jet. The spectral index of the two components is alpha(N2) similar to -0.99 +/- 0.12 and alpha(N3) similar to - 0.84 +/- 0.23 ( S proportional to nu(alpha)). Our images show the presence of an extended structure surrounding component N2, suggestive of strong interaction between the jet and the interstellar medium ( ISM) of the host galaxy. A steep- spectrum component, labelled S, located 0.25 " southwest to the flat- spectrum component which could be the core of 3C 48, is detected at a significance of > 15 sigma. Both the location and the steepness of the spectrum of component S suggest the presence of a counter- jet in 3C 48. C1 Chinese Acad Sci, Shanghai Astron Observ, Shanghai 200030, Peoples R China. Chinese Acad Sci, Grad Sch, Beijing 100039, Peoples R China. Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CNR, Ist Radioastron, I-4129 Bologna, Italy. RP Feng, WX (reprint author), Chinese Acad Sci, Shanghai Astron Observ, Shanghai 200030, Peoples R China. EM wfeng@shao.ac.cn OI Venturi, Tiziana/0000-0002-8476-6307 NR 31 TC 13 Z9 13 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 APR PY 2005 VL 434 IS 1 BP 101 EP 107 DI 10.1051/0004-6361:20042316 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 912RN UT WOS:000228097300013 ER PT J AU Williams, SJ Fuller, GA Sridharan, TK AF Williams, SJ Fuller, GA Sridharan, TK TI The circumstellar environments of high-mass protostellar objects - II. Dust continuum models SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars : formation; stars : circumstellar matter; ISM : clouds; ISM : dust, extinction ID YOUNG STELLAR OBJECTS; STAR-FORMATION; SUBMILLIMETER CONTINUUM; INFRARED-EMISSION; PHYSICAL STRUCTURE; REGIONS; CORES; COLLAPSE; GRAINS; PROTOSTARS AB We analyse the dust continuum emission seen towards a sample of candidate high-mass protostellar objects, modelling the cores we recently observed at 850 mu m with a one-dimensional radiative transfer code. Fitting radial slices in a range of directions across sources, we identify a number of objects that have non-spherical density profiles and show that for such sources fitting the azimuthal averaged emission produces erroneous estimates of the source properties. We find the majority of cores can be successfully modelled using envelopes of power-law density structure (where rho proportional to r(-alpha)), finding a mean power-law index of (alpha) over bar = 1.3 +/- 0.4. These envelopes extend considerably further, are more dense, and have a more shallow density profile than those bearing low-mass protostars. The majority of best-fit models have a SED resembling the cold-component dust bodies previously proposed for the sample, implying the short wavelength emission seen towards the HMPOs either originates from a separate hot dust component(s), or involves mechanisms such as accretion disks, stochastic heating and/or optically thin cavities not included in the radiative transfer model. We find evidence of smaller dust-free cavities towards some pre-UCHII sources. The modelling indicates a correlation between a and optical depth, suggesting that the densest cores also tend to have the most strongly peaked power-law density profiles. C1 Univ Manchester, Sch Phys & Astron, Manchester M60 1QD, Lancs, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Williams, SJ (reprint author), Univ Manchester, Sch Phys & Astron, Sackville St,POB 88, Manchester M60 1QD, Lancs, England. EM G.Fuller@manchester.ac.uk NR 41 TC 30 Z9 30 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 APR PY 2005 VL 434 IS 1 BP 257 EP 274 DI 10.1051/0004-6361:20034114 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 912RN UT WOS:000228097300027 ER PT J AU Overzier, RA Harris, DE Carilli, CL Pentericci, L Rottgering, HJA Miley, GK AF Overzier, RA Harris, DE Carilli, CL Pentericci, L Rottgering, HJA Miley, GK TI On the X-ray emission of z similar to 2 radio galaxies: IC scattering of the CMB and no evidence for fully-formed potential wells SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies : high-redshift; galaxies : active; X-rays : galaxies : clusters; X-rays : general ID MAGNETIC-FIELD STRENGTHS; XMM-NEWTON OBSERVATIONS; CHANDRA OBSERVATION; ELLIPTIC GALAXIES; ROTATION MEASURES; FARADAY-ROTATION; OPTICAL SURVEY; HOT-SPOTS; 4C 41.17; CLUSTER AB We present the results of 20 ks Chandra observations for each of 5 radio galaxies in the redshift range 2.0 < z < 2.6. The goals were to ( i) study the nature of their non-thermal X-ray emission; (ii) investigate the presence and amount of hot gas; and (iii) look for active galactic nuclei (AGN) overdensities in fields around high redshift radio galaxies. For 4 of the 5 targets we detect unresolved X-ray components coincident with the radio nuclei. From spectral analysis of one of the cores and comparison to the empirical radio to X-ray luminosity ratio (L-R/L-X) correlation for AGN, we find that the cores are underluminous in the X-rays indicating that obscuring material (n( HI) similar to 10(22) cm(-2)) may be surrounding the nuclei. We detect X-ray emission coincident with the radio hotspots or lobes in 4 of the 5 targets. This extended emission can be explained by the Inverse-Compton ( IC) scattering of photons that make up the cosmic microwave background (CMB). The magnetic field strengths of similar to 100- 200 mu G that we derive agree with the equipartition magnetic field strengths. The relative ease with which the lobe X-ray emission is detected is a consequence of the ( 1 + z)(4) increase in the energy density of the CMB. For one of the lobes, the X-ray emission could also be produced by a reservoir of hot, shocked gas. An HST image of the region around this radio component shows bright optical emission reminiscent of a bow-shock. By co-adding the 5 fields we created a deep, 100 ks exposure to search for diffuse X-ray emission from thermal intra-cluster gas. We detect no diffuse emission and derive upper limits of similar to 10(44) erg s(-1), thereby ruling out a virialized structure of cluster-size scale at z similar to 2. The average number of soft X-ray sources in the field surrounding the radio sources is consistent with the number density of AGN in the Chandra Deep Fields, with only one of the fields showing a marginally statistically significant factor 2 excess of sources with f(0.5-2) (keV) > 3 x 10(-15) erg s(-1) cm(-2). Analysis of the angular distribution of the field sources shows no evidence for large-scale structure associated with the radio galaxies, as was observed in the case of PKS 1138- 262 by Pentericci et al. ( 2002). C1 Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. Harvard Smithsonian Ctr Astrophys, Smithsonian Astron Observ, Cambridge, MA 02138 USA. New Mexico Array Operat Ctr VLA VLBA, Natl Radio Astron Observ, Socorro, NM 87801 USA. Univ Roma Tre, Dipartimento Fis, Rome, Italy. RP Overzier, RA (reprint author), Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. EM overzier@strw.leideuniv.nl NR 58 TC 30 Z9 30 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 APR PY 2005 VL 433 IS 1 BP 87 EP 100 DI 10.1051/0004-6361:20041657 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 906TD UT WOS:000227665300011 ER PT J AU Schlegel, EM AF Schlegel, EM TI Serendipitous XMM-Newton observation of the intermediate polar WX Pyx SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE X-rays : individuals : WX Pyx; X-rays : binaries; stars : novae; cataclysmic variables ID MAGNETIC CATACLYSMIC VARIABLES; GALACTIC PLANE; POWER AB We briefly describe a serendipitous observation of the little-studied intermediate polar WX Pyx using XMM-Newton. The X-ray spin period is 1557.3 s, confirming the optical period published in 1996. An orbital period of similar to 5.54 h is inferred from the separation of the spin-orbit sidelobe components. The soft and hard band spin-folded light curves are roughly sinusoidal in shape. The best-fit spectrum is consistent with a bremsstrahlung temperature of similar to 18 keV. An upper limit of similar to 300 eV is assigned to the presence of Fe line emission. WX Pyx lies near TX and TV Col in the P-spin - P-orb plane. C1 Smithsonian Astrophys Observ, High Energy Astrophys Div, Cambridge, MA 02138 USA. RP Schlegel, EM (reprint author), Smithsonian Astrophys Observ, High Energy Astrophys Div, Cambridge, MA 02138 USA. EM eschlegel@cfa.harvard.edu NR 19 TC 6 Z9 6 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 APR PY 2005 VL 433 IS 2 BP 635 EP 639 DI 10.1051/0004-6361:20042314A PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 909JS UT WOS:000227856800032 ER PT J AU Merand, A Borde, P du Foresto, VC AF Merand, A Borde, P du Foresto, VC TI A catalog of bright calibrator stars for 200-m baseline near-infrared stellar interferometry SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE catalogs; stars : fundamental parameters; techniques : interferometric; instrumentation : interferometers ID SPECTRAL IRRADIANCE CALIBRATION; ANGULAR RESOLUTION MEASUREMENTS; OPTICAL INTERFEROMETRY; MODEL ATMOSPHERES; RADIAL-VELOCITIES; VLTI; INSTRUMENT AB We present in this paper a catalog of reference starts suitable for calibrating infrared interferometric observations. In the K band, visibilities can be calibrated with a precision of 1% on baselines up to 200 meters for the whole sky, and up to 300 meters for some part of the sky. This work, extending to longer baselines a previous catalog compiled by Borde et al. (2002, AWA, 393, 183), is particularly well adapted to hectometric-class interferometers such as the Very Large Telescope Interferometer (VLTI, Glindemann et al. 2003, Proc. SPIE, 4838, 89) or the CHARA array (ten Brummelaar et al. 2003, Proc. SPIE, 4838, 69) when one is observing well-resolved, high-surface brightness objects (K less than or similar to 8). We use the absolute spectrophotometric calibration method introduced by Cohen et al. (1999, AJ, 117, 1864) to derive the angular diameters of our new set of 948 G8-M0 calibrator stars extracted from the IRAS, 2MASS and MSX catalogs. Angular stellar diameters range from 0.6 mas to 1.8 mas (median is 1.1 mas) with a median precision of 1.35%. For both the northern and southern hemispheres, the closest calibrator star is always less than 10 degrees away. C1 Observ Paris, LESIA, UMR8109, F-92195 Meudon, France. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Merand, A (reprint author), Observ Paris, LESIA, UMR8109, 5 Pl Jules Janssen, F-92195 Meudon, France. EM Antoine.Merand@obspm.fr; Foresto@obspm.fr; pborde@cfa.harvard.edu NR 28 TC 71 Z9 71 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 APR PY 2005 VL 433 IS 3 BP 1155 EP 1162 DI 10.1051/0004-6361:20041323 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 911XC UT WOS:000228039100040 ER PT J AU Krongold, Y Nicastro, F Brickhouse, NS Elvis, M Mathur, S AF Krongold, Y Nicastro, F Brickhouse, NS Elvis, M Mathur, S TI Opacity variations in the ionized absorption in NGC 3783: A compact absorber SO ASTROPHYSICAL JOURNAL LA English DT Article DE quasars : absorption lines; galaxies : active; galaxies : individual (NGC 985); galaxies : Seyfert; X-rays : galaxies ID ACTIVE GALACTIC NUCLEI; CHANDRA-X-RAY; REFLECTION GRATING SPECTROMETER; SEYFERT-1 GALAXY NGC-7469; XMM-NEWTON; UV OBSERVATIONS; WARM ABSORBERS; GAS; ENVIRONMENT; MULTIWAVELENGTH AB We show that the Fe VII-Fe XII M-shell unresolved transition array (UTA) in the Chandra HETGS observation of NGC 3783 (900 ks) clearly changes in opacity on a timescale of 31 days, responding to a factor of similar to 2 change in the ionizing continuum. The opacity variation is observed at a level >10 sigma. There is also evidence for variability in the O VI K edge (at similar to 3 sigma). The observed changes are consistent with the gas producing these absorption features (i.e., the low-ionization component) being close to photoionization equilibrium. The gas responsible for the Fe XVII-Fe XXII L-shell absorption (i.e., the high-ionization component) does not seem to be responding as expected in photoionization equilibrium. The observed change in opacity for the UTA implies a density >1 x 10(4) cm(-3), thus locating the gas within 6 pc of the X-ray source. The scenario in which the gas is composed of a continuous radial range of ionization structures is ruled out, as in such scenario, no opacity variations are expected. Rather, the structure of the absorber is likely composed of heavily clumped gas. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Astron Univ Nacl Autonoma Mexico, Mexico City 04510, DF, Mexico. 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. OI Nicastro, Fabrizio/0000-0002-6896-1364; Brickhouse, Nancy/0000-0002-8704-4473 NR 36 TC 42 Z9 42 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 APR 1 PY 2005 VL 622 IS 2 BP 842 EP 846 DI 10.1086/427621 PN 1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 912QD UT WOS:000228093400007 ER PT J AU Crocker, RM Fatuzzo, M Jokipii, JR Melia, F Volkas, RR AF Crocker, RM Fatuzzo, M Jokipii, JR Melia, F Volkas, RR TI The AGASA and sugar anisotropies and TeV gamma rays from the Galactic center: A possible signature of extremely high energy neutrons SO ASTROPHYSICAL JOURNAL LA English DT Article DE acceleration of particles; cosmic rays; Galaxy : center; radiation mechanisms : nonthermal; supernova remnants ID SAGITTARIUS-A-EAST; SUPERMASSIVE BLACK-HOLE; SUPERNOVA-REMNANTS; COSMIC-RAYS; RELATIVISTIC NEUTRONS; SHOCK ACCELERATION; INCLUSIVE NEUTRON; MAXIMUM ENERGY; GALAXY; EMISSION AB Recent analysis of data sets from two extensive air shower cosmic-ray detectors shows tantalizing evidence of an anisotropic overabundance of cosmic rays toward the Galactic center region that "turns on'' around 10(18) eV. We demonstrate that the anisotropy could be due to neutrons created in the Galactic center region through charge exchange in proton-proton collisions, where the incident, high-energy protons obey a similar to E-2 power law associated with acceleration at a strong shock. We show that the normalization supplied by the gamma-ray signal from EGRET GC source 3EG J1746-2851 (ascribed to p-p-induced neutral pion decay at GeV energies), together with a very reasonable spectral index of 2.2, predicts a neutron flux at similar to 10(18) eV fully consistent with the extremely high energy cosmic-ray data. Likewise, the normalization supplied by the very recent GC data from the HESS air Cerenkov telescope at similar to TeV energies is almost equally compatible with the similar to 10(18) eV cosmic-ray data. Interestingly, however, the EGRET and HESS data appear to be themselves incompatible. We find a plausible resolution of this discrepancy in an effective two-source model. Finally, we argue that the shock acceleration is probably occurring in the shell of Sagittarius A East, an unusual supernova remnant located very close to the Galactic center. In support of this contention we note that (1) the extended shell of this object could provide both of the sources suggested by the gamma-ray data and (2) the unusually strong magnetic field at this remnant, together with a perpendicular shock geometry, allow for acceleration of protons up to the extreme energies required to explain the cosmic-ray anisotropy. If the connection between the anisotropy and Sagittarius A East could be firmly established, it would be the first direct evidence for a particular Galactic source of cosmic rays up to energies near 10(19) eV. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Melbourne, Sch Phys, High Energy Phys Res Ctr, Parkville, Vic 3010, Australia. Xavier Univ, Dept Phys, Cincinnati, OH 45207 USA. Univ Arizona, Lunar & Planetary Observ, Dept Planetary Sci, Tucson, AZ 85721 USA. Univ Arizona, Dept Phys, Tucson, AZ 85721 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. RP Crocker, RM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM rcrocker@cfa.harvard.edu; fatuzzo@cerebro.cs.xu.edu; jokipii@lpl.arizona.edu; melia@physics.arizona.edu; r.volkas@physics.unimelb.edu.au NR 85 TC 71 Z9 71 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 APR 1 PY 2005 VL 622 IS 2 BP 892 EP 909 DI 10.1086/427972 PN 1 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 912QD UT WOS:000228093400012 ER PT J AU Goldsmith, PF Li, D AF Goldsmith, PF Li, D TI HI narrow self-absorption in dark clouds: Correlations with molecular gas and implications for cloud evolution and star formation SO ASTROPHYSICAL JOURNAL LA English DT Review DE ISM : atoms; ISM : clouds; ISM : globules ID C-12/C-13 ISOTOPE RATIO; COSMIC-RAY IONIZATION; INTER-STELLAR CLOUDS; RHO-OPHIUCHI REGION; INTERSTELLAR DUST; CARBON-MONOXIDE; ROTATIONAL-EXCITATION; REFLECTION NEBULAE; AROMATIC-MOLECULES; HYDROGEN FORMATION AB We present the results of a comparative study of H I narrow self-absorption (HINSA), OH, (CO)-C-13, and (CO)-O-18 in five dark clouds. We find that the HINSA generally follows the distribution of the emission of the carbon monoxide isotopologs and has a characteristic size close to that of (CO)-C-13. This confirms earlier work that determined that the HINSA is produced by cold H I that is well mixed with molecular gas in well-shielded regions. The OH and (CO)-C-13 column densities are essentially uncorrelated for the sources other than L1544. Our observations indicate that the central number densities of H I are between 2 and 6 cm(-3) and that the ratio of the hydrogen density to total proton density for these sources is (5-27) x 10(-4). Using cloud temperatures and the density of atomic hydrogen, we set an upper limit to the cosmic-ray ionization rate of 10(-16) s(-1). We present a model for H I to H-2 conversion in well-shielded regions that includes cosmic-ray destruction of H-2 and formation of this species on grain surfaces. We include the effect of a distribution of grain sizes, and we find that for an MRN distribution, the rate of H-2 formation is increased by a factor of 3.4 relative to that for a model with a single grain radius of 1700 angstrom. Comparison of observed and modeled fractional H I abundances indicates ages for these clouds, defined as the time since the initiation of H I -> H-2 conversion, to be 10(6.5)-10(7) yr. Several effects may make this time a lower limit, but the low values of n(H I) that we have determined make it certain that the timescale for evolution from a possibly less dense atomic phase to an almost entirely molecular phase must be a minimum of several million years. This clearly sets a lower limit to the overall timescale for the process of star formation and the lifetime of molecular clouds. C1 Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. Cornell Univ, Natl Astron & Ionosphere Ctr, Ithaca, NY 14853 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Goldsmith, PF (reprint author), Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. EM dli@cfa.harvard.edu RI Goldsmith, Paul/H-3159-2016 NR 102 TC 67 Z9 67 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 APR 1 PY 2005 VL 622 IS 2 BP 938 EP 958 DI 10.1086/428032 PN 1 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 912QD UT WOS:000228093400015 ER PT J AU Bellm, EC Vaillancourt, JE AF Bellm, EC Vaillancourt, JE TI Origins of the 1/4 keV soft X-ray background SO ASTROPHYSICAL JOURNAL LA English DT Article DE X-rays : diffuse background; X-rays : ISM ID ROSAT SURVEY; EMISSION; MAPS; RADIATION; SPECTRUM; PLASMAS; LIMITS; GAS AB Snowden and coworkers have presented a model for the 1/4 keV soft X-ray diffuse background in which the observed flux is dominated by a similar to 10(6) K thermal plasma located in a 100-300 pc diameter bubble surrounding the Sun but has significant contributions from a very patchy Galactic halo. Halo emission provides about 11% of the total observed flux and is responsible for half of the H I anticorrelation. The remainder of the anticorrelation is presumably produced by displacement of disk H I by the varying extent of the Local Hot Bubble (LHB). The ROSAT R1 and R2 bands used for this work had the unique spatial resolution and statistical precision required for separating the halo and local components but provide little spectral information. Some consistency checks had been made with older observations at lower X-ray energies, but we have made a careful investigation of the extent to which the model is supported by existing sounding rocket data in the Be (73-111 eV) and B (115-188 eV) bands, where the sensitivities to the model are qualitatively different from the ROSAT bands. We conclude that the two-component model is well supported by the low-energy data. We find that these combined observations of the local component may be consistent with single-temperature thermal emission models in collisional ionization equilibrium if depleted abundances are assumed. However, different model implementations give significantly different results, offering little support for the conclusion that the astrophysical situation is so simple. C1 Univ Wisconsin, Dept Phys, Madison, WI 53706 USA. RP Bellm, EC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM bellm@fas.harvard.edu; johnv@oddjob.uchicago.edu OI Vaillancourt, John/0000-0001-8916-1828 NR 28 TC 10 Z9 10 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 APR 1 PY 2005 VL 622 IS 2 BP 959 EP 964 DI 10.1086/428385 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 912QD UT WOS:000228093400016 ER PT J AU Lee, JC Ravel, B AF Lee, JC Ravel, B TI Determining the grain composition of the interstellar medium with high-resolution X-ray spectroscopy SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; dust, extinction; X-rays : ISM ID ABSORPTION-FINE-STRUCTURE; EDGE; OXYGEN; ABUNDANCE; AMPLITUDE; SPECTRUM; IRON AB We investigate the ability of high-resolution X-ray spectroscopy to directly probe the grain composition of the interstellar medium. Using iron K-edge experimental data of likely ISM dust candidates taken at the National Synchrotron Light Source at Brookhaven National Laboratory and the Advanced Photon Source at Argonne National Laboratory, we explore the prospects for determining the chemical composition of astrophysical dust and discuss a technique for doing so. Focusing on the capabilities of the Astro-E2 XRS microcalorimeters, we assess the limiting effects of spectral resolution and noise for detecting significant X-ray absorption fine structure signal in astrophysical environments containing dust. We find that given sufficient signal, the resolution of the XRS will allow us to definitively distinguish gas-phase from dust-phase absorption and certain chemical compositions. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. MIT, Ctr Space Res, Cambridge, MA 02139 USA. USN, Ctr Corros Chem & Engn, Res Lab, Washington, DC 20375 USA. RP Lee, JC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 6, Cambridge, MA 02138 USA. EM jclee@cfa.harvard.edu RI XRAY, SUZAKU/A-1808-2009; Lee, Julia/G-2381-2015 OI Lee, Julia/0000-0002-7336-3588 NR 27 TC 13 Z9 13 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 APR 1 PY 2005 VL 622 IS 2 BP 970 EP 976 DI 10.1086/428118 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 912QD UT WOS:000228093400018 ER PT J AU Fransson, C Challis, PM Chevalier, RA Filippenko, AV Kirshner, RP Kozma, C Leonard, DC Matheson, T Baron, E Garnavich, P Jha, S Leibundgut, B Lundqvist, P Pun, CSJ Wang, LF Wheeler, JC AF Fransson, C Challis, PM Chevalier, RA Filippenko, AV Kirshner, RP Kozma, C Leonard, DC Matheson, T Baron, E Garnavich, P Jha, S Leibundgut, B Lundqvist, P Pun, CSJ Wang, LF Wheeler, JC TI Hubble Space Telescope and ground-based observations of SN 1993J and SN1998S: CNO processing in the progenitors SO ASTROPHYSICAL JOURNAL LA English DT Article ID CASSIOPEIA-A EVIDENCE; CIRCUMSTELLAR INTERACTION; II SUPERNOVAE; OPTICAL-SPECTRA; EMISSION-LINES; MASSIVE STARS; LIGHT-CURVE; X-RAY; SN-1993J; ULTRAVIOLET AB Ground-based and Hubble Space Telescope observations are presented for SN 1993J and SN 1998S. SN 1998S shows strong, relatively narrow circumstellar emission lines of N III-V and C III-IV, as well as broad lines from the ejecta. Both the broad ultraviolet and optical lines in SN 1998S indicate an expansion velocity of similar to 7000 km s(-1). The broad emission components of Ly alpha and Mg II are strongly asymmetrical after day 72 past the explosion and differ in shape from H alpha. Different models based on dust extinction from dust in the ejecta or shock region, in combination with H alpha from a circumstellar torus, are discussed. It is concluded, however, that the double-peaked line profiles are more likely to arise as a result of optical depth effects in the narrow, cool, dense shell behind the reverse shock than in a torus-like region. The ultraviolet lines of SN 1993J are broad, with a boxlike shape, coming from the ejecta and a cool, dense shell. The shapes of the lines are well fitted by a shell with inner velocity similar to 7000 km s(-1) and outer velocity similar to 10,000 km s(-1). For both SN 1993J and SN 1998S a strong nitrogen enrichment is found, with N/C approximate to 12.4 in SN 1993J and N/C approximate to 6.0 in SN 1998S. From a compilation of all supernovae with determined CNO ratios, we discuss the implications of these observations for the structure of the progenitors of Type II supernovae. C1 Stockholm Univ, AlbaNova, Dept Astron, SE-10691 Stockholm, Sweden. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Univ Massachusetts, Five Coll Astron Dept, Amherst, MA 01003 USA. CALTECH, Dept Astron, Pasadena, CA 91125 USA. Univ Oklahoma, Dept Phys & Astron, Norman, OK 73019 USA. Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. European So Observ, D-85748 Garching, Germany. Univ Hong Kong, Dept Phys, Hong Kong, Hong Kong, Peoples R China. Univ Calif Berkeley, Lawrence Berkeley Lab, Inst Nucl & Particle Astrophys, Berkeley, CA 94720 USA. Univ Texas, Dept Astron, Austin, TX 78712 USA. RP Fransson, C (reprint author), Stockholm Univ, AlbaNova, Dept Astron, SE-10691 Stockholm, Sweden. EM claes@astro.su.se.email RI Baron, Edward/A-9041-2009 OI Baron, Edward/0000-0001-5393-1608 NR 86 TC 56 Z9 56 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 2005 VL 622 IS 2 BP 991 EP 1007 DI 10.1086/426495 PN 1 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 912QD UT WOS:000228093400021 ER PT J 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 TI Direct observations of the magnetic reconnection site of an eruption on 2003 November 18 SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun : coronal mass ejections (CMEs); Sun : flares; Sun : magnetic fields ID CORONAL MASS EJECTIONS; CURRENT SHEET; SOLAR-FLARES; FLUX ROPES; FIELD; EVOLUTION; RHESSI; MOTION; LOOPS AB We report direct observations of the magnetic reconnection site during an eruptive process that occurred on 2003 November 18. 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 the ground, including the EUV Imaging Telescope, Ultraviolet Coronagraph Spectrometer, and Large Angle Spectrometric Coronagraph experiment on board the Solar and Heliospheric Observatory, the Reuven Ramaty High Energy Solar Spectroscopic Imager, and 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 maximum velocities of the CME leading edge and the core were 1939 and 1484 km s(-1), respectively. The average reconnection inflow velocities near the current sheet over different time intervals ranged from 10.5 to 106 km s(-1), and the average outflow velocities ranged from 460 to 1075 km s(-1). This leads to a corresponding rate of reconnection in terms of the Alfven Mach number MA ranging from 0.01 to 0.23. The composite of images from different instruments specifies 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. Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. Chinese Acad Sci, Natl Astron Observ, Yunnan Observ, Kunming 650011, Peoples R China. INAF, Osservatorio Astron Torino, I-10025 Pino Torinese, Italy. RP Lin, J (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI LIN, JUN/B-9890-2017 NR 41 TC 169 Z9 179 U1 2 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 APR 1 PY 2005 VL 622 IS 2 BP 1251 EP 1264 DI 10.1086/428110 PN 1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 912QD UT WOS:000228093400044 ER PT J AU Krot, AN Hutcheon, ID Yurimoto, H Cuzzi, JN McKeegan, KD Scott, ERD Libourel, G Chaussidon, M Aleon, J Petaev, MI AF Krot, AN Hutcheon, ID Yurimoto, H Cuzzi, JN McKeegan, KD Scott, ERD Libourel, G Chaussidon, M Aleon, J Petaev, MI TI Evolution of oxygen isotopic composition in the inner solar nebula SO ASTROPHYSICAL JOURNAL LA English DT Article DE meteors, meteoroids; nuclear reactions, nucleosynthesis, abundances; planetary systems : formation; solar system : formation ID ALUMINUM-RICH INCLUSIONS; CARBONACEOUS CHONDRITE ACFER-094; SHORT-LIVED NUCLIDES; REFRACTORY INCLUSIONS; FERROMAGNESIAN CHONDRULES; CONTEMPORANEOUS FORMATION; SYSTEM; ALLENDE; ORIGIN; AL-26 AB Changes in the chemical and isotopic composition of the solar nebula with time are reflected in the properties of different constituents that are preserved in chondritic meteorites. CR-group carbonaceous chondrites are among the most primitive of all chondrite types and must have preserved solar nebula records largely unchanged. We have analyzed the oxygen and magnesium isotopes in a range of the CR constituents of different formation temperatures and ages, including refractory inclusions and chondrules of various types. The results provide new constraints on the time variation of the oxygen isotopic composition of the inner (<5 AU) solar nebula - the region where refractory inclusions and chondrules most likely formed. A chronology based on the decay of short-lived Al-26 (t(1/2) similar to 0.73 Myr) indicates that the inner solar nebula gas was O-16-rich when refractory inclusions formed, but less than 0.8 Myr later, gas in the inner solar nebula became O-16-poor, and this state persisted at least until CR chondrules formed similar to 1-2 Myr later. We suggest that the inner solar nebula became O-16-poor because meter-sized icy bodies, which were enriched in O-17 and O-18 as a result of isotopic self-shielding during the ultraviolet photo-dissociation of CO in the protosolar molecular cloud or protoplanetary disk, agglomerated outside the snow line, drifted rapidly toward the Sun, and evaporated at the snow line. This led to significant enrichment in O-16-depleted water, which then spread through the inner solar system. Astronomical studies of the spatial and temporal variations of water abundance in protoplanetary disks may clarify these processes. C1 Univ Hawaii Manoa, Sch Ocean & Earth Sci & Technol, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA. Lawrence Livermore Natl Lab, Livermore, CA 94451 USA. Tokyo Inst Technol, Dept Earth & Planetary Sci, Meguro Ku, Tokyo 1528551, Japan. NASA, Space Sci & Astrobiol Div, Ames Res Ctr, Moffett Field, CA 94035 USA. Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA. Ctr Rech Petrog & Geochim, CNRS, UPR 2300, F-54501 Vandoeuvre Les Nancy, France. Inst Natl Polytech Lorraine, Ecole Natl Super Geol, F-54501 Vandoeuvre Les Nancy, France. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA. RP Krot, AN (reprint author), Univ Hawaii Manoa, Sch Ocean & Earth Sci & Technol, Hawaii Inst Geophys & Planetol, 1680 East West Rd, Honolulu, HI 96822 USA. EM sasha@higp.hawaii.edu RI McKeegan, Kevin/A-4107-2008; UCLA, SIMS/A-1459-2011; Chaussidon, Marc/E-7067-2017 OI McKeegan, Kevin/0000-0002-1827-729X; NR 90 TC 62 Z9 62 U1 4 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 APR 1 PY 2005 VL 622 IS 2 BP 1333 EP 1342 DI 10.1086/428382 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 912QD UT WOS:000228093400050 ER PT J AU Megeath, ST Wilson, TL Corbin, MR AF Megeath, ST Wilson, TL Corbin, MR TI Hubble Space Telescope NICMOS imaging of W3IRS 5: A trapezium in the making? SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared : stars; ISM : individual (W3 IRS 5); stars : formation ID STELLAR CLUSTERS; RADIO-CONTINUUM; MASSIVE STARS; HII-REGIONS; W3; ACCRETION; KINEMATICS; PARAMETERS; SYSTEMS; IRS-5 AB We present Hubble Space Telescope NICMOS imaging of W3 IRS 5, a binary high-mass protostar. In addition to the two protostars, NICMOS images taken in the F222M and F160W filters show three new 2.22 mu m sources with very red colors; these sources fall within a region 5600 AU in diameter and are coincident with an similar to 100 M-circle dot, dense molecular clump. Two additional point sources are found within 0.'' 4 (800 AU) of one of the high-mass protostars; these may be stellar companions or unresolved emission knots from an outflow. We propose that these sources constitute a nascent Trapezium system in the center of the W3 IRS 5 cluster containing as many as five proto-OB stars. This would be the first identification of a Trapezium still deeply embedded in its natal gas. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. European So Observ, D-85748 Garching, Germany. Arizona State Univ, Dept Phys & Astron, Tempe, AZ 85287 USA. RP Megeath, ST (reprint author), Harvard Smithsonian Ctr Astrophys, MS-65,60 Garden St, Cambridge, MA 02138 USA. EM tmegeath@cfa.harvard.edu NR 33 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 APR 1 PY 2005 VL 622 IS 2 BP L141 EP L144 DI 10.1086/429720 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 912QH UT WOS:000228093800017 ER PT J AU Li, LX Zimmerman, ER Narayan, R McClintock, JE AF Li, LX Zimmerman, ER Narayan, R McClintock, JE TI Multitemperature blackbody spectrum of a thin accretion disk around a Kerr black hole: Model computations and comparison with observations SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE accretion, accretion disks; black hole physics; radiation mechanisms : thermal; X-rays : binaries ID ACTIVE GALACTIC NUCLEI; X-RAY SOURCES; FORCE-FREE MAGNETOSPHERE; MARGINALLY STABLE ORBIT; GRO J1655-40; LINE-PROFILES; MAGNETIZED ACCRETION; OPTICAL OBSERVATIONS; CYGNUS X-1; LMC X-1 AB We use a ray-tracing technique to compute the observed spectrum of a thin accretion disk around a Kerr black hole. We include all relativistic effects such as frame-dragging, Doppler boost, gravitational redshift, and bending of light by the gravity of the black hole. We also include self-irradiation of the disk as a result of light deflection. Assuming that the disk emission is locally blackbody, we show how the observed spectrum depends on the spin of the black hole, the inclination of the disk, and the torque at the inner edge of the disk. We find that the effect of a nonzero torque on the spectrum can, to a good approximation, be absorbed into a zero-torque model by adjusting the mass accretion rate and the normalization. We describe a computer model, called KERRBB, which we have developed for fitting the spectra of black hole X-ray binaries. Using KERRBB within the X-ray data reduction package XSPEC, and assuming a spectral hardening factor f(col) = 1.7, we analyze the spectra of three black hole X-ray binaries: 4U 1543-47, XTE J1550-564, and GRO J1655-40. We estimate the spin parameters of the black holes in 4U 1543-47 and GRO J1655-40 to be a/M similar to 0.6 and similar to 0.6-0.7, respectively. If f(col) similar to 1.5-1.6, as in a recent study, then we find a/M similar to 0.7-0.8 and similar to 0.8-0.9, respectively. These estimates are subject to additional uncertainties in the assumed black hole masses, distances, and disk inclinations. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Li, LX (reprint author), Max Planck Inst Astrophys, Karl Schwarzschild Str 1,Postfach 1317, D-85741 Garching, Germany. EM lli@cfa.harvard.edu; ezimmerman@cfa.harvard.edu; rnarayan@cfa.harvard.edu; jmcclintock@cfa.harvard.edu OI Narayan, Ramesh/0000-0002-1919-2730 NR 74 TC 171 Z9 171 U1 0 U2 3 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 APR PY 2005 VL 157 IS 2 BP 335 EP 370 DI 10.1086/428089 PG 36 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 907TG UT WOS:000227740300008 ER PT J AU Isler, ML Isler, PR Brumfield, RT AF Isler, ML Isler, PR Brumfield, RT TI Clinal variation in vocalizations of an antbird (Thamnophilidae) and implications for defining species limits SO AUK LA English DT Article DE clinal variation; hybrid zone; speciation; systematics; Thamnophilidae; Thamnophilus caerulescens; Variable Antshrike; vocalizations ID PASSERIFORMES; COMPLEX AB In avian taxa in which vocalizations are considered innate, such as suboscine passerines, vocal characters are increasingly being used to help determine whether populations have achieved species status. In comparing vocal characteristics of distant populations, however, one must be concerned with the possibility of character gradation through intermediate populations. The first quantitative study of a species in a suboscine family to test for clinal vocal variation, our vocal study found clinal variation in the pace (number of notes per second) of male loudsongs, and revealed that the geographic pattern of the clines was consistent with genetic variation found in the companion molecular study (Brumfield 2005). The result underscores the necessity of searching for intermediacy when analyzing vocalizations of geographically distant populations. Furthermore, given that male loudsong pace was the only vocal character that varied across the intergrading populations, the result also provides support to the guideline that one should expect thamnophilid species to differ in at least three vocal characters (Isler et al. 1998) and indicates that this degree of vocal character differences can be a valuable "yard stick" in determining which thamnophilid populations have achieved biological species status. C1 Natl Museum Nat Hist, Smithsonian Inst, Dept Zool Birds, Washington, DC 20013 USA. Univ Washington, Dept Biol, Seattle, WA 98195 USA. Louisiana State Univ, Museum Nat Sci, Baton Rouge, LA 70803 USA. RP Isler, ML (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Dept Zool Birds, POB 37012, Washington, DC 20013 USA. EM antbird@cox.net RI Brumfield, Robb/K-6108-2015 OI Brumfield, Robb/0000-0003-2307-0688 NR 23 TC 31 Z9 31 U1 1 U2 7 PU AMER ORNITHOLOGISTS UNION PI LAWRENCE PA ORNITHOLOGICAL SOC NORTH AMER PO BOX 1897, LAWRENCE, KS 66044-8897 USA SN 0004-8038 J9 AUK JI AUK PD APR PY 2005 VL 122 IS 2 BP 433 EP 444 DI 10.1642/0004-8038(2005)122[0433:CVIVOA]2.0.CO;2 PG 12 WC Ornithology SC Zoology GA 924UI UT WOS:000229005600004 ER PT J AU Jonsell, S Saenz, A Froelich, P Zygelman, B Dalgarno, A AF Jonsell, S Saenz, A Froelich, P Zygelman, B Dalgarno, A TI Including the strong nuclear force in antihydrogen-scattering calculations SO CANADIAN JOURNAL OF PHYSICS LA English DT Article; Proceedings Paper CT International Conference on Precision Physics of Simple Atomic Systems (PSAS 2004) CY AUG 01, 2004-AUG 04, 2005 CL Rio de Janeiro, BRAZIL ID ANNIHILATION CROSS-SECTION; SUB-KELVIN TEMPERATURES; VERY-LOW ENERGY; ANTIPROTONIC-HYDROGEN; ATOMS; COLLISIONS AB We investigate two methods to include the strong nuclear force in hydrogen-antihydrogen scattering calculations. First, we construct a model optical potential with parameters determined by the measured shift and width of the protonium ground state. Although this potential is a very crude model for the strong nuclear force, its parameters may be adjusted to reproduce both bound states and low-energy annihilation cross sections to within the experimental accuracy. It is then shown that this potential may be reduced to a short-distance boundary condition in terms of the proton-antiproton strong-interaction scattering length. Elastic and annihilation cross sections for ground-state hydrogen-antihydrogen scattering are calculated for s- and p-waves, and collision energies up to 1 atomic unit. The two methods are found to agree to within about 1%. The main source of discrepancy is that the scattering-length approach does not account for vacuum polarization, relativistic, and finite-size corrections. We verify that the range of the strong interaction potential does not affect the hydrogen-antihydrogen s-wave scattering properties, and that the strong interaction has negligible influence on p-wave scattering. C1 Umea Univ, Dept Phys, SE-90187 Umea, Sweden. Humboldt Univ, Inst Phys, AG Moderne Opt, D-10117 Berlin, Germany. Uppsala Univ, Dept Quantum Chem, SE-75121 Uppsala, Sweden. Univ Nevada, Dept Phys, Las Vegas, NV 89154 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Jonsell, S (reprint author), Umea Univ, Dept Phys, SE-90187 Umea, Sweden. EM jonsell@tp.umu.se RI Jonsell, Svante/J-2251-2016 OI Jonsell, Svante/0000-0003-4969-1714 NR 27 TC 13 Z9 13 U1 0 U2 3 PU NATL RESEARCH COUNCIL CANADA PI OTTAWA PA RESEARCH JOURNALS, MONTREAL RD, OTTAWA, ONTARIO K1A 0R6, CANADA SN 0008-4204 J9 CAN J PHYS JI Can. J. Phys. PD APR PY 2005 VL 83 IS 4 BP 435 EP 445 DI 10.1139/P05-017 PG 11 WC Physics, Multidisciplinary SC Physics GA 933AB UT WOS:000229595000018 ER PT J AU Borrell, BJ LaDuc, TJ Dudley, R AF Borrell, BJ LaDuc, TJ Dudley, R TI Respiratory cooling in rattlesnakes SO COMPARATIVE BIOCHEMISTRY AND PHYSIOLOGY A-MOLECULAR & INTEGRATIVE PHYSIOLOGY LA English DT Article DE Crotalus; evaporative cooling; rattlesnake; thermoregulation ID BODY TEMPERATURE DIFFERENCES; THERMAL PREFERENDA; AUSTRALIAN PYTHONS; PANTING LIZARD; HEAD; THERMOREGULATION; MUSCLE; BRAIN AB We used infrared thermography to study respiratory cooling in the rattlesnakes (Viperidae: Crotalinae) and to partition the effects of air temperature, humidity, and activity levels on head-body temperature differences. We observed a single, cooled region centered around the mouth and nasal capsule that extended across the pit membrane at air temperatures above 20 degrees C. Both head and body temperatures of rattlesnakes increased linearly with air temperature. Head-body temperature differentials also increased with air temperature, but declined significantly at higher relative humidities. Rattling rattlesnakes exhibited significantly greater head-body temperature differentials than did resting rattlesnakes. We suggest that respiratory cooling may provide a thermal buffer for the thermoreceptive pit organs at high air temperatures, but caution that this adaptive hypothesis must be tested with direct neural or behavioral assays. (c) 2005 Elsevier Inc. All rights reserved. C1 Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. Univ Texas, Sect Integrat Biol, Austin, TX 78712 USA. Smithsonian Trop Res Inst, Balboa, Panama. RP Borrell, BJ (reprint author), Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. EM bborrell@uclink.berkeley.edu OI LaDuc, Travis J./0000-0003-4402-8745 NR 30 TC 5 Z9 5 U1 7 U2 13 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 1095-6433 J9 COMP BIOCHEM PHYS A JI Comp. Biochem. Physiol. A-Mol. Integr. Physiol. PD APR PY 2005 VL 140 IS 4 BP 471 EP 476 DI 10.1016/j.cbpb.2005.02.012 PG 6 WC Biochemistry & Molecular Biology; Physiology; Zoology SC Biochemistry & Molecular Biology; Physiology; Zoology GA 940QW UT WOS:000230160100011 PM 15936707 ER PT J AU Wright, SJ Muller-Landau, HC Calderon, O Hernandez, A AF Wright, SJ Muller-Landau, HC Calderon, O Hernandez, A TI Annual and spatial variation in seedfall and seedling recruitment in a neotropical forest SO ECOLOGY LA English DT Article DE Barro Colorado Island; density dependence; lianas; masting; Panama; pest satiation; seedling recruitment; seed production; tropical trees ID EVOLUTIONARY ECOLOGY; TROPICAL FORESTS; HAMAMELIS-VIRGINIANA; PREDATOR SATIATION; DECIDUOUS FOREST; FRUIT PRODUCTION; FAGUS-SILVATICA; EL-NINO; TREE; DISPERSAL AB An economy of scale may lead to selection to increase interannual variation in seed production when the per seed probability of seedling establishment. increases with seed production. Variable annual seedfall will, however, reduce this probability when post-dispersal seed fate is negatively density dependent on the local density of seeds, and seed dispersal and density dependence act identically across years. Intuitively, more variable annual seedfall causes the representative seed to experience a greater density of conspecific seeds and suffer greater density-dependent effects. This handicap must be overcome for the per seed probability of recruitment to be greater in years with greater seed production. We quantified spatial and annual variation in seedfall and seedling recruitment, evaluated density dependence and economies of scale during the seed-to-seedling transition, and investigated the synergistic consequences of density dependence and variable annual seedfall for seedling recruitment on Barro Colorado Island (BCI), Panama. Weekly censuses of 200 0.5-m(2) seed traps documented seedfall for 15 years and 108 plant species. Annual censuses of 600 1-m(2) seedling plots documented recruitment for nine years and 32 species. The density of seedling recruits tended to increase with the density of seeds; however, the per seed probability of recruitment invariably decreased with seedfall density. Negative density dependence characterized the seed-to-seedling transition. Observed levels of spatial and interannual variation in seedfall density would reduce long-term recruitment by up to 28% if negatively density-dependent survival acted identically across years; however, the strength of negative density dependence varied significantly among years for 12 of 32 species. Negative density dependence occurred in all years for these species but was significantly weaker during the one or two years of greatest seedfall than during the remaining years of lower seedfall. The per seed probability of recruitment increased significantly with annual seedfall for eight of these species. These eight species realized postdispersal economies of scale despite the reduction in long-term recruitment expected from the synergism between variable annual seed production and negatively density-dependent seed fate. C1 Smithsonian Trop Res Inst, Balboa, Ancon, Panama. Natl Ctr Ecol Anal & Synth, Santa Barbara, CA 93101 USA. RP Wright, SJ (reprint author), Smithsonian Trop Res Inst, Apartado 2072, Balboa, Ancon, Panama. EM wrightj@si.edu RI Wright, Stuart/M-3311-2013 OI Wright, Stuart/0000-0003-4260-5676 NR 51 TC 103 Z9 124 U1 4 U2 78 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 APR PY 2005 VL 86 IS 4 BP 848 EP 860 DI 10.1890/03-0750 PG 13 WC Ecology SC Environmental Sciences & Ecology GA 914YF UT WOS:000228263300005 ER PT J AU Carpenter, KE Springer, VG AF Carpenter, KE Springer, VG TI The center of the center of marine shore fish biodiversity: the Philippine Islands SO ENVIRONMENTAL BIOLOGY OF FISHES LA English DT Article DE Indo-Pacific biogeography; vicariance; island integration; conservation ID INDO-PACIFIC REGION; WEST PACIFIC; CORAL-REEFS; COMPARATIVE PHYLOGEOGRAPHY; EQUATORIAL PACIFIC; BIOGEOGRAPHY; PATTERNS; CONSERVATION; SEA; MODEL AB Multiple datasets show global maxima of marine biodiversity in the Indo-Malay-Philippines archipelago (IMPA). Analysis of distribution data for 2983 species reveals a pattern of richness on a finer scale and identifies a peak of marine biodiversity in the central Philippine Islands and a secondary peak between peninsular Malaysia and Sumatra. This pattern is repeated in diverse habitat and higher taxa classes, most rigorously for marine shore fishes, supporting geohistorical hypotheses as the most general unifying explanations. Specific predictions based on area of overlap, area of accumulation, and area of refuge hypotheses suggest that present day eastern Indonesia, or Wallacea, should be the center of marine biodiversity. Processes suggested by these three hypotheses contribute to the diversity in this region and are also a likely explanation for the secondary center of diversity. Our study indicates, however, that there is a higher concentration of species per unit area in the Philippines than anywhere in Indonesia, including Wallacea. The Philippine center of diversity is consistent with hypotheses that this area experienced numerous vicariant and island integration events and these hypotheses warrant further testing. Special attention to marine conservation efforts in the Philippines is justified because of the identification of it as an epicenter of biodiversity and evolution. C1 Old Dominion Univ, Dept Biol Sci, Norfolk, VA 23529 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Zool MRC159, Div Fishes, Washington, DC 20013 USA. RP Carpenter, KE (reprint author), Old Dominion Univ, Dept Biol Sci, Norfolk, VA 23529 USA. EM kcarpent@odu.edu NR 57 TC 163 Z9 175 U1 1 U2 34 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013 USA SN 0378-1909 J9 ENVIRON BIOL FISH JI Environ. Biol. Fishes PD APR PY 2005 VL 72 IS 4 BP 467 EP 480 DI 10.1007/s10641-004-3154-4 PG 14 WC Ecology; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 922ZI UT WOS:000228878000012 ER PT J AU Gallegos, CL AF Gallegos, CL TI Optical water quality of a blackwater river estuary: the Lower St. Johns River, Florida, USA SO ESTUARINE COASTAL AND SHELF SCIENCE LA English DT Article DE St. Johns River; estuaries; optical properties; light penetration; water quality; colored dissolved organic matter; chlorophyll; total suspended solids ID DISSOLVED ORGANIC-MATTER; ABSORPTION-COEFFICIENTS; NATURAL PHYTOPLANKTON; SPECTRAL ABSORPTION; LIGHT-ABSORPTION; PARTICLES; CHLOROPHYLL; COASTAL; PLANTS; SEA AB This paper reports measurements of absorption and scattering coefficients in relation to standard water quality measurements in the St. Johns River (Florida, USA), a blackwater river in which phytoplankton chlorophyll and non-algal particulates as well as colored dissolved organic matter (CDOM) contribute substantially to the inherent optical properties of the water. Extremely high concentrations of CDOM in this river present special problems for the measurement of inherent optical properties, such as the presence of very fine particulate matter that passes through most glass fiber filters. Empirical relationships are presented for estimating true dissolved absorption at very high CDOM concentrations. Specific-absorption and -scattering coefficients of suspended particulate matter varied widely, but appeared to decline steadily with salinity at salinities above 5, consistent with increasing influence of large-sized, unconsolidated mineral particulates with increasing tidal energy near the estuary mouth. Relationships are given for prediction of inherent optical properties from water quality concentrations for use in radiative transfer modeling, and changes in water quality measurements are recommended that can avoid the need for empirical corrections. (c) 2004 Elsevier Ltd. All rights reserved. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Gallegos, CL (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM gallegosc@si.edu OI Gallegos, Charles/0000-0001-5112-0166 NR 31 TC 35 Z9 41 U1 1 U2 10 PU ACADEMIC PRESS LTD ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0272-7714 J9 ESTUAR COAST SHELF S JI Estuar. Coast. Shelf Sci. PD APR PY 2005 VL 63 IS 1-2 BP 57 EP 72 DI 10.1016/j.ecss.2004.10.010 PG 16 WC Marine & Freshwater Biology; Oceanography SC Marine & Freshwater Biology; Oceanography GA 908FR UT WOS:000227773300006 ER PT J AU Krot, AN Fagan, TJ Nagashima, K Petaev, MI Yurimoto, H AF Krot, AN Fagan, TJ Nagashima, K Petaev, MI Yurimoto, H TI Origin of low-Ca pyroxene in amoeboid olivine aggregates: Evidence from oxygen isotopic compositions SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article ID ALUMINUM-RICH INCLUSIONS; EARLY SOLAR-SYSTEM; CARBONACEOUS CHONDRITES; FERROMAGNESIAN CHONDRULES; ALLENDE METEORITE; GENETIC LINK; CONDENSATION; MINERALOGY; NEBULA; HETEROGENEITY AB Amoeboid olivine aggregates (AOAs) in primitive carbonaceous chondrites consist of forsterite (Fa(< 2)), Fe,Ni-metal, spinel, Al-diopside, anorthite, and rare gehlenitic melilite (angstrom k(< 15)) similar to 10% of AOAs contain low-Ca pyroxene (Fs(1-3)Wo(1-5)) that is in corrosion relationship with forsterite, and is found in three major textural occurrences: (i) thin (< 15 mu m) discontinuous layers around forsterite grains or along forsterite grain boundaries in AOA peripheries; (ii) 5-10-mu m-thick haloes and subhedral grains around Fe,Ni-metal nodules in AOA peripheries, and (iii) shells of variable thickness (up to 70 mu m), commonly with abundant tiny (3-5 mu m) inclusions of Fe,Ni-metal grains, around AOAs. AOAs with the low-Ca pyroxene shells are compact and contain euhedral grains of Al-diopside surrounded by anorthite, suggesting small (10%-20%) degree of melting. AOAs with other textural occurrences of low-Ca pyroxene are rather porous. Forsterite grains in AOAs with low-Ca pyroxene have generally O-16-rich isotopic compositions (Delta(17)O < -20%). Low-Ca pyroxenes of the textural occurrences (i) and (ii) are O-16-enriched (Delta(17)O < -20%), whereas those of (iii) are O-16-depleted (Delta(17)O = -6% to -4%). One of the extensively melted (> 50%) objects is texturally and mineralogically intermediate between AOAs and Al-rich chondrules. It consists of euhedral forsterite grains, pigeonite, augite, anorthitic mesostasis, abundant anhedral spinel grains, and minor Fe,Ni-metal; it is surrounded by a coarse-grained igneous rim largely composed of low-Ca pyroxene with abundant Fe,Ni-metal-sulfide nodules. The mineralogical observations suggest that only spinel grains in this igneous object were not melted. The spinel is O-16-rich (Delta(17)O similar to -22%), whereas the neighboring plagioclase mesostasis is O-16-depleted (Delta(17)O similar to -11%). We conclude that AOAs are aggregates of solar nebular condensates (forsterite, Fe,Ni-metal, and CAls composed of Al-diopside, anorthite, spinel, and +/- melilite) formed in an O-16-rich gaseous reservoir, probably CAI-forming region(s). Solid or incipiently melted forsterite, in some AOAs reacted with gaseous SiO in the same nebular region to form low-Ca pyroxene. Some other AOAs appear to have accreted O-16-poor pyroxene-normative dust and experienced varying degrees of melting, most likely in chondrule-forming region(s). The most extensively melted AOAs experienced oxygen isotope exchange with O-16-poor nebular gas and may have been transformed into chondrules. The original O-16-rich signature of the precursor materials of such chondrules is preserved only in incompletely melted grains. Copyright (c) 2005 Elsevier Ltd. C1 Univ Hawaii Manoa, Sch Ocean & Earth Sci & Technol, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA. Tokyo Inst Technol, Dept Earth & Planetary Sci, Tokyo 1528551, Japan. Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA. RP Univ Hawaii Manoa, Sch Ocean & Earth Sci & Technol, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA. EM sasha@higp.hawaii.edu NR 52 TC 18 Z9 18 U1 0 U2 4 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 EI 1872-9533 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD APR 1 PY 2005 VL 69 IS 7 BP 1873 EP 1881 DI 10.1016/j.gca.2004.06.046 PG 9 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 916EC UT WOS:000228367200017 ER PT J AU Robbins, MB Braun, MJ Huddleston, CJ Finch, DW Milensky, CM AF Robbins, MB Braun, MJ Huddleston, CJ Finch, DW Milensky, CM TI First Guyana records, natural history and systematics of the White-naped Seedeater Dolospingus fringilloides SO IBIS LA English DT Article ID DARWINS FINCHES; EVOLUTION; PRIMERS; BIRDS; AVES AB We report the first records of the White-naped Seedeater Dolospingus fringilloides for Guyana, provide new information on its natural history and plumage sequences, and clarify its systematic relationships based on DNA sequence data. Dolospingus is a rare and patchily distributed endemic of white-sand scrub of the Guianan shield region. Phylogenetic analyses of a broad sampling of emberizine cytochrome b sequences identified a 'seed finch' clade consisting of the genera Sporophila, Oryzoborus and Dolospingus with 100% bootstrap support. More intensive maximum-likelihood (ML) and Bayesian analyses conducted with a reduced data set indicated strong support for the same 'seed finch' clade, but could not distinguish the three genera. In the optimal ML trees, Dolospingus and Oryzoborus were nested within Sporophila, and the two Oryzoborus sequences did not cluster together. However, resolution within the seed-finch clade was weak, so the possibility that all three genera are monophyletic cannot be excluded on the basis of the available molecular data. Thus, whether to group these genera on the basis of genetic similarity or retain them on the basis of diagnostic bill and skull differences will remain a matter of preference until a more fully resolved phylogeny of the seed-finch clade is achieved. C1 Univ Kansas, Museum Nat Hist, Div Birds, Lawrence, KS 66045 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Suitland, MD 20746 USA. WINGS, Tucson, AZ 85712 USA. Smithsonian Inst, Div Birds, Washington, DC 20013 USA. RP Robbins, MB (reprint author), Univ Kansas, Museum Nat Hist, Div Birds, Lawrence, KS 66045 USA. EM mrobbins@ku.edu NR 41 TC 6 Z9 7 U1 2 U2 3 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0019-1019 J9 IBIS JI Ibis PD APR PY 2005 VL 147 IS 2 BP 334 EP 341 DI 10.1111/j.1474-919x.2005.00408.x PG 8 WC Ornithology SC Zoology GA 912AC UT WOS:000228048500010 ER PT J AU Gutierrez, M Capson, TL Guzman, CM Gonzalez, J Ortega-Barria, E Quinoa, E Riguera, R AF Gutierrez, M Capson, TL Guzman, CM Gonzalez, J Ortega-Barria, E Quinoa, E Riguera, R TI Leptolide, a new furanocembranolide diterpene from Leptogorgia alba SO JOURNAL OF NATURAL PRODUCTS LA English DT Article ID CHEMICAL DEFENSES; NATURAL-PRODUCTS; 12-BETA-EPOXYPUKALIDE; OCTOCORALLIA; LOPHOGORGIA; LOPHOTOXIN; 11-BETA AB Six faranocembranolides (1-6) and one pseudopterolide (7) have been isolated from the octocorals Leptogorgia alba and Leptogorgia rigida, collected on the Pacific coast of Panama. Compound 1, named leptolide, has a new structure closely related to the neurotoxin lophotoxin (3). The X-ray structures of 1-3 were determined, and the absolute configurations of 2-7 are discussed. Compounds 1-7 were evaluated in vitro against drug-resistant Plasmodium falciparum. C1 Univ Santiago de Compostela, CSIC, Dept Quim Organ, Inst Acuicultura, E-15782 Santiago De Compostela, Spain. Univ Santiago de Compostela, Unidad RMN Biomol Asociada, Dept Quim Organ, Inst Acuicultura, E-15782 Santiago De Compostela, Spain. Smithsonian Trop Res Inst, Balboa 2072, Panama. Inst Adv Sci Invest & High Technol Serv, Secretariat Sci & Technol, Clayton, Panama. RP Riguera, R (reprint author), Univ Santiago de Compostela, CSIC, Dept Quim Organ, Inst Acuicultura, E-15782 Santiago De Compostela, Spain. EM ricardo@usc.es RI Quinoa, Emilio/D-8920-2011; Riguera, Ricardo/I-6476-2015 OI Quinoa, Emilio/0000-0003-3019-3408; Riguera, Ricardo/0000-0001-5133-0454 FU FIC NIH HHS [1U01 TW006634-01, 1U01 TW01021-01] NR 20 TC 34 Z9 34 U1 0 U2 8 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 APR PY 2005 VL 68 IS 4 BP 614 EP 616 DI 10.1021/np049745z PG 3 WC Plant Sciences; Chemistry, Medicinal; Pharmacology & Pharmacy SC Plant Sciences; Pharmacology & Pharmacy GA 920GI UT WOS:000228677000031 PM 15844963 ER PT J AU Riley, S AF Riley, S TI Everything changes. SO LIBRARY JOURNAL LA English DT Book Review C1 Smithsonian Inst Lib, Washington, DC USA. RP Riley, S (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 APR 1 PY 2005 VL 130 IS 6 BP 89 EP 90 PG 2 WC Information Science & Library Science SC Information Science & Library Science GA 913CK UT WOS:000228127800105 ER PT J AU Schroll, S AF Schroll, S TI Steinberg at the New Yorker. 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 APR 1 PY 2005 VL 130 IS 6 BP 93 EP 93 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 913CK UT WOS:000228127800121 ER PT J AU Aiello, A AF Aiello, A TI Field guide to grasshoppers, katydids, and crickets of the United States. SO LIBRARY JOURNAL LA English DT Book Review C1 Smithsonian Trop Res Inst, Panama City, FL USA. RP Aiello, A (reprint author), Smithsonian Trop Res Inst, Panama City, FL 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 APR 1 PY 2005 VL 130 IS 6 BP 120 EP 120 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 913CK UT WOS:000228127800253 ER PT J AU Mair, RW Hrovat, MI Patz, S Rosen, MS Ruset, IC Topulos, GP Tsai, LL Butler, JP Hersman, FW Walsworth, RL AF Mair, RW Hrovat, MI Patz, S Rosen, MS Ruset, IC Topulos, GP Tsai, LL Butler, JP Hersman, FW Walsworth, RL TI He-3 lung imaging in an open access, very-low-field human magnetic resonance imaging system SO MAGNETIC RESONANCE IN MEDICINE LA English DT Article DE orientation; lung function; lung imaging; open-access; very-low-field MRI ID HYPERPOLARIZED NOBLE-GASES; PULMONARY BLOOD-FLOW; HEALTHY-VOLUNTEERS; DISEASED LUNGS; MRI; DIFFUSION; LASER; GRAVITY; SPACE; ECHO AB The human lung and its functions are extremely sensitive to gravity; however, the conventional high-field magnets used for most laser-polarized He-3 MRI of the human lung restrict subjects to lying horizontally. Imaging of human lungs using inhaled laser-polarized 3 He gas is demonstrated in an open-access very-low-magnetic-field (< 5 mT) MRI instrument. This prototype device employs a simple, low-cost electromagnet, with an open geometry that allows variation of the orientation of the imaging subject in a two-dimensional plane. As a demonstration, two-dimensional lung images were acquired with 4-mm in-plane resolution from a subject in two orientations: lying supine and sitting in a vertical position with one arm raised. Experience with this prototype device will guide optimization of a second-generation very-low-field imager to enable studies of human pulmonary physiology as a function of subject orientation. Magn Reson Med 53:745-749, 2005. (c) 2005 WileyLiss, Inc. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Mirtech Inc, Brockton, MA USA. Brigham & Womens Hosp, Boston, MA 02115 USA. Univ New Hampshire, Dept Phys, Durham, NH 03824 USA. MIT, Harvard Mit Div Hlth Sci & Technol, Cambridge, MA 02139 USA. Harvard Univ, Sch Publ Hlth, Boston, MA 02115 USA. RP Mair, RW (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 59, Cambridge, MA 02138 USA. EM rmair@cfa.harvard.edu RI Patz, Samuel/I-2879-2012 FU NCRR NIH HHS [RR14297] NR 30 TC 37 Z9 37 U1 1 U2 9 PU JOHN WILEY & SONS INC PI HOBOKEN PA 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 0740-3194 J9 MAGNET RESON MED JI Magn. Reson. Med. PD APR PY 2005 VL 53 IS 4 BP 745 EP 749 DI 10.1002/mrm.20456 PG 5 WC Radiology, Nuclear Medicine & Medical Imaging SC Radiology, Nuclear Medicine & Medical Imaging GA 912HL UT WOS:000228068100001 PM 15799045 ER PT J AU O'Dea, A AF O'Dea, A TI Zooid size parallels contemporaneous oxygen isotopes in a large colony of Pentapora foliacea (Bryozoa) SO MARINE BIOLOGY LA English DT Article ID CHEILOSTOME BRYOZOANS; GROWTH; TEMPERATURE; ECTOTHERMS; PUZZLE; RULE; SEA AB The relationship between seasonal changes in temperature and the size of zooids within cheilostome bryozoans is explored by comparing zooid size and contemporaneous carbonate mineralogy within a single colony of a perennial species that grew in a highly seasonal environment. Previously published oxygen isotope profile data from two fronds of a large colony of Pentapora foliacea from the Irish Sea record the cyclical patterns related to seasonal changes in temperature experienced by the colony over 3 years of growth. Zooid size data gathered from the same points at which the oxygen isotope data were taken reveal that zooid size and contemporaneous delta(18)O values covary. These and previously published data show that zooid size profiling can be confidently used to easily estimate rates of growth and longevity of bryozoan colonies, and further illustrate the negative relationship between zooid size and ambient temperature. Some inconsistencies in timing between zooid size and delta(18)O data may provide insights into the mechanisms behind temperature mediated body size changes in poikilothermic animals. C1 Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP O'Dea, A (reprint author), Smithsonian Trop Res Inst, Box 2072, Balboa, Ancon, Panama. EM odeaa@si.edu RI O'Dea, Aaron/D-4114-2011 NR 33 TC 21 Z9 21 U1 0 U2 4 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0025-3162 J9 MAR BIOL JI Mar. Biol. PD APR PY 2005 VL 146 IS 6 BP 1075 EP 1081 DI 10.1007/s00227-004-1523-3 PG 7 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 919ST UT WOS:000228638600003 ER PT J AU Wright, TF Rodriguez, AM Fleischer, RC AF Wright, TF Rodriguez, AM Fleischer, RC TI Vocal dialects, sex-biased dispersal, and microsatellite population structure in the parrot Amazona auropalliata SO MOLECULAR ECOLOGY LA English DT Article DE Amazona auropalliata; gene flow; microsatellite; parrot; sex-biased dispersal; vocal dialect ID WHITE-CROWNED SPARROWS; BROWN-HEADED COWBIRD; LAGOPUS-LAGOPUS-SCOTICUS; YELLOW-NAPED AMAZON; GENETIC-STRUCTURE; SONG DIALECTS; ZONOTRICHIA-CAPENSIS; MITOCHONDRIAL-DNA; SECONDARY CONTACT; BIRD SONG AB Geographic variation in microsatellite allele frequencies was assessed at nine sites in two regional vocal dialects of the parrot Amazona auropalliata (yellow-naped amazon) to test for correspondence between dialects and population structure. There was no relationship between the genetic distances between individuals and their dialect membership. High rates of gene flow were estimated between vocal dialects based on genetic differentiation. In addition, 5.5% of pairs of individuals compared across the dialect boundary were estimated to be related at the level of half siblings, indicating that dispersal is ongoing. The number of effective migrants per generation between dialects estimated with the microsatellite data was roughly one-seventh the number estimated with mitochondrial control region sequence data from the same individuals, suggesting that gene flow may be female-biased. Together, these results suggest that the observed mosaic pattern of geographic variation in vocalizations is maintained by learning of local call types by immigrant birds after dispersal. We found no evidence that ongoing habitat fragmentation has contributed to cryptic population structure. C1 Smithsonian Natl Zoo, Genet Program, Washington, DC 20008 USA. Univ Costa Rica, Posgrado Biol, San Jose, Costa Rica. RP Wright, TF (reprint author), New Mexico State Univ, Dept Biol, Las Cruces, NM 88003 USA. EM wright@nmsu.edu NR 64 TC 61 Z9 63 U1 1 U2 29 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0962-1083 J9 MOL ECOL JI Mol. Ecol. PD APR PY 2005 VL 14 IS 4 BP 1197 EP 1205 DI 10.1111/j.1365-294X.2005.02466.x PG 9 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 907MJ UT WOS:000227721900023 PM 15773946 ER PT J AU Helbig, AJ Kocum, A Seibold, I Braun, MJ AF Helbig, AJ Kocum, A Seibold, I Braun, MJ TI A multi-gene phylogeny of aquiline eagles (Aves : Accipitriformes) reveals extensive paraphyly at the genus level SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article DE diurnal birds of prey; Accipitriformes; systematics; cytochrome b; RAG-1; nuclear introns; plumage evolution; biogeography ID MITOCHONDRIAL-DNA SEQUENCES; BETA-FIBRINOGEN INTRON-7; CYTOCHROME-B GENE; ADENYLATE KINASE; NUCLEAR GENE; CHARACTERS; EVOLUTION; GAPS; WOODPECKERS; INSERTIONS AB The phylogeny of the tribe Aquilini (eagles with fully feathered tarsi) was investigated using 4.2 kb of DNA sequence of one mitochondrial (cyt b) and three nuclear loci (RAG-1 coding region, LDH intron 3, and adenylate-kinase intron 5). Phylogenetic signal was highly congruent and complementary between mtDNA and nuclear genes. In addition to single-nucleotide variation, shared deletions in nuclear introns supported one basal and two peripheral clades within the Aquilini. Monophyly of the Aquilini relative to other birds of prey was confirmed. However, all polytypic genera within the tribe, Spizaetus, Aquila, Hieraaetus, turned out to be non-monophyletic. Old World Spizaetus and Stephanoaetus together appear to be the sister group of the rest of the Aquilini. Spizastur melanoleucus and Oroaetus isidori are nested among the New World Spizaetus species and should be merged with that genus. The Old World 'Spizaetus' species should be assigned to the genus Nisaetus (Hodgson, 1836). The sister species of the two spotted eagles (Aquila clanga and Aquila pomarina) is the African Long-crested Eagle (Lophaetus occipitalis). Hieraaetus fasciatus/spilogaster are closest to Aquila verreauxii and should be merged with that genus. Wahlberg's Eagle H. wahlbergi, formerly placed in Aquila, is part of a clade including three small Hieraaetus species (pennatus, ayresii, and morphnoides). The Martial Eagle (Polemaetus bellicosus) is the sister species of the Aquila/Hieraaetus/Lophaetus clade. Basal relationships within this clade remained unresolved. Parsimony reconstruction of the evolution of plumage pattern within Aquilini suggests that: (1) transverse barring of parts of the body plumage was lost in the Palearctic Aquila-Hieraaetus clade, (2) pale underparts in adult plumage evolved three times independently, and (3) dimorphic adult plumage is a derived character of the small-bodied Hieraaetus clade. (c) 2004 Elsevier Inc. All rights reserved. C1 Univ Greifswald, Inst Zool, D-18565 Kloster Andechs, Germany. Natl Museum Nat Hist, Smithsonian Inst, Dept Zool, Suitland, MD 20746 USA. RP Helbig, AJ (reprint author), Univ Greifswald, Inst Zool, Vogelwarte Hiddensee, D-18565 Kloster Andechs, Germany. EM helbig@uni-greifswald.de NR 56 TC 42 Z9 52 U1 2 U2 14 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 1055-7903 J9 MOL PHYLOGENET EVOL JI Mol. Phylogenet. Evol. PD APR PY 2005 VL 35 IS 1 BP 147 EP 164 DI 10.1016/j.ympev.2004.10.003 PG 18 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 905WU UT WOS:000227602600011 PM 15737588 ER PT J AU Sheldon, FH Whittingham, LA Moyle, RG Slikas, B Winkler, DW AF Sheldon, FH Whittingham, LA Moyle, RG Slikas, B Winkler, DW TI Phylogeny of swallows (Aves : Hirundinidae) estimated from nuclear and mitochondrial DNA sequences SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article DE swallow phylogeny; Hirundinidae; DNA sequencing; mitochondrial DNA; nuclear DNA ID LENGTH DIFFERENCE TEST; CYTOCHROME-B GENE; EVOLUTION; INCONGRUENCE; HYBRIDIZATION; SUBSTITUTION; SYSTEMATICS; LIKELIHOOD; UTILITY AB The phylogeny of swallows was reconstructed by comparing segments of three genes, nuclear beta-fibrinogen intron 7 (beta fib7), mitochondrial cytochrome b (cytb), and mitochondrial ND2, in a variety of combinations using maximum likelihood and Bayesian methods. beta fib7 was sequenced for 47 species, cytb for 74 species, and ND2 for 61 species to yield comparisons among 75 of the 84 currently recognized swallow species. The family Hirundinidae was confirmed to consist of two clades, Pseudochelidoninae (river martins) and Hirundininae (typical swallows). The Hirundininae is further divided into mud nesters (Hirundo sensu lato), core martins (Phedina, Riparia, and New World endemic genera), and basal relicts (Psalidoprocne, Cheramoeca, and Pseudhirundo). We did not resolve the hierarchy among these three hirundinine groups, but discovered many relationships within them. Mud-nesting genera have the following relationships: (Hirundo sensu stricto, Ptyonoprogne), (Delichon, (Petrochelidon, Cecropis)). Core martins have the following topology: (Phedina, Riparia cincta), (Riparia sensu stricto, Tachycineta, ((Stelgidopteryx, Progne), (Neotropical endemic genera))). Interspecific relationships among the Neotropical endemics were resolved completely; Atticora and Notiochelidon are paraphyletic, and all Neotropical endemics probably should be lumped into one or two genera. The final group of hirundinines, the basal relicts, consists of a sister pair, the Australian Cheramoeca and African Pseudhirundo. The African saw-wings (Psalidoprocne) are their likely sister group. (c) 2004 Elsevier Inc. All rights reserved. C1 Louisiana State Univ, Museum Nat Sci, Baton Rouge, LA 70803 USA. Univ Wisconsin, Dept Biol Sci, Milwaukee, WI 53201 USA. Amer Museum Nat Hist, Dept Ornithol, New York, NY 10024 USA. Smithsonian Inst, Natl Zool Pk, Washington, DC 20008 USA. Cornell Univ, Museum Vertebrates, Dept Ecol & Evolutionary Biol, Ithaca, NY 14853 USA. RP Sheldon, FH (reprint author), Louisiana State Univ, Museum Nat Sci, 119 Foster Hall, Baton Rouge, LA 70803 USA. EM fsheld@lsu.edu RI Slikas, Beth/E-7275-2013 NR 58 TC 58 Z9 67 U1 1 U2 16 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 1055-7903 J9 MOL PHYLOGENET EVOL JI Mol. Phylogenet. Evol. PD APR PY 2005 VL 35 IS 1 BP 254 EP 270 DI 10.1016/j.ympev.2004.11.008 PG 17 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 905WU UT WOS:000227602600018 PM 15737595 ER PT J AU Grissell, EE Revel, GE AF Grissell, EE Revel, GE TI First report of Theocolax ingens Xiao and Huang (Hymenoptera : Pteromalidae) in the Western Hemisphere, with a synopsis of the genus SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Hymenoptera; Chalcidoidea; Pteromalidae; Theocolax; Cerocephala; new record; synonymy; Western Hemisphere AB Theocolax ingens Xiao and Huang is reported for the first time from the Western Hemisphere (Silver Spring, Maryland, USA). The known species of Theocolax Westwood are discussed and their host data summarized. Theocolax fasciata (Ishii 1956) is transferred from the genus and synonymized with Cerocephala aquila (Girault 1920) (n. syn.). C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Agr, Agr Res Serv,Systemat Entomol Lab, Washington, DC 20013 USA. Natl Museum Nat Hist, Dept Entomol, Washington, DC 20013 USA. RP Grissell, EE (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Agr, Agr Res Serv,Systemat Entomol Lab, POB 37012,MRC 168, Washington, DC 20013 USA. NR 18 TC 1 Z9 1 U1 0 U2 0 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD APR PY 2005 VL 107 IS 2 BP 254 EP 258 PG 5 WC Entomology SC Entomology GA 915CL UT WOS:000228275100002 ER PT J AU Smith, DR AF Smith, DR TI Two new fern-feeding sawflies of the genus Aneugmenus hartig (Hymenoptera : Tenthredinidae) from South America SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE selandriinae; ferns; Venezuela; Colombia AB Aueugmenus merida, n. sp., from Venezuela and Ecuador and A. colombia, n. sp., from Colombia are described. Aneugmenus merida was reared from larvae feeding on bracken fern, Pteridium aquilinum (L.) Kuhn. in Venezuela. These are the only two species of this Holarctic genus known from South America. The species are illustrated and separated from other New World species of Aneugmenus. Aneugmenus leucopoda (Cameron 1883) is a new combination. C1 USDA, Agr Res Serv, Systemat Entomol Lab, Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20013 USA. RP Smith, DR (reprint author), USDA, Agr Res Serv, Systemat Entomol Lab, Natl Museum Nat Hist,Smithsonian Inst, POB 37012,MRC 168, Washington, DC 20013 USA. EM dsmith@sel.barc.usda.gov NR 6 TC 5 Z9 7 U1 0 U2 0 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD APR PY 2005 VL 107 IS 2 BP 273 EP 278 PG 6 WC Entomology SC Entomology GA 915CL UT WOS:000228275100005 ER PT J AU Neunzig, HH Solis, MA AF Neunzig, HH Solis, MA TI A review of the neotropical genus Difundella Dyar (Lepidoptera : Pyralidae : Phycitinae) SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Brazil; Costa Rica; Neftundella; Coptarthria; Rampylla AB The genus Difundella is redescribed. Seven species are recognized as belonging to the genus: D. cancerella n. sp., D. corynophora Dyar, D. dumiella Neunzig and Dow, D. parana n. sp., D. subsutella (Schaus), D. teresina n. sp., and D. unguifera n. sp. A key to species based on male adults is included. Difundella is compared to the similar genera Nefundello Neunzig, Coptarthria Ragonot, and Rampylla Dyar. C1 N Carolina State Univ, Dept Entomol, Raleigh, NC 27695 USA. USDA, Smithsonian Inst, Natl Museum Nat Hist, Systemat Entomol Lab, Washington, DC 20013 USA. RP Solis, MA (reprint author), N Carolina State Univ, Dept Entomol, Raleigh, NC 27695 USA. EM asolis@sel.barc.usda.gov NR 5 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 APR PY 2005 VL 107 IS 2 BP 303 EP 314 PG 12 WC Entomology SC Entomology GA 915CL UT WOS:000228275100007 ER PT J AU Saini, MS Smith, DR AF Saini, MS Smith, DR TI Revision of the southeastern Asian sawfly genus Busarbia Cameron (Hymenoptera : Tenthredinidae) SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE sawflies; Symphyta; Selandriinae; ferns AB Six species of Busarbia Cameron, a genus of the subfamily Selandriinae restricted to southeastern Asia, are known: B. viridipes Cameron, B. shinoharai, n. sp., B. okutanii, n. sp., and B. santokhi, n. sp., from India; B. formosana (Rohwer) from Taiwan, Myanmar, and India; and B. isshikii (Takeuchi) from Taiwan. Busarbia formosana is recorded from India for the first tine. An identification key is provided, and each species is described and illustrated. C1 Punjabi Univ, Dept Zool, Patiala 147002, Punjab, India. USDA, Natl Museum Nat Hist, Smithsonian Inst, Agr Res Serv,Systemat Entomol Lab, Washington, DC 20013 USA. RP Saini, MS (reprint author), Punjabi Univ, Dept Zool, Patiala 147002, Punjab, India. EM saini20@hotmail.com; dsmith@sel.barc.usda.gov NR 14 TC 1 Z9 2 U1 0 U2 1 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD APR PY 2005 VL 107 IS 2 BP 346 EP 356 PG 11 WC Entomology SC Entomology GA 915CL UT WOS:000228275100012 ER PT J AU Mathis, WN Zumbado, MA AF Mathis, WN Zumbado, MA TI Description of Scatella savegre, a new species from Costa Rica in the triseta group (Diptera : Ephydridae) SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Scatella; the triseta group; ephydridae; shore flies; Costa Rica AB A new species of Scatella belonging to the triseta group, S. savegre, is described from specimens collected in Costa Rica (San Jose: Rio Savegre, San Gerardo de Dota (9 degrees 39.5'N, 83 degrees 51'W; 2,180 m)). For perspective, diagnoses for Scatella and the triseta group are provided, and to facilitate identification a key to species of the triseta group as well as figures of the head and wings (male and female) are provided. C1 Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, Washington, DC 20013 USA. Inst Nacl Biodiversidad, Santo Domingo, Heredia, Costa Rica. RP Mathis, WN (reprint author), Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, POB 37012,CE 619,MRC 169, Washington, DC 20013 USA. EM mathis.wayne@nmnh.si.edu; mzumbado@inbio.ac.cr NR 9 TC 1 Z9 1 U1 1 U2 1 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD APR PY 2005 VL 107 IS 2 BP 386 EP 391 PG 6 WC Entomology SC Entomology GA 915CL UT WOS:000228275100017 ER PT J AU Robbins, RK Duarte, M AF Robbins, RK Duarte, M TI Phylogenetic analysis of Cyanophrys clench, a synopsis of its species, and the potentially threatened C-bertha (Jones) (Lycaenidae : Theclinae : Eumaeini) SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Callophrys; phylogeny; venation; genitalia; androconia; brush organs AB A species level phylogenetic analysis of Cyanophrys Clench was performed using 14 characters of the frons, wing venation, wing shape, androconia, and genitalia. There were 15 most parsimonious cladograms, and a successive weighting iteration resulted in three of these 15. Cyanophrys is characterized in this paper by two hypothesized synapomorphies (an expanded hindwing anal lobe that is tan-brown and a pair of dorsal brush organs), and adults can be readily identified in the field. Cyanophrys has been divided into Plesiocyanophrys K. Johnson, Eisele and MacPherson, Apophrys K. Johnson and Le Crom, Antephrys K. Johnson, Eisele and MacPherson, Mesocyanophrys K. Johnson, and Cyanophrys (as delimited in Johnson and Le Crom 1997a), but only the monotypic Antephrys is monophyletic on the most parsimonious cladograms. A synopsis of Cyanophrys species includes notes on their distribution, habitat, identification, nomenclature, larval food plants, and male behavior. Cyanophrys bertha, which occurs in moist evergreen and seasonally deciduous forests in the mountains of southern Brazil from 800 to 1,400 m elevation, has been proposed for threatened status. It is "cladistically distinct" (sensu Vane-Wright et al. 1991) in that its sister is a lineage of five montane species or seven primarily lowland species. C1 Smithsonian Inst, Dept Entomol, Washington, DC 20013 USA. Univ Sao Paulo, Museum Zool, BR-04263000 Sao Paulo, Brazil. RP Robbins, RK (reprint author), Smithsonian Inst, Dept Entomol, POB 37012,NHB Stop 127, Washington, DC 20013 USA. EM RobbinsR@si.edu; mduartes@usp.br RI Duarte, Marcelo/K-7633-2012; Museu de Zoologia da USP, MZ-USP/Q-2192-2016 NR 49 TC 8 Z9 14 U1 0 U2 0 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD APR PY 2005 VL 107 IS 2 BP 398 EP 416 PG 19 WC Entomology SC Entomology GA 915CL UT WOS:000228275100019 ER PT J AU Robinson, H Woodley, NE AF Robinson, H Woodley, NE TI A new species of Harmstonia (Diptera : Dolichopodidae) from Bolivia SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Harmstonia; Bolivia; South America AB Harmstonia ichilo Robinson and Woodley, new species, is described from Ichilo Province, Santa Cruz Department, Bolivia and is the first record for the genus in South America. C1 Natl Museum Nat Hist, Dept Bot, Smithsonian Inst, Washington, DC 20013 USA. USDA ARS, Systemat Entomol Lab, PSI, Washington, DC 20013 USA. RP Robinson, H (reprint author), Natl Museum Nat Hist, Dept Bot, Smithsonian Inst, POB 37012,MRC 168, Washington, DC 20013 USA. EM nwoodley@sel.barc.usda.gov RI Woodley, Norman/M-6160-2014 NR 4 TC 0 Z9 0 U1 0 U2 1 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD APR PY 2005 VL 107 IS 2 BP 436 EP 440 PG 5 WC Entomology SC Entomology GA 915CL UT WOS:000228275100023 ER PT J AU Steiner, WE AF Steiner, WE TI Studies on the darkling beetles (Coleoptera : Tenebrionidae) known from Grand Bahama Island, with descriptions of new species of Branchus and Adelina SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Bahamas; Casuarina; endemic insects; introduced species; island biogeography; new synonymy; threatened habitats ID GENUS; AMERICA; NORTH AB An annotated checklist of the darkling and comb-clawed beetles (Coleoptera: Tenebrionidae) of Grand Bahama Island is given, with observations on habitats, biology, and biogeography. More than 55% are new records for the Bahamas and some others are new island records. Branchus saxatilis Steiner, new species, and Adeliua maryjoae Steiner, new species, are described and illustrated. Nautes viridimicans (Horn 1878), described from Tampa, Florida, is placed as a new synonym under Nautes azurescens (Jacquelin du Val 1857), described from Cuba. Threats to some species via degradation of the native maritime scrub habitats are discussed. Of the 31 species now known from Grand Bahama, 25 also occur in Florida, and a subset of 18 of the Florida species also are known from Cuba. Five of the species are known or suspected to be adventure. C1 Smithsonian Inst, Dept Entomol, Washington, DC 20560 USA. RP Steiner, WE (reprint author), Smithsonian Inst, Dept Entomol, NHB-187, Washington, DC 20560 USA. EM steinerw@si.edu NR 50 TC 3 Z9 3 U1 0 U2 1 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD APR PY 2005 VL 107 IS 2 BP 441 EP 459 PG 19 WC Entomology SC Entomology GA 915CL UT WOS:000228275100024 ER PT J AU Bito, D Smith, DR AF Bito, D Smith, DR TI Larva and possible food plant of Ancyloneura varipes (Cameron) (Hymenoptera : Pergidae) in Papua New Guinea SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Editorial Material C1 Univ Papua New Guinea, Madang, Papua N Guinea. New Guinea Binatang Res Ctr, Madang, Papua N Guinea. USDA ARS, Systemat Entomol Lab, PSI, Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20013 USA. RP Bito, D (reprint author), Univ Papua New Guinea, POB 604, Madang, Papua N Guinea. EM binatangi@datec.com.pg; dsmith@sel.barc.usda.gov NR 9 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 APR PY 2005 VL 107 IS 2 BP 463 EP 465 PG 3 WC Entomology SC Entomology GA 915CL UT WOS:000228275100026 ER PT J AU Reinert, JF Harbach, RE Sallum, MAM AF Reinert, JF Harbach, RE Sallum, MAM TI Checklist of aedine mosquito species (Diptera, Culicidae, Aedini) occurring in Middle and South America (south of the United States) reflecting current generic and subgeneric status SO REVISTA BRASILEIRA DE ENTOMOLOGIA LA English DT Article DE Aedini; Culicidae; checklist AB Checklist of aedine mosquito species (Diptera, Culicidae, Aedini) occurring in Middle and South America (south of the United States) reflecting current generic and subgeneric status. A list of species of tribe Aedini from Middle and South American, south of the United States, with their current generic combinations is provided. Its purpose is to enable entomologists, public health personnel and mosquito control workers to more quickly become familiar with recent formal taxonomic changes within the tribe. C1 Agr Res Serv, CMAVE, USDA, Gainesville, FL 32608 USA. Smithsonian Inst, WRBU, Natl Museum Nat Hist, Washington, DC 20560 USA. Nat Hist Museum, Dept Entomol, London SW7 5BD, England. Sch Publ Hlth, Dept Epidemiol, Med Entomol Unit Taxon & Syst Res, Sao Paulo, Brazil. RP Reinert, JF (reprint author), Agr Res Serv, CMAVE, USDA, 1600-1700 SW 23rd Dr, Gainesville, FL 32608 USA. RI Sallum, Maria/B-8537-2012 NR 5 TC 9 Z9 10 U1 0 U2 1 PU SOCIEDADE BRASILEIRA DE ENTOMOLOGIA PI CURITIBA PA CAIXA POSTAL 19030, CURITIBA, PR 81531-980, BRAZIL SN 0085-5626 J9 REV BRAS ENTOMOL JI Rev. Bras. Entomol. PD APR-JUN PY 2005 VL 49 IS 2 BP 249 EP 252 DI 10.1590/S0085-56262005000200009 PG 4 WC Entomology SC Entomology GA 946EL UT WOS:000230555000009 ER PT J AU D'Alessio, P Merin, B Calvet, N Hartmann, L Montesinos, B AF D'Alessio, P Merin, B Calvet, N Hartmann, L Montesinos, B TI Www database of models of accretion disks irradiated by the central star SO REVISTA MEXICANA DE ASTRONOMIA Y ASTROFISICA LA English DT Article DE accretion disks; astronomical data bases; stars : pre-main sequence ID T-TAURI STARS; SPECTRAL ENERGY-DISTRIBUTIONS; YOUNG STELLAR OBJECTS; EMISSION-LINE DIAGNOSTICS; INTERMEDIATE-MASS STARS; VERTICAL STRUCTURE; MAGNETOSPHERIC ACCRETION; CIRCUMSTELLAR DISKS; PROTOPLANETARY DISK; DM-TAU AB We announce the release of a catalog of physical models of irradiated accretion disks around young stars based on the modelling techniques by D'Alessio et al. The WWW catalog includes similar to 3000 disk models for different central stars, disk sizes, inclinations, dust contents and mass accretion rates. For any of them, radial profiles of disk physical parameters and synthetic spectral energy distributions can be browsed and downloaded to compare with observations. The catalog can be accessed at http://cfa-www.harvard.edu/youngstars/dalessio/ US), http: //www. astrosmo. unam. mx/similar to dalessio/ (Mexico), and at http: // www.laeff.esa.es/models/dalessio/ (Spain). C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Nacl Autonoma Mexico, Ctr Radioastron & Astrofis, Morelia 58090, Michoacan, Mexico. INTA, Lab Astrofis Espacial & Fis Fundamental, E-28080 Madrid, Spain. CSIC, Inst Astrofis Andalucia, E-18008 Granada, Spain. RP D'Alessio, P (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM p.dalessio@astrosmo.unam.mx; merin@strw.leidenuniv.nl; ncalvet@cfa.harvard.edu; hartmann@cfa.harvard.edu; bmm@laeff.esa.es RI Montesinos, Benjamin/C-3493-2017 OI Montesinos, Benjamin/0000-0002-7982-2095 NR 58 TC 41 Z9 41 U1 0 U2 0 PU UNIV NACIONAL AUTONOMA MEXICO, INST DE ASTRONOMIA PI MEXICO CITY PA APDO POSTAL 70-264, MEXICO CITY 04510, MEXICO SN 0185-1101 J9 REV MEX ASTRON ASTR JI Rev. Mex. Astron. Astrofis. PD APR PY 2005 VL 41 IS 1 BP 61 EP 67 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 920QU UT WOS:000228706000008 ER PT J AU Small, LM AF Small, LM TI Invention at play - The Lemelson Center celebrates a decade of nurturing the inventor in each of us 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 APR PY 2005 VL 36 IS 1 BP 14 EP 14 PG 1 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA 908SX UT WOS:000227811600002 ER PT J AU Wagner, WL AF Wagner, WL TI Systematics of Oenothera sections Contortae, Eremia, and Ravenia (Onagraceae) SO SYSTEMATIC BOTANY LA English DT Article ID OBSERVING POLLEN TUBES; POPULATION; ORGANENSIS; FLUORESCENCE; EUOENOTHERA; EMERSONIA; RAIMANNIA; EVOLUTION; BIOLOGY AB Previous classifications based on morphology recognized a distinctive but poorly delimited group of species from western North America as Oenothera subg. Pachylophus. In earlier papers, I split this group into four sections more comparable to others in the genus, but nevertheless assumed the whole group was monophyletic based on morphological analyses. Recent molecular analyses indicate that the morphological analysis was incorrect, however, and suggest instead that the sections are part of a basal grade within the genus. The two yellow flowered sections are shown by the molecular study to be sister taxa, yet because of highly distinctive morphology, especially of the capsules and seeds, I maintain them as separate sections, sect. Contortae (O. xylocarpa) and sect. Eremia (O. primiveris) comparable to others in the genus. The two white flowered sections, sect. Pachylophus (O. brandegeei, O cespitosa, O. cavernae, O. harringtonii, and O. psammophila) and sect. Ravenia (O. muelleri, O. riskindii, and O. tubifera with two subspecies, tubifera and macrocarpa), are not so closely related and the shift to white petals appears to have been independent. Detailed taxonomic descriptions are given for the species of sects. Contortae, Eremia, and Ravenia. Taxonomic treatment of the species of sect. Pachylophus was given elsewhere. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA. RP Wagner, WL (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, MRC 166,POB 37012, Washington, DC 20013 USA. EM wagnerw@si.edu NR 50 TC 3 Z9 4 U1 1 U2 9 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 APR-JUN PY 2005 VL 30 IS 2 BP 332 EP 356 DI 10.1600/0363644054223558 PG 25 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA 938QX UT WOS:000230019000010 ER PT J AU Schiffer, MB AF Schiffer, MB TI The electric lighthouse in the nineteenth century - Aid to navigation and political technology SO TECHNOLOGY AND CULTURE LA English DT Review C1 Univ Arizona, Tucson, AZ 85721 USA. Smithsonian Inst, Natl Museum Amer Hist, Lemelson Ctr, Washington, DC 20560 USA. RP Schiffer, MB (reprint author), Univ Arizona, Tucson, AZ 85721 USA. NR 137 TC 8 Z9 8 U1 0 U2 2 PU JOHNS HOPKINS UNIV PRESS PI BALTIMORE PA JOURNALS PUBLISHING DIVISION, 2715 NORTH CHARLES ST, BALTIMORE, MD 21218-4363 USA SN 0040-165X J9 TECHNOL CULT JI Technol. Cult. PD APR PY 2005 VL 46 IS 2 BP 275 EP 305 DI 10.1353/tech.2005.0098 PG 31 WC History & Philosophy Of Science SC History & Philosophy of Science GA 939VE UT WOS:000230099700001 ER PT J AU Wappes, JE Lingafelter, SW AF Wappes, JE Lingafelter, SW TI The genus Canidia Thomson, 1857 (Coleoptera : Cerambycidae, Lamiinae, Acanthocinini) SO ZOOTAXA LA English DT Article DE Insecta; Coleoptera; Cerambycidae; Lamiinae; Acanthocinini; Canidia; Dectes; Canidiopsis; Pseudocanidia; new species; key AB The lamiine genus Canidia Thomson is redefined with Canidiopsis Dillon and Pseudocanidia Dillon as new synonyms. Three new species from Mexico are described and illustrated: Canidia chemsaki, C. giesberti, and C. turnbowi. The following new synonymies are proposed: Canidiopsis similis Dillon, 1955 and Canidiopsis hebes Dillon, 1955 = Canidia mexicana Thomson, 1860; Pseudocanidia cuernavacae Dillon, 1955 = Dectes spinicornis Bates, 1881; and Dectes ( Canidia) balteata var. inapicalis Tippmann, 1960 = Dectes balteatus Lacordaire, 1872. A key to the eight species and one subspecies is presented. C1 Amer Coleoptera Museum, Bulverde, TX 78163 USA. ARS, Systemat Entomol Lab, Inst Plant Sci, USDA,Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20013 USA. RP Wappes, JE (reprint author), Amer Coleoptera Museum, 179 Fall Creek, Bulverde, TX 78163 USA. EM beetle@wireweb.net; slingafe@sel.barc.usda.gov NR 15 TC 2 Z9 2 U1 0 U2 0 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, 1030, NEW ZEALAND SN 1175-5334 J9 ZOOTAXA JI Zootaxa PD MAR 31 PY 2005 IS 927 BP 1 EP 27 PG 27 WC Zoology SC Zoology GA 911RU UT WOS:000228023100001 ER PT J AU Li, LX AF Li, LX TI Vacuum polarization in an anti-de Sitter space as an origin for a cosmological constant in a brane world SO MODERN PHYSICS LETTERS A LA English DT Article DE brane world; quantum gravity; cosmology ID QUANTUM FIELD-THEORY; EFFECTIVE POTENTIALS; DESITTER SPACETIME; EXTRA DIMENSIONS; TIME; PROPAGATORS; MILLIMETER; HIERARCHY; UNIVERSE; GRAVITY AB We show that the vacuum polarization of quantum fields in an anti-de Sitter space can naturally give rise to a small but nonzero cosmological constant in a brane world living in it. To explain the extremely small ratio of mass density in the cosmological constant to the Planck mass density in our universe ( approximate to 10(-123)) as suggested by cosmological observations, all we need is a four-dimensional brane world (our universe) living in a five-dimensional anti-de Sitter space with a curvature radius r(0) similar to 10(-3) cm and a fundamental Planck energy M-p - 10(9) GeV, and a scalar field with a mass m similar to r(0)(-1) similar to 10(-2) eV. Probing gravity down to a scale - 10(-3) cm, which is attainable in the near future, will provide a test of the model. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Li, LX (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM lli@cfa.harvard.edu NR 61 TC 1 Z9 1 U1 0 U2 1 PU WORLD SCIENTIFIC PUBL CO PTE LTD PI SINGAPORE PA 5 TOH TUCK LINK, SINGAPORE 596224, SINGAPORE SN 0217-7323 J9 MOD PHYS LETT A JI Mod. Phys. Lett. A PD MAR 28 PY 2005 VL 20 IS 10 BP 733 EP 743 DI 10.1142/S0217732305016944 PG 11 WC Physics, Nuclear; Physics, Particles & Fields; Physics, Mathematical SC Physics GA 919AA UT WOS:000228589500003 ER PT J AU Sues, H AF Sues, H TI Mammals from the age of dinosaurs - Origins, evolution, and structure SO SCIENCE LA English DT Book Review C1 Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Sues, H (reprint author), Smithsonian Inst, Natl Museum Nat Hist, MRC 106,POB 37012, Washington, DC 20013 USA. EM suesh@si.edu NR 5 TC 0 Z9 0 U1 1 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 MAR 25 PY 2005 VL 307 IS 5717 BP 1878 EP 1879 DI 10.1126/science.1109678 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 910UI UT WOS:000227957300031 ER PT J AU Stanton, JF Dudek, J Theule, P Gupta, H McCarthy, MC Thaddeus, P AF Stanton, JF Dudek, J Theule, P Gupta, H McCarthy, MC Thaddeus, P TI Laser spectroscopy of Si3C SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID SILICON-CARBON CLUSTERS; MANY-BODY METHODS; VIBRATIONAL-SPECTRA; ENERGY GRADIENTS; EXCITED-STATE; EXCITATION-ENERGIES; RESPONSE FUNCTIONS; RHOMBOIDAL SIC3; MASER EMISSION; WAVE-FUNCTION AB The C B-1(1)<- X (1)A(1) band system of the potential interstellar species Si3C has been recorded in a silane/acetylene discharge by resonant two-color two-photon ionization spectroscopy. The origin band is located near 24 925 cm(-1) (3.09 eV). Several other features in the spectrum are assigned to progressions in the Si-Si stretching modes as well as to sequence and hot band transitions. The assignment was facilitated by ab initio calculations, which also indicate that this is the strongest electronic transition of Si3C in the visible region of the spectrum. Features in the spectrum are broadened considerably (ca. 10 cm(-1)), and suggest an excited state lifetime of a few picoseconds. Possible reasons for the short-lived nature of the excited state are discussed. C1 Univ Texas, Ctr Theoret Chem, Dept Chem & Biochem, Austin, TX 78712 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Harvard Univ, Div Engn & Appl Sci, Cambridge, MA 02138 USA. RP Stanton, JF (reprint author), Univ Texas, Ctr Theoret Chem, Dept Chem & Biochem, Austin, TX 78712 USA. OI McCarthy, Michael/0000-0001-9142-0008 NR 52 TC 11 Z9 11 U1 1 U2 11 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0021-9606 J9 J CHEM PHYS JI J. Chem. Phys. PD MAR 22 PY 2005 VL 122 IS 12 AR 124314 DI 10.1063/1.1869981 PG 6 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 915HD UT WOS:000228287900023 PM 15836385 ER PT J AU Rocha, LA Robertson, DR Roman, J Bowen, BW AF Rocha, LA Robertson, DR Roman, J Bowen, BW TI Ecological speciation in tropical reef fishes SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE biodiversity; coral reef; marine biogeography; mtDNA; speciation ID LIFE-HISTORY TRAITS; MITOCHONDRIAL-DNA; COMPARATIVE PHYLOGEOGRAPHY; GENETIC-DIVERGENCE; MARINE-SPECIATION; SELF-RECRUITMENT; POPULATIONS; DISPERSAL; TELEOSTEI; PATTERNS AB The high biodiversity in tropical seas provides a long-standing challenge to allopatric speciation models. Physical barriers are few in the ocean and larval dispersal is often extensive, a combination that should reduce opportunities for speciation. Yet coral reefs are among the most species-rich habitats in the world, indicating evolutionary processes beyond conventional allopatry. In a survey of mtDNA sequences of five congeneric west Atlantic reef fishes (wrasses, genus Halichoeres) with similar dispersal potential, we observed phylogeographical patterns that contradict expectations of geographical isolation, and instead indicate a role for ecological speciation. In Halichoeres bivittatus and the species pair Halichoeres radiatus/brasiliensis, we observed strong partitions (3.4% and 2.3% divergence, respectively) between adjacent and ecologically distinct habitats, but high genetic connectivity between similar habitats separated by thousands of kilometres. This habitat partitioning is maintained even at a local scale where H. bivittatus lineages are segregated between cold- and warm-water habitats in both Bermuda and Florida. The concordance of evolutionary partitions with habitat types, rather than conventional biogeographical barriers, indicates parapatric ecological speciation, in which adaptation to alternative environmental conditions in adjacent locations overwhelms the homogenizing effect of dispersal. This mechanism can explain the long-standing enigma of high biodiversity in coral reef faunas. C1 Univ Florida, Dept Fisheries & Aquat Sci, Gainesville, FL 32653 USA. Smithsonian Trop Res Inst, Miami, FL 34002 USA. Harvard Univ, Dept Organism & Evolutionary Biol, Cambridge, MA 02138 USA. Univ Hawaii, Hawaii Inst Marine Biol, Kaneohe, HI 96744 USA. RP Rocha, LA (reprint author), Univ Florida, Dept Fisheries & Aquat Sci, 7922 NW 71st St, Gainesville, FL 32653 USA. EM rochal@naos.si.edu RI Rocha, Luiz/C-5107-2011 NR 52 TC 183 Z9 187 U1 8 U2 71 PU ROYAL SOCIETY PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8452 J9 P ROY SOC B-BIOL SCI JI Proc. R. Soc. Lond. Ser. B-Biol. Sci. PD MAR 22 PY 2005 VL 272 IS 1563 BP 573 EP 579 DI 10.1098/2004.3005 PG 7 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 921YU UT WOS:000228802900002 PM 15817431 ER PT J AU Furlanetto, SR Schaye, J Springel, V Hernquist, L AF Furlanetto, SR Schaye, J Springel, V Hernquist, L TI Ly alpha emission from structure formation SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : theory; galaxies : formation; intergalactic medium ID LYMAN-BREAK GALAXIES; PARTICLE HYDRODYNAMICS SIMULATIONS; SUBARU DEEP FIELD; STAR-FORMATION; INTERGALACTIC MEDIUM; FORMING GALAXIES; HIGH REDSHIFTS; REIONIZATION; EMITTERS; FOREST AB The nature of the interaction between galaxies and the intergalactic medium (IGM) is one of the most fundamental problems in astrophysics. The accretion of gas onto galaxies provides fuel for star formation, while galactic winds transform the nearby IGM in a number of ways. One exciting technique to study this gas is through the imaging of hydrogen Ly alpha emission. We use cosmological simulations to study the Ly alpha signals expected from the growth of cosmic structure from z = 0-5. We show that if dust absorption is negligible, recombinations following the absorption of stellar ionizing photons dominate the total Ly alpha photon production rate. However, galaxies are also surrounded by "Ly alpha coronae'' of diffuse IGM gas. These coronae are composed of a combination of accreting gas and material ejected from the central galaxy by winds. The Ly alpha emission from this phase is powered by a combination of gravitational processes and the photoionizing background. While the former dominates at z similar to 0, collisional excitation following photoheating may well dominate the total emission at higher redshifts. The central regions of these systems are dense enough to shield themselves from the metagalactic ionizing background; unfortunately, in this regime our simulations are no longer reliable. We therefore consider several scenarios for the emission from the central cores, including one in which self-shielded gas does not emit at all. We show that the combination of star formation and cooling IGM gas can explain most of the observed "Ly alpha blobs'' at z similar to 3, with the important exception of the largest sources. On the other hand, except under the most optimistic assumptions, cooling IGM gas cannot explain the observations on its own. C1 CALTECH, Pasadena, CA 91125 USA. Inst Adv Study, Sch Nat Sci, Princeton, NJ 08540 USA. Max Planck Inst Astrophys, D-85740 Garching, Germany. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Furlanetto, SR (reprint author), CALTECH, Mail Code 130-33, Pasadena, CA 91125 USA. EM sfurlane@tapir.caltech.edu NR 68 TC 75 Z9 75 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 MAR 20 PY 2005 VL 622 IS 1 BP 7 EP 27 DI 10.1086/426808 PN 1 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 907TM UT WOS:000227740900002 ER PT J AU Gugliucci, NE Taylor, GB Peck, AB Giroletti, M AF Gugliucci, NE Taylor, GB Peck, AB Giroletti, M TI Dating coins: Kinematic ages for compact symmetric objects SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : ISM; galaxies : jets; galaxies : nuclei; radio continuum : galaxies ID SPECTRUM RADIO-SOURCES; ACTIVE GALACTIC NUCLEI; HUBBLE-SPACE-TELESCOPE; HOST GALAXY; OPTICAL IDENTIFICATIONS; VLBI OBSERVATIONS; 1ST DETECTION; PKS 1413+135; SAMPLE; PKS-1413+135 AB We present multiepoch VLBA observations of compact symmetric objects (CSOs) from the COINS sample (CSOs Observed In the Northern Sky). These observations allow us to make estimates of, or place limits on, the kinematic ages for those sources with well-identified hot spots. This study significantly increases the number of CSOs with well-determined ages or limits. The age distribution is found to be sharply peaked under 500 yr, suggesting that many CSOs die young, or are episodic in nature, and very few survive to evolve into FR II sources such as Cygnus A. Jet components are found to have higher velocities than hot spots, which is consistent with their movement down cleared channels. We also report on the first detections of significant polarization in two CSOs, J0000+4054 (2.1%) and J1826+1831 (8.8%). In both cases the polarized emission is found in jet components on the stronger side of the center of activity. C1 Lycoming Coll, Dept Astron & Phys, Williamsport, PA 17701 USA. Natl Radio Astron Observ, Socorro, NM 87801 USA. Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA. Harvard Smithsonian Ctr Astrophys, SAO SMA Project, Hilo, HI 96720 USA. CNR, Ist Radioastron, I-40129 Bologna, Italy. RP Lycoming Coll, Dept Astron & Phys, Williamsport, PA 17701 USA. EM gugnico@lycoming.edu; gtaylor@nrao.edu; apeck@cfa.harvard.edu; giroletti@ira.cnr.it NR 53 TC 70 Z9 71 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 20 PY 2005 VL 622 IS 1 BP 136 EP 148 DI 10.1086/427934 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 907TM UT WOS:000227740900012 ER PT J AU Kraft, RP Hardcastle, MJ Worrall, DM Murray, SS AF Kraft, RP Hardcastle, MJ Worrall, DM Murray, SS TI A Chandra study of the multicomponent X-ray emission from the X-shaped radio galaxy 3C 403 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : individual (3C 403); galaxies : ISM; X-rays : galaxies ID XMM-NEWTON OBSERVATIONS; HIGH-RESOLUTION MAPS; CENTAURUS-A; HOT-SPOTS; 3.6 CM; JET; LOBES; GAS; Z-LESS-THAN-0.3; LUMINOSITIES AB We present results from a 49.4 ks Chandra ACIS-S observation of the nearby (z = 0.059) X-shaped FR type II (FR II) radio galaxy 3C 403. This is the first Chandra observation of an X-shaped radio galaxy, and one of the goals of this pioneering study is to determine the relationship between the X-ray-emitting gas and the X-shaped radio morphology. We find that the X-ray isophotes of the hot gas within similar to 3.'' 5 of the central galaxy are highly elliptical (eccentricity similar to 0.57) and coaligned with the elliptical optical isophotes. This supports the hypothesis that X-shaped radio sources are created by propagation of jets through asymmetric density distributions. Within large uncertainties, there is no evidence that the lobes or wings are overpressurized relative to the interstellar medium (ISM), supporting the scenario in which the wings are the result of strong backflows of material from the jet head and subsequent buoyant evolution. We have detected X-ray emission from several of the radio knots to the east of the active nucleus and diffuse emission from the radio lobe to the west. The X-ray emission from the eastern knots cannot be explained by an inverse Compton model unless they are far from equipartition. Using archival Hubble Space Telescope (HST) data, optical emission is detected from two knots, and the radio/optical/X-ray spectra are well fitted by simple synchrotron models. This is one of the strongest examples to date of X-ray synchrotron emission from multiple knots in the jet of an FR II radio galaxy. X-ray emission is also detected from the radio wings at a flux consistent with inverse Compton scattering of cosmic microwave background (CMB) photons from relativistic electrons if the wings are near equipartition. The nuclear spectrum is well described by a multicomponent model that includes a heavily absorbed power law (N-H similar to 4 x 10(23) cm(-2)) and a bright (EW similar to 244 eV), broadened Fe line. A second, less absorbed, power-law component, likely representing unresolved emission from a parsec-scale jet, is also required. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Hertfordshire, Sch Phys Astron & Math, Hatfield AL10 9AB, Herts, England. Univ Bristol, Dept Phys, Bristol BS8 1TL, Avon, England. RP Kraft, RP (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-67, Cambridge, MA 02138 USA. RI Hardcastle, Martin/E-2264-2012 OI Hardcastle, Martin/0000-0003-4223-1117 NR 54 TC 64 Z9 64 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 MAR 20 PY 2005 VL 622 IS 1 BP 149 EP 159 DI 10.1086/427822 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 907TM UT WOS:000227740900013 ER PT J AU Mahdavi, A Finoguenov, A Bohringer, H Geller, MJ Henry, JP AF Mahdavi, A Finoguenov, A Bohringer, H Geller, MJ Henry, JP TI Xmm-Newton and Gemini observations of eight RASSCALS galaxy groups SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : clusters : general; galaxies : distances and redshifts; plasmas; X-rays : galaxies : clusters ID X-RAY-PROPERTIES; CLUSTER SCALING PROJECT; CHANDRA OBSERVATIONS; INTRACLUSTER MEDIUM; REDSHIFT SURVEY; COMPACT-GROUPS; TEMPERATURE RELATION; DENSITY PROFILE; ABELL CLUSTERS; RICH CLUSTERS AB We study the distribution of gas pressure and entropy in eight groups of galaxies belonging to the ROSAT All-Sky Survey/Center for Astrophysics Loose Systems (RASSCALS). We use archival and proprietary XMM-Newton observations, supplementing the X-ray data with redshifts derived from the literature; we also list 127 new redshifts measured with the Gemini North telescope. The groups are morphologically heterogeneous in both the optical and the X-ray, and several suffer from superpositions with background galaxies or clusters of galaxies. Nevertheless, they show remarkable self-similarity in their azimuthally averaged entropy and temperature profiles. The entropy increases with radius; the behavior of the entropy profiles is consistent with an increasing broken power law with inner and outer slope 0.92(-0.05)(+0.04) and 0.42(-0.04)(+0.05) (68% confidence), respectively. There is no evidence of a central, isentropic core, and the entropy distribution in most of the groups is flatter at large radii than in the inner region, challenging earlier reports, as well as theoretical models predicting large isentropic cores or asymptotic slopes of 1.1 as r --> infinity. The pressure profiles are consistent with a self-similar decreasing broken power law in radius; the inner and outer slopes are -0.78(-0.03)(+0.04) and 1.7(-0.3)(+0.1), respectively. The results suggest that the larger scatter in the entropy distribution reflects the varied gasdynamical histories of the groups; the regularity and self-similarity of the pressure profiles is a sign of a similarity in the underlying dark matter distributions. C1 Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Mahdavi, A (reprint author), Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA. EM amahdavi@ifa.hawaii.edu NR 77 TC 50 Z9 51 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 MAR 20 PY 2005 VL 622 IS 1 BP 187 EP 204 DI 10.1086/427916 PN 1 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 907TM UT WOS:000227740900017 ER PT J AU Heinke, CO Grindlay, JE Edmonds, PD AF Heinke, CO Grindlay, JE Edmonds, PD TI Three additional quiescent low-mass X-ray binary candidates in 47 Tucanae SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; binaries : close; binaries : eclipsing globular; clusters : individual (NGC 104); stars : neutron; X-rays : binaries ID GLOBULAR-CLUSTER NGC-6397; SPACE-TELESCOPE COUNTERPARTS; ACCRETING NEUTRON-STARS; 47 TUCANAE; MILLISECOND PULSARS; CENTAURUS X-4; THERMAL EMISSION; EXTENSIVE CENSUS; PSR J1740-5340; TIME-SERIES AB We identify through their X-ray spectra one certain (W37) and two probable (W17 and X4) quiescent low-mass X-ray binaries (qLMXBs) containing neutron stars in a long Chandra X-ray exposure of the globular cluster 47 Tucanae, in addition to the two previously known qLMXBs. W37's spectrum is dominated by a blackbody-like component consistent with radiation from the hydrogen atmosphere of a 10 km neutron star. W37's light curve shows strong X-ray variability, which we attribute to variations in its absorbing column depth, and eclipses with a probable 3.087 hr period. For most of our exposures, W37's blackbody-like emission ( assumed to be from the neutron star surface) is almost completely obscured, yet some soft X-rays ( of uncertain origin) remain. Two additional candidates, W17 and X4, present X-ray spectra dominated by a harder component, fitted by a power law of photon index similar to 1.6-3. An additional soft component is required for bothW17 and X4, which can be fitted with a 10 km hydrogen atmosphere neutron star model. X4 shows significant variability, which may arise from either its power-law or hydrogen atmosphere spectral component. Both W17 and X4 show rather low X-ray luminosities, L-X(0.5-10 keV) similar to 5 x 10(31) ergs s(-1). All three candidate qLMXBs would be difficult to identify in other globular clusters, suggesting an additional reservoir of fainter qLMXBs in globular clusters that may be of similar numbers as the group of previously identified objects. The number of millisecond pulsars inferred to exist in 47 Tuc is less than 10 times larger than the number of qLMXBs in 47 Tuc, indicating that for typical inferred lifetimes of 10 and 1 Gyr, respectively, their birthrates are comparable. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM cheinke@cfa.harvard.edu; josh@cfa.harvard.edu; pedmonds@cfa.harvard.edu OI Heinke, Craig/0000-0003-3944-6109 NR 62 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 EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 20 PY 2005 VL 622 IS 1 BP 556 EP 564 DI 10.1086/427795 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 907TM UT WOS:000227740900046 ER PT J AU Dupree, AK Lobel, A Young, PR Ake, TB Linsky, JL Redfield, S AF Dupree, AK Lobel, A Young, PR Ake, TB Linsky, JL Redfield, S TI A far-ultraviolet spectroscopic survey of luminous cool stars SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars : chromospheres; stars : winds, outflows; ultraviolet : stars ID LOCAL INTERSTELLAR-MEDIUM; HYBRID-CHROMOSPHERE STARS; CORONAL FORBIDDEN LINES; LOW-GRAVITY STARS; LATE-TYPE GIANTS; TRANSITION REGION; EMISSION-LINES; X-RAY; EXPLORER-SURVEY; LYMAN-ALPHA AB The Far Ultraviolet Spectroscopic Explorer ( FUSE) ultraviolet spectra of eight giant and supergiant stars reveal that high-temperature (3 x 10(5) K) atmospheres are common in luminous cool stars and extend across the color-magnitude diagram from alpha Car (F0 II) to the cool giant alpha Tau (K5 III). Emission present in these spectra includes chromospheric H Ly beta, Fe II, C I, and transition region lines of C III, O VI, Si III, and Si IV. Emission lines of Fe XVIII and Fe XIX signaling temperatures of similar to 107 K and coronal material are found in the most active stars, beta Cet and 31 Com. A short-term flux variation, perhaps a flare, was detected in beta Cet during our observation. Stellar surface fluxes of the emission of C III and O vi are correlated and decrease rapidly toward the cooler stars, reminiscent of the decay of magnetically heated atmospheres. Profiles of the C III lambda 977 lines suggest that mass outflow is underway at T similar to 80,000 K and the winds are warm. Indications of outflow at higher temperatures (3 x 10(5) K) are revealed by O VI asymmetries and the line widths themselves. High-temperature species are absent in the M supergiant alpha Ori. Narrow fluorescent lines of Fe II appear in the spectra of many giants and supergiants, apparently pumped by H Ly alpha, and formed in extended atmospheres. Instrumental characteristics that affect cool star spectra are discussed. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Johns Hopkins Univ, CSC, Baltimore, MD 21218 USA. Univ Colorado, JILA, Boulder, CO 80309 USA. NIST, Boulder, CO 80309 USA. RP Dupree, AK (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM adupree@cfa.harvard.edu; alobel@cfa.harvard.edu; p.r.young@rl.ac.uk; ake@pha.jhu.edu; jlinsky@jila.colorado.edu; sredfiel@astro.as.utexas.edu OI Redfield, Seth/0000-0003-3786-3486 NR 87 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 MAR 20 PY 2005 VL 622 IS 1 BP 629 EP 652 DI 10.1086/428111 PN 1 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 907TM UT WOS:000227740900054 ER PT J AU Brown, WR Geller, MJ Kenyon, SJ Kurtz, MJ AF Brown, WR Geller, MJ Kenyon, SJ Kurtz, MJ TI Discovery of an unbound hypervelocity star in the Milky Way halo SO ASTROPHYSICAL JOURNAL LA English DT Article DE Galaxy : center; Galaxy : halo; Galaxy : kinematics and dynamics; Galaxy : stellar content; stars : early-type ID HORIZONTAL-BRANCH STARS; PALOMAR-GREEN SURVEY; DIGITAL SKY SURVEY; A-TYPE STARS; B-TYPE STARS; GALACTIC HALO; BLACK-HOLE; GALAXY; SAMPLE; VELOCITY AB We have discovered a star, SDSS J090745.0 + 024507, leaving the Galaxy with a heliocentric radial velocity of 853 +/- 12 km s(-1), the largest velocity ever observed in the Milky Way halo. The star is either a hot blue horizontal-branch star or a B9 main-sequence star with a heliocentric distance of 39 or 71 kpc, respectively. Corrected for the solar reflex motion and to the local standard of rest, the Galactic rest-frame velocity is 709 km s(-1). We suggest that this star is the first example of a hypervelocity star ejected from the Galactic center, as predicted by Hills and later discussed by Yu W Tremaine. The star's radial velocity vector points 174 degrees from the Galactic center. The star has [Fe/H] similar to 0, consistent with a Galactic center origin, and a travel time of less than or similar to 80 Myr from the Galactic center, consistent with its stellar lifetime. If the star is indeed traveling from the Galactic center, it should have a proper motion of similar to 0.3 mas yr(-1) observable with the Space Interferometry Mission or the Global Astrometric Interferometer for Astrophysics. Identifying additional hypervelocity stars throughout the halo will constrain the production rate history of hypervelocity stars at the Galactic center. C1 Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Brown, WR (reprint author), Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM wbrown@cfa.harvard.edu; mgeller@cfa.harvard.edu; skenyon@cfa.harvard.edu; mkurtz@cfa.harvard.edu RI KURTZ, Michael /B-3890-2009; OI Kenyon, Scott/0000-0003-0214-609X; Kurtz, Michael/0000-0002-6949-0090 NR 37 TC 166 Z9 167 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 MAR 20 PY 2005 VL 622 IS 1 BP L33 EP L36 DI 10.1086/429378 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 907TR UT WOS:000227741400009 ER PT J AU Crocker, RM Melia, F Volkas, RR AF Crocker, RM Melia, F Volkas, RR TI Neutrinos from the Galactic center in the light of its gamma-ray detection at tev energy SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic rays; elementary particles; Galaxy : center; neutrinos radiation; mechanisms : nonthermal; supernova remnants ID SUPERNOVA-REMNANTS; SAGITTARIUS-A; DIRECTION; ANTINEUTRINOS; SPECTRUM; EAST AB We reevaluate the event rate expected in km(3)-scale detectors for neutrinos from the direction of the Galactic center (GC) in light of recent spectral measurements obtained by the HESS instrument for similar to TeV gamma-radiation from this direction. In the most plausible scenario the reevaluated event rate is smaller than that previously calculated - and here recalculated - on the basis of EGRET data. However, the GC TeV gamma-ray detections by the Whipple, CANGAROO, and HESS instruments, together with the strong indications for an overabundance of cosmic rays coming from the GC at EeV energies, strengthen the expectation for a detectable, TeV-PeV GC neutrino signal from proton-proton interactions in that region. If the TeV gamma-ray - EeV cosmic-ray anisotropy connection is correct, this signal will be detectable within a year and half for km(3)-scale neutrino detectors in the Northern Hemisphere at super-TeV energies and, significantly, should also be detectable in 1.6 yr by the South Polar IceCube detector at energies greater than or similar to 10(14) eV. The GC neutrino signal should also produce a detectable signal from neutrino showering and resonant W- production by (nu) over bar (e) in the volume of a km(3)-scale detector. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Melbourne, Sch Phys, High Energy Phys Res Ctr, Parkville, Vic 3010, Australia. Univ Arizona, Dept Phys, Tucson, AZ 85721 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. RP Crocker, RM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM rcrocker@cfa.harvard.edu; melia@physics.arizona.edu; r.volkas@physics.unimelb.edu.au NR 29 TC 11 Z9 11 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 MAR 20 PY 2005 VL 622 IS 1 BP L37 EP L40 DI 10.1086/429539 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 907TR UT WOS:000227741400010 ER PT J AU Springel, V Hernquist, L AF Springel, V Hernquist, L TI Formation of a spiral galaxy in a major merger SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : interactions; galaxies : starburst; galaxies : structure; methods : numerical ID PARTICLE HYDRODYNAMICS SIMULATIONS; STAR-FORMATION; GALACTIC DISKS; INTERACTING GALAXIES; SINKING SATELLITES; MINOR MERGERS; MODEL; TRANSFORMATIONS; PROGENITORS; GASDYNAMICS AB We use numerical simulations to examine the structure of merger remnants resulting from collisions of gas-rich spiral galaxies. When the gas fraction of the progenitors is small, the remnants structurally and kinematically resemble elliptical galaxies, in agreement with earlier work. However, if the progenitor disks are gas-dominated, new types of outcomes are possible, where a prominent disk may survive in certain cases. To illustrate this scenario, we analyze an extreme example with progenitor galaxies consisting of dark matter halos, pure gas disks, and no bulges, as might be appropriate for mergers at high redshifts. While rapid star formation triggered by tidal torques during the merger forms a central, rotating bulge in the remnant, not all the gas is consumed in the burst. The remaining gas cools quickly and settles into an extended star-forming disk, yielding an object similar to a spiral galaxy and not an early-type galaxy. This is contrary to the usual view that major mergers invariably destroy disks. The morphological evolution of galaxies can therefore be more complicated than often assumed, and in particular, theoretical constraints based on the fragility of spiral disks need to be reevaluated. 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, D-85740 Garching, Germany. EM volker@mpa-garching.mpg.de; lars@cfa.harvard.edu OI Springel, Volker/0000-0001-5976-4599 NR 39 TC 215 Z9 218 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 MAR 20 PY 2005 VL 622 IS 1 BP L9 EP L12 DI 10.1086/429486 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 907TR UT WOS:000227741400003 ER PT J AU Pandolfi, JM Jackson, JBC Baron, N Bradbury, RH Guzman, HM Hughes, TP Kappel, CV Micheli, F Ogden, JC Possingham, HP Sala, E AF Pandolfi, JM Jackson, JBC Baron, N Bradbury, RH Guzman, HM Hughes, TP Kappel, CV Micheli, F Ogden, JC Possingham, HP Sala, E TI Ecology - Are US coral reefs on the slippery slope to slime? SO SCIENCE LA English DT Article ID RESILIENCE; ECOSYSTEMS C1 Univ Queensland, Ctr Marine Studies, St Lucia, Qld 4072, Australia. Univ Queensland, Dept Earth Sci, St Lucia, Qld 4072, Australia. Univ Queensland, Dept Math, St Lucia, Qld 4072, Australia. Univ Queensland, Sch Life Sci, St Lucia, Qld 4072, Australia. Univ Calif San Diego, Scripps Inst Oceanog, Ctr Ctr Marine Biodivers & Conservat, La Jolla, CA 92093 USA. Smithsonian Trop Res Inst, Balboa, Panama. Natl ctr Ecol Anal & Synth, Santa Barbara, CA USA. Australian Natl Univ, Ctr Resource & Environm Studies, Canberra, ACT 0200, Australia. James Cook Univ N Queensland, Sch Marine Biol, Ctr Coral Reef Biodivers, Townsville, Qld 4811, Australia. Stanford Univ, Hopkins Marine Stn, Pacific Grove, CA 93950 USA. Florida Inst Oceanog, St Petersburg, FL 33701 USA. RP Pandolfi, JM (reprint author), Univ Queensland, Ctr Marine Studies, St Lucia, Qld 4072, Australia. EM j.pandolfi@uq.edu.au RI Kappel, Carrie/B-9534-2009; Possingham, Hugh/B-1337-2008; Pandolfi, John/A-3121-2009; Hughes, Terry/L-4721-2013 OI Possingham, Hugh/0000-0001-7755-996X; Pandolfi, John/0000-0003-3047-6694; Hughes, Terry/0000-0002-5257-5063 NR 22 TC 272 Z9 290 U1 5 U2 87 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD MAR 18 PY 2005 VL 307 IS 5716 BP 1725 EP 1726 DI 10.1126/science.1104258 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 909TP UT WOS:000227883900028 PM 15774744 ER PT J AU Holland, ND Clague, DA Gordon, DP Gebruk, A Pawson, DL Vecchione, M AF Holland, ND Clague, DA Gordon, DP Gebruk, A Pawson, DL Vecchione, M TI Lophenteropneust' hypothesis refuted by collection and photos of new deep-sea hemichordates SO NATURE LA English DT Article ID PACIFIC AB The deep ocean is home to a group of broad-collared hemichordates - the so-called 'lophenteropneusts' - that have been photographed gliding on the sea floor(1-8) but have not previously been collected. It has been claimed that these worms have collar tentacles and blend morphological features of the two main hemichordate body plans, namely the tentacle-less enteropneusts and the tentacle-bearing pterobranchs. Consequently, lophenteropneusts have been invoked as missing links to suggest that the former evolved into the latter(5). The most significant aspect of the lophenteropneust hypothesis is its prediction that the fundamental body plan within a basal phylum of deuterostomes was enteropneust-like. The assumption of such an ancestral state influences ideas about the evolution of the vertebrates from the invertebrates(9-14). Here we report on the first collected specimen of a broad-collared, deep-sea enteropneust and describe it as a new family, genus and species. The collar, although disproportionately broad, lacks tentacles. In addition, we find no evidence of tentacles in the available deep-sea photographs ( published and unpublished) of broad-collared enteropneusts, including those formerly designated as lophenteropneusts. Thus, the lophenteropneust hypothesis was based on misinterpretation of deep-sea photographs of low quality and should no longer be used to support the idea that the enteropneust body plan is basal within the phylum Hemichordata. C1 Univ Calif San Diego, Scripps Inst Oceanog, Div Marine Biol Res, La Jolla, CA 92093 USA. Monterey Bay Aquarium Res Inst, Moss Landing, CA 95039 USA. Natl Inst Water & Atmospher Res, Wellington, New Zealand. Russian Acad Sci, PP Shirshov Oceanol Inst, Moscow 117851, Russia. Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. Natl Museum Nat Hist, NOAA, Natl Systemat Lab, Washington, DC 20013 USA. RP Holland, ND (reprint author), Univ Calif San Diego, Scripps Inst Oceanog, Div Marine Biol Res, La Jolla, CA 92093 USA. EM nholland@ucsd.edu NR 25 TC 31 Z9 31 U1 1 U2 11 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 MAR 17 PY 2005 VL 434 IS 7031 BP 374 EP 376 DI 10.1038/nature03382 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 907KG UT WOS:000227715100049 PM 15772659 ER PT J AU Hutchinson, A AF Hutchinson, A TI Encyclopedia of animal behavior. 3 volumns. SO LIBRARY JOURNAL LA English DT Book Review C1 Smithsonian Inst Libs, Washington, DC 20560 USA. RP Hutchinson, A (reprint author), Smithsonian Inst Libs, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 2 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 MAR 15 PY 2005 VL 130 IS 5 BP 110 EP 110 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 905OL UT WOS:000227578300193 ER PT J AU Ricaud, P Lefevre, F Berthet, G Murtagh, D Llewellyn, EJ Megie, G Kyrola, E Leppelmeier, GW Auvinen, H Boonne, C Brohede, S Degenstein, DA de La Noe, J Dupuy, E El Amraoui, L Eriksson, P Evans, WFJ Frisk, U Gattinger, RL Girod, F Haley, CS Hassinen, S Hauchecorne, A Jimenez, C Kyro, E Lautie, N Le Flochmoen, E Lloyd, ND McCconnell, JC McDade, IC Nordh, L Olberg, M Pazmino, A Petelina, SV Sandqvist, A Seppala, A Sioris, CE Solheim, BH Stegman, J Strong, K Taalas, P Urban, J von Savigny, C von Scheele, F Witt, G AF Ricaud, P Lefevre, F Berthet, G Murtagh, D Llewellyn, EJ Megie, G Kyrola, E Leppelmeier, GW Auvinen, H Boonne, C Brohede, S Degenstein, DA de La Noe, J Dupuy, E El Amraoui, L Eriksson, P Evans, WFJ Frisk, U Gattinger, RL Girod, F Haley, CS Hassinen, S Hauchecorne, A Jimenez, C Kyro, E Lautie, N Le Flochmoen, E Lloyd, ND McCconnell, JC McDade, IC Nordh, L Olberg, M Pazmino, A Petelina, SV Sandqvist, A Seppala, A Sioris, CE Solheim, BH Stegman, J Strong, K Taalas, P Urban, J von Savigny, C von Scheele, F Witt, G TI Polar vortex evolution during the 2002 Antarctic major warming as observed by the Odin satellite SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID 3-DIMENSIONAL MODEL SIMULATIONS; STRATOSPHERIC OZONE PROFILES; POAM-III OBSERVATIONS; SUBMILLIMETER RADIOMETER; OSIRIS INSTRUMENT; MCMURDO-STATION; RETRIEVAL; HNO3; CLO; WINTER AB In September 2002 the Antarctic polar vortex split in two under the influence of a sudden warming. During this event, the Odin satellite was able to measure both ozone (O-3) and chlorine monoxide (ClO), a key constituent responsible for the so-called "ozone hole'', together with nitrous oxide (N2O), a dynamical tracer, and nitric acid (HNO3) and nitrogen dioxide (NO2), tracers of denitrification. The submillimeter radiometer (SMR) microwave instrument and the Optical Spectrograph and Infrared Imager System (OSIRIS) UV-visible light spectrometer (VIS) and IR instrument on board Odin have sounded the polar vortex during three different periods: before (19-20 September), during (24-25 September), and after (1-2 and 4-5 October) the vortex split. Odin observations coupled with the Reactive Processes Ruling the Ozone Budget in the Stratosphere (REPROBUS) chemical transport model at and above 500 K isentropic surfaces (heights above 18 km) reveal that on 19-20 September the Antarctic vortex was dynamically stable and chemically nominal: denitrified, with a nearly complete chlorine activation, and a 70% O-3 loss at 500 K. On 25-26 September the unusual morphology of the vortex is monitored by the N2O observations. The measured ClO decay is consistent with other observations performed in 2002 and in the past. The vortex split episode is followed by a nearly complete deactivation of the ClO radicals on 1-2 October, leading to the end of the chemical O-3 loss, while HNO3 and NO2 fields start increasing. This acceleration of the chlorine deactivation results from the warming of the Antarctic vortex in 2002, putting an early end to the polar stratospheric cloud season. The model simulation suggests that the vortex elongation toward regions of strong solar irradiance also favored the rapid reformation of ClONO2. The observed dynamical and chemical evolution of the 2002 polar vortex is qualitatively well reproduced by REPROBUS. Quantitative differences are mainly attributable to the too weak amounts of HNO3 in the model, which do not produce enough NO2 in presence of sunlight to deactivate chlorine as fast as observed by Odin. C1 OASU, L3AB, F-33270 Floirac, France. Finnish Meteorol Inst, Dept Geophys, FIN-00101 Helsinki, Finland. Chalmers, Dept Radio & Space Sci, SE-41296 Gothenburg, Sweden. Univ Saskatchewan, Inst Space & Atmospher Studies, Saskatoon, SK S7N 5E2, Canada. Trent Univ, Dept Phys, Peterborough, ON K9J 7B8, Canada. Swedish Space Corp, SE-17104 Solna, Sweden. Ctr Natl Etud Spatiales, F-31401 Toulouse, France. York Univ, Ctr Res Earth & Space Sci, Toronto, ON M3J 1P3, Canada. SCFAB, Stockholm Observ, SE-10691 Stockholm, Sweden. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Stockholm, Dept Meteorol, SE-10691 Stockholm, Sweden. Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada. Univ Bremen, Inst Environm Phys, D-28359 Bremen, Germany. RP Observ Midi Pyrenees, Lab Aerol, F-31400 Toulouse, France. EM philippe.ricaud@aero.obsmip.fr RI Eriksson, Patrick/A-5321-2009; The Odin satellite, aeronomy mission/F-1671-2011; Strong, Kimberly/D-2563-2012; Hauchecorne, Alain/A-8489-2013; Urban, Jo/F-9172-2010; von Savigny, Christian/B-3910-2014; Seppala, Annika/C-8031-2014; Kyrola, Erkki/E-1835-2014; Murtagh, Donal/F-8694-2011; OI Eriksson, Patrick/0000-0002-8475-0479; Urban, Jo/0000-0001-7026-793X; Seppala, Annika/0000-0002-5028-8220; Murtagh, Donal/0000-0003-1539-3559; Sioris, Christopher/0000-0003-1168-8755; Hauchecorne, Alain/0000-0001-9888-6994 NR 39 TC 26 Z9 27 U1 1 U2 6 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD MAR 11 PY 2005 VL 110 IS D5 AR D05302 DI 10.1029/2004JD005018 PG 12 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 906LD UT WOS:000227641500003 ER PT J AU Emry, RJ Korth, WW Bell, MA AF Emry, RJ Korth, WW Bell, MA TI A tree squirrel (Rodentia, Sciuridae, Sciurini) from the late Miocene (Clarendonian) of Nevada SO JOURNAL OF VERTEBRATE PALEONTOLOGY LA English DT Article ID FAUNA AB A new species of squirrel, Sciurus olsoni, from the late Miocene (Clarendonian) of Nevada, is distinguished from other species of Sciurus by its smaller size and minor differences in the cheek teeth. It is the first Miocene record of the extant genus Sciurus, and the first record of a tree squirrel (tribe Sciurim) in North America between the early Miocene (Arikareean) and the Pleistocene. This late Miocene occurrence in North America suggests that the history of tree squirrels in North America was probably continuous through the Neogene, and the intermittent fossil record is due both to preservation bias and to their never having been abundant as living elements of fossil faunas; they are rare even where they do occur in deposits that are otherwise very richly fossiliferous. The later Tertiary and Pleistocene radiation of tree squirrels may have originated in North America. C1 SUNY Stony Brook, Dept Ecol & Evolut, New York, NY 11794 USA. Rochester Inst Vertebrate Paleontol, Rochester, NY 14610 USA. Smithsonian Inst, Natl Museum Amer Hist, Dept Paleobiol, Washington, DC 20560 USA. RP Emry, RJ (reprint author), Smithsonian Inst, Natl Museum Amer Hist, Dept Paleobiol, Washington, DC 20560 USA. EM emryr@nmnh.si.edu NR 26 TC 7 Z9 7 U1 1 U2 4 PU SOC VERTEBRATE PALEONTOLOGY PI NORTHBROOK PA 60 REVERE DR, STE 500, NORTHBROOK, IL 60062 USA SN 0272-4634 J9 J VERTEBR PALEONTOL JI J. Vertebr. Paleontol. PD MAR 11 PY 2005 VL 25 IS 1 BP 228 EP 235 DI 10.1671/0272-4634(2005)025[0228:ATSRSS]2.0.CO;2 PG 8 WC Paleontology SC Paleontology GA 905NI UT WOS:000227575000021 ER PT J AU Head, JJ Holroyd, PA Hutchison, JH Ciochon, RL AF Head, JJ Holroyd, PA Hutchison, JH Ciochon, RL TI First report of snakes (Serpentes) from the late middle Eocene Pondaung Formation, Myanmar SO JOURNAL OF VERTEBRATE PALEONTOLOGY LA English DT Article ID WESTERN INDIA; MUSEUM C1 Smithsonian Inst, Dept Paleobiol, Natl Museum Nat Hist, Washington, DC 20012 USA. Queen Mary Univ London, Sch Biol Sci, London E1 4NS, England. Univ Calif Berkeley, Museum Paleontol, Berkeley, CA 94720 USA. Univ Iowa, Dept Anthropol, Iowa City, IA 52242 USA. RP Head, JJ (reprint author), Smithsonian Inst, Dept Paleobiol, Natl Museum Nat Hist, POB 37012, Washington, DC 20012 USA. EM head.jason@nmnh.si.edu NR 49 TC 27 Z9 27 U1 1 U2 2 PU SOC VERTEBRATE PALEONTOLOGY PI NORTHBROOK PA 60 REVERE DR, STE 500, NORTHBROOK, IL 60062 USA SN 0272-4634 J9 J VERTEBR PALEONTOL JI J. Vertebr. Paleontol. PD MAR 11 PY 2005 VL 25 IS 1 BP 246 EP 250 DI 10.1671/0272-4634(2005)025[0246:FROSSF]2.0.CO;2 PG 5 WC Paleontology SC Paleontology GA 905NI UT WOS:000227575000024 ER PT J AU O'Sullivan, E Vrtilek, JM Kempner, JC David, LP Houck, JC AF O'Sullivan, E Vrtilek, JM Kempner, JC David, LP Houck, JC TI AWM 4 - an isothermal cluster observed with XMM-Newton SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies : clusters : individual : AWM 4; galaxies : individual : NGC 6051; X-rays : galaxies; X-rays : galaxies : clusters ID GALAXY GROUP NGC-5044; X-RAY SPECTROSCOPY; INTRACLUSTER MEDIUM; POOR CLUSTERS; HOT GAS; CHANDRA OBSERVATIONS; METAL ABUNDANCES; SCALING PROJECT; PERSEUS CLUSTER; COOLING FLOWS AB We present an analysis of an XMM-Newton observation of the poor cluster AWM4. The cluster is relaxed and its X-ray halo is regular with no apparent substructure. Azimuthally averaged radial spectral profiles suggest that the cluster is isothermal to a radius of at least 160 kpc, with no evidence of a central cooling region. Spectral mapping shows some significant temperature and abundance substructure, but no evidence of strong cooling in the cluster core. Abundance increases in the core, but not to the extent expected, and we find some indication of gas mixing. Modelling the three-dimensional properties of the system, we show that ongoing heating by an active galactic nuclei (AGN) in the dominant elliptical, NGC 6051, is likely to be responsible for the lack of cooling. We also compare AWM4 to MKW4, a cluster of similar mass observed recently with XMM- Newton. While the two systems have similar gravitational mass profiles, MKW 4 has a cool core and a somewhat steeper gas density profile, which leads to a lower core entropy. AWM 4 has a considerably larger gas fraction at 0.1R(200), and we show that these differences result from the difference in mass between the two dominant galaxies and the activity cycles of their AGN. We estimate the energy required to raise the temperature profile of MKW 4 to match that of AWM 4 to be 9 x 10(58) erg or 3 x 10(43) erg s(-1) for 100 Myr, comparable to the likely power output of the AGN in AWM 4. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Bowdoin Coll, Dept Phys & Astron, Brunswick, ME 04011 USA. MIT, Ctr Space Res, Cambridge, MA 02139 USA. RP O'Sullivan, E (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM ejos@head.cfa.harvard.edu OI O'Sullivan, Ewan/0000-0002-5671-6900; Houck, John/0000-0002-6761-6796 NR 67 TC 47 Z9 47 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 MAR 11 PY 2005 VL 357 IS 4 BP 1134 EP 1150 DI 10.1111/j.1365.2005.08749.x PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 902JA UT WOS:000227349800003 ER PT J AU Barros, SCC Marsh, TR Groot, P Nelemans, G Ramsay, G Roelofs, G Steeghs, D Wilms, J AF Barros, SCC Marsh, TR Groot, P Nelemans, G Ramsay, G Roelofs, G Steeghs, D Wilms, J TI Geometrical constraints upon the unipolar model of V407 Vul and RXJ0806.3+1527 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE binaries : close; stars : individual : RX J0806.3+1527; stars : individual : V407 Vul; stars : magnetic fields; white dwarfs; X-rays : stars ID SHORTEST PERIOD BINARY; SPIN-UP; RX J0806.3+1527; CHANDRA; ROSAT; RX-J0806.3+1527; RX-J0806+15 AB V407 Vul and RX J0806.3 + 1527 are X-ray emitting stars with X-ray light curves that are 100 per cent modulated on periods of 569 and 321 s, respectively. These periods and no others are also seen at optical and infrared wavelengths. These properties have led to the suggestion that the periods are the orbital periods of ultracompact pairs of white dwarfs. There are two main double white dwarf models: the unipolar inductor model analogous to the Jupiter-Io system and the direct impact model analogous to Algol. In this paper, we consider geometrical constraints on the unipolar inductor model, in particular what parameter values (component masses, orbital inclination and magnetic colatitude) can describe the X-ray and optical light curves. We find that for a dipole field on the primary star, the unipolar inductor model fails to match the data on V407 Vul for any combination of parameters and can only match RX J0806.3 + 1527 if the sparser set of observations of this star have been unluckily timed. C1 Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. Univ Nijmegen, NL-6500 GL Nijmegen, Netherlands. Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. UCL, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Barros, SCC (reprint author), Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. EM s.c.barros@warwick.ac.uk RI Nelemans, Gijs/D-3177-2012; Wilms, Joern/C-8116-2013; Steeghs, Danny/C-5468-2009; Groot, Paul/K-4391-2016; OI Nelemans, Gijs/0000-0002-0752-2974; Wilms, Joern/0000-0003-2065-5410; Steeghs, Danny/0000-0003-0771-4746; Groot, Paul/0000-0002-4488-726X; Barros, Susana/0000-0003-2434-3625 NR 20 TC 13 Z9 13 U1 0 U2 0 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAR 11 PY 2005 VL 357 IS 4 BP 1306 EP 1312 DI 10.1111/j.1365-2966.2005.08740.x PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 902JA UT WOS:000227349800019 ER PT J AU LaPolla, JS AF LaPolla, JS TI Academy of Natural Sciences: Job cuts SO SCIENCE LA English DT Letter C1 Smithsonian Inst, Dept Entomol, Washington, DC 20013 USA. RP LaPolla, JS (reprint author), Smithsonian Inst, Dept Entomol, POB 37012,NHB,CE518,MRC 188, Washington, DC 20013 USA. NR 1 TC 0 Z9 0 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 MAR 11 PY 2005 VL 307 IS 5715 BP 1560 EP 1560 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 906ED UT WOS:000227622400016 PM 15765557 ER PT J AU Gaensler, BM Haverkorn, M Staveley-Smith, L Dickey, JM McClure-Griffiths, NM Dickel, JR Wolleben, M AF Gaensler, BM Haverkorn, M Staveley-Smith, L Dickey, JM McClure-Griffiths, NM Dickel, JR Wolleben, M TI The magnetic field of the Large Magellanic Cloud revealed through Faraday rotation SO SCIENCE LA English DT Article ID GALACTIC DYNAMOS; GALAXIES; DEPOLARIZATION; EVOLUTION; DRIVEN; ORIGIN; SCALE AB We have measured the Faraday rotation toward a large sample of polarized radio sources behind the Large Magellanic Cloud (LMC) to determine the structure of this galaxy's magnetic field. The magnetic field of the LMC consists of a coherent axisymmetric spiral of field strength similar to1 microgauss. Strong fluctuations in the magnetic field are also seen on small (<0.5 parsec) and large (similar to 100 parsecs) scales. The large bursts of recent star formation and supernova activity in the LMC argue against standard dynamo theory, adding to the growing evidence for rapid field amplification in galaxies. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Sydney, Sch Phys, Sydney, NSW 2006, Australia. CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. Univ Tasmania, Dept Phys, Hobart, Tas 7001, Australia. Univ Illinois, Dept Astron, Urbana, IL 61801 USA. Max Planck Inst Radioastron, D-53121 Bonn, Germany. RP Gaensler, BM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,Mail Stop 6, Cambridge, MA 02138 USA. EM bgaensler@cfa.harvard.edu RI Gaensler, Bryan/F-8655-2010; Staveley-Smith, Lister/A-1683-2011; Dickey, John/C-6156-2013; OI Staveley-Smith, Lister/0000-0002-8057-0294; McClure-Griffiths, Naomi/0000-0003-2730-957X; Dickey, John/0000-0002-6300-7459; Gaensler, Bryan/0000-0002-3382-9558 NR 29 TC 101 Z9 101 U1 0 U2 4 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD MAR 11 PY 2005 VL 307 IS 5715 BP 1610 EP 1612 DI 10.1126/science.1108832 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 906ED UT WOS:000227622400043 PM 15761149 ER PT J AU Machacek, M Dosaj, A Forman, W Jones, C Markevitch, M Vikhlinin, A Warmflash, A Kraft, R AF Machacek, M Dosaj, A Forman, W Jones, C Markevitch, M Vikhlinin, A Warmflash, A Kraft, R TI Infall of the elliptical galaxy NGC 1404 into the Fornax Cluster SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : clusters : general; galaxies : individual (NGC 1404); intergalactic medium; X-rays : galaxies ID VIRGO CLUSTER; CHANDRA OBSERVATION; RAY; GAS; ABUNDANCES; MORPHOLOGY; NGC-1399 AB We use three Chandra observations, totaling 134.3 ks, to constrain the dynamical motion of NGC 1404 falling toward the dominant elliptical NGC 1399 through the Fornax Cluster gas. The surface brightness profile of NGC 1404 shows a sharp edge at similar to 8 kpc from its center in the direction of NGC 1399, characteristic of jumplike temperature and density discontinuities from ram pressure stripping of the galaxy gas, caused by its motion through the surrounding intracluster medium (ICM). We find that the temperature of the galaxy gas inside the edge is similar to 2.8 times cooler (kT = 0.55(-0.02)(+0.01) keV with abundance A = 0.73(-0.16)(+0.65) Z(.)) than the cluster gas (kT = 1.53(-0.13)(+0.10) keV, A = 0.42(-0.13)(+0.2) Z(.)). We use the shape of the surface brightness profile across the edge to fit the position of the edge, the power-law behavior of NGC 1404' s density distribution in the leading direction, and the density discontinuity at the edge. The electron density inside the edge (3.9-4.3) x 10(-3) cm(-3) depends strongly on the gas abundance, while the density of the ICM (7-8) x 10(-4) cm(-3) depends strongly on the assumed geometry ( relative distance) between NGC 1404 and NGC 1399. The corresponding pressure jump of 1.7 - 2.1 across the leading edge of the galaxy and the cluster free-stream region implies near sonic motion ( Mach number 0.83 - 1.03) for NGC 1404 with a velocity 531 - 657 km s(-1) relative to the surrounding cluster gas. The inclination angle of the motion, inferred using the relative radial velocity between NGC 1404 and 1399 as representative of that between NGC 1404 and the cluster ICM, is uncomfortably large (greater than or similar to 40 degrees) given the sharpness of the surface brightness edge, suggesting either a non-zero impact parameter between NGC 1404 and 1399 or that NGC 1399 is also moving radially with respect to the cluster ICM. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mmachacek@cfa.harvard.edu NR 36 TC 55 Z9 55 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 10 PY 2005 VL 621 IS 2 BP 663 EP 672 DI 10.1086/427548 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 905CM UT WOS:000227545300010 ER PT J AU Sun, M Vikhlinin, A AF Sun, M Vikhlinin, A TI Revealing the interaction between the X-ray gas of starburst galaxy UGC 6697 and the hot intracluster medium of A1367 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : clusters : general; galaxies : clusters : individual (A1367); galaxies : individual (UGC 6697); X-rays : galaxies ID STAR-FORMATION RATE; SPIRAL GALAXIES; CHANDRA OBSERVATIONS; ABELL 1367; H-ALPHA; CLUSTERS; EVOLUTION; PRESSURE; A-1367; ANTENNAE AB We present the result from a Chandra observation of an X-ray -luminous starburst galaxy, UGC 6697, which is embedded in the northwest hot region of A1367 ( 5 - 6 keV). A very sharp X-ray edge ( similar to 13-fold surface brightness jump) at the southeast and a long tail ( at least 60 kpc from the nucleus) at the northwest of the galaxy are detected, as expected if the galaxy is moving to the southeast. The X-ray edge, at the midway of the nucleus and the southeast optical disk edge, is also at the same position where the H alpha emission is truncated and a radio sharp edge is observed. The X-ray diffuse emission is also enhanced at the southeast, implying ram pressure compression. No extraplanar X-ray component is detected, probably because of the combining effects of weaker outflow activity than that in nuclear starbursts, and external confinement plus stripping. The diffuse thermal gas in UGC 6697 has a temperature of similar to 0.7 keV and a low iron abundance ( similar to 0.1 - 0.2 solar). An X-ray point source (L0.5-10 keV similar to 2.8 x 10(40) ergs s(-1)) is detected on the nucleus, but not highly absorbed. Three off-center ultraluminous X-ray sources, all with L0.5-10 keV > 10(40) ergs s(-1), are also detected. Based on the multiwavelength data available, we favor that the interaction between the interstellar medium and the intracluster medium plays a major role in triggering the starburst in UGC 6697. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM msun@cfa.harvard.edu NR 36 TC 40 Z9 40 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 10 PY 2005 VL 621 IS 2 BP 718 EP 724 DI 10.1086/427728 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 905CM UT WOS:000227545300013 ER PT J AU Hussain, GAJ Brickhouse, NS Dupree, AK Jardine, MM van Ballegooijen, AA Hoogerwerf, R Cameron, AC Donati, JF Favata, F AF Hussain, GAJ Brickhouse, NS Dupree, AK Jardine, MM van Ballegooijen, AA Hoogerwerf, R Cameron, AC Donati, JF Favata, F TI Inferring coronal structure from X-ray light curves and Doppler shifts: A Chandra study of AB Doradus SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars : activity; stars : coronae; stars : individual (AB Doradus); stars : late-type; ultraviolet : stars; X-rays : stars ID SPECTROSCOPIC-EXPLORER-SURVEY; EXTREME-ULTRAVIOLET; CHARACTERIZING NONLINEARITIES; STELLAR CORONAE; SOLAR CORONA; 44I BOOTIS; XMM-NEWTON; EMISSION; STARS; DOR AB The Chandra X-Ray Observatory continuously monitored the single cool star AB Dor for a period lasting 88 ks (1.98P(rot)) in 2002 December with the Low-Energy Transmission Grating HRC- S. The X-ray light curve shows rotational modulation with three peaks that repeat in two consecutive rotation cycles. These peaks may indicate the presence of compact emitting regions in the quiescent corona. Centroid shifts as a function of phase in the strongest line profile, O VIII lambda 18.97, indicate Doppler rotational velocities with a semiamplitude of 30 +/- 10 km s(-1). By taking these diagnostics into account along with constraints on the rotational broadening of line profiles ( provided by archival Chandra High-Energy Transmission Grating Fe XVII and Far Ultraviolet Spectroscopic Explorer Fe XVIII profiles), we can construct a simple model of the X-ray corona that requires two components. One of these components is responsible for 80% of the X-ray emission and arises from the pole and/or a homogeneously distributed corona. The second component consists of two or three compact active regions that cause modulation in the light curve and contribute to the O XIII centroid shifts. These compact regions account for 16% of the emission and are located near the stellar surface with heights of less than 0.3R(*). At least one of the compact active regions is located in the partially obscured hemisphere of the inclined star, while another of the active regions may be located at 40 degrees. High-quality X-ray data such as these can test the models of the coronal magnetic field configuration as inferred from magnetic Zeeman Doppler imaging. C1 ESA, ESTEC, Res & Sci Support Dept, Div Astrophys, Noordwijk, Netherlands. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. Observ Midi Pyrenees, Astrophys Lab, F-31400 Toulouse, France. RP ESA, ESTEC, Res & Sci Support Dept, Div Astrophys, Postbus 299, Noordwijk, Netherlands. OI Brickhouse, Nancy/0000-0002-8704-4473; Cameron, Andrew/0000-0002-8863-7828 NR 40 TC 23 Z9 23 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 10 PY 2005 VL 621 IS 2 BP 999 EP 1008 DI 10.1086/427647 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 905CM UT WOS:000227545300041 ER PT J AU Garcia-Alvarez, D Drake, JJ Lin, LW Kashyap, VL Ball, B AF Garcia-Alvarez, D Drake, JJ Lin, LW Kashyap, VL Ball, B TI The coronae of AB Doradus and V471 Tauri: Primordial angular momentum versus tidal spin-up SO ASTROPHYSICAL JOURNAL LA English DT Review DE stars : abundances; stars : activity; stars : coronae; stars : late-type; Sun : corona; X-rays : stars ID X-RAY SPECTROSCOPY; BINARY V471 TAURI; EMISSION MEASURE DISTRIBUTIONS; HYADES OPEN CLUSTER; K-DWARF COMPONENT; XMM-NEWTON VIEW; WHITE-DWARF; ECLIPSING BINARY; STELLAR CORONAE; RADIO-EMISSION AB The zero-age main-sequence star AB Dor and the K dwarf component of the V471 Tau close binary have essentially identical rotation rates and spectral types. An analysis of their high-resolution Chandra X-ray spectra reveals remarkably similar coronal characteristics in terms of both temperature structure and element abundances. Both stars show depletions of low first ionization potential (FIP) elements by factors of similar to 3, with higher FIP elements showing more mild depletions. No evidence for enhancements of very low FIP (< 7 eV) elements, such as Na, Al, and Ca, as compared to other low-FIP elements, was found. The abundance anomaly pattern for AB Dor and V471 Tau is similar to, although less extreme than, the abundance anomalies exhibited by active RS CVn - type binaries. While we find statistically significant structure in the underlying differential emission measure distributions of these stars over narrow temperature intervals, this structure is strongly dependent on the lines used in the analysis and is probably spurious. On the basis of their X-ray similarities, we conclude that the exact evolutionary state of a star has little effect on coronal characteristics and that the parameters that dominate coronal structure and composition are simply the rotation rate and spectral type. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 110 TC 24 Z9 24 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 10 PY 2005 VL 621 IS 2 BP 1009 EP 1022 PN 1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 905CM UT WOS:000227545300042 ER PT J AU Mandushev, G Torres, G Latham, DW Charbonneau, D Alonso, R White, RJ Stefanik, RP Dunham, EW Brown, TM O'Donovan, FT AF Mandushev, G Torres, G Latham, DW Charbonneau, D Alonso, R White, RJ Stefanik, RP Dunham, EW Brown, TM O'Donovan, FT TI The challenge of wide-field transit surveys: The case of GSC 01944-02289 SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : eclipsing; line : profiles; planetary systems; techniques : photometric; techniques : radial velocities ID GRAVITATIONAL LENSING EXPERIMENT; LUMINOSITY OBJECT TRANSITS; SPECTROSCOPIC FOLLOW-UP; RADIAL-VELOCITIES; GALACTIC DISK; 2001 CAMPAIGN; PLANET; STARS; CANDIDATES; SEARCH AB Wide-field searches for transiting extrasolar giant planets face the difficult challenge of separating true transit events from the numerous false positives caused by isolated or blended eclipsing binary systems. We describe here the investigation of GSC 01944-02289, a very promising candidate for a transiting brown dwarf detected by the Trans-Atlantic Exoplanet Survey (TrES) network. The photometry and radial velocity observations suggested that the candidate was an object of substellar mass in orbit around an F star. However, careful analysis of the spectral line shapes revealed a pattern of variations consistent with the presence of another star whose motion produced the asymmetries observed in the spectral lines of the brightest star. Detailed simulations of blend models composed of an eclipsing binary plus a third star diluting the eclipses were compared with the observed light curve and used to derive the properties of the three components. Using the predicted stellar parameters, we were able to identify a second set of spectral lines corresponding to the primary of the eclipsing binary and derive its spectroscopic orbit. Our photometric and spectroscopic observations are fully consistent with a blend model of a hierarchical triple system composed of an eclipsing binary with G0 V and M3 V components in orbit around a slightly evolved F5 dwarf. The rotational broadening of the spectral lines of the F5 primary (v sin i approximate to 34 km s(-1)) and its brightness relative to the eclipsing binary (similar to 89% of the total light) made the discovery of the true nature of the system particularly difficult. We believe that this investigation will be helpful to other groups pursuing wide-field transit searches as this type of false detection could be more common than true transiting planets and difficult to identify. C1 Lowell Observ, Flagstaff, AZ 86001 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CALTECH, Pasadena, CA 91125 USA. Inst Astrofis Canarias, Tenerife 38200, Canary Isl, Spain. Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA. RP Lowell Observ, 1400 W Mars Hill Rd, Flagstaff, AZ 86001 USA. EM gmand@lowell.edu; gtorres@cfa.harvard.edu; dlatham@cfa.harvard.edu; dcharbonneau@cfa.harvard.edu; ras@iac.es; rjw@astro.caltech.edu; rstefanik@cfa.harvard.edu; Ted.Dunham@lowell.edu; timbrown@hao.ucar.edu; ftod@astro.caltech.edu RI Alonso, Roi/D-8799-2014; O'Donovan, Francis/I-2423-2014 OI Alonso, Roi/0000-0001-8462-8126; O'Donovan, Francis/0000-0002-4858-6106 NR 40 TC 63 Z9 63 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 10 PY 2005 VL 621 IS 2 BP 1061 EP 1071 DI 10.1086/427727 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 905CM UT WOS:000227545300046 ER PT J AU Furlan, E Calvet, N D'Alessio, P Hartmann, L Forrest, WJ Watson, DM Luhman, KL Uchida, KI Green, JD Sargent, B Najita, J Sloan, GC Keller, LD Herter, TL AF Furlan, E Calvet, N D'Alessio, P Hartmann, L Forrest, WJ Watson, DM Luhman, KL Uchida, KI Green, JD Sargent, B Najita, J Sloan, GC Keller, LD Herter, TL TI Spitzer IRS spectra of young stars near the hydrogen-burning mass limit SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; infrared : stars; stars : individual (V410 Anon 13, V410 X-ray 3); stars : low-mass, brown dwarfs ID T-TAURI STARS; BROWN DWARFS; SPACE-TELESCOPE; INFRARED SPECTROGRAPH; ISOCAM OBSERVATIONS; FORMING REGION; SILICATE DUST; RHO-OPHIUCHI; DISKS; OBJECTS AB We present Spitzer Infrared Spectrograph measurements for two young stars near the hydrogen-burning mass limit in the Taurus star-forming region. While one of the objects, V410 X-ray 3, displays no mid-infrared excess, the other one, V410 Anon 13, shows a clear excess at wavelengths longward of 10 mu m, indicative of a circumstellar disk. Moreover, the disk surrounding V410 Anon 13 is reminiscent of flared accretion disks around classical T Tauri stars; small dust grains in the disk photosphere generate the broad 10 mu m silicate emission feature, whose structure suggests the presence of crystalline components. This demonstrates that very low mass objects, like their more massive counterparts, experience dust processing in their disks. C1 Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Nacl Autonoma Mexico, Ctr Radioastron & Astrofis, Morelia 58089, Michoacan, Mexico. Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. Natl Opt Astron Observ, Tucson, AZ 85719 USA. Ithaca Coll, Dept Phys, Ithaca, NY 14850 USA. RP Furlan, E (reprint author), Cornell Univ, Ctr Radiophys & Space Res, 208 Space Sci Bldg, Ithaca, NY 14853 USA. EM furlan@astro.cornell.edu; ncalvet@cfa.harvard.edu; p.dalessio@astrosmo.unam.mx; hartmann@cfa.harvard.edu; forrest@pas.rochester.edu; dmw@pas.rochester.edu; kluhman@cfa.harvard.edu; kuchida@astro.cornell.edu; joel@pas.rochester.edu; basargent@pas.rochester.edu; najita@noao.edu; sloan@astro.cornell.edu; lkeller@ithaca.edu; hlth10@cornell.edu OI Furlan, Elise/0000-0001-9800-6248 NR 40 TC 16 Z9 16 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 10 PY 2005 VL 621 IS 2 BP L129 EP L132 DI 10.1086/429273 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 905CQ UT WOS:000227545700011 ER PT J AU Rodriguez, LF Loinard, L D'Alessio, P Wilner, DJ Ho, PTP AF Rodriguez, LF Loinard, L D'Alessio, P Wilner, DJ Ho, PTP TI IRAS 16293-2422b: A compact, possibly isolated protoplanetary disk in a class 0 object SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : individual (IRAS 16293-2422); planetary systems : protoplanetary disks; stars : pre-main-sequence ID T-TAURI STARS; YOUNG BINARY-SYSTEM; CIRCUMSTELLAR DISK; ACCRETION DISKS; PROPER MOTIONS; IRAS-16293-2422; EVOLUTION; CONTINUUM; EMISSION; ENVELOPE AB Theoretical arguments suggest that protoplanetary disks around young stars should start small and grow with the addition of high angular momentum material to reach the radii of several hundred AU that characterize the disks around optically visible T Tauri stars. Examples of much more compact disks, with radii much less than 100 AU, have been found around some very young stars, but in all cases tidal truncation from a near binary companion provides a ready explanation for the small disk size. We report here an example of a compact, possibly isolated disk around the Class 0 object IRAS 16293 - 2422B, which is thought to be among the youngest protostars known. This disk has a Gaussian half-power radius of only similar to 8 AU, and a detailed, self-consistent accretion disk model indicates an outer radius of only 26 AU. This discovery supports the notion that protoplanetary disks start small and grow with time, although other explanations for the compact size cannot be ruled out, including gravitational instability in its outer parts and tidal truncation from the close approach of a now distant stellar companion. C1 Univ Nacl Autonoma Mexico, Ctr Radioastron & Astrofis, Morelia 58089, Michoacan, Mexico. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Rodriguez, LF (reprint author), Univ Nacl Autonoma Mexico, Ctr Radioastron & Astrofis, Apartado Postal 3-72, Morelia 58089, Michoacan, Mexico. EM l.rodriguez@astrosmo.unam.mx; l.loinard@astrosmo.unam.mx; p.dalessio@astrosmo.unam.mx; dwilner@cfa.harvard.edu; ho@cfa.harvard.edu NR 41 TC 48 Z9 48 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 10 PY 2005 VL 621 IS 2 BP L133 EP L136 DI 10.1086/429223 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 905CQ UT WOS:000227545700012 ER PT J AU Salawitch, RJ Weisenstein, DK Kovalenko, LJ Sioris, CE Wennberg, PO Chance, K Ko, MKW McLinden, CA AF Salawitch, RJ Weisenstein, DK Kovalenko, LJ Sioris, CE Wennberg, PO Chance, K Ko, MKW McLinden, CA TI Sensitivity of ozone to bromine in the lower stratosphere SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID BRO; TROPOSPHERE; BROMOFORM; BUDGET; GASES AB Measurements of BrO suggest that inorganic bromine (Br-y) at and above the tropopause is 4 to 8 ppt greater than assumed in models used in past ozone trend assessment studies. This additional bromine is likely carried to the stratosphere by short-lived biogenic compounds and their decomposition products, including tropospheric BrO. Including this additional bromine in an ozone trend simulation increases the computed ozone depletion over the past similar to 25 years, leading to better agreement between measured and modeled ozone trends. This additional Bry (assumed constant over time) causes more ozone depletion because associated BrO provides a reaction partner for ClO, which increases due to anthropogenic sources. Enhanced Bry causes photochemical loss of ozone below similar to 14 km to change from being controlled by HOx catalytic cycles (primarily HO2+ O-3) to a situation where loss by the BrO+HO2 cycle is also important. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91106 USA. NASA, Langley Res Ctr, Hampton, VA 23681 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. Meteorol Serv Canada, Toronto, ON M3H 5T4, Canada. Atmospher & Environm Res Inc, Lexington, MA 02421 USA. RP Salawitch, RJ (reprint author), CALTECH, Jet Prop Lab, MS 183-601, Pasadena, CA 91106 USA. EM ross.j.salawitch@jpl.nasa.gov RI Salawitch, Ross/B-4605-2009; McLinden, Chris/A-7710-2010; Wennberg, Paul/A-5460-2012; Ko, Malcolm/D-5898-2015; OI Salawitch, Ross/0000-0001-8597-5832; McLinden, Chris/0000-0001-5054-1380; Chance, Kelly/0000-0002-7339-7577; Sioris, Christopher/0000-0003-1168-8755 NR 18 TC 129 Z9 130 U1 3 U2 31 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD MAR 9 PY 2005 VL 32 IS 5 AR L05811 DI 10.1029/2004GL021504 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 906KX UT WOS:000227640800002 ER PT J AU Reinert, JF Harbach, RE AF Reinert, JF Harbach, RE TI Generic and subgeneric status of aedine mosquito species (Diptera : Culicidae : Aedini) occurring in the Australasian Region SO ZOOTAXA LA English DT Article DE Diptera; Culicidae; Aedini; Australasian region; checklist; mosquitoes AB Species of Aedini occurring in the Australasian Region are listed with their current generic-level assignments. The purpose of this list is to enable entomologists, public health personnel, and mosquito control workers to more quickly become familiar with recent formal taxonomic changes within the tribe. C1 USDA, ARS, CMAVE, Gainesville, FL 32608 USA. Smithsonian Inst, WRBU, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Reinert, JF (reprint author), USDA, ARS, CMAVE, 1600-1700 SW 23rd Ave, Gainesville, FL 32608 USA. EM jreinert@gainesville.usda.ufl.edu; R.Harbach@nhm.ac.uk NR 6 TC 7 Z9 7 U1 0 U2 0 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, 1030, NEW ZEALAND SN 1175-5334 J9 ZOOTAXA JI Zootaxa PD MAR 7 PY 2005 IS 887 BP 1 EP 10 PG 10 WC Zoology SC Zoology GA 903CI UT WOS:000227402600001 ER PT J AU Sorensen, AS Demler, E Lukin, MD AF Sorensen, AS Demler, E Lukin, MD TI Fractional quantum hall states of atoms in optical lattices SO PHYSICAL REVIEW LETTERS LA English DT Article ID MAGNETIC-FIELDS; WAVE-FUNCTIONS; LANDAU-LEVEL; CONDENSATION; ELECTRONS; EXCITATIONS; HIERARCHY; INSULATOR; FLUID; GAS AB We describe a method to create fractional quantum Hall states of atoms confined in optical lattices. We show that the dynamics of the atoms in the lattice is analogous to the motion of a charged particle in a magnetic field if an oscillating quadrupole potential is applied together with a periodic modulation of the tunneling between lattice sites. In a suitable parameter regime the ground state in the lattice is of the fractional quantum Hall type, and we show how these states can be reached by melting a Mott-insulator state in a superlattice potential. Finally, we discuss techniques to observe these strongly correlated states. C1 Harvard Univ, ITAMP, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. RP Sorensen, AS (reprint author), Harvard Univ, ITAMP, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RI Sorensen, Anders/L-1868-2013 OI Sorensen, Anders/0000-0003-1337-9163 NR 36 TC 272 Z9 272 U1 1 U2 18 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 MAR 4 PY 2005 VL 94 IS 8 AR 086803 DI 10.1103/PhysRevLett.94.086803 PG 4 WC Physics, Multidisciplinary SC Physics GA 902VY UT WOS:000227386000050 PM 15783916 ER PT J AU Didham, RK Ewers, RM Gemmell, NJ AF Didham, RK Ewers, RM Gemmell, NJ TI Comment on "Avian extinction and mammalian introductions on oceanic islands" SO SCIENCE LA English DT Editorial Material ID HABITAT LOSS; BIODIVERSITY; DEFORESTATION; BIRDS C1 Univ Canterbury, Sch Biol Sci, Christchurch 1, New Zealand. Smithsonian Trop Res Inst, Panama City, Panama. RP Didham, RK (reprint author), Univ Canterbury, Sch Biol Sci, Private Bag 4800, Christchurch 1, New Zealand. EM Raphael.Didham@canterbury.ac.nz RI Gemmell, Neil/C-6774-2009; Didham, Raphael/B-5953-2011 OI Gemmell, Neil/0000-0003-0671-3637; NR 14 TC 30 Z9 32 U1 2 U2 12 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD MAR 4 PY 2005 VL 307 IS 5714 BP 1412 EP 1412 DI 10.1126/science.1107333 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 904MT UT WOS:000227503100025 PM 15746412 ER PT J AU Fitzhugh, WW AF Fitzhugh, WW TI Maps, myths, and men - The story of the Vinland Map SO SCIENCE LA English DT Book Review C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Arctic Studies Ctr, Washington, DC 20560 USA. RP Fitzhugh, WW (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Arctic Studies Ctr, Washington, DC 20560 USA. EM fitzhugh.william@nmnh.si.edu NR 9 TC 0 Z9 0 U1 1 U2 2 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD MAR 4 PY 2005 VL 307 IS 5714 BP 1413 EP 1414 DI 10.1126/science.1103089 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 904MT UT WOS:000227503100027 ER PT J AU Brunthaler, A Reid, MJ Falcke, H Greenhill, LJ Henkel, C AF Brunthaler, A Reid, MJ Falcke, H Greenhill, LJ Henkel, C TI The geometric distance and proper motion of the Triangulum Galaxy (M33) SO SCIENCE LA English DT Article ID LARGE-MAGELLANIC-CLOUD; WATER-VAPOR MASERS; SPIRAL NEBULA; LOCAL GROUP; MESSIER 33; MASS AB We measured the angular rotation and proper motion of the Triangulum Galaxy (M33) with the Very Long Baseline Array by observing two H2O masers on opposite sides of the galaxy. By comparing the angular rotation rate with the inclination and rotation speed, we obtained a distance of 730 +/- 168 kiloparsecs. This distance is consistent With the most recent Cepheid distance measurement M33 is moving with a velocity of 190 +/- 59 kilometers per second relative to the Milky Way. These measurements promise a method to determine dynamical models for the Local Group and the mass and dark-matter halos of M31, M33, and the Milky Way. C1 Max Planck Inst Radioastron, D-53121 Bonn, Germany. Joint Inst Very Long Baseline Interferometry Euro, NL-7990 AA Dwingeloo, Netherlands. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. ASTRON, NL-7990 AA Dwingeloo, Netherlands. Radboud Univ Nijmegen, Dept Astron, NL-6500 GL Nijmegen, Netherlands. RP Brunthaler, A (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. EM brunthaler@jive.nl RI Falcke, Heino/H-5262-2012 OI Falcke, Heino/0000-0002-2526-6724 NR 24 TC 90 Z9 92 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 MAR 4 PY 2005 VL 307 IS 5714 BP 1440 EP 1443 DI 10.1126/science.1108342 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 904MT UT WOS:000227503100038 PM 15746420 ER PT J AU Randall, CE Harvey, VL Manney, GL Orsolini, Y Codrescu, M Sioris, C Brohede, S Haley, CS Gordley, LL Zawodny, JM Russell, JM AF Randall, CE Harvey, VL Manney, GL Orsolini, Y Codrescu, M Sioris, C Brohede, S Haley, CS Gordley, LL Zawodny, JM Russell, JM TI Stratospheric effects of energetic particle precipitation in 2003-2004 SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID ATMOSPHERE; ENHANCEMENTS; SIMULATIONS; NITROGEN; VORTEX AB Upper stratospheric enhancements in NOx (NO and NO2) were observed at high northern latitudes from March through at least July of 2004. Multi-satellite data analysis is used to examine the temporal evolution of the enhancements, to place them in historical context, and to investigate their origin. The enhancements were a factor of 4 higher than nominal at some locations, and are unprecedented in the northern hemisphere since at least 1985. They were accompanied by reductions in O-3 of more than 60% in some cases. The analysis suggests that energetic particle precipitation led to substantial NOx production in the upper atmosphere beginning with the remarkable solar storms in late October 2003 and possibly persisting through January. Downward transport of the excess NOx, facilitated by unique meteorological conditions in 2004 that led to an unusually strong upper stratospheric vortex from late January through March, caused the enhancements. C1 Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA. CALTECH, NASA, Jet Prop Lab, Pasadena, CA 91125 USA. New Mexico Highlands Univ, Dept Nat Resources Management, Las Vegas, NM USA. Norwegian Inst Air Res, N-2007 Kjeller, Norway. Univ Colorado, NOAA, Space Environm Ctr, Boulder, CO 80305 USA. Univ Colorado, Cooperat Inst Res Environm Sci, Space Environm Ctr, Boulder, CO 80309 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Chalmers, Dept Radio & Space Sci, S-41296 Gothenburg, Sweden. Univ York, Ctr Res Earth & Space Sci, Toronto, ON M3J 1PE, Canada. GATS Inc, Newport News, VA 23606 USA. NASA, Langley Res Ctr, Hampton, VA USA. Hampton Univ, Dept Phys, Ctr Atmospher Sci, Hampton, VA 23668 USA. RP Randall, CE (reprint author), Univ Colorado, Atmospher & Space Phys Lab, Campus Box 392, Boulder, CO 80309 USA. EM cora.randall@lasp.colorado.edu RI Randall, Cora/L-8760-2014; OI Randall, Cora/0000-0002-4313-4397; Sioris, Christopher/0000-0003-1168-8755 NR 14 TC 148 Z9 149 U1 2 U2 7 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD MAR 2 PY 2005 VL 32 IS 5 AR L05802 DI 10.1029/2004GL022003 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 905DO UT WOS:000227548100004 ER PT J AU Liu, XQ Hueber, FM Li, CS Wang, YF AF Liu, XQ Hueber, FM Li, CS Wang, YF TI Emendation of Sorosaccus gracilis Harris 1935, a gymnospermous pollen cone SO ACTA PHYTOTAXONOMICA SINICA LA English DT Article DE Sorosaccus gracilis; pollen cone; evolution; Late Triassic; Liaoning AB Study of gymnospermous pollen cones, identified with Sorosaccus gracilis Harris 1935, from the Yangcaogou Formation, Late Triassic of China, has led to the identification of new and significant characteristics of the species. The new specimens show distinct variations in the morphology of the distal laminar portions of the microsporophylls. These well-preserved fossils are helpful in elucidating, reconstructing and revising the diagnostic features of S. gracilis. After comparing the characteristics of the specimens from China with those of S. sibiricus Prynada 1962, and of the pollen cones which were respectively assigned to Baiera longifolia (Pom.) Heer 1876 from Siberia, Russia, S. minor Harris 1935 from Greenland, and S. umaltensis Krassilov 1972 from Bureya River of Russia, we consider that these four names should be reduced to the synonymy of S. gracilis. Thus we revise the diagnosis of Sorosaccus. The significance of Sorosaccus in evolution of pollen cones is discussed. We consider that Sorosaccus is possibly basic to the evolution of the genus Ginkgo by the reduction of the number of microsporangia and of microsporophylls. Ginkgo liaoningensis Liu, Crane, Li S Wang 2005 from the Early Cretaceous of Liaoning Province, China represents likely one of morphologically intermediate steps between Sorosaccus and G. biloba in evolution. C1 Chinese Acad Sci, Lab Systemat & Evolut Bot, Beijing 100093, Peoples R China. Chinese Acad Sci, Grad Sch, Beijing 100039, Peoples R China. Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA. RP Li, CS (reprint author), Chinese Acad Sci, Lab Systemat & Evolut Bot, Beijing 100093, Peoples R China. EM lics@ibcas.ac.cn NR 7 TC 2 Z9 7 U1 0 U2 3 PU SCIENCE CHINA PRESS PI BEIJING PA 16 DONGHUANGCHENGGEN NORTH ST, BEIJING 100717, PEOPLES R CHINA SN 0529-1526 J9 ACTA PHYTOTAXON SIN JI Acta Phytotaxon. Sin. PD MAR PY 2005 VL 43 IS 2 BP 182 EP 190 DI 10.1360/aps050005 PG 9 WC Plant Sciences SC Plant Sciences GA 912WO UT WOS:000228110800009 ER PT J AU Davis, CC Webb, CO Wurdack, KJ Jaramillo, CA Donoghue, MJ AF Davis, CC Webb, CO Wurdack, KJ Jaramillo, CA Donoghue, MJ TI Explosive radiation of malpighiales supports a mid-Cretaceous origin of modern tropical rain forests SO AMERICAN NATURALIST LA English DT Review DE biome evolution; fossils; K/T boundary; Malpighiales; penalized likelihood; tropical rain forest ID SOUTHEASTERN UNITED-STATES; PHYLOGENETIC-RELATIONSHIPS; LIKELIHOOD APPROACH; DNA-SEQUENCES; NORTHERN HEMISPHERE; MOLECULAR EVOLUTION; FLOWERING PLANTS; DIVERGENCE TIMES; CHLOROPLAST DNA; ABSOLUTE RATES AB Fossil data have been interpreted as indicating that Late Cretaceous tropical forests were open and dry adapted and that modern closed-canopy rain forest did not originate until after the Cretaceous-Tertiary (K/T) boundary. However, some mid-Cretaceous leaf floras have been interpreted as rain forest. Molecular divergence-time estimates within the clade Malpighiales, which constitute a large percentage of species in the shaded, shrub, and small tree layer in tropical rain forests worldwide, provide new tests of these hypotheses. We estimate that all 28 major lineages (i.e., traditionally recognized families) within this clade originated in tropical rain forest well before the Tertiary, mostly during the Albian and Cenomanian ( 112 - 94 Ma). Their rapid rise in the mid-Cretaceous may have resulted from the origin of adaptations to survive and reproduce under a closed forest canopy. This pattern may also be paralleled by other similarly diverse lineages and supports fossil indications that closed-canopy tropical rain forests existed well before the K/T boundary. This case illustrates that dated phylogenies can provide an important new source of evidence bearing on the timing of major environmental changes, which may be especially useful when fossil evidence is limited or controversial. C1 Univ Michigan, Herbarium, Dept Ecol & Evolutionary Biol, Ann Arbor, MI 48108 USA. Yale Univ, Dept Ecol & Evolutionary Biol, New Haven, CT 06520 USA. Natl Museum Nat Hist, Smithsonian Inst, Dept Bot, Washington, DC 20013 USA. Natl Museum Nat Hist, Smithsonian Inst, Labs Analyt Biol, Washington, DC 20013 USA. Inst Colombiano Petroleo, Biostratig Team, Bucaramanga, Colombia. RP Davis, CC (reprint author), Univ Michigan, Herbarium, Dept Ecol & Evolutionary Biol, Ann Arbor, MI 48108 USA. EM chdavis@umich.edu; campbell.webb@yale.edu; kwurdack@lms.si.edu; carlos.jaramillo@ecopetrol.com.co; michael.donoghue@yale.edu NR 226 TC 169 Z9 181 U1 2 U2 25 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0003-0147 J9 AM NAT JI Am. Nat. PD MAR PY 2005 VL 165 IS 3 BP E36 EP E65 DI 10.1086/428296 PG 30 WC Ecology; Evolutionary Biology SC Environmental Sciences & Ecology; Evolutionary Biology GA 904RY UT WOS:000227516600001 PM 15729659 ER PT J AU Stanley, JD AF Stanley, JD TI The near-destruction of Giza SO AMERICAN SCIENTIST LA English DT Article C1 Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA. RP Stanley, JD (reprint author), Smithsonian Inst, Dept Paleobiol, E-206 NMNH,Constitut Ave & 10th St, Washington, DC 20560 USA. EM stanley.daniel@nmnh.si.edu NR 1 TC 0 Z9 0 U1 0 U2 1 PU SIGMA XI-SCI RES SOC PI RES TRIANGLE PK PA PO BOX 13975, RES TRIANGLE PK, NC 27709 USA SN 0003-0996 J9 AM SCI JI Am. Scientist PD MAR-APR PY 2005 VL 93 IS 2 BP 110 EP 112 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 896OC UT WOS:000226942400007 ER PT J AU Hayek, LAC Heyer, WR AF Hayek, LAC Heyer, WR TI Determining sexual dimorphism in frog measurement data: integration of statistical significance, measurement error, effect size and biological significance SO ANAIS DA ACADEMIA BRASILEIRA DE CIENCIAS LA English DT Article DE statistics; sexual dimorphism; measurement error index; effect size; frogs ID POWER ANALYSIS; POPULATIONS; SELECTION; AMPHIBIA AB Several analytic techniques have been used to determine sexual dimorphism in vertebrate morphological measurement data with no emergent consensus on which technique is superior. A further confounding! problem for frog data is the existence of considerable measurement error. To determine dimorphism. We examine a single hypothesis (Ho = equal means) for two groups (females and males). We demonstrate that frog measurement data meet assumptions for clearly defined statistical hypothesis testing with statistical linear models rather than those of exploratory multivariate techniques such as principal components. correlation or correspondence analysis. In order to distinguish biological front statistical significance of hypotheses. we propose a new protocol that incorporates measurement error and effect size. Measurement error is evaluated with a novel measurement error index. Effect size, widely used in the behavioral sciences and in meta-analysis studies in biology, proves to be the most useful single metric to evaluate whether statistically significant results are biologically meaningful. Definitions for a range of small. medium. and large effect sizes specifically for frog measurement data are provided. Examples with measurement data for species of the frog genus Leptodactylus are presented. The new protocol is recommended not only to evaluate sexual dimorphism for frog data but for any animal measurement data for which the measurement error index and observed or a priori effect sizes can be calculated. C1 Smithsonian Inst, Natl Museum Nat Hist, MRC 162, Washington, DC 20013 USA. Smithsonian Inst, Natl Museum Nat Hist, MRC 136, Washington, DC 20013 USA. RP Heyer, WR (reprint author), Smithsonian Inst, Natl Museum Nat Hist, MRC 162, POB 37012, Washington, DC 20013 USA. EM heyer.ron@nmnh.si.edu NR 20 TC 12 Z9 18 U1 1 U2 6 PU ACAD BRASILEIRA DE CIENCIAS PI RIO JANEIRO PA RUA ANFILOFIO DE CARVALHO, 29, 3 ANDAR, 20030-060 RIO JANEIRO, BRAZIL SN 0001-3765 J9 AN ACAD BRAS CIENC JI An. Acad. Bras. Cienc. PD MAR PY 2005 VL 77 IS 1 BP 45 EP 76 PG 32 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 892PT UT WOS:000226663200005 PM 15692678 ER PT J AU Lynch, KS Rand, AS Ryan, MJ Wilczynski, W AF Lynch, KS Rand, AS Ryan, MJ Wilczynski, W TI Plasticity in female mate choice associated with changing reproductive states SO ANIMAL BEHAVIOUR LA English DT Article ID MATING CALL PHONOTAXIS; PHYSALAEMUS-PUSTULOSUS; SEXUAL SELECTION; TUNGARA FROG; SENSORY EXPLOITATION; POECILIA-RETICULATA; ARGININE VASOTOCIN; NEOTROPICAL FROG; HORMONAL-CONTROL; PREDATION RISK AB Flexibility in female mate choice occurs over a range of timescales. We examined this plasticity over the course of a single breeding cycle using phonotaxis tests that assay acoustic-based mating preferences of female tungara frogs, Physalaemus pustulosus. Tests were performed throughout three reproductive stages: unamplexed, amplexed and postmated. We tested whether the approach of the time at which a female needs to release her eggs (i.e. amplexed stage) influences her mate decisions. We examined three aspects of female mate choice behaviour: receptivity, permissiveness and discrimination. We considered a female receptive if she accepted a conspecific male's call, permissive if she accepted a call that was less attractive than a conspecific call and discriminating if she maintained her preference for a 'whine-chuck' over a 'whine'. Our results show that the proportion of females responding receptively and permissively peaks during the amplexed stage. Individual females also increase receptive and permissive responses in the amplexed stage. Furthermore, time to respond to mate signals is lowest in the amplexed stage. The increase in permissive mate decisions was not associated with a decrease in the probability of expressing discriminatory behaviour. We suggest that the increase in permissive mate choice is due to a decrease in female choosiness, that is, a lowering of her threshold for accepting unattractive calls, as her receptivity increases. This study provides empirical support for theoretical models predicting that females will reduce their threshold criteria for choosing mates as critical time points approach. (c) 2004 The Association for the Study of Animal Behaviour. Published by Elsevier Ltd. All rights reserved. C1 Univ Texas, Inst Neurosci, Austin, TX 78712 USA. Smithsonian Trop Res Inst, Balboa, Panama. Univ Texas, Sect Integrat Biol, Austin, TX 78712 USA. Univ Texas, Dept Psychol, Austin, TX 78712 USA. RP Lynch, KS (reprint author), Univ Texas, Inst Neurosci, 108 E Dean Keaton,Seay Psychol Bldg, Austin, TX 78712 USA. EM lynchks@mail.utexas.edu NR 45 TC 82 Z9 82 U1 3 U2 31 PU ACADEMIC PRESS LTD ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0003-3472 J9 ANIM BEHAV JI Anim. Behav. PD MAR PY 2005 VL 69 BP 689 EP 699 DI 10.1016/j.anbehav.2004.06.016 PN 3 PG 11 WC Behavioral Sciences; Zoology SC Behavioral Sciences; Zoology GA 905KV UT WOS:000227567900021 ER PT J AU Kim, HC Hofmann, EE AF Kim, HC Hofmann, EE TI Evaluation and derivation of cloud-cover algorithms for calculation of surface irradiance in sub-Antarctic and Antarctic environments SO ANTARCTIC SCIENCE LA English DT Article DE albedo; McMurdo Station; multiple reflection; Palmer Station; radiative transfer model ID SOLAR SPECTRAL IRRADIANCE; RADIATIVE-TRANSFER MODEL; OCEANIC PRIMARY PRODUCTION; ULTRAVIOLET-B RADIATION; OZONE DEPLETION; ATMOSPHERE; CHLOROPHYLL; INVESTIGATE; ALBEDO; RANGE AB To investigate approaches for parameterizing cloud cover effects in models of surface irradiance, the daily-averaged and hourly irradiances measured at Palmer Station (64 degrees 46'S, 64 degrees 3'W), McMurdo Station (77 degrees 51'S, 166 degrees 40'E) and Ushuaia (54 degrees 49'S, 68 degrees 19'W) between 1993 and 1997 were compared to irradiance values computed with a clear sky radiative transfer model in which nine empirical cloud-cover correction relationships were included. The cloud cover correction algorithms improved the simulated irradiance by factors of 3 and 3.7 for Palmer Station and Ushuaia, respectively, over the non-corrected irradiances. No single cloud cover correction algorithm worked consistently at the three sites. Therefore, a power function cloud cover correction algorithm was derived from comparisons between the observed spectrally-integrated irradiances and the simulated irradiances at the three locations. New coefficient values for the power function cloud cover correction algorithm for the spectrally-resolved irradiances were also derived at the three sites, and were found to be spectrally-neutral and to differ in magnitude. The general trends in the values obtained for the three sites provide an approach for generalizing cloud cover correction algorithm coefficients to other parts of the Antarctic. C1 Old Dominion Univ, Ctr Coastal Phys Oceanog, Norfolk, VA 23508 USA. RP Kim, HC (reprint author), Smithsonian Environm Res Ctr, POB 28,647 Contees Wharf Rd, Edgewater, MD 21037 USA. EM kimh@si.edu NR 43 TC 5 Z9 6 U1 0 U2 5 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 40 WEST 20TH ST, NEW YORK, NY 10011-4211 USA SN 0954-1020 J9 ANTARCT SCI JI Antarct. Sci. PD MAR PY 2005 VL 17 IS 1 BP 135 EP 149 DI 10.1017/S0954102005002518 PG 15 WC Environmental Sciences; Geography, Physical; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Physical Geography; Geology GA 911QF UT WOS:000228018700017 ER PT J AU Chance, K Kurosu, TP Sioris, CE AF Chance, K Kurosu, TP Sioris, CE TI Undersampling correction for array detector-based satellite spectrometers SO APPLIED OPTICS LA English DT Article ID NITROGEN-DIOXIDE AB Array detector-based instruments are now fundamental to measurements of ozone and other atmospheric trace gases from space in the ultraviolet, visible, and infrared. The present generation of such instruments suffers, to a greater or lesser degree, from undersampling of the spectra, leading to difficulties in the analysis of atmospheric radiances. We provide extended analysis of the undersampling suffered by modern satellite spectrometers, which include the Global Ozone Monitoring Experiment, Scanning Imaging Absorption Spectrometer for Atmospheric Chartography, Ozone Monitoring Instrument, and Ozone Mapping and Profiler Suite. The analysis includes basic undersampling, the effects of binning into separate detector pixels, and the application of high-resolution Fraunhofer spectral data to correct for undersampling in many useful cases. (C) 2005 Optical Society of America. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Chance, K (reprint author), Harvard Smithsonian Ctr Astrophys, Mail Stop 50,60 Garden St, Cambridge, MA 02138 USA. EM kchance@cfa.harvard.edu OI Chance, Kelly/0000-0002-7339-7577; Sioris, Christopher/0000-0003-1168-8755 NR 18 TC 40 Z9 41 U1 1 U2 6 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 1559-128X EI 2155-3165 J9 APPL OPTICS JI Appl. Optics PD MAR 1 PY 2005 VL 44 IS 7 BP 1296 EP 1304 DI 10.1364/AO.44.001296 PG 9 WC Optics SC Optics GA 903XT UT WOS:000227459600022 PM 15765710 ER PT J AU Dove, CJ Hare, PG Heacker, M AF Dove, CJ Hare, PG Heacker, M TI Identification of ancient feather fragments found in melting alpine ice patches in Southern Yukon SO ARCTIC LA English DT Article DE Yukon ice patches; feather identification; archaeological artifacts; radiocarbon dates ID SOUTHWEST YUKON; CANADA AB Twelve ancient artifacts or fragmented feather samples recovered from melting alpine ice patches in southern Yukon were analyzed in order to identify the species of birds associated with the ice patches or used on weapons recovered from these sites. The identification of bird species used by ancient hunters as long ago as 4500 BP enhances our insight into the customs, culture, and sophistication of life at that time. Downy feather barbs were found on two samples and microscopically identified as duck (Anatidae) and falcon (Falconidae). Further examination and comparisons using museum specimens resulted in a total of six identifications: Anatidae, eagle (Aquila or Haliaeetus), gyrfalcon (Falco rusticolus), white-tailed ptarmigan (Lagopus leucurus), short-eared owl (Asio flammeus), and northern flicker (Colaptes auratus luteus). Three of the feather samples were complete enough to show apparent modification, or notching, along the feather shaft. The identification of non-game birds such as gyrfalcon and eagles, together with evidence of possible worked or notched feathers, indicates that as long as 4500 years ago, Subarctic hunters selected feathers not only for their utility in fletching, but also possibly for symbolic or decorative purposes. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA. Govt Yukon, Heritage Branch, Whitehorse, YT Y1A 5H4, Canada. RP Dove, CJ (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Room E-600 MRC 116, Washington, DC 20560 USA. EM dovec@si.edu NR 20 TC 20 Z9 21 U1 1 U2 8 PU ARCTIC INST N AMER PI CALGARY PA UNIV OF CALGARY 2500 UNIVERSITY DRIVE NW 11TH FLOOR LIBRARY TOWER, CALGARY, ALBERTA T2N 1N4, CANADA SN 0004-0843 J9 ARCTIC JI Arctic PD MAR PY 2005 VL 58 IS 1 BP 38 EP 43 PG 6 WC Environmental Sciences; Geography, Physical SC Environmental Sciences & Ecology; Physical Geography GA 912NY UT WOS:000228087200006 ER PT J AU Rappole, JH AF Rappole, JH TI Evolution of old and new world migration systems: a response to Bell SO ARDEA LA English DT Article ID AVIAN MIGRATION AB In Rappole & Jones (2002), a hypothesis was presented explaining how migration between temperate and tropical regions could have evolved from normal dispersal of tropical-breeding resident birds, cit.ng taxonomic, ecological, biogeographic, physiological, and behavioral evidence in support of the theory. In addition, contrasts were made between old and New World migration systems, e.g., the relative absence of long-distance migrants from European forests, and an explanation was provided for how these differences could have developed given a tropical origin for most temperate migrants. Bell (2005 - this issue) has presented a detailed critique of this hypothesis in which he dismisses much of the reasoning and evidence for the theory, and proposes an alternative "northern home" theory in which migration derives from gradual genetic change in dispersal direction and distance favored by an environmental gradient, presumably climatic deterioration on temperate, breeding grounds. Herein a response is provided to Bell's critique, clarifying our arguments where they appear to have been misunderstood, and providing additional information in support of ideas on tropical origin for many migratory bird species. C1 Smithsonian Conservat & Res Ctr, Front Royal, VA 22630 USA. RP Rappole, JH (reprint author), Smithsonian Conservat & Res Ctr, 1500 Remount Rd, Front Royal, VA 22630 USA. EM rappolej@crc.si.edu NR 26 TC 5 Z9 5 U1 0 U2 7 PU NEDERLANDSE ORNITHOLOGISCHE UNIE PI ZEIST PA C/O PAUL STARMANS, OUDE ARNHEMSEWEG 261, 3705 BD ZEIST, NETHERLANDS SN 0373-2266 J9 ARDEA JI Ardea PD SPR PY 2005 VL 93 IS 1 BP 125 EP 131 PG 7 WC Ornithology SC Zoology GA 992VM UT WOS:000233912100013 ER PT J AU Schild, RE AF Schild, RE TI Accretion disk structure and orientation in the lensed and microlensed Q0957+561 quasar SO ASTRONOMICAL JOURNAL LA English DT Article DE dark matter; galaxies : halos; gravitational lensing; methods : data analysis quasars; general; quasars : individual (0957+561) ID ACTIVE GALACTIC NUCLEI; INTRINSIC MAGNETIC-MOMENTS; BLACK-HOLE CANDIDATES; BROAD-LINE REGION; GRAVITATIONAL LENS; OPTICAL WAVELENGTHS; TIME-DELAY; MAGNETOHYDRODYNAMIC SIMULATIONS; VARIABILITY; STARS AB Because quasars are unresolved in optical imaging, their structures must currently be inferred. Gravitational microlensing offers the possibility of producing information about the luminous structure provided that the Einstein ring diameter of the microlensing particle is comparable to or smaller than the radiating quasar components. Particularly interesting is the case of multiple-image gravitational lenses, where differences in the brightness histories of the multiple images can reveal the presence of the microlensing particles and allow inferences about the quasar's structure. The long brightness history measured for the Q0957 quasar has been analyzed previously for information about the microlensing particles, and evidence for the existence of a cosmologically significant population of planetary-mass particles has been reported. The microlensing results have also directly determined the sizes of the ultraviolet light emitting surfaces in the quasar. Autocorrelation analysis of the same brightness record has produced evidence for complex structure in the quasar; if the quasar suddenly brightens today, it is probable that it will brighten again after 129, 190, 540, and 620 days. We interpret these lags as the result of luminous structure around the quasar, and in particular we interpret them in the context of the Elvis model of the quasar's structure. We find that the autocorrelation peaks imply that beyond the luminous inner edge of the accretion disk, the biconic structures of the Elvis model must lie at a radial distance of 2; 10(17) cm from the black hole, and 2; 10(16) cm above and below the plane of the accretion disk. The quasar is apparently inclined 55 degrees to the line of sight. A second possible solution with lower inclination and larger structure is also indicated but statistically less probable. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Schild, RE (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 40 TC 12 Z9 12 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD MAR PY 2005 VL 129 IS 3 BP 1225 EP 1230 DI 10.1086/427965 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 904UL UT WOS:000227523100004 ER PT J AU Rosenberg, JL Schneider, SE Posson-Brown, J AF Rosenberg, JL Schneider, SE Posson-Brown, J TI Gas and stars in an HI-selected galaxy sample SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies : fundamental parameters; galaxies : stellar content; infrared : galaxies ID TULLY-FISHER RELATION; SURFACE BRIGHTNESS GALAXIES; DUAL-BEAM SURVEY; SPIRAL GALAXIES; 21 CENTIMETER; MASS FUNCTION; DEEP SURVEY; ARECIBO AB We present the results of a J-band study of the H I-selected Arecibo Dual-Beam Survey and Arecibo Slice Survey galaxy samples using Two Micron All Sky Survey data. We find that these galaxies span a wide range of stellar and gas properties. However, despite the diversity within the samples, we find a very tight correlation between luminosity and size in the J band, similar to that found in a previous paper by Rosenberg W Schneider between the H I mass and size. We also find that the correlation between the baryonic mass and the J-band diameter is even tighter than that between the baryonic mass and the rotational velocity. C1 Univ Colorado, Ctr Astrophys & Space Astron, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. Smith Coll, Northampton, MA 01063 USA. RP Rosenberg, JL (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 28 TC 12 Z9 12 U1 0 U2 2 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 MAR PY 2005 VL 129 IS 3 BP 1311 EP 1330 DI 10.1086/427397 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 904UL UT WOS:000227523100009 ER PT J AU Beasley, MA Brodie, JP Strader, J Forbes, DA Proctor, RN Barmby, P Huchra, JP AF Beasley, MA Brodie, JP Strader, J Forbes, DA Proctor, RN Barmby, P Huchra, JP TI The chemical properties of milky way and M31 globular clusters. II. Stellar population model predictions SO ASTRONOMICAL JOURNAL LA English DT Review DE galaxies : individual (M31); globular clusters : general ID HUBBLE-SPACE-TELESCOPE; HORIZONTAL-BRANCH STARS; LARGE-MAGELLANIC-CLOUD; EARLY-TYPE GALAXIES; MAIN-SEQUENCE PHOTOMETRY; DWARF SPHEROIDAL GALAXY; ELLIPTICAL GALAXIES; LOCAL GROUP; INTEGRATED SPECTRA; FORMATION HISTORY AB We derive ages, metallicities, and abundance ratios ([alpha/Fe]) from the integrated spectra of 23 globular clusters in M31 by employing multivariate fits to two different stellar population models. We also perform a parallel analysis on 21 Galactic globular clusters as a consistency check and in order to facilitate a differential analysis. Our analysis shows that the M31 globular clusters separate into three distinct components in age and metallicity; we identify an old, metal-poor group ( seven clusters), an old, metal-rich group ( 10 clusters), and an intermediate-age ( 3 - 6 Gyr), intermediate-metallicity ([Z/H] similar to -1) group (six clusters). This third group is not identified in the Galactic globular cluster sample. We also see evidence that the old, metal-rich Galactic globular clusters are 1 - 2 Gyr older than their counterparts in M31. The majority of globular clusters in both samples appear to be enhanced in alpha-elements, but the degree of enhancement is rather model-dependent. The intermediate-age globular clusters appear to be the most enhanced, with [alpha/Fe] similar to 0.4. These clusters are clearly depressed in CN with respect to the models and the bulk of the M31 and Milky Way sample. Compared with the bulge of M31, M32, and NGC 205, these clusters most resemble the stellar populations in NGC 205 in terms of age, metallicity, and CN abundance. We infer horizontal branch morphologies for the M31 clusters using the Rose Ca II index and demonstrate that blue horizontal branches are not leading to erroneous age estimates in our analysis. We discuss and reject as unlikely the hypothesis that these objects are in fact foreground stars contaminating the optical catalogs. The intermediate-age clusters have generally higher velocities than the bulk of the M31 cluster population. Spatially, three of these clusters are projected onto the bulge region, and the remaining three are distributed at large radii. We discuss these objects within the context of the build-up of the M31 halo and suggest that these clusters possibly originated in a gas-rich dwarf galaxy, which may or may not be presently observable in M31. C1 Univ Calif Santa Cruz, Lick Observ, Santa Cruz, CA 95064 USA. Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Beasley, MA (reprint author), Univ Calif Santa Cruz, Lick Observ, Santa Cruz, CA 95064 USA. EM mbeasley@ucolick.org; brodie@ucolick.org; strader@ucolick.org; dforbes@astro.swin.edu.au; rproctor@astro.swin.edu.au; pbarmby@cfa.harvard.edu; huchra@cfa.harvard.edu RI Barmby, Pauline/I-7194-2016 OI Barmby, Pauline/0000-0003-2767-0090 NR 124 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 0004-6256 J9 ASTRON J JI Astron. J. PD MAR PY 2005 VL 129 IS 3 BP 1412 EP 1427 DI 10.1086/427715 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 904UL UT WOS:000227523100015 ER PT J AU Kim, JS Walter, FM Wolk, SJ AF Kim, JS Walter, FM Wolk, SJ TI Low-mass star formation in the gum nebula: The CG 30/31/38 complex SO ASTRONOMICAL JOURNAL LA English DT Article DE circumstellar matter; HII regions; ISM : globules; stars : formation; stars : low-mass; brown dwarfs; stars : pre-main-sequence ID T-TAURI STARS; X-RAY SOURCES; GLOBULES CG 30/31/38; MAIN-SEQUENCE STARS; COMETARY GLOBULES; ORION-NEBULA; INTERSTELLAR CLOUDS; MOLECULAR CLOUD; STANDARD STARS; BROWN DWARFS AB We present photometric and spectroscopic results for the low-mass pre-main-sequence (PMS) stars with spectral types K-M in the cometary globule (CG) 30/31/38 complex. We obtained multiobject high-resolution spectra for the targets selected as possible PMS stars from multiwavelength photometry. We identified 11 PMS stars brighter than V = 16:5 with ages <= 5 Myr at a distance of approximately 200 pc. The spatial distribution of the PMS stars, CG clouds, and ionizing sources (O stars and supernova remnants) suggests a possible triggered origin of the star formation in this region. We confirm the youth of the photometrically selected PMS stars using the lithium abundances. The radial velocities of the low-mass PMS stars are consistent with those of the cometary globules. Most of the PMS stars show weak H alpha emission with W-lambda(H alpha) < 10 angstrom. Only one out of the 11 PMS stars shows a moderate near-IR excess, which suggests a short survival time (t < 5 Myr) of circumstellar disks in this star-forming environment. In addition, we find five young late-type stars and one Ae star that have no obvious relation to the CG 30/31/38 complex. We also discuss a possible scenario of the star formation history in the CG 30/31/38 region. C1 SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kim, JS (reprint author), SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA. EM serena@as.arizona.edu OI Wolk, Scott/0000-0002-0826-9261 NR 84 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 0004-6256 J9 ASTRON J JI Astron. J. PD MAR PY 2005 VL 129 IS 3 BP 1564 EP 1579 DI 10.1086/428002 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 904UL UT WOS:000227523100022 ER PT J AU Hartman, JD Kaluzny, J Szentgyorgyi, A Stanek, KZ AF Hartman, JD Kaluzny, J Szentgyorgyi, A Stanek, KZ TI BVI photometric variability survey of M3 SO ASTRONOMICAL JOURNAL LA English DT Article DE binaries : eclipsing; delta Scuti; globular clusters : individual (M3); stars : variables : other; surveys ID GLOBULAR-CLUSTER M3; IMAGE-SUBTRACTION PHOTOMETRY; VARIABLE-STARS; BLUE STRAGGLERS; IDENTIFICATION; PARAMETERS; BINARIES; CATALOG; SEARCH; FIELD AB We have conducted a three-band (BVI) variability survey of the globular cluster M3. This is the first three-band survey of the cluster using modern image subtraction techniques. Observations were made over nine nights in 1998 on the 1.2 m telescope at the F. L. Whipple Observatory in Arizona. We present photometry for 180 variable stars in the M3 field, 12 of which are newly discovered. New discoveries include six SX Phoenicis-type variables that all lie in the blue straggler region of the color-magnitude diagram, two new first-overtone RR Lyrae variables, a candidate multimode RR Lyrae variable, a detached eclipsing binary, and two unclassified variables. We also provide revised periods for 52 of the 168 previously known variables that we observe. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Nicolaus Copernicus Astron Ctr, PL-00716 Warsaw, Poland. RP Hartman, JD (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jhartman@cfa.harvard.edu; jka@camk.edu.pl; aszentgyorgyi@cfa.harvard.edu; kstanek@cfa.harvard.edu OI Hartman, Joel/0000-0001-8732-6166 NR 29 TC 8 Z9 8 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD MAR PY 2005 VL 129 IS 3 BP 1596 EP 1606 DI 10.1086/427252 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 904UL UT WOS:000227523100025 ER PT J AU Kanaan, A Nitta, A Winget, DE Kepler, SO Montgomery, MH Metcalfe, TS Oliveira, H Fraga, L da Costa, AFM Costa, JES Castanheira, BG Giovannini, O Nather, RE Mukadam, A Kawaler, SD O'Brien, MS Reed, MD Kleinman, SJ Provencal, JL Watson, TK Kilkenny, D Sullivan, DJ Sullivan, T Shobbrook, B Jiang, XJ Ashoka, BN Seetha, S Leibowitz, E Ibbetson, P Mendelson, H Meistas, EG Kalytis, R Alisauskas, D O'Donoghue, D Buckley, D Martinez, P van Wyk, F Stobie, R Marang, F van Zyl, L Ogloza, W Krzesinski, J Zola, S Moskalik, P Breger, M Stankov, A Silvotti, R Piccioni, A Vauclair, G Dolez, N Chevreton, M Deetjen, J Dreizler, S Schuh, S Perez, JMG Ostensen, R Ulla, A Manteiga, M Suarez, O Burleigh, MR Barstow, MA AF Kanaan, A Nitta, A Winget, DE Kepler, SO Montgomery, MH Metcalfe, TS Oliveira, H Fraga, L da Costa, AFM Costa, JES Castanheira, BG Giovannini, O Nather, RE Mukadam, A Kawaler, SD O'Brien, MS Reed, MD Kleinman, SJ Provencal, JL Watson, TK Kilkenny, D Sullivan, DJ Sullivan, T Shobbrook, B Jiang, XJ Ashoka, BN Seetha, S Leibowitz, E Ibbetson, P Mendelson, H Meistas, EG Kalytis, R Alisauskas, D O'Donoghue, D Buckley, D Martinez, P van Wyk, F Stobie, R Marang, F van Zyl, L Ogloza, W Krzesinski, J Zola, S Moskalik, P Breger, M Stankov, A Silvotti, R Piccioni, A Vauclair, G Dolez, N Chevreton, M Deetjen, J Dreizler, S Schuh, S Perez, JMG Ostensen, R Ulla, A Manteiga, M Suarez, O Burleigh, MR Barstow, MA TI Whole Earth Telescope observations of BPM 37093: A seismological test of crystallization theory in white dwarfs SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars : evolution; stars : individual : BPM 37093; stars : interiors; stars : oscillations; white dwarfs ID ZZ-CETI STARS; PULSATIONAL PROPERTIES; MODE-IDENTIFICATION; TEMPERATURE; ASTEROSEISMOLOGY; SPECTROSCOPY; DISCOVERY; G117-B15A; EVOLUTION; G29-38 AB BPM 37093 is the only hydrogen-atmosphere white dwarf currently known which has sufficient mass (similar to 1.1 M-.) to theoretically crystallize while still inside the ZZ Ceti instability strip (T-eff similar to 12 000 K). As a consequence, this star represents our first opportunity to test crystallization theory directly. If the core is substantially crystallized, then the inner boundary for each pulsation mode will be located at the top of the solid core rather than at the center of the star, affecting mainly the average period spacing. This is distinct from the "mode trapping" caused by the stratified surface layers, which modifies the pulsation periods more selectively. In this paper we report on Whole Earth Telescope observations of BPM 37093 obtained in 1998 and 1999. Based on a simple analysis of the average period spacing we conclude that a large fraction of the total stellar mass is likely to be crystallized. C1 Univ Fed Santa Catarina, Dept Fis, BR-88040900 Florianopolis, SC, Brazil. Apache Point Observ, Sunspot, NM 88349 USA. Univ Texas, Dept Astron, Austin, TX 78712 USA. Univ Fed Rio Grande Sul, Inst Fis, BR-91501970 Porto Alegre, RS, Brazil. Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. UCS, Dept Quim & Fis, Caxias Do Sul, Brazil. Iowa State Univ, Dept Phys & Astron, Ames, IA USA. SW Missouri State Univ, Dept Astron, Springfield, MO USA. Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. Southwestern Univ, Georgetown, TX USA. S African Astron Observ, ZA-7935 Cape Town, South Africa. Victoria Univ Wellington, Wellington, New Zealand. Univ Sydney, Chatterton Astron Dept, Sydney, NSW 2006, Australia. Acad Sinica, Astron Observ, Beijing, Peoples R China. Indian Space Res Org, Bangalore 562140, Karnataka, India. Tel Aviv Univ, Wise Observ, IL-69978 Tel Aviv, Israel. Inst Theoret Phys & Astron, Vilnius, Lithuania. Vilnius State Univ, Vilnius, Lithuania. Cracow Pedag Univ, Mt Suhora Observ, Krakow, Poland. Jagiellonian Univ, Astron Observ, PL-31007 Krakow, Poland. Copernicus Astron Ctr, Torun, Poland. Univ Vienna, Inst Astron, A-1010 Vienna, Austria. INAF, Osservatorio Astron Capodimonte, Naples, Italy. Univ Bologna, Dipartimento Astron, I-40126 Bologna, Italy. Univ Toulouse 3, Observ Midi Pyrenees, F-31062 Toulouse, France. Observ Paris, Paris, France. Inst Astron & Astrophys, Tubingen, Germany. Univ Sternwarte Gottingen, D-3400 Gottingen, Germany. Univ Tromso, N-9001 Tromso, Norway. Isaac Newton Grp, Tenerife, Spain. Univ Vigo, Dept Fis Aplicada, Vigo, Spain. Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. RP Kanaan, A (reprint author), Univ Fed Santa Catarina, Dept Fis, BR-88040900 Florianopolis, SC, Brazil. EM kanaan@astro.ufsc.br RI Metcalfe, Travis/A-9388-2008; Kepler, S. O. /H-5901-2012; Fraga, Luciano/K-9075-2013; Ulla Miguel, Ana Maria/M-2860-2014; Manteiga, Minia/K-9773-2014; OI Metcalfe, Travis/0000-0003-4034-0416; Kepler, S. O. /0000-0002-7470-5703; Manteiga, Minia/0000-0002-7711-5581; Silvotti, Roberto/0000-0002-1295-8174; Kawaler, Steven/0000-0002-6536-6367 NR 29 TC 40 Z9 40 U1 1 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 MAR PY 2005 VL 432 IS 1 BP 219 EP 224 DI 10.1051/0004-6361:20041125 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 904JR UT WOS:000227493100024 ER PT J AU Young, PR Berrington, KA Lobel, A AF Young, PR Berrington, KA Lobel, A TI FeVII lines in the spectrum of RR telescopii SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars : binaries : symbiotic; stars : individual : RR Telescopii; ultraviolet : stars; atomic data ID ATOMIC DATABASE; EMISSION-LINES; IRON PROJECT; RATES; ANGSTROM; CHIANTI; TEL; VI AB Thirteen transitions within the ground 3d(2) configuration of Fe VII are identified in ultraviolet and optical spectra of the symbiotic star RR Telescopii obtained with the STIS instrument of the Hubble Space Telescope. The line fluxes are compared with theoretical data computed with the recent atomic data of Berrington et al., and high resolution optical spectra from VLT/UVES are used to identify blends. Seven branching ratios are measured, with three in good agreement with theory and one affected by blending. The lambda5277/lambda4943 branching ratio is discrepant by >3sigma, indicating errors in the atomic data for the lambda5277 line. A least-squares minimization scheme is used to simultaneously derive the temperature, T, and density, N-e, of the RR Tel nebula, and the interstellar extinction, E( B - V), towards RR Tel from the complete set of emission lines. The derived values are: log T/K = 4.50 +/- 0.23, log N-e/ cm(-3) = 7.25 +/- 0.05, and E(B - V) less than or equal to 0.27. The extinction is not well-constrained by the Fe VII lines, but is consistent with the more accurate value E(B- V) = 0.109(-0.059)(+0.052) derived here from the Ne V lambda2974/lambda1574 ratio in the STIS spectrum. Large differences between the K. A. Berrington et al. electron excitation data and the earlier F. P. Keenan & P. H. Norrington data-set are demonstrated, and the latter is shown to give worse agreement with observations. C1 Rutherford Appleton Lab, CCLRC, Didcot OX11 0QX, Oxon, England. Sheffield Hallam Univ, Sch Sci & Math, Sheffield S1 1WB, S Yorkshire, England. Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Young, PR (reprint author), Rutherford Appleton Lab, CCLRC, Didcot OX11 0QX, Oxon, England. EM p.r.young@rl.ac.uk NR 16 TC 12 Z9 12 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 MAR PY 2005 VL 432 IS 2 BP 665 EP 670 DI 10.1051/0004-6361:20042033 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 904JS UT WOS:000227494200036 ER PT J AU Durret, F Neto, GBL Forman, A AF Durret, F Neto, GBL Forman, A TI An XMM-Newton view of the cluster of galaxies Abell 85 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE plasmas; galaxies : intergalactic medium; X-rays : galaxies : clusters; galaxies : clusters : individual : A85 ID X-RAY-CLUSTERS; RICH CLUSTER; DARK-MATTER; NEARBY CLUSTERS; RADIO-SOURCES; GAS; TEMPERATURE; ABUNDANCES; ABSORPTION; CATALOG AB We have observed the cluster of galaxies Abell 85 with XMM-Newton. These data have allowed us in a previous paper to confirm the existence of the extended 4 Mpc filament detected by the ROSAT PSPC in the neighbourhood of this cluster, and to determine an X-ray temperature of about similar to2 keV. We now present a thorough analysis of the properties of the X-ray gas in the cluster itself, including temperature and metallicity maps for the entire cluster. These results show that Abell 85 had intense merging activity in the past and is not fully relaxed, even in the central region. We have also determined the individual abundances for some iron-group metals and alpha-elements in various regions; the ratios of these metallicities to the iron abundance show that both supernova types Ia and II must be involved in the intra-cluster gas enrichment. Spectral analysis of the central region suggests a different redshift of the X-ray emitting gas compared to the mean cluster velocity derived from galaxy member redshifts. We discuss the implications of the difference between the cD galaxy redshift, the mean galaxy redshift and the hot gas redshift, as well as the possibility of several groups being accreted on to Abell 85. Finally, we obtain the dynamical mass profile and baryon fraction taking into account the newly determined temperature profile. The dynamical mass in Abell 85 has a steep density profile, similar to the ones found in N-body simulations. C1 CNRS, Inst Astrophys Paris, F-75014 Paris, France. USP, Inst Astron Geofis & C Atmosf, BR-05508090 Sao Paulo, Brazil. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Durret, F (reprint author), CNRS, Inst Astrophys Paris, 98bis Bd Arago, F-75014 Paris, France. EM durret@iap.fr RI Lima Neto, Gastao/J-6117-2014 NR 60 TC 72 Z9 73 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 MAR PY 2005 VL 432 IS 3 BP 809 EP 821 DI 10.1051/0004-6361:20041666 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 904JT UT WOS:000227494400007 ER PT J AU Stuart, J Wyithe, B Loeb, A AF Stuart, J Wyithe, B Loeb, A TI Calibrating the galaxy halo-black hole relation based on the clustering of quasars SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : observations; cosmology : theory; quasars : general ID DIGITAL SKY SURVEY; QSO REDSHIFT SURVEY; OPTICAL LUMINOSITY FUNCTION; DARK-MATTER HALOES; EVOLUTION; OBJECTS; MODEL; BULGE; CONSTRAINTS; ACCRETION AB The observed number counts of quasars can be explained either by long-lived activity within rare massive hosts or by short-lived activity within smaller, more common hosts. It has been argued that quasar lifetimes can therefore be inferred from their clustering length, which determines the typical mass of the quasar host. Here we point out that the relationship between the mass of the black hole and the circular velocity of its host dark matter halo is more fundamental to the determination of the clustering length. In particular, the clustering length observed in the Two-Degree Field (2dF) quasar redshift survey is consistent with the galactic halo-black hole relation observed in local galaxies, provided that quasars shine at similar to10%-100% of their Eddington luminosity. The slow evolution of the clustering length with redshift inferred in the 2dF quasar survey favors a black hole mass whose redshift-independent scaling is with halo circular velocity rather than halo mass. These results are independent from observations of the number counts of bright quasars, which can be used to determine the quasar lifetime and its dependence on redshift. We show that if quasar activity results from galaxy mergers, then the number counts of quasars imply an episodic quasar lifetime that is set by the dynamical time of the host galaxy rather than by the Salpeter time. Our results imply that as the redshift increases, the central black holes comprise a larger fraction of their host galaxy mass, and the quasar lifetime gets shorter. C1 Univ Melbourne, Parkville, Vic 3010, Australia. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Stuart, J (reprint author), Univ Melbourne, Parkville, Vic 3010, Australia. EM swyithe@isis.ph.unimelb.edu.au; aloeb@cfa.harvard.edu OI Wyithe, Stuart/0000-0001-7956-9758 NR 44 TC 26 Z9 26 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 MAR 1 PY 2005 VL 621 IS 1 BP 95 EP 103 DI 10.1086/425263 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 903DR UT WOS:000227406200008 ER PT J AU Daniel, MK Badran, HM Bond, IH Boyle, PJ Bradbury, SM Buckley, JH Carter-Lewis, DA Catanese, M Celik, O Cogan, P Cui, W D'Vali, M Perez, ID Duke, C Falcone, A Fegan, DJ Fegan, SJ Finley, JP Fortson, LF Gaidos, JA Gammell, S Gibbs, K Gillanders, GH Grube, J Hall, J Hall, TA Hanna, D Hillas, AM Holder, J Horan, D Humensky, TB Jarvis, A Jordan, M 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 Milovanovic, A Moriarty, P Muller, D Nagai, T Nolan, S Ong, RA Pallassini, R Petry, D Power-Mooney, B Quinn, J Quinn, M Ragan, K Rebillot, P Reynolds, PT Rose, HJ Schroedter, M Sembroski, GH Swordy, SP Syson, A Vassiliev, VV Wakely, SP Walker, G Weekes, TC Zweerink, J AF Daniel, MK Badran, HM Bond, IH Boyle, PJ Bradbury, SM Buckley, JH Carter-Lewis, DA Catanese, M Celik, O Cogan, P Cui, W D'Vali, M Perez, ID Duke, C Falcone, A Fegan, DJ Fegan, SJ Finley, JP Fortson, LF Gaidos, JA Gammell, S Gibbs, K Gillanders, GH Grube, J Hall, J Hall, TA Hanna, D Hillas, AM Holder, J Horan, D Humensky, TB Jarvis, A Jordan, M 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 Milovanovic, A Moriarty, P Muller, D Nagai, T Nolan, S Ong, RA Pallassini, R Petry, D Power-Mooney, B Quinn, J Quinn, M Ragan, K Rebillot, P Reynolds, PT Rose, HJ Schroedter, M Sembroski, GH Swordy, SP Syson, A Vassiliev, VV Wakely, SP Walker, G Weekes, TC Zweerink, J TI Spectrum of very high energy gamma-rays from the blazar 1ES 1959+650 during flaring activity in 2002 SO ASTROPHYSICAL JOURNAL LA English DT Article DE BL Lacertae objects : individual (1ES 1959+650); gamma rays : observations; techniques : spectroscopic ID CHERENKOV TELESCOPES; STRONG FLARES; TEV ENERGIES; RADIATION; SYSTEM; MARKARIAN-421; CALIBRATION; H1426+428; PROJECT AB The blazar 1ES 1959+650 was observed in a flaring state with the Whipple 10 m Imaging Atmospheric Cerenkov Telescope in 2002 May. A spectral analysis has been carried out on the data from that time period, and the resulting very high energy gamma-ray spectrum (E greater than or equal to 316 GeV) can be well fitted by a power law of differential spectral index alpha = 2.78 +/- 0.12(stat) +/- 0.21(sys). On 2002 June 4, the source flared dramatically in the gamma-ray range without any coincident increase in the X-ray emission, providing the first unambiguous example of an "orphan'' gamma-ray flare from a blazar. The gamma-ray spectrum for these data can also be described by a simple power-law fit with alpha = 2.82 +/- 0.15(stat) +/- 0.30(sys). There is no compelling evidence for spectral variability or for any cutoff to the spectrum. C1 Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. Tanta Univ, Dept Phys, Tanta, Egypt. Univ Leeds, Dept Phys, Leeds LS2 9JT, W Yorkshire, England. Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. Washington Univ, Dept Phys, St Louis, MO 63130 USA. Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. Univ Calif Los Angeles, Dept Phys, Los Angeles, CA 90095 USA. Natl Univ Ireland, Expt Phys Dept, Dublin 4, Ireland. Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. Grinnell Coll, Dept Phys, Grinnell, IA 50112 USA. Univ Arizona, Dept Phys, Tucson, AZ 85721 USA. Natl Univ Ireland, Dept Phys, Galway, Ireland. Univ Utah, High Energy Astrophys Inst, Salt Lake City, UT USA. Univ Arkansas, Dept Phys & Astron, Little Rock, AR 72204 USA. McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA. Galway Mayo Inst Technol, Sch Sci, Galway, Ireland. Univ Maryland Baltimore Cty, Baltimore, MD 21228 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Colk Inst Technol, Dept Appl Phys & Instrumentat, Cork, Ireland. RP Daniel, MK (reprint author), Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. EM mkdaniel@iastate.edu RI Hall, Jeter/E-9294-2015; 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 32 TC 28 Z9 28 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 MAR 1 PY 2005 VL 621 IS 1 BP 181 EP 187 DI 10.1086/427406 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 903DR UT WOS:000227406200016 ER PT J AU Burstein, D Ho, LC Huchra, JP Macri, LM AF Burstein, D Ho, LC Huchra, JP Macri, LM TI The K-band luminosities of galaxies: Do S0s come from spiral galaxies? SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : clusters : general; galaxies : elliptical and lenticular, cD; galaxies : evolution; galaxies : formation ID TULLY-FISHER RELATION; STELLAR POPULATION HISTORIES; HUBBLE-SPACE-TELESCOPE; LINE STRENGTHS; RICH CLUSTERS; POOR GROUPS; HOT GAS; X-RAY; EVOLUTION; PARAMETERS AB There are two main theories for the formation of S0 galaxies: that S0 and elliptical galaxies are formed in the same manner ab initio, or that S0s are mainly spiral galaxies from which the gas has been stripped by interactions with either hot cluster gas or other galaxies. Perhaps the best way to test these formation ideas is to calculate the luminosities of S0 and spiral galaxies in the K band, where dust effects for the spiral galaxies are minimal. If S0s are stripped spirals whose star formation has been quenched, we expect from existing models that S0s should be similar to0.75 mag less luminous in K absolute magnitudes than early-type spirals. Using the nearly 25,000 galaxies in the Two Micron All Sky Survey that have total K magnitudes less than or equal to11.25, we are able to select over 19,000 of these galaxies for analysis. Of these, 10,977 are in the Third Reference Catalogue of Bright Galaxies and 8230 are not. We separate galaxies by both Hubble type and whether they are in or out of nearby clusters and near or far from us. K-band absolute magnitudes are predicted using the velocity field model of Faber & Burstein for galaxies with a velocity of 6000 km s(-1) or less with respect to the cosmic background radiation. We present histograms, medians, and means for galaxies of all Hubble types in absolute K magnitudes. In all cases, we find that giant ellipticals are more luminous than S0s, and that S0s are at least as luminous, if not more luminous, in the K band than are spiral galaxies. The K absolute magnitudes of the S0s compared to those of the spirals show that S0s are not gas-stripped spiral galaxies. While a few S0s can be gas-stripped spirals, as a class they are not. We suggest that the E+A galaxies seen in clusters at moderate redshift are S0s onto which hot gas has cooled, producing a temporary sprinkling of star formation. C1 Arizona State Univ, Dept Phys & Astron, Tempe, AZ 85287 USA. Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. Natl Opt Astron Observ, Tucson, AZ 85726 USA. RP Burstein, D (reprint author), Arizona State Univ, Dept Phys & Astron, Box 871504, Tempe, AZ 85287 USA. EM burstein@samuri.la.asu.edu OI Macri, Lucas/0000-0002-1775-4859 NR 44 TC 32 Z9 32 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 2005 VL 621 IS 1 BP 246 EP 255 DI 10.1086/427408 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 903DR UT WOS:000227406200021 ER PT J AU Teegarden, BJ Watanabe, K Jean, P Knodlseder, J Lonjou, V Roques, JP Skinner, GK von Ballmoos, P Weidenspointner, G Bazzano, A Butt, YM Decourchelle, A Fabian, AC Goldwurm, A Gudel, M Hannikainen, DC Hartmann, DH Hornstrup, A Lewin, WHG Makishima, K Malzac, A Miller, J Parmar, AN Reynolds, SP Rothschild, RE Schonfelder, V Tomsick, JA Vink, J AF Teegarden, BJ Watanabe, K Jean, P Knodlseder, J Lonjou, V Roques, JP Skinner, GK von Ballmoos, P Weidenspointner, G Bazzano, A Butt, YM Decourchelle, A Fabian, AC Goldwurm, A Gudel, M Hannikainen, DC Hartmann, DH Hornstrup, A Lewin, WHG Makishima, K Malzac, A Miller, J Parmar, AN Reynolds, SP Rothschild, RE Schonfelder, V Tomsick, JA Vink, J TI INTEGRAL SPI limits on electron-positron annihilation radiation from the Galactic plane SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma rays : observations ID 511 KEV LINE; CENTER REGION; CENTER DIRECTION; INNER GALAXY; EMISSION AB The center of our Galaxy is a known strong source of electron-positron 511 keVannihilation radiation. Thus far, however, there have been no reliable detections of annihilation radiation outside of the central radian of our Galaxy. One of the primary objectives of the INTEGRAL ( International Gamma-Ray Astrophysics Laboratory) mission, launched in 2002 October, is the detailed study of this radiation. The Spectrometer on INTEGRAL (SPI) is a high-resolution, coded-aperture gamma-ray telescope with an unprecedented combination of sensitivity, angular resolution, and energy resolution. We report results from the first 10 months of observation. During this period a significant fraction of the observing time was spent in or near the Galactic plane. No positive annihilation flux was detected outside of the central region (\l\> 40degrees) of our Galaxy. In this paper we describe the observations and data analysis methods and give limits on the 511 keV flux. C1 NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. CNRS, UPS, Ctr Etud Spatiale Rayonnements, F-31028 Toulouse 4, France. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CE Saclay, Serv Astrophys, F-91191 Gif Sur Yvette, France. Ist Astrofis Spaziale & Fis Cosm, IASF, Rome, Italy. Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. Paul Scherrer Inst, CH-5232 Villigen, Switzerland. Univ Helsinki, FIN-00014 Helsinki, Finland. Clemson Univ, Clemson, SC 29634 USA. MIT, Ctr Space Res, Cambridge, MA 02139 USA. Univ Tokyo, Dept Phys, Bunkyo Ku, Tokyo 1130033, Japan. European Space Agcy, Estec, Div Astrophys, Res & Sci Support Dept, NL-2200 AG Noordwijk, Netherlands. N Carolina State Univ, Dept Phys, Raleigh, NC 27695 USA. Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA. Max Planck Inst Extraterr Phys, D-85740 Garching, Germany. SRON, Natl Inst Space Res, NL-3584 CA Utrecht, Netherlands. RP NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Code 661, Greenbelt, MD 20771 USA. RI Guedel, Manuel/C-8486-2015; OI Guedel, Manuel/0000-0001-9818-0588; Parmar, Arvind/0000-0002-3307-6517; Bazzano, Angela/0000-0002-2017-4396 NR 33 TC 49 Z9 50 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 2005 VL 621 IS 1 BP 296 EP 300 DI 10.1086/426859 PN 1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 903DR UT WOS:000227406200027 ER PT J AU Jeffers, SV Cameron, AC Barnes, JR Aufdenberg, JP Hussain, GAJ AF Jeffers, SV Cameron, AC Barnes, JR Aufdenberg, JP Hussain, GAJ TI Direct evidence for a polar spot on SV Camelopardalis SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : eclipsing; stars : activity; stars : individual (SV Camelopardalis); stars : late-type; stars : spots ID STELLAR SURFACE-STRUCTURE; SYMMETRIC MODEL ATMOSPHERES; EFFECTIVE TEMPERATURES; DIFFERENTIAL ROTATION; ACTIVE STARS; 6800 K; BINARY; PARAMETERS; PERIOD; LIGHT AB We have used spectrophotometric data from the Hubble Space Telescope (HST) to eclipse-map the primary component of the RS CVn binary SV Cam over nine HST orbits. We find from these observations and the Hipparcos parallax that the surface flux in the eclipsed low-latitude region of the primary is about 30% lower than that computed from a PHOENIX model atmosphere at the effective temperature that best fits the spectral energy distribution of the eclipsed flux. This can only be accounted for if about a third of the primary's surface is covered with unresolved dark starspots. Extending this to the full surface of the primary, we find that, even taking into account this spot-filling factor, there is an additional flux deficit on the primary star. This can only be explained if there is a large polar spot on the primary star extending from the pole to latitude 48degrees +/- 6degrees. C1 Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. Natl Opt Astron Observ, Tucson, AZ 85726 USA. European Space Agcy, European Space Res & Technol Ctr, Div Astrophys, Res & Sci Support Dept, NL-2200 AG Noordwijk, Netherlands. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Jeffers, SV (reprint author), Univ St Andrews, Sch Phys & Astron, N Haugh, St Andrews KY16 9SS, Fife, Scotland. EM svj1@st-and.ac.uk OI Cameron, Andrew/0000-0002-8863-7828 NR 25 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 MAR 1 PY 2005 VL 621 IS 1 BP 425 EP 431 DI 10.1086/426583 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 903DR UT WOS:000227406200039 ER PT J AU D'Alessio, P Hartmann, L Calvet, N Franco-Hernandez, R Forrest, WJ Sargent, B Furlan, E Uchida, K Green, JD Watson, DM Chen, CH Kemper, F Sloan, GC Najita, J AF D'Alessio, P Hartmann, L Calvet, N Franco-Hernandez, R Forrest, WJ Sargent, B Furlan, E Uchida, K Green, JD Watson, DM Chen, CH Kemper, F Sloan, GC Najita, J TI The truncated disk of CoKu Tau/4 SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; infrared : stars; planetary systems : formation; planetary systems : protoplanetary disks; stars : pre-main-sequence ID T-TAURI STARS; AURIGA MOLECULAR CLOUD; INTERSTELLAR SILICATE MINERALOGY; MAIN-SEQUENCE EVOLUTION; ACCRETION DISKS; YOUNG OBJECTS; CIRCUMSTELLAR DISKS; HYDRAE ASSOCIATION; OPTICAL-PROPERTIES; MASS STARS AB We present a model of a dusty disk with an inner hole that accounts for the Spitzer Space Telescope Infrared Spectrograph observations of the low-mass pre-main-sequence star CoKu Tau/4. We have modeled the mid-infrared spectrum ( between 8 and 25 mum) as arising from the inner wall of a disk. Our model disk has an evacuated inner zone of radius similar to 10 AU, with a dusty inner "wall'' of half- height similar to 2 AU that is illuminated at normal incidence by the central star. The radiative equilibrium temperature decreases from the inner disk edge outward through the optically thick disk; this temperature gradient is responsible for the emission of the silicate bands at 10 and 20 mum. The observed spectrum is consistent with being produced by Fe-Mg amorphous glassy olivine and/or pyroxene, with no evidence of a crystalline component. The mid-infrared spectrum of CoKu Tau/4 is reminiscent of that of the much older star TW Hya, where it has been suggested that the significant clearing of its inner disk is due to planet formation. However, no inner disk remains in CoKu Tau/4, consistent with the star being a weak-emission (nonaccreting) T Tauri star. The relative youth of CoKu Tau/4 ( similar to 1 Myr) may indicate much more rapid planet formation than typically assumed. C1 Ctr Radioastron & Astrofis, Morelia 58089, Michoacan, Mexico. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. Natl Opt Astron Observ, Tucson, AZ 85719 USA. RP D'Alessio, P (reprint author), Ctr Radioastron & Astrofis, Apdo Postal 72-3 Xangari, Morelia 58089, Michoacan, Mexico. EM p.dalessio@astrosmo.unam.mx RI Kemper, Francisca/D-8688-2011; OI Kemper, Francisca/0000-0003-2743-8240; Furlan, Elise/0000-0001-9800-6248 NR 55 TC 165 Z9 165 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 MAR 1 PY 2005 VL 621 IS 1 BP 461 EP 472 DI 10.1086/427490 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 903DR UT WOS:000227406200042 ER PT J AU Mackay, DH van Ballegooijen, AA AF Mackay, DH van Ballegooijen, AA TI New results in modeling the hemispheric pattern of solar filaments SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun : filaments; Sun : magnetic fields; Sun : prominences ID MAGNETIC-FIELDS; QUIESCENT PROMINENCES; CHIRALITY; CHANNELS; SUN AB New results in modeling the hemispheric pattern of solar filaments through magnetic flux transport and magnetofrictional simulations are presented. The simulations consider for the first time what type of chirality forms along the polarity inversion line lying in between two magnetic bipoles as they interact. Such interactions are important for filament formation, as observations by F. Tang show that the majority of filaments form in between bipolar regions rather than within a single magnetic bipole. The simulations also include additional physics of coronal diffusion and a radial outflow velocity at the source surface, which was not included in previous studies. The results clearly demonstrate for the first time not only the origin of the dominant hemispheric pattern but also why exceptions to it may occur. The dominant hemispheric pattern may be attributed to the dominant range of bipole tilt angles and helicities in each hemisphere. Exceptions to the hemispheric pattern are found to only occur in cases of no initial helicity or for helicity of the minority type in each hemisphere when large positive bipole tilt angles (alpha > 20degrees) are used. As the simulations show a clear dependence of the hemispheric pattern and its exceptions on observational quantities, this may be used to check the validity of the results. Future programs to consider this are put forward. C1 Univ St Andrews, Sch Math & Stat, St Andrews KY16 9SS, Fife, Scotland. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Mackay, DH (reprint author), Univ St Andrews, Sch Math & Stat, St Andrews KY16 9SS, Fife, Scotland. EM duncan@mcs.st-and.ac.uk; vanballe@cfa.harvard.edu OI van Ballegooijen, Adriaan/0000-0002-5622-3540 NR 17 TC 52 Z9 53 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 2005 VL 621 IS 1 BP L77 EP L80 DI 10.1086/428904 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 903DT UT WOS:000227406400020 ER PT J AU Torres, DF Dame, TM Digel, SW AF Torres, DF Dame, TM Digel, SW TI High-latitude molecular clouds as gamma-ray sources for the Gamma-Ray Large Area Space Telescope SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic rays; gamma rays : observations; gamma rays : theory; ISM : clouds ID HIGH GALACTIC LATITUDES; CO SURVEY; EGRET SOURCES; RADIO GALAXY; MILKY-WAY; GAS; EMISSION; ASSOCIATION; VARIABILITY; HEMISPHERE AB For about two decades, a population of relatively small and nearby molecular clouds has been known to exist at high Galactic latitudes. Lying more than 10degrees from the Galactic plane, these clouds have typical distances of similar to150 pc, angular sizes of similar to1degrees, and masses of order tens of solar masses. These objects are passive sources of high-energy gamma-rays through cosmic-ray-gas interactions. Using a new wide-angle CO survey of the northern sky, we show that typical high-latitude clouds are not bright enough in gamma-rays to have been detected by EGRET but that of order 100 of them will be detectable by the Large Area Telescope on the Gamma-Ray Large Area Space Telescope. Thus, we predict a new steady population of gamma-ray sources at high Galactic latitudes, perhaps the most numerous after active galactic nuclei. C1 Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Stanford Linear Accelerator Ctr, Menlo Pk, CA 94025 USA. RP Torres, DF (reprint author), Lawrence Livermore Natl Lab, 7000 East Ave,L-413, Livermore, CA 94550 USA. EM dtorres@igpp.ucllnl.org; tdame@cfa.harvard.edu; digel@slac.stanford.edu RI Torres, Diego/O-9422-2016 OI Torres, Diego/0000-0002-1522-9065 NR 43 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 MAR 1 PY 2005 VL 621 IS 1 BP L29 EP L32 DI 10.1086/428903 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 903DT UT WOS:000227406400008 ER PT J AU Toth, E Duffy, JE AF Toth, E Duffy, JE TI Coordinated group response to nest intruders in social shrimp SO BIOLOGY LETTERS LA English DT Article DE communication; defence; shrimp; social evolution; Synalpheus ID SYNALPHEUS; EUSOCIALITY AB A key characteristic of highly social animals is collective group response to important stimuli such as invasion by enemies. The marine societies of social snapping shrimp share many convergences with terrestrial eusocial animals, including aggressive reaction to strangers, but no group actions have yet been observed in shrimp. Here we describe 'coordinated snapping', during which a sentinel shrimp reacts to danger by recruiting other colony members to snap in concert for several to tens of seconds. This distinctive behaviour is a specific response to intrusion by strange shrimp into the colony's sponge and is highly successful at repelling these intruders. Although coordinated snapping apparently functions analogously to alarm responses in other social animals, colony members in social shrimp do not rush to the site of the attack. Coordinated snapping appears instead to be a warning signal to would-be intruders that the sponge is occupied by a cooperative colony ready to defend it. This is the first evidence for coordinated communication in social shrimp and represents yet another remarkable convergence between social shrimp, insects and vertebrates. C1 Coll William & Mary, Sch Marine Sci, Virginia Inst Marine Sci, Gloucester Point, VA 23062 USA. RP Toth, E (reprint author), Smithsonian Trop Res Inst, Unit 0948,APO AA 34002-0948, Miami, FL 34002 USA. EM tothev@si.edu NR 16 TC 25 Z9 25 U1 5 U2 23 PU ROYAL SOCIETY PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 1744-9561 J9 BIOL LETT-UK JI Biol. Lett. PD MAR PY 2005 VL 1 IS 1 BP 49 EP 52 DI 10.1098/rsbl.2004.0237 PG 4 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 968BF UT WOS:000232135300013 PM 17148125 ER PT J AU Laurance, SGW Gomez, MS AF Laurance, SGW Gomez, MS TI Clearing width and movements of understory rainforest birds SO BIOTROPICA LA English DT Article DE Amazon birds; bird movements; bird translocations; rainforest fragmentation; roads; understory birds ID INSECTIVOROUS BIRDS; CENTRAL AMAZONIA; FRAGMENTS; EXTINCTION; COMMUNITY; DIVERSITY; RESPONSES; EDGES AB We assessed the capacity of three species of disturbance-sensitive understory birds to traverse a highway (50-75 in width) and large farm clearing (250 m width), by radio-tracking translocated individuals in central Amazonia, Brazil. Most individuals translocated across the highway (eight of nine birds) or moved within continuous forest (five of seven birds) returned to their home ranges, whereas none of five birds moved across the large clearing returned. Our results suggest that large clearings (>250 in width) can significantly reduce the movements of some understory rainforest birds. C1 Smithsonian Trop Res Inst, Balboa, Panama. Univ Cambridge, Dept Physiol, Cambridge CB2 3EA, England. RP Laurance, SGW (reprint author), Smithsonian Trop Res Inst, Apdo 2072, Balboa, Panama. RI Laurance, Susan/G-6021-2011 OI Laurance, Susan/0000-0002-2831-2933 NR 21 TC 35 Z9 35 U1 1 U2 23 PU ASSOC TROPICAL BIOLOGY INC PI LAWRENCE PA 810 EAST 10TH ST, LAWRENCE, KS 66044 USA SN 0006-3606 J9 BIOTROPICA JI Biotropica PD MAR PY 2005 VL 37 IS 1 BP 149 EP 152 PG 4 WC Ecology SC Environmental Sciences & Ecology GA 903HS UT WOS:000227417200019 ER PT J AU Eames, JC Hla, H Leimgruber, P Kelly, DS Aung, SM Moses, S Tin, USN AF Eames, JC Hla, H Leimgruber, P Kelly, DS Aung, SM Moses, S Tin, USN TI The rediscovery of Gurney's Pitta Pitta gurneyi in Myanmar and an estimate of its population size based on remaining forest cover SO BIRD CONSERVATION INTERNATIONAL LA English DT Article AB A preliminary survey for Gurney's Pitta Pitta gurneyi was undertaken at five sites within the species' historical range in the Tanintharyi (Tenasserim) Division of Myanmar from 14 to 24 May 2003. During the surveys, Gurney's Pittas were heard and/or observed at four sites with a maximum Of 10-12 pairs recorded at one site. Birds were encountered in logged primary and secondary forest below 100 m on flat ground, sometimes less than 10 m from forest edge. All encounters were within 2 kin of the main trans-Tanintharyi highway. Landsat satellite imagery was used to map remaining lowland forests and Gurney's Pitta habitat ill the Tanintharyi Division. Our analysis demonstrated that Only 4,705 km(2) of lowland forest remain with about 3,496 km(2) in flat areas with slopes < 10&DEG;. On the basis of previously reported population densities, these habitats My Support a population Of 5,152-8,586 pairs. Much of the remaining habitat is restricted to small and fragmented patches < 1 km(2), in area. The five largest patches have a total area Of 1,431 km(2) and range in size from 137 to 467 km(2). This survey demonstrated that Gurney's Pitta still occurs within its historical range in Myanmar, although probably not at any of the historical collecting localities visited. The global population of Gurney's Pitta is at least 100% greater than the latest published estimate. This Survey has also shown that the Gurney's Pitta population in southern Taninthiryi Division is under pressure from forest conversion to oil palm. Contrary to the Situation in neighbouring Thailand, sufficient forest remains to establish landscape level protected areas covering a broad ecological continuum. Securing populations of Gurney's Pitta within either expanded or entirely new protected areas must be the best chance for the species and the Sundaic flora and fauna of which it is part. C1 Birdlife Int Indochina, Hanoi, Vietnam. Wildbird Adventrure Travels & Tours, Yangon, Myanmar. Smithsonian Inst, Conservat & Res Ctr, Front Royal, VA 22630 USA. RP Eames, JC (reprint author), Birdlife Int Indochina, 4 Lane 209,Doi Can St, Hanoi, Vietnam. EM Eames@birdlife.netnam.vn; wildbirdtt@mptmail.net.mn; leimgruberp@crc.si.edu; kellyd@crc.si.edu RI Leimgruber, Peter/O-1304-2015 OI Leimgruber, Peter/0000-0002-3682-0153 NR 19 TC 11 Z9 11 U1 1 U2 6 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 40 WEST 20TH ST, NEW YORK, NY 10011-4211 USA SN 0959-2709 J9 BIRD CONSERV INT JI Bird Conserv. Int. PD MAR PY 2005 VL 15 IS 1 BP 3 EP 26 DI 10.1017/S095927090500002X PG 24 WC Ornithology SC Zoology GA 924GQ UT WOS:000228967400001 ER PT J AU van der Linden, FR AF van der Linden, FR TI Inside the iron works: How Grumman's glory days faded. SO BUSINESS HISTORY REVIEW LA English DT Book Review C1 Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA. RP van der Linden, FR (reprint author), Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA. NR 1 TC 1 Z9 1 U1 0 U2 0 PU HARVARD BUSINESS SCHOOL PI BOSTON PA BUSINESS HISTORY REVIEW, 60 HARVARD WAY, BOSTON, MA 02163 USA SN 0007-6805 J9 BUS HIST REV JI Bus. Hist. Rev. PD SPR PY 2005 VL 79 IS 1 BP 156 EP 159 PG 4 WC Business; History Of Social Sciences SC Business & Economics; Social Sciences - Other Topics GA 936JB UT WOS:000229850200022 ER PT J AU Eberhard, WG AF Eberhard, WG TI Threading a needle with reinforced thread: intromission in Ceratitis capitata (Diptera, Tephritidae) SO CANADIAN ENTOMOLOGIST LA English DT Article ID STORAGE AB The intromission of the male's long, flexible, threadlike phallus into the female's similarly long, thin, S-shaped vagina in tephritid flies is mechanically challenging. The male of the Mediterranean fruit fly, Ceratitis capitata (Wiedemann, 1824), folds the basal portion of his phallus back on itself, inserts the folded portion into the female, and then gradually unfolds his phallus inside her vagina. The site of the fold in the phallus gradually moves distally, deeper into the female, dragging the distal portion of the phallus into her vagina. At the same time, the male pulls the tip of the female's ovipositor distally with his surstyli, straightening her vagina. The male uses his phallapodeme and asymmetrical syntergosternite to periodically clamp and release portions of his phallus that have not yet entered the female. Once the entire distal portion of the male's phallus is inside the female, he unfolds it and then moves its distal tip even deeper, reaching the inner end of her copulatory bursa. Straightening movements of the phallus due to increases in fluid pressure probably supply at least part of the force that drives the phallus into the female. C1 Univ Costa Rica, Escuela Biol, Smithsonian Trop Res Inst, San Jose, Costa Rica. RP Eberhard, WG (reprint author), Univ Costa Rica, Escuela Biol, Smithsonian Trop Res Inst, Ciudad Univ, San Jose, Costa Rica. EM archisepsis@biologia.ucr.ac.cr NR 10 TC 10 Z9 10 U1 0 U2 0 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 MAR-APR PY 2005 VL 137 IS 2 BP 174 EP 181 PG 8 WC Entomology SC Entomology GA 923VU UT WOS:000228938300007 ER PT J AU Andrefouet, S Guzman, HM AF Andrefouet, S Guzman, HM TI Coral reef distribution, status and geomorphology-biodiversity relationship in Kuna Yala (San Blas) archipelago, Caribbean Panama SO CORAL REEFS LA English DT Article DE Landsat; remote sensing; geomorphology; mapping; San Blas; coral reef diversity ID SPECIES RICHNESS; SATELLITE DATA; DIVERSITY; CONSERVATION; CLASSIFICATION; AUSTRALIA; SCALE AB Most of the knowledge of the reef geomorphology and benthic communities of Kuna Yala coral reefs (Caribbean Panama) comes from the western side of the archipelago, a few tens of kilometers around Punta San Blas (Porvenir). To bridge the gap between Porvenir and the Colombia-Panama border, we investigated with Landsat images the extent and geomorphological diversity of the entire Kuna Yala to provide geomorphologic maps of the archipelago in 12 classes. In addition to remote sensing data, in situ survey conducted in May-June 2001 provided a Kuna Yala-wide first synoptic vision of reef status, in terms of benthic diversity (number of species of coral, octocorals, and sponges) and reef health (coral versus algal cover). For a total reef system estimated to cover 638 km(2) along 480 km of coastline, 195 km(2) include coral dominated areas and only 35 km(2) can be considered covered by corals. A total of 69 scleractinian coral, 38 octocoral, and 82 sponge species were recorded on the outer slopes of reef formations, with a slightly higher diversity in the area presenting the most abundant and diverse reef formations (western Kuna Yala). Attempts to relate benthic diversity and geomorphological diversity provided only weak relationships regardless of the taxa, and suggest that habitat heterogeneity within geomorphological areas explain better the patterns of coral diversity. This study confirms the potential of combined remote sensing and in situ surveys for regional scale assessment, and we suggest that similar approaches should be generalized for reef mapping and assessment for other reef sites. C1 Smithsonian Trop Res Inst, Unit 0948, Miami, FL 34002 USA. Univ S Florida, Coll Marine Sci, Inst Marine Remote Sensing, St Petersburg, FL 33701 USA. RP Andrefouet, S (reprint author), UR Coreus Inst Rech Dev, BP A5, Noumea 98848, New Caledonia. EM serge@seas.marine.usf.edu; guzmanh@naos.si.edu NR 44 TC 43 Z9 45 U1 3 U2 27 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013 USA SN 0722-4028 J9 CORAL REEFS JI Coral Reefs PD MAR PY 2005 VL 24 IS 1 BP 31 EP 42 DI 10.1007/s00338-004-0444-4 PG 12 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 907UB UT WOS:000227742400006 ER PT J AU Lessios, HA AF Lessios, HA TI Diadema antillarum populations in Panama twenty years following mass mortality SO CORAL REEFS LA English DT Article DE mass mortality; population monitoring; population recovery; long-term data; Caribbean; San Blas Archipelago coral reefs ID SEA-URCHIN DIADEMA; REEF ALGAL COMMUNITIES; CORAL-REEF; MACROALGAL COVER; FLORIDA-KEYS; DYNAMICS; ECHINODERMATA; ECHINOIDEA; HERBIVORY; RECOVERY C1 Smithsonian Trop Res Inst, Balboa, Panama. RP Lessios, HA (reprint author), Smithsonian Trop Res Inst, Box 2072, Balboa, Panama. EM Lessiosh@stri.org NR 34 TC 52 Z9 61 U1 3 U2 27 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013 USA SN 0722-4028 J9 CORAL REEFS JI Coral Reefs PD MAR PY 2005 VL 24 IS 1 BP 125 EP 127 DI 10.1007/s00338-004-0443-5 PG 3 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 907UB UT WOS:000227742400022 ER PT J AU Ritson-Williams, R Becerro, MA Paul, VJ AF Ritson-Williams, R Becerro, MA Paul, VJ TI Spawning of the giant barrel sponge Xestospongia muta in Belize SO CORAL REEFS LA English DT Editorial Material ID PORIFERA C1 CSIC, Ctr Adv Studies, CEAB, Girona 17300, Spain. RP Ritson-Williams, R (reprint author), Smithsonian Marine Stn Ft Pierce, 701 Seaway Dr, Ft Pierce, FL 34949 USA. EM williams@sms.si.edu RI Becerro, Mikel/A-5325-2008; OI Becerro, Mikel/0000-0002-6047-350X NR 2 TC 6 Z9 6 U1 0 U2 8 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013 USA SN 0722-4028 J9 CORAL REEFS JI Coral Reefs PD MAR PY 2005 VL 24 IS 1 BP 160 EP 160 DI 10.1007/s00338-004-0460-4 PG 1 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 907UB UT WOS:000227742400030 ER PT J AU Rader, R Reed, S AF Rader, R Reed, S TI A method of tagging Aratus pisonii (H. Milne Edwards, 1837) (Decapoda, Brachyura, Grapsidae) crabs for population and behavioural studies SO CRUSTACEANA LA English DT Editorial Material ID LIFE-HISTORY; GROWTH C1 Smithsonian Marine Stn, Ft Pierce, FL USA. RP Rader, R (reprint author), POB 258, Palm Cove, Qld 4879, Australia. EM Romina.Rader@jcu.edu.au RI Rader, Romina/A-1054-2012 NR 11 TC 0 Z9 0 U1 0 U2 2 PU BRILL ACADEMIC PUBLISHERS PI LEIDEN PA PLANTIJNSTRAAT 2, P O BOX 9000, 2300 PA LEIDEN, NETHERLANDS SN 0011-216X J9 CRUSTACEANA JI Crustaceana PD MAR PY 2005 VL 78 BP 361 EP 365 DI 10.1163/1568540054286538 PN 3 PG 5 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 946FX UT WOS:000230558900010 ER PT J AU Heaney, PJ Vicenzi, EP De, S AF Heaney, PJ Vicenzi, EP De, S TI Strange diamonds: The mysterious origins of carbonado and framesite SO ELEMENTS LA English DT Article DE carbonado; framesite; polycrystalline diamond ID NATURAL POLYCRYSTALLINE DIAMOND; EARTH ELEMENT PATTERNS; IMPACT ORIGIN; ISOTOPIC COMPOSITION; MAGNETIC-PROPERTIES; CRUSTAL ORIGIN; CRYSTALS; RIES AB Polycrystalline aggregates of diamond called carbonado and framesite have excited the attention of scientists because their crystallization histories are thought to depart markedly from established modes of diamond genesis. In contrast to kimberlitic diamonds, the geochemical signatures of carbonados are systematically crustal. Since the apparent age of carbonados is Archean (similar to 3.2 Ga), a number of exotic formation theories have been invoked, including metamorphism of the earliest subducted lithosphere, radioactive transformation of mantle hydrocarbon, and meteorite impact on concentrated biomass. Unlike carbonados, framesites are known to originate in the mantle. They appear to have crystallized very rapidly, shortly before the eruption of the kimberlites that brought them to Earth's surface, suggesting that old cratonic materials can be remobilized after long-term storage in the lithosphere. C1 Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. Smithsonian Inst, Dept Mineral Sci, Washington, DC 20013 USA. RP Heaney, PJ (reprint author), Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. EM heaney@geosc.psu.edu NR 50 TC 35 Z9 36 U1 3 U2 16 PU MINERALOGICAL SOC AMER PI WASHINGTON PA 1015 EIGHTEENTH ST, NW SUITE 601, WASHINGTON, DC 20036 USA SN 1811-5209 J9 ELEMENTS JI Elements PD MAR PY 2005 VL 1 IS 2 BP 85 EP 89 DI 10.2113/gselements.1.2.85 PG 5 WC Geochemistry & Geophysics; Mineralogy SC Geochemistry & Geophysics; Mineralogy GA 009AK UT WOS:000235083300005 ER PT J AU Gates, MW Schauff, ME AF Gates, MW Schauff, ME TI The first report of Oncastichus goughi (Hymenoptera : Eulophidae): An introduced pest of waxflower (Myrtaceae : Chamelaucium uncinatum) from South America SO ENTOMOLOGICAL NEWS LA English DT Editorial Material C1 Smithsonian Inst, Syst Entomol Lab, USDA ARS, PSI,Natl Museum Nat Hist, Washington, DC 20013 USA. RP Gates, MW (reprint author), Smithsonian Inst, Syst Entomol Lab, USDA ARS, PSI,Natl Museum Nat Hist, MRC-168, Washington, DC 20013 USA. EM mgates@sel.barc.usda.gov; mschauff@sel.barc.usda.gov NR 10 TC 4 Z9 4 U1 0 U2 0 PU AMER ENTOMOL SOC PI PHILADELPHIA PA 1900 BENJ FRANKLIN PARKWAY, PHILADELPHIA, PA 19103-1195 USA SN 0013-872X J9 ENTOMOL NEWS JI Entomol. News PD MAR-APR PY 2005 VL 116 IS 2 BP 115 EP 116 PG 2 WC Entomology SC Entomology GA 919VG UT WOS:000228645100013 ER PT J AU Kirby, MX Miller, HM AF Kirby, MX Miller, HM TI Response of a benthic suspension feeder (Crassostrea virginica Gmelin) to three centuries of anthropogenic eutrophication in Chesapeake Bay SO ESTUARINE COASTAL AND SHELF SCIENCE LA English DT Article DE eutrophication; paleoproductivity; growth rate; bivalve mollusc; oyster; Crassostrea virginica; Chesapeake Bay ID STABLE-ISOTOPE SCLEROCHRONOLOGY; WADDEN SEA; TROPICAL AMERICA; OYSTER MORTALITY; PACIFIC OYSTER; GROWTH; TEMPERATURE; ANOXIA; PHYTOPLANKTON; BIOMASS AB Biogenic reefs built by oysters and other suspension feeders are vital components of estuarine ecosystems. By consuming phytoplankton, suspension feeders act to suppress accumulation of organic matter in the water column. Nutrient loading increases the rate of primary production, thereby causing eutrophication. As suspension feeders consume more organic matter from increasing abundance of phytoplankton, their rate of growth should also increase if they are food limited. We show here that the eastern oyster, Crassostrea virginica (Gmelin), from St. Mary's and Patuxent rivers, Chesapeake Bay, grew faster during anthropogenic eutrophication relative to C. virginica before eutrophication. Growth of shell height, shell thickness and adductor muscle increased after eutrophication began in the late 18th century. After 1860, growth decreased, perhaps reflecting the negative effects of hypoxia, harmful algal blooms, disease and fishing on oyster growth. These results are consistent with the view that an increasing supply of phytoplankton resulting from eutrophication enhanced growth of C. virginica between 1760 and 1860, before oyster reefs were degraded by destructive fishing practices between 1870 and 1930. Alternative factors, such as changes in water temperature, salinity, and fishing are less likely to be responsible for this pattern. These results have implications for restoration of oyster reefs in order to mitigate the effects of eutrophication in estuaries, as well as the paleoecological relationship between suspension feeders and paleoproductivity. (C) 2004 Elsevier Ltd. All rights reserved. C1 Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA. Hist St Marys City, St Marys City, MD 20686 USA. RP Kirby, MX (reprint author), Smithsonian Trop Res Inst, Ctr Trop Paleoecol & Archaeol, Box 2072, Balboa, Panama. EM kirbym@si.edu NR 74 TC 35 Z9 36 U1 3 U2 28 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0272-7714 J9 ESTUAR COAST SHELF S JI Estuar. Coast. Shelf Sci. PD MAR PY 2005 VL 62 IS 4 BP 679 EP 689 DI 10.1016/j.ecss.2004.10.004 PG 11 WC Marine & Freshwater Biology; Oceanography SC Marine & Freshwater Biology; Oceanography GA 902AC UT WOS:000227322500010 ER PT J AU McMullen, A AF McMullen, A TI A strange likeness: Becoming red and white in eighteenth-century North America SO ETHNOHISTORY LA English DT Book Review C1 Smithsonian Inst, Natl Museum Amer Indian, Washington, DC 20560 USA. RP McMullen, A (reprint author), Smithsonian Inst, Natl Museum Amer Indian, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU DUKE UNIV PRESS PI DURHAM PA 905 W MAIN ST, STE 18-B, DURHAM, NC 27701 USA SN 0014-1801 J9 ETHNOHISTORY JI Ethnohistory PD SPR PY 2005 VL 52 IS 2 BP 491 EP 492 DI 10.1215/00141801-52-2-491 PG 2 WC Anthropology; History SC Anthropology; History GA 920HN UT WOS:000228680100014 ER PT J AU Ribblett, SG Palmer, MA Coats, DW AF Ribblett, SG Palmer, MA Coats, DW TI The importance of bacterivorous protists in the decomposition of stream leaf litter SO FRESHWATER BIOLOGY LA English DT Article DE bacteria; leaf decomposition; litter; protist; stream ID FRESH-WATER; CHEMICAL-COMPOSITION; FUNCTIONAL-GROUPS; PIEDMONT STREAM; WOODLAND STREAM; FOOD WEBS; PROTOZOA; BREAKDOWN; DYNAMICS; LEAVES AB 1. Allochthonous organic matter, in the form of senesced leaves, is a major source of carbon supporting detrital food webs. While studies have documented the role of bacteria and fungi in the decomposition of leaf litter, little information is available regarding the role of protists in the decomposition process. 2. We tested the hypothesis that the presence of stream-dwelling bacterivorous protists leads to an increased rate of leaf decomposition through grazing pressure on bacteria. We isolated live protists from decomposing leaves collected in a stream in Northern Virginia, U.S.A. (Goose Creek) and established laboratory cultures of common bacterivorous protists. 3. Recently senesced leaves from the field were used in laboratory microcosm experiments to determine if the rate of litter decomposition differed between four treatments: bacteria only, bacteria + flagellates, bacteria + flagellates + ciliates, autoclaved stream water (control). We determined the dry weight of leaf remaining, bacterial abundance, flagellate abundance and ciliate abundance for each replicate on days 0, 7, 14, 30, 60 and 120. 4. The rate of leaf decomposition was significantly higher in treatments with protists than without and bacterial abundance declined in protist treatments compared with bacteria only treatment. Weight loss in the presence of flagellates was three to four times higher when protists were present compared with treatments with bacteria alone. These results provide experimental evidence that protists could play a significant role in the detrital processes of streams. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Univ Maryland, Dept Entomol, College Pk, MD 20742 USA. RP Ribblett, SG (reprint author), Smithsonian Environm Res Ctr, POB 28,647 Contees Wharf Rd, Edgewater, MD 21037 USA. EM ribbletts@si.edu NR 57 TC 38 Z9 38 U1 5 U2 23 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0046-5070 J9 FRESHWATER BIOL JI Freshw. Biol. PD MAR PY 2005 VL 50 IS 3 BP 516 EP 526 DI 10.1111/j.1365-2427.2005.01338.x PG 11 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 896VM UT WOS:000226962200011 ER PT J AU Rasse, DP Peresta, G Drake, BG AF Rasse, DP Peresta, G Drake, BG TI Seventeen years of elevated CO2 exposure in a Chesapeake Bay Wetland: sustained but contrasting responses of plant growth and CO2 uptake SO GLOBAL CHANGE BIOLOGY LA English DT Article DE acclimation; CO2 response; NEE; OTC; wetlands ID CARBON-DIOXIDE CONCENTRATION; SCRUB-OAK ECOSYSTEM; OPEN-TOP CHAMBER; ATMOSPHERIC CO2; LONG-TERM; SCIRPUS-OLNEYI; ENRICHMENT FACE; CLIMATE-CHANGE; WATER AVAILABILITY; MODEL ANALYSIS AB Increased atmospheric CO2 concentration (Ca) produces a short-term stimulation of photosynthesis and plant growth across terrestrial ecosystems. However, the long-term response remains uncertain and is thought to depend on environmental constraints. In the longest experiment on natural ecosystem response to elevated Ca, we measured the shoot-density, biomass and net CO2 exchange (NEE) responses to elevated Ca from 1987 to 2003 in a Scirpus olneyi wetland sedge community of the Chesapeake Bay, MD, USA. Measurements were conducted in five replicated open-top chambers per CO2 treatment (ambient and elevated). In addition, unchambered control plots were monitored for shoot density. Responses of daytime NEE, Scirpus plant biomass and shoot density to elevated Ca were positive for any single year of the 17-year period of study. Daytime NEE stimulation by elevated Ca rapidly dropped from 80% at the onset of the experiment to a long-term stimulation average of about 35%. Shoot-density stimulation by elevated Ca increased linearly with duration of exposure (r(2)=0.89), exceeding 120% after 17 years. Although of lesser magnitude, the shoot biomass response to elevated Ca was similar to that of the shoot density. Daytime NEE response to elevated Ca was not explained by the duration of exposure, but negatively correlated with salinity of the marsh, indicating that this elevated-Ca response was decreased by water-related stress. By contrast, circumstantial evidence suggested that salinity stress increased the stimulation of shoot density by elevated Ca, which highlights the complexity of the interaction between water-related stresses and plant community responses to elevated Ca. Notwithstanding the effects of salinity stress, we believe that the most important finding of the present research is that a species response to elevated Ca can continually increase when this species is under stress and declining in its natural environment. This is particularly important because climate changes associated with elevated Ca are likely to increase environmental stresses on numerous species and modify their present distribution. Our results point to an increased resilience to change under elevated Ca when plants are exposed to adverse environmental conditions. C1 Ctr INRA Versailles Grignon, Lab Biogeochim Milieux Continentaux, F-78850 Thiverval Grignon, France. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Rasse, DP (reprint author), Ctr INRA Versailles Grignon, Lab Biogeochim Milieux Continentaux, Bat IFR EGER, F-78850 Thiverval Grignon, France. EM daniel.rasse@grignon.inra.fr NR 53 TC 65 Z9 70 U1 0 U2 31 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 1354-1013 J9 GLOBAL CHANGE BIOL JI Glob. Change Biol. PD MAR PY 2005 VL 11 IS 3 BP 369 EP 377 DI 10.1111/j.1365-2486.2005.00913.x PG 9 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 909CQ UT WOS:000227837000001 ER PT J AU Robinson, SA Turnbull, JD Lovelock, CE AF Robinson, SA Turnbull, JD Lovelock, CE TI Impact of changes in natural ultraviolet radiation on pigment composition, physiological and morphological characteristics of the Antarctic moss, Grimmia antarctici SO GLOBAL CHANGE BIOLOGY LA English DT Article DE anthocyanins; beta-carotene; chlorophyll; chlorophyll fluorescence; leaf morphology; surface reflectance; UV-B-absorbing pigments; xanthophyll cycle pigments ID UV-B RADIATION; TIERRA-DEL-FUEGO; STRATOSPHERIC OZONE DEPLETION; ALPINE LIFE ZONE; SUB-ARCTIC BOG; DNA-DAMAGE; CONTINENTAL ANTARCTICA; TERRESTRIAL ECOSYSTEMS; SOUTHERN ARGENTINA; OPTICAL-PROPERTIES AB The impact of ambient ultraviolet (UV)-B radiation on the endemic bryophyte, Grimmia antarctici, was studied over 14 months in East Antarctica. Over recent decades, Antarctic plants have been exposed to the largest relative increase in UV-B exposure as a result of ozone depletion. We investigated the effect of reduced UV and visible radiation on the pigment concentrations, surface reflectance and physiological and morphological parameters of this moss. Plexiglass screens were used to provide both reduced UV levels (77%) and a 50% decrease in total radiation. The screen combinations were used to separate UV photoprotective from visible photoprotective strategies, because these bryophytes are growing in relatively high light environments compared with many mosses. G. antarctici was affected negatively by ambient levels of UV radiation. Chlorophyll content was significantly lower in plants grown under near-ambient UV, while the relative proportions of photoprotective carotenoids, especially beta-carotene and zeaxanthin, increased. However, no evidence for the accumulation of UV-B-absorbing pigments in response to UV radiation was observed. Although photosynthetic rates were not affected, there was evidence of UV effects on morphology. Plants that were shaded showed fewer treatment responses and these were similar to the natural variation observed between moss growing on exposed microtopographical ridges and in more sheltered valleys within the turf. Given that other Antarctic bryophytes possess UV-B-absorbing pigments which should offer better protection under ambient UV-B radiation, these findings suggest that G. antarctici may be disadvantaged in some settings under a climate with continuing high levels of springtime UV-B radiation. C1 Univ Wollongong, Inst Conservat Biol, Wollongong, NSW 2522, Australia. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Robinson, SA (reprint author), Univ Wollongong, Inst Conservat Biol, Northfields Ave, Wollongong, NSW 2522, Australia. EM sharonr@uow.edu.au RI Robinson, Sharon/B-2683-2008; Lovelock, Catherine/G-7370-2012; OI Robinson, Sharon/0000-0002-7130-9617; Lovelock, Catherine/0000-0002-2219-6855; Turnbull, Johanna/0000-0002-4214-1675 NR 61 TC 40 Z9 50 U1 2 U2 20 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1354-1013 J9 GLOBAL CHANGE BIOL JI Glob. Change Biol. PD MAR PY 2005 VL 11 IS 3 BP 476 EP 489 DI 10.1111/j.1365-2486.2005.00911.x PG 14 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 909CQ UT WOS:000227837000008 ER PT J AU Gallegos, CL Bergstrom, PW AF Gallegos, CL Bergstrom, PW TI Effects of a Prorocentrum minimum bloom on light availability for and potential impacts on submersed aquatic vegetation in upper Chesapeake Bay SO HARMFUL ALGAE LA English DT Article; Proceedings Paper CT Symposium on Ecology and Physiology of Prorocentrum Minimum CY 2003 CL MD SP Maryland Dept Nat Resouce DE Chesapeake Bay; dinollagellate bloom; light attenuation; Prorocentrum minimum; submersed aquatic vegetation ID EELGRASS ZOSTERA-MARINA; ABSORPTION-COEFFICIENTS; NATURAL PHYTOPLANKTON; SPECTRAL ABSORPTION; OPTICAL-PROPERTIES; WATERS; DINOFLAGELLATE; VARIABILITY; SCATTERING; PARTICLES AB Extraordinary spring blooms of the dinoflagellate Prorocentrum minimum have been a recurring feature of upper Chesapeake Bay for many years. Though not thought to be toxic in Chesapeake Bay, these blooms produce extraordinarily high concentrations of chlorophyll, thereby increasing light attenuation. A particularly large event occurred in the spring of 2000. Here, we assess the impact of the spring 2000 P. minimum bloom on habitat quality for submerged aquatic vegetation (SAV) in the mesohaline region of Chesapeake Bay and its tributaries. We determined the light absorption and scattering spectrum of P minimum on a per cell basis by analyzing inherent optical properties of natural samples from the Rhode River, Maryland, which were overwhelmingly dominated by P. minimum. Using these per cell properties, we constructed a model of light penetration incorporating observed cell counts of P. minimum to predict the impact of the bloom on other tributaries and main stem locations that experienced the bloom. Model estimates of diffuse attenuation coefficients agreed well with the limited measurements that were available. Impacts of the mahogany tide on diffuse attenuation coefficient ranged from negligible (10-30% increase above the seasonal median in the Patapsco and Magothy rivers), to a greater than six-fold increase (Potomac River). Attenuation coefficients in tributaries to the north and south of the bloom region either decreased or were unchanged relative to seasonal medians. Segments with SAV losses in 2000 were mostly the same as those that experienced the P minimum bloom. Segments north and south of the bloom area mostly had SAV increases in 2000. Though all of the segments that experienced a decline in SAV area after the spring 2000 bloom showed an increase in 2002, the 2000 setback interrupted what otherwise has been a slow recovery in mid-Bay SAV, demonstrating the adverse impact of P. minimum blooms on SAV populations in Chesapeake Bay. (C) 2004 Elsevier B.V. All rights reserved. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. NOAA, Chesapeake Bay Off, Annapolis, MD 21403 USA. RP Gallegos, CL (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM gallegosc@si.edu OI Gallegos, Charles/0000-0001-5112-0166 NR 43 TC 23 Z9 25 U1 0 U2 5 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 1568-9883 J9 HARMFUL ALGAE JI Harmful Algae PD MAR PY 2005 VL 4 IS 3 BP 553 EP 574 DI 10.1016/j.hal.2004.08.016 PG 22 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 902WQ UT WOS:000227387800010 ER PT J AU Torres-Carvajal, O AF Torres-Carvajal, O TI A new species of iguanian lizard (Stenocercus) from the western lowlands of southern Ecuador and northern Peru SO HERPETOLOGICA LA English DT Article DE Ecuador; iguania; new species; Peru; Stenocercus; systematics ID TROPIDURIDAE AB I describe a new species of Stenocercus from the lowlands of southwestern Ecuador and northwestern Pet-it. The new species differs from other Stenocercus by the combination of the following projecting angulate temporals absent, canthals two, ventrals smooth, posthumeral and postfemoral mite pockets shallow, dorsolateral crests absent, inscriptional ribs not articulating midventrally, throat yellow and venter lavender in males. Some evidence suggests that the new species is closely related to Stenocerrus iridescens, which occurs allopatrically in the lowlands of western Ecuador and southwestern Colombia. C1 Univ Kansas, Museum Nat Hist, Lawrence, KS 66045 USA. Univ Kansas, Biodivers Res Ctr, Lawrence, KS 66045 USA. Univ Kansas, Dept Ecol & Evolutionary Biol, Lawrence, KS 66045 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA. RP Torres-Carvajal, O (reprint author), Univ Kansas, Museum Nat Hist, Dyche Hall,1345 Jayhawk Blvd, Lawrence, KS 66045 USA. EM otorres@ku.edu NR 14 TC 10 Z9 10 U1 2 U2 2 PU HERPETOLOGISTS LEAGUE PI EMPORIA PA EMPORIA STATE UNIV, DIVISION BIOLOGICAL SCIENCES, 1200 COMMERCIAL ST, EMPORIA, KS 66801-5087 USA SN 0018-0831 EI 1938-5099 J9 HERPETOLOGICA JI Herpetologica PD MAR PY 2005 VL 61 IS 1 BP 78 EP 85 DI 10.1655/04-32.2 PG 8 WC Zoology SC Zoology GA 901PH UT WOS:000227293900010 ER EF